DARTS Astro

total 37

No.
target_name
center_ra
center_dec
center_ra_b1950
center_dec_b1950
center_ecliptic_lon
center_ecliptic_lat
center_galactic_lon
center_galactic_lat
roll_angle
observation_start_time_mjd
observation_start_time
observation_end_time_mjd
observation_end_time
observation_id
exposure
proposal_exposure
xis0_exposure
xis1_exposure
xis2_exposure
xis3_exposure
xis0_observation_mode
xis1_observation_mode
xis2_observation_mode
xis3_observation_mode
hxd_observation_mode
hxd_coarse_clock_rate_exposure
hxd_first_clock_rate_exposure
hxd_normal_clock_rate_exposure
hxd_all_clock_rate_exposure
hxd_wam_exposure
hxd_burst_num
processing_status
processing_end_time_mjd
processing_end_time
public_date_mjd
public_date
distribute_start_date_mjd
distribute_start_date
processing_version
processing_quantity
processing_software
proposal_id
proposal_abstract
proposal_category
proposal_category_code
proposal_priority
pi_name
co_pi_name
proposal_affiliated_country
proposal_cycle_count
observation_type
proposal_title
main_detector
xis_injection_flag
data_access_url
ql_access_url
ql_image_url
1 CYGNUS X-1 299.5392 35.2589 299.069624 35.122644 313.628523 54.317489 71.36219421 3.13231837 55.3254 54957.7006828704 2009-05-06 16:48:59 54958.1356365741 2009-05-07 03:15:19 404075060 19.4345 300 19.4345 19.4505 0 19.4345 2 1 0 2 1 0 0 15.2795 15.2795 37.5579 0 PROCESSED 57546.5121412037 2016-06-07 12:17:29 54922 2009-04-01 00:00:00 54976.0885300926 2009-05-25 02:07:29 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A JON MILLER SHIN YAMADA USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075060/ Quick Look
2 CYGNUS X-1 299.5373 35.2573 299.067717 35.121052 313.625096 54.316504 71.3600172 3.13281014 53.4895 54976.3582060185 2009-05-25 08:35:49 54976.8259722222 2009-05-25 19:49:24 404075090 20.9252 300 20.9252 20.9332 0 20.9252 2 1 0 2 1 0 0 16.1164 16.1164 40.412 1 PROCESSED 57546.6796296296 2016-06-07 16:18:40 54922 2009-04-01 00:00:00 54992.6651736111 2009-06-10 15:57:51 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A JON MILLER SHIN YAMADA USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075090/ Quick Look
3 CYGNUS X-1 299.5294 35.2515 299.059794 35.115286 313.611339 54.313209 71.35169447 3.13529932 46.7675 54984.481400463 2009-06-02 11:33:13 54984.9870833333 2009-06-02 23:41:24 404075110 17.4502 300 19.037 17.7782 0 17.4502 1 1 0 1 1 0 0 15.0409 15.0409 43.6879 1 PROCESSED 57547.4475462963 2016-06-08 10:44:28 54922 2009-04-01 00:00:00 54994.4091087963 2009-06-12 09:49:07 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A JON MILLER SHIN YAMADA USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075110/ Quick Look
4 CYGNUS X-1 299.6354 35.1397 299.164908 35.003038 313.686688 54.178801 71.30132058 3.00311627 241.1557 55159.514224537 2009-11-24 12:20:29 55160.1328587963 2009-11-25 03:11:19 404075180 21.7685 300 21.7685 22.4805 0 22.4725 5 2 0 3 1 0 0 11.4064 11.4064 53.4358 0 PROCESSED 57549.5783680556 2016-06-10 13:52:51 54922 2009-04-01 00:00:00 55176.294849537 2009-12-11 07:04:35 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A JON MILLER SHIN YAMADA USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075180/ Quick Look
5 CYGNUS X-1 299.5895 35.2721 299.119922 35.135631 313.702443 54.316106 71.39489928 3.10413213 91.3103 54929.2562847222 2009-04-08 06:09:03 54929.8224421296 2009-04-08 19:44:19 404075020 21.3361 300 21.3361 21.3361 0 21.3361 2 1 0 2 1 0 0 13.1258 13.1258 48.914 0 PROCESSED 57546.0782638889 2016-06-07 01:52:42 54922 2009-04-01 00:00:00 54949.4903125 2009-04-28 11:46:03 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A JON MILLER SHIN YAMADA USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075020/ Quick Look
6 A3112 49.3542 -44.4494 48.920816 -44.631605 25.154749 -59.092558 253.34888003 -56.10584592 209.0003 57003.8439467593 2014-12-12 20:15:17 57006.6182407407 2014-12-15 14:50:16 809116020 97.989 200 97.989 97.989 0 97.989 2 2 0 2 0 0 0 0 0 0 0 PROCESSED 57617.5061458333 2016-08-17 12:08:51 57387 2015-12-31 00:00:00 57017.4238425926 2014-12-26 10:10:20 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 094527 The hot X-ray emitting gas in clusters of galaxies is a very large repository of metals produced by stars and galaxies. These metals enter the intra-cluster medium (ICM) via strong galactic winds, supernovae explosions, and ram-pressure stripping. However, the details of the mechanisms that transport metals to the ICM and the origin of these metals remain still unclear. We aim to accurately measure the temperature and abundance patterns of a bright nearby galaxy cluster A3112 out to the virial radius and compare these data with metal abundance yields produced by supernovae. Our proposed observation will provide information about how these metals are created, as well as how and when the metals were transported to the ICM. EXTRAGALACTIC DIFFUSE SOURCES 8 A ESRA BULBUL USJ 9 AO9 A DETAILED STUDY OF CHEMICAL ENRICHMENT OF A3112 OUT TO THE VIRIAL RADIUS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809116020/ Quick Look
7 CYGNUS X-1 299.6277 35.1371 299.157204 35.000471 313.675062 54.178467 71.29581116 3.00713364 246.5433 55145.8193981482 2009-11-10 19:39:56 55146.4377199074 2009-11-11 10:30:19 404075160 26.0222 300 26.0222 26.0382 0 26.0265 2 1 0 2 1 0 0 18.2505 18.2505 53.416 0 PROCESSED 57549.2577199074 2016-06-10 06:11:07 54922 2009-04-01 00:00:00 55176.2027430556 2009-12-11 04:51:57 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A JON MILLER SHIN YAMADA USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075160/ Quick Look
8 VELA X (REGION A) 128.7666 -45.458 128.346603 -45.284447 153.579861 -60.62666 263.74862198 -2.99483781 337.7597 53927.7846990741 2006-07-11 18:49:58 53929.4703819444 2006-07-13 11:17:21 501107010 60.7735 60 60.7735 60.7735 60.7735 60.7735 2 2 2 2 1 0 0 54.1611 54.1611 145.6058 3 PROCESSED 57534.9641203704 2016-05-26 23:08:20 54401 2007-10-28 00:00:00 53942.4562037037 2006-07-26 10:56:56 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 014211 The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band. GALACTIC DIFFUSE EMISSION 5 B OLEG KARGALTSEV KOJI MORI USJ 1 AO1 THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501107010/ Quick Look
9 VELA X (REGION C) 127.7806 -46.2716 127.370041 -46.101802 153.218075 -61.676794 263.99736145 -4.03006469 349.189 53933.9133796296 2006-07-17 21:55:16 53934.7730787037 2006-07-18 18:33:14 501108010 29.2028 30 29.2028 29.2028 29.2028 29.2028 2 2 2 2 1 0 0 25.5929 25.5929 74.248 1 PROCESSED 57534.9868055556 2016-05-26 23:41:00 54404 2007-10-31 00:00:00 53943.4988773148 2006-07-27 11:58:23 3.0.22.43 7 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 014211 The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band. GALACTIC DIFFUSE EMISSION 5 B OLEG KARGALTSEV KOJI MORI USJ 1 AO1 THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501108010/ Quick Look
10 F05189-2524 80.2383 -25.4117 79.728122 -25.460147 76.667297 -48.403351 227.93752087 -30.32292957 290.8212 53835.6784259259 2006-04-10 16:16:56 53837.6467708333 2006-04-12 15:31:21 701097010 78.1555 80 78.1555 78.1635 78.1555 78.1555 2 2 2 2 1 0 0 51.7402 51.7402 169.9899 2 PROCESSED 57533.4937268518 2016-05-25 11:50:58 54401 2007-10-28 00:00:00 53906.8811689815 2006-06-20 21:08:53 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 014341 We wish to take advantage of the unprecedented sensitivity of Suzaku Observatory to very hard X-rays (> 10 keV) to constrain the energy source -- starburst or black-hole driven activity -- in two of the nearest and brightest ultraluminous infrared galaxies, Mrk 273 and F05189-2524. These objects are arguably the best local laboratories to study the basic physical processes involved in creating massive early type hosts on the one hand, and feeding embedded supermassive black holes on the other hand, in major galaxy mergers. The Suzaku data will be used to search for the high-energy signature of deeply buried active black holes and to look for short timescale variability, another signature of black-hole driven activity. These data will be part of S. Teng's PhD thesis at Maryland. EXTRAGALACTIC COMPACT SOURCES 7 A SYLVAIN VEILLEUX NAOHISA ANABUKI USJ 1 AO1 THE DOMINANT ENERGY SOURCE OF ULTRALUMINOUS INFRARED GALAXIES HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701097010/ Quick Look
11 SN 1978K 49.5382 -66.5402 49.387343 -66.721221 341.369857 -74.185234 283.41338803 -44.62366671 13.2585 56804.2369097222 2014-05-27 05:41:09 56806.5279398148 2014-05-29 12:40:14 709023010 107.3136 100 107.3216 107.3216 0 107.3136 2 2 0 2 0 0 0 0 0 0 0 PROCESSED 57615.1724074074 2016-08-15 04:08:16 57234 2015-07-31 00:00:00 56866.7205092593 2014-07-28 17:17:32 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 094341 SN 1978K is a remarkable Type IIn supernova that remains bright at X-ray through radio wavelengths 35 years after its explosion. Our ongoing multiwavelength observations probe the dense medium that was ejected by the progenitor star, possibly a Luminous Blue Variable. While the radio flux dropped steadily, the X-ray and UV/optical fluxes remained surprisingly constant for a decade. However, our most recent XMM observation in 2013 June reveals a significant fading compared to the 2006 Oct Suzaku observation. Here we request a 100 ksec observation to study the spectral evolution during the decay. This will serve as a pathfinder for younger Type IIn supernovae. As secondary science, we will obtain data on the ULXs X-1 and X-2, and the other luminous sources in NGC 1313. EXTRAGALACTIC COMPACT SOURCES 7 B IAN SMITH SHOGO KOBAYASHI USJ 9 AO9 STUDYING THE LATE-TIME DECAY OF SN 1978K XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709023010/ Quick Look
12 NGC 1332 51.5732 -21.333 51.017829 -21.507123 42.191625 -38.615675 212.17958034 -54.36451308 243.6482 55581.2509027778 2011-01-20 06:01:18 55584.0883333333 2011-01-23 02:07:12 805095010 101.423 100 101.423 101.423 0 101.423 2 2 0 2 1 0 0 89.9683 89.9683 245.1259 2 PROCESSED 57600.7603935185 2016-07-31 18:14:58 55965 2012-02-08 00:00:00 55599.216724537 2011-02-07 05:12:05 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 054502 Recent observations of relaxed galaxy groups have revealed ubiquitous abundance gradients. The broad peaks of Fe abundance indicate (turbulent) diffusion of metals possibly driven by AGN feedback. Exploiting the low background and good sensitivity of Suzaku XIS, we have found similar gradients in three lower mass (virial mass 5-10E12 Msun) elliptical galaxies, which has important implications for models of feedback and chemical enrichment. We propose to observe another two carefully chosen galaxies, thus starting to build a sample for determining the frequency and properties of such abundance gradients in early-type galaxies. EXTRAGALACTIC DIFFUSE SOURCES 8 C PHILIP HUMPHREY RYO NAGINO USJ 5 AO5 ABUNDANCE GRADIENTS IN EARLY-TYPE GALAXIES XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805095010/ Quick Look
13 A3112 49.3536 -44.4489 48.920211 -44.631107 25.15452 -59.09191 253.34827073 -56.10640985 209.0009 57000.6762037037 2014-12-09 16:13:44 57003.8439351852 2014-12-12 20:15:16 809116010 107.9651 200 107.9651 107.9651 0 107.9651 2 2 0 2 1 0 0 8.1487 8.1487 33.9079 1 PROCESSED 57617.53125 2016-08-17 12:45:00 57387 2015-12-31 00:00:00 57016.2346180556 2014-12-25 05:37:51 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 094527 The hot X-ray emitting gas in clusters of galaxies is a very large repository of metals produced by stars and galaxies. These metals enter the intra-cluster medium (ICM) via strong galactic winds, supernovae explosions, and ram-pressure stripping. However, the details of the mechanisms that transport metals to the ICM and the origin of these metals remain still unclear. We aim to accurately measure the temperature and abundance patterns of a bright nearby galaxy cluster A3112 out to the virial radius and compare these data with metal abundance yields produced by supernovae. Our proposed observation will provide information about how these metals are created, as well as how and when the metals were transported to the ICM. EXTRAGALACTIC DIFFUSE SOURCES 8 A ESRA BULBUL KOSUKE SATO USJ 9 AO9 A DETAILED STUDY OF CHEMICAL ENRICHMENT OF A3112 OUT TO THE VIRIAL RADIUS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809116010/ Quick Look
14 CYGNUS X-1 299.6653 35.165 299.194917 35.028212 313.740573 54.19441 71.33570459 2.99545336 212.8004 55182.0619328704 2009-12-17 01:29:11 55182.5508564815 2009-12-17 13:13:14 404075070 22.1019 300 22.1019 22.1099 0 23.664 1 1 0 1 1 0 0 3.4607 3.4607 42.236 0 PROCESSED 57549.8755671296 2016-06-10 21:00:49 54922 2009-04-01 00:00:00 55200.4490046296 2010-01-04 10:46:34 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A JON MILLER SHIN YAMADA USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075070/ Quick Look
15 CYGNUS X-1 299.6549 35.1555 299.184474 35.018756 313.721426 54.188323 71.32314713 2.99775182 222.7295 55173.647349537 2009-12-08 15:32:11 55174.1043287037 2009-12-09 02:30:14 404075200 20.0166 300 20.0166 21.7526 0 21.8593 1 1 0 1 1 0 0 17.4426 17.4426 39.4719 0 PROCESSED 57549.7233912037 2016-06-10 17:21:41 54922 2009-04-01 00:00:00 55189.2752430556 2009-12-24 06:36:21 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A JON MILLER SHIN YAMADA USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075200/ Quick Look
16 CYGNUS X-1 299.5891 35.272 299.119523 35.135533 313.701858 54.316122 71.39464341 3.10435878 91.3113 54935.7650462963 2009-04-14 18:21:40 54936.1473958333 2009-04-15 03:32:15 404075030 17.1088 300 17.1088 17.1168 0 17.1088 2 1 0 2 1 0 0 12.986 12.986 33.0279 1 PROCESSED 57546.1452662037 2016-06-07 03:29:11 54922 2009-04-01 00:00:00 54949.5303240741 2009-04-28 12:43:40 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A JON MILLER SHIN YAMADA USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075030/ Quick Look
17 CYGNUS X-1 299.6021 35.1308 299.131607 34.994279 313.637751 54.179562 71.27949874 3.02171591 263.2299 55125.3772106482 2009-10-21 09:03:11 55125.8404398148 2009-10-21 20:10:14 404075130 20.4985 300 20.4985 20.5065 0 20.4985 2 1 0 2 1 0 0 15.163 15.163 40.0159 0 PROCESSED 57548.9405208333 2016-06-09 22:34:21 54922 2009-04-01 00:00:00 55134.2701967593 2009-10-30 06:29:05 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A JON MILLER SHIN YAMADA USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075130/ Quick Look
18 CYGNUS X-1 299.6206 35.1339 299.150096 34.997301 313.663881 54.177403 71.29004535 3.01042005 252.1788 55138.8946180556 2009-11-03 21:28:15 55139.4106365741 2009-11-04 09:51:19 404075150 22.6168 300 22.6168 22.6248 0 22.6168 2 1 0 2 1 0 0 14.061 14.061 44.5759 1 PROCESSED 57549.0593981482 2016-06-10 01:25:32 54922 2009-04-01 00:00:00 55149.4202199074 2009-11-14 10:05:07 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A JON MILLER SHIN YAMADA USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075150/ Quick Look
19 VELA PULSAR/PWN 3 128.6368 -45.8007 128.219858 -45.627635 153.778024 -60.967724 263.96966687 -3.27226783 344.1164 53925.347974537 2006-07-09 08:21:05 53926.0467476852 2006-07-10 01:07:19 501110010 17.5886 20 17.6046 17.5886 17.5886 17.6046 1 1 1 1 1 0 0 17.2252 17.2252 60.3519 0 PROCESSED 57534.8715509259 2016-05-26 20:55:02 54401 2007-10-28 00:00:00 53930.634224537 2006-07-14 15:13:17 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 014211 The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band. GALACTIC DIFFUSE EMISSION 5 B OLEG KARGALTSEV KOJI MORI USJ 1 AO1 THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501110010/ Quick Look
20 VELA PULSAR/PWN 1 128.7701 -45.1981 128.348103 -45.024538 153.316878 -60.401286 263.5414959 -2.83747227 337.9628 53926.0492592593 2006-07-10 01:10:56 53927.7841782407 2006-07-11 18:49:13 501109010 60.2913 60 60.3446 60.2913 60.3313 60.3233 2 2 2 2 1 0 0 52.6899 52.6899 149.8659 1 PROCESSED 57534.9239699074 2016-05-26 22:10:31 54401 2007-10-28 00:00:00 53942.4588078704 2006-07-26 11:00:41 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 014211 The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band. GALACTIC DIFFUSE EMISSION 5 B OLEG KARGALTSEV KOJI MORI USJ 1 AO1 THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501109010/ Quick Look
21 3C382 278.7516 32.7087 278.287499 32.667445 283.134608 55.751017 61.3132426 17.46021716 69.589 54217.9621412037 2007-04-27 23:05:29 54220.8119097222 2007-04-30 19:29:09 702125010 130.58 120 130.588 130.58 0 130.588 2 2 0 2 1 0 0 122.4707 122.4707 246.1958 2 PROCESSED 57538.5400694444 2016-05-30 12:57:42 54777 2008-11-07 00:00:00 54228.2765740741 2007-05-08 06:38:16 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 024353 We propose Suzaku observations of the X-ray bright Broad-Line Radio Galaxy 3C382 to study its complex broad-band X-ray spectrum and its variability on longer timescales. To this end, we ask for 3 separate observations of 40 ks each, to be scheduled randomly but not less than a couple of days apart. We aim at probing the origin of the reflection features and strong soft excess in 3C382, ultimately determining the structure and ionization state of the accretion flow. The addition of 3C382 to the Suzaku program (already including 3C120 and 3C390.3) will allow us to explore BLRGs central engines over a wide range of accretion/jet parameters. EXTRAGALACTIC COMPACT SOURCES 7 B RITA SAMBRUNA Jun Kataoka USJ 2 AO2 THE HIGH-ENERGY SPECTRA OF BROAD-LINE RADIO GALAXIES XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702125010/ Quick Look
22 COMA RADIO HALO 194.9267 27.9061 194.323466 28.175433 181.517491 31.325949 56.39742233 88.00849705 295.2687 53886.8435300926 2006-05-31 20:14:41 53890.7439699074 2006-06-04 17:51:19 801097010 178.6572 180 178.6892 178.6572 178.7132 178.6892 2 2 2 2 1 0 0 167.4506 167.4506 336.9758 7 PROCESSED 57534.5953472222 2016-05-26 14:17:18 54401 2007-10-28 00:00:00 53926.6760416667 2006-07-10 16:13:30 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 014446 We will observe the central regions of the Coma cluster with the HXD/PIN to detect and characterize the nonthermal Inverse Compton (IC) emission from the radio halo. Coma has the best-studied and brightest radio halo, which makes it the best case to detect IC and the most useful one for testing theories for the origin of radio halos. Previous detections with BeppoSAX and RXTE are controversial. Suzaku is more sensitive, will avoid contamination by nearby AGNs including X Comae, and will detect IC even if it is fainter than the claimed BeppoSAX detection. The HXD/PIN data will allow the cluster magnetic field, and nonthermal energy and pressure to be derived. The XIS observations will be used to determine accurate abundances and gradients in Coma, and to test theories for ICM enrichment. EXTRAGALACTIC DIFFUSE SOURCES 8 A CRAIG SARAZIN KYOKO MATSUSHITA USJ 1 AO1 NAILING DOWN THE HARD X-RAY INVERSE COMPTON EMISSION FROM THE RADIO HALO IN THE COMA CLUSTER HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801097010/ Quick Look
23 COMA11 194.6305 28.3939 194.027281 28.663593 180.9862 31.643484 72.26601068 87.98563538 292.5148 54270.6441782407 2007-06-19 15:27:37 54272.0078009259 2007-06-21 00:11:14 802082010 53.0217 50 53.0217 53.0217 0 53.0217 2 2 0 2 1 0 0 46.6673 46.6673 117.806 2 PROCESSED 57539.0191203704 2016-05-31 00:27:32 54695 2008-08-17 00:00:00 54322.5438888889 2007-08-10 13:03:12 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 024438 Several authors have claimed to detect soft X-ray excesses toward some clusters of galaxies, but most are contested by other studies. The only exception is the Coma cluster, where all investigators agree on the presence of the excess, which is especially bright toward one off-centered region, a potential cosmic filament draining into Coma. This excess has bright OVIII emission, so the gas must be thermal, and at the distance of Coma, the mass is of cosmological importance. However, it is possible that this soft excess is due to emission from the halo of the Milky Way, as Coma lies in a valley of particularly low Galactic column density. We propose to distinguish between the Milky Way and Coma origins by measuring the redshift of the OVIII emission line. EXTRAGALACTIC DIFFUSE SOURCES 8 A JOEL BREGMAN Yoh Takei USJ 2 AO2 THE SOFT X-RAY EXCESS TOWARD THE COMA CLUSTER XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802082010/ Quick Look
24 A496 P-CENTER 68.4146 -13.2791 67.835234 -13.38285 64.149602 -34.804694 209.60984883 -36.48888222 55.8718 54680.8514814815 2008-08-02 20:26:08 54682.0543865741 2008-08-04 01:18:19 803073010 44.2607 30 44.2607 44.2607 0 44.2607 1 1 0 1 1 0 0 36.9355 36.9355 103.904 2 PROCESSED 57543.1885416667 2016-06-04 04:31:30 55059 2009-08-16 00:00:00 54693.2133796296 2008-08-15 05:07:16 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 034424 A496 is a "normal" nearby cluster that has been the testbed for metal enrichment models in clusters and, more recently, of different mechanisms to generate cold fronts. Suzaku's excellent spectral resolution, low background and high effective area, combined with the moderate temperatures of this cluster allows us to probe, with two short exposures, into the large scale metal enrichment processes through determination of elemental abundance ratios out to half the virial radius for the first time. EXTRAGALACTIC DIFFUSE SOURCES 8 B RENATO DUPKE KYOKO MATSUSHITA USJ 3 AO3 LARGE SCALE METAL ENRICHMENT MECHANISMS IN ABELL 496 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803073010/ Quick Look
25 CYGNUS X-1 299.5814 35.2712 299.11183 35.134765 313.691248 54.317484 71.39067981 3.10930809 85.1433 54949.7099884259 2009-04-28 17:02:23 54950.2175925926 2009-04-29 05:13:20 404075050 20.5212 300 20.5292 20.5354 0 20.5212 2 1 0 2 1 0 0 12.4013 12.4013 43.8459 0 PROCESSED 57546.4475462963 2016-06-07 10:44:28 54922 2009-04-01 00:00:00 54976.2030671296 2009-05-25 04:52:25 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A JON MILLER SHIN YAMADA USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075050/ Quick Look
26 CYGNUS X-1 299.6355 35.1397 299.165007 35.003038 313.68682 54.178773 71.30136328 3.00304649 241.2259 55152.2855092593 2009-11-17 06:51:08 55152.9418287037 2009-11-17 22:36:14 404075170 23.4485 300 23.4485 23.8885 0 23.8805 2 1 0 2 1 0 0 18.7071 18.7071 56.6918 3 PROCESSED 57549.4356597222 2016-06-10 10:27:21 54922 2009-04-01 00:00:00 55162.2019212963 2009-11-27 04:50:46 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A JON MILLER SHIN YAMADA USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075170/ Quick Look
27 CYGNUS X-1 299.6537 35.1518 299.183253 35.015061 313.717721 54.185168 71.31947353 2.99665901 225.8159 55166.2922453704 2009-12-01 07:00:50 55166.8904398148 2009-12-01 21:22:14 404075190 22.4155 300 22.4155 22.4315 0 22.4235 2 1 0 2 1 0 0 13.1578 13.1578 51.6739 0 PROCESSED 57549.6647222222 2016-06-10 15:57:12 54922 2009-04-01 00:00:00 55181.288912037 2009-12-16 06:56:02 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A JON MILLER SHIN YAMADA USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075190/ Quick Look
28 COMABKG 198.7472 31.648 198.161117 31.912033 183.000201 36.170261 75.72732699 83.16527783 295.0754 54272.0100347222 2007-06-21 00:14:27 54272.7015046296 2007-06-21 16:50:10 802083010 30.7831 30 30.7831 30.7831 0 30.7831 2 2 0 2 1 0 0 26.5058 26.5058 59.7399 0 PROCESSED 57539.0181597222 2016-05-31 00:26:09 54702 2008-08-24 00:00:00 54333.4315393518 2007-08-21 10:21:25 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 024438 Several authors have claimed to detect soft X-ray excesses toward some clusters of galaxies, but most are contested by other studies. The only exception is the Coma cluster, where all investigators agree on the presence of the excess, which is especially bright toward one off-centered region, a potential cosmic filament draining into Coma. This excess has bright OVIII emission, so the gas must be thermal, and at the distance of Coma, the mass is of cosmological importance. However, it is possible that this soft excess is due to emission from the halo of the Milky Way, as Coma lies in a valley of particularly low Galactic column density. We propose to distinguish between the Milky Way and Coma origins by measuring the redshift of the OVIII emission line. EXTRAGALACTIC DIFFUSE SOURCES 8 A JOEL BREGMAN Yoh Takei USJ 2 AO2 THE SOFT X-RAY EXCESS TOWARD THE COMA CLUSTER XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802083010/ Quick Look
29 1E 1841-045 280.3141 -4.8735 279.649841 -4.921767 280.812771 18.180712 27.4352849 0.03686802 77.3227 53844.4525462963 2006-04-19 10:51:40 53847.1328009259 2006-04-22 03:11:14 401100010 97.9622 100 97.9622 97.9702 97.9709 97.9709 2 2 2 2 1 0 0 63.474 63.474 231.5399 2 PROCESSED 57533.5748032407 2016-05-25 13:47:43 54401 2007-10-28 00:00:00 53907.2806597222 2006-06-21 06:44:09 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 014204 Anomalous X-ray Pulsars are young radio-quiet pulsars with unconventional properties challenging conventional wisdom on neutron star formation and evolution. Their slow rotation periods, unprecedented for their apparent youth, point to enormous surface magnetic fields, a thousand times stronger than the typical inferred radio-pulsar field. The origin of the X-ray emission from these pulsars is still being debated. The recent discovery of a hard nonthermal pulsed X-ray emission from 1E 1841-045 with RXTE well beyond 10keV, can probably be explain by a magnetospheric origin and should extend above 100keV. The HXD onboard Suzaku gives us a unique opportunity to characterize the high-energy part of the emission with the added advantage to use the XIS to characterize the lower energy data. GALACTIC POINT SOURCES 4 A ILANA HARRUS MIKIO NORII USJ 1 AO1 SUZAKU OBSERVATIONS OF THE ANOMALOUS X-RAY PULSAR 1E~1841-045 IN THE SNR KES 73 HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401100010/ Quick Look
30 CYGNUS X-1 299.6086 35.1319 299.138103 34.995352 313.646938 54.178814 71.28321336 3.01775246 259.2069 55130.2652314815 2009-10-26 06:21:56 55130.7481365741 2009-10-26 17:57:19 404075140 23.1042 300 23.1042 23.1282 0 23.1202 2 1 0 2 1 0 0 20.011 20.011 41.716 0 PROCESSED 57548.9943171296 2016-06-09 23:51:49 54922 2009-04-01 00:00:00 55141.3539467593 2009-11-06 08:29:41 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A JON MILLER SHIN YAMADA USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075140/ Quick Look
31 CYGNUS X-1 299.5964 35.2723 299.126812 35.135802 313.711652 54.314398 71.39800953 3.09942804 95.8123 54924.0537384259 2009-04-03 01:17:23 54924.5654282407 2009-04-03 13:34:13 404075010 15.3091 300 15.3091 15.3188 0 15.3108 2 1 0 2 1 0 0 15.5374 15.5374 44.2039 1 PROCESSED 57546.0113425926 2016-06-07 00:16:20 54922 2009-04-01 00:00:00 54949.4917824074 2009-04-28 11:48:10 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A JON MILLER SHIN YAMADA USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075010/ Quick Look
32 CYGNUS X-1 299.5337 35.2545 299.064105 35.118267 313.618737 54.314854 71.35609035 3.13386262 50.0944 54980.4956712963 2009-05-29 11:53:46 54981.0586226852 2009-05-30 01:24:25 404075100 28.7845 300 28.7845 28.7845 0 28.7845 1 1 0 1 1 0 0 25.7389 25.7389 48.6319 1 PROCESSED 57546.7292476852 2016-06-07 17:30:07 54922 2009-04-01 00:00:00 54994.3872800926 2009-06-12 09:17:41 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A JON MILLER SHIN YAMADA USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075100/ Quick Look
33 CYGNUS X-1 299.5272 35.2497 299.057586 35.113495 313.607401 54.312117 71.34921869 3.1358965 44.7834 54986.8208333333 2009-06-04 19:42:00 54987.3356944444 2009-06-05 08:03:24 404075120 16.8733 300 16.8813 16.8894 0 16.8733 2 1 0 2 1 0 0 6.7647 6.7647 44.4779 1 PROCESSED 57547.4806018518 2016-06-08 11:32:04 54922 2009-04-01 00:00:00 55001.0163078704 2009-06-19 00:23:29 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A JON MILLER SHIN YAMADA USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075120/ Quick Look
34 COMABKG2 194.3428 28.1403 193.738458 28.410336 180.855412 31.302815 70.87532192 88.34137752 297.3385 54272.7041550926 2007-06-21 16:53:59 54273.4897453704 2007-06-22 11:45:14 802084010 31.9731 30 31.9731 33.5956 0 33.5956 2 2 0 2 1 0 0 28.853 28.853 67.8501 1 PROCESSED 57539.0184143518 2016-05-31 00:26:31 54695 2008-08-17 00:00:00 54318.5135648148 2007-08-06 12:19:32 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 024438 Several authors have claimed to detect soft X-ray excesses toward some clusters of galaxies, but most are contested by other studies. The only exception is the Coma cluster, where all investigators agree on the presence of the excess, which is especially bright toward one off-centered region, a potential cosmic filament draining into Coma. This excess has bright OVIII emission, so the gas must be thermal, and at the distance of Coma, the mass is of cosmological importance. However, it is possible that this soft excess is due to emission from the halo of the Milky Way, as Coma lies in a valley of particularly low Galactic column density. We propose to distinguish between the Milky Way and Coma origins by measuring the redshift of the OVIII emission line. EXTRAGALACTIC DIFFUSE SOURCES 8 A JOEL BREGMAN Yoh Takei USJ 2 AO2 THE SOFT X-RAY EXCESS TOWARD THE COMA CLUSTER XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802084010/ Quick Look
35 HESSJ1813-178 273.3946 -17.7704 272.66469 -17.785118 273.238499 5.632147 12.87014503 0.01155473 90.9367 54160.8999768518 2007-03-01 21:35:58 54162.2814699074 2007-03-03 06:45:19 401101010 63.8391 65 63.8471 63.8391 0 63.8471 2 2 0 2 1 0 0 57.7561 57.7561 119.3519 1 PROCESSED 57537.5358449074 2016-05-29 12:51:37 54736 2008-09-27 00:00:00 54167.6346990741 2007-03-08 15:13:58 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 014214 Radio and X-ray observations towards the VHE gamma-ray source HESS J1813-178, initially dubbed being a dark accelerator , suggested its association with a SNR. However, a recent XMM observation confirmed earlier ASCA findings of an extended, center-filled X-ray source, not resembling the contours of the radio-detected SNR. We propose hard X-ray observations to investigate the alternatively plerionic origin of HESS J1813-178, given the wide spectral coverage possible by XIS/HXD. This will clarify the discrepancy between ASCA and recent INTEGRAL data. Constructing a valid spectral energy distribution will enable us to constrain the age and field strength of the particle accelerator powering the synchrotron emission and accurately model the radiation processes up to VHE energies. GALACTIC POINT SOURCES 4 B OLAF REIMER KEN EBISAWA USJ 1 AO1 IS THE ASSOCIATION OF HESS J1813-178/SNR G12.8-0.0 CONCEALING ITS TRUE PLERIONIC NATURE? HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401101010/ Quick Look
36 CYGNUS X-1 299.5791 35.2719 299.109539 35.135475 313.68862 54.318776 71.39029863 3.11127562 84.0536 54944.1674768518 2009-04-23 04:01:10 54944.6252777778 2009-04-23 15:00:24 404075040 18.014 300 18.0166 18.014 0 18.0166 1 1 0 1 1 0 0 16.3277 16.3277 39.55 0 PROCESSED 57546.2094097222 2016-06-07 05:01:33 54922 2009-04-01 00:00:00 54966.3125 2009-05-15 07:30:00 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A JON MILLER SHIN YAMADA USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075040/ Quick Look
37 CYGNUS X-1 299.5434 35.2592 299.073819 35.122926 313.634234 54.316619 71.36423878 3.12954641 57.7977 54971.0242592593 2009-05-20 00:34:56 54971.6043865741 2009-05-20 14:30:19 404075080 21.3404 300 21.3404 21.3484 0 21.3404 2 1 0 2 1 0 0 17.4954 17.4954 50.1199 1 PROCESSED 57546.6088888889 2016-06-07 14:36:48 54922 2009-04-01 00:00:00 54992.6546875 2009-06-10 15:42:45 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A JON MILLER SHIN YAMADA USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075080/ Quick Look

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SELECT * FROM suzaku_master_data WHERE SUBSTRING(proposal_id,3,1) = '4'

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