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 518
No. |
object_name
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center_ra
|
center_dec
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center_ra_b1950
|
center_dec_b1950
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center_ecliptic_lon
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center_ecliptic_lat
|
center_galactic_lon
|
center_galactic_lat
|
roll_angle
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observation_start_time_mjd
|
observation_start_time
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observation_end_time_mjd
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observation_end_time
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observation_id
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exposure
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awarded_exposure
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xis0_exposure
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xis1_exposure
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xis2_exposure
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xis3_exposure
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xis0_observation_mode
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xis1_observation_mode
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xis2_observation_mode
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xis3_observation_mode
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hxd_observation_mode
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hxd_coarse_clock_rate_exposure
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hxd_first_clock_rate_exposure
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hxd_normal_clock_rate_exposure
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hxd_all_clock_rate_exposure
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hxd_wam_exposure
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quantity_of_hxd_burst
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processing_status
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processing_date_mjd
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processing_date
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public_date_mjd
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public_date
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distribution_date_mjd
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distribution_date
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processing_version
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processing_count
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processing_software
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proposal_id
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proposal_abstract
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proposal_category
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proposal_category_code
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proposal_priority
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pi_name
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co_pi_name
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proposal_affiliated_country
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proposal_cycle
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observation_type
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proposal_title
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main_instrument
|
has_xis_injection
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data_access_url
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ql_access_url
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ql_image_url
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1 | NGC 3660 | 170.883 | -8.6561 | 170.2492 | -8.381454 | 175.088091 | -11.559037 | 269.10006798 | 48.35629614 | 109.6283 | 56624.1463773148 | 2013-11-28 03:30:47 | 56627.0001967593 | 2013-12-01 00:00:17 | 708043010 | 124.7774 | 120 | 124.7854 | 124.7854 | 0 | 124.7774 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 109.7692 | 109.7692 | 246.5434 | 2 | PROCESSED | 57613.5216550926 | 2016-08-13 12:31:11 | 57058 | 2015-02-05 00:00:00 | 56691.7534953704 | 2014-02-03 18:05:02 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082003 | We propose a 120-ks observation of NGC 3660, which is a strong candidate for a True Seyfert 2, a Seyfert that intrinsically lacks the broad line regions (BLRs), and challenges the AGN unified scheme. However, a puzzling BeppoSAX observation lingers, which shows excess emission above 10 keV indicative of a Compton thick AGN. Nevertheless, rapid variability below 10 keV and meagre iron line emission (EW=60 eV) strongly argue against this conclusion. Data from the HXD will elucidate the situation, and either dispel this evidence, adding weight to the True Seyfert 2 scenario, or confirm the presence of heavily obscured emission, which may be explained by a partial covering scenario. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MURRAY BRIGHTMAN | EUR | 8 | AO8 | NGC 3660: A TRUE SEYFERT 2? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708043010/ | Quick Look | ![]() |
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2 | NGC 4051 | 180.8556 | 44.5807 | 180.217538 | 44.859022 | 159.275193 | 40.404023 | 148.68917976 | 70.06918189 | 135.3482 | 53684.8015509259 | 2005-11-10 19:14:14 | 53687.4315277778 | 2005-11-13 10:21:24 | 700004010 | 119.578 | 150 | 119.61 | 119.61 | 119.586 | 119.578 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 120.0047 | 120.0047 | 227.1918 | 3 | PROCESSED | 57528.0225810185 | 2016-05-20 00:32:31 | 54247 | 2007-05-27 00:00:00 | 54037.5713078704 | 2006-10-29 13:42:41 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001012 | We propose to obtain a broad band spectrum of the narrow-line Seyfert 1 (NLS1) NGC 4051. NLS1s are often presumed that they host a relatively small black hole with a very high accretion rate. Such a class would have played an important role in the growth of black holes in a cosmological context. We will measure the intrinsic photon index, amount of reflection, and high energy cutoff for the first time to investigate an accretion disk under a high accretion rate and compare them with conventional broad-line Seyferts. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YUICHI TERASHIMA | JAP | 0 | SWG | THE ACCRETION IN THE NARROW-LINE SEYFERT 1 NGC 4051 PROBED BY A BROAD BAND SPECTRUM | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700004010/ | Quick Look | ![]() |
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3 | MRK 1073 | 48.7759 | 41.9723 | 47.948749 | 41.787366 | 57.835678 | 23.02641 | 149.56255257 | -13.3516285 | 258.3737 | 54135.7651851852 | 2007-02-04 18:21:52 | 54136.6641087963 | 2007-02-05 15:56:19 | 701007020 | 39.5111 | 40 | 39.5191 | 39.5111 | 0 | 39.5191 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.1814 | 37.1814 | 77.6519 | 0 | PROCESSED | 57537.3263657407 | 2016-05-29 07:49:58 | 54735 | 2008-09-26 00:00:00 | 54151.4969444445 | 2007-02-20 11:55:36 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010037 | We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YUICHI TERASHIMA | JAP | 1 | AO1 | COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701007020/ | Quick Look | ![]() |
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4 | EMS0071 | 16.6433 | 48.9425 | 15.913472 | 48.675321 | 36.903288 | 38.099489 | 125.49064727 | -13.85403968 | 69.9406 | 55392.4123148148 | 2010-07-15 09:53:44 | 55392.8855092593 | 2010-07-15 21:15:08 | 705010010 | 23.0102 | 20 | 23.0102 | 23.0102 | 0 | 23.0102 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.568 | 19.568 | 40.8819 | 0 | PROCESSED | 57552.6419560185 | 2016-06-13 15:24:25 | 55779 | 2011-08-06 00:00:00 | 55411.2637384259 | 2010-08-03 06:19:47 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050050 | We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 5 | AO5 | SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705010010/ | Quick Look | ![]() |
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5 | HOLMBERG IX X-1 | 149.4869 | 69.0752 | 148.468802 | 69.313718 | 119.773156 | 51.703341 | 141.91661656 | 41.06840873 | 124.5 | 56224.1252199074 | 2012-10-24 03:00:19 | 56226.4168981482 | 2012-10-26 10:00:20 | 707019030 | 106.9454 | 500 | 106.9454 | 106.9534 | 0 | 106.9614 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 105.0119 | 105.0119 | 197.9478 | 1 | PROCESSED | 57607.8725462963 | 2016-08-07 20:56:28 | 56018 | 2012-04-01 00:00:00 | 56240.5429050926 | 2012-11-09 13:01:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071251 | Recent X-ray observations have found evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in a super-Eddington state. Current data are unable to deliver a clear answer, but the diagnostics possible in a long observation will be decisive. We request a 500 ks observation of the ULX Holmberg IX X-1 to place crucial constraints on atomic features that would signal a super-Eddington flow. Detecting or ruling out atomic features naturally requires a deep exposure. The strong spectral constraints derived will reveal the nature of the accreting black holes in these systems. A definitive statement on the existence of 100-1000 Msun black holes or extreme accretion states will be an important Suzaku legacy. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JON MILLER | USA | 7 | AO7 | A DECISIVE LEGACY OBSERVATION OF AN ULTRALUMINOUS X-RAY SOURCE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707019030/ | Quick Look | ![]() |
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6 | DA 240 EAST LOBE | 117.3573 | 55.877 | 116.349381 | 56.002734 | 108.151975 | 34.146502 | 161.8466677 | 30.16323196 | 293.7777 | 55274.9306134259 | 2010-03-19 22:20:05 | 55276.7238657407 | 2010-03-21 17:22:22 | 704020010 | 81.7834 | 80 | 81.7834 | 81.7914 | 0 | 81.7914 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74.3033 | 74.3033 | 154.9218 | 1 | PROCESSED | 57550.9753587963 | 2016-06-11 23:24:31 | 55654 | 2011-04-03 00:00:00 | 55286.3268518518 | 2010-03-31 07:50:40 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040096 | Suzaku observations of two giant radio galaxies, 3C 35 and DA 240, with a total size of about 1 Mpc are proposed, in order to detect diffuse inverse Compton X-ray emission from their radio lobes. The X-ray flux from the lobes, in comparison with the radio one, provides a precise determination of electron and magnetic field energies there. A comparison of them with those in smaller radio galaxies is used to probe into the history of jets and lobes. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | NAOKI ISOBE | JAP | 4 | AO4 | SUZAKU OBSERVATION OF GIANT RADIO GALAXIES AS A PROBE OF JET HISTORY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704020010/ | Quick Look | ![]() |
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7 | VII ZW 403 | 172.0164 | 79.0077 | 171.163549 | 79.283023 | 114.484764 | 62.884943 | 127.82558857 | 37.31615306 | 108.8488 | 56627.0107638889 | 2013-12-01 00:15:30 | 56628.7884027778 | 2013-12-02 18:55:18 | 708039010 | 88.6616 | 87 | 88.6616 | 88.6616 | 0 | 88.6616 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 87.3974 | 87.3974 | 153.5578 | 1 | PROCESSED | 57613.4969328704 | 2016-08-13 11:55:35 | 57008 | 2014-12-17 00:00:00 | 56639.6396990741 | 2013-12-13 15:21:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081443 | The source of energetic photons that reionized the early universe remains uncertain. Recently, it has been proposed that X-ray binaries in early galaxies made a significant contribution to reionization. Early galaxies had low metallicity and the best local analogs are blue compact dwarf galaxies (BCDs) with low metallicity. We propose to observe two such galaxies known to be luminous in X-rays and accurately measure their spectra with the Suzaku XIS. These observations are important to our understanding of reionization and the formation of early galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | PHILIP KAARET | USA | 8 | AO8 | X-RAYS FROM LOW-METALLICITY BLUE COMPACT DWARF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708039010/ | Quick Look | ![]() |
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8 | 3C 390.3 | 280.4556 | 79.7798 | 281.326844 | 79.727189 | 82.097994 | 76.490616 | 111.44649344 | 27.08887917 | 37.561 | 56436.3002777778 | 2013-05-24 07:12:24 | 56438.6036921296 | 2013-05-26 14:29:19 | 708034010 | 100.3668 | 100 | 100.3668 | 100.3668 | 0 | 100.3668 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 109.3267 | 109.3267 | 198.9817 | 3 | PROCESSED | 57611.4065740741 | 2016-08-11 09:45:28 | 56816 | 2014-06-08 00:00:00 | 56449.7081365741 | 2013-06-06 16:59:43 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081431 | We propose simultaneous Suzaku (100 ks) and NuSTAR observations of the broad-line radio galaxy 3C 390.3, to measure Fe K-alpha emission and Compton reflection from the accretion disk. This is crucial for understanding the geometry of the accretion disk and its relation to the production of a powerful, relativistic radio jet. The combination of accurate Compton reflection parameters measured with NuSTAR and a simultaneous estimate of the accretion disk inner radius from Fe K-alpha with Suzaku will place strong constraints on accretion disk models for radio loud AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | PATRICK OGLE | USA | 8 | AO8 | ACCRETION AND BLACK HOLE SPIN IN THE POWERFUL, RADIO-LOUD AGN 3C 390.3 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708034010/ | Quick Look | ![]() |
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9 | M82 X-1 | 149.1432 | 69.7042 | 148.108278 | 69.941832 | 119.044016 | 52.159559 | 141.33659361 | 40.60182861 | 163.0524 | 54367.135775463 | 2007-09-24 03:15:31 | 54367.8716898148 | 2007-09-24 20:55:14 | 702026010 | 35.5999 | 40 | 36.0319 | 35.5999 | 0 | 36.0239 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.4749 | 30.4749 | 63.5699 | 1 | PROCESSED | 57540.0638194444 | 2016-06-01 01:31:54 | 54770 | 2008-10-31 00:00:00 | 54402.2563657407 | 2007-10-29 06:09:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020092 | We propose Suzaku observations of the intermediate-mass black hole candidate M82 X-1 for spectral study with a wide-band energy range including over 10 keV. In particular, the purpose is to determine a spectral cut-off energy in details in order to improve unified understanding of different mass black holes in comparison with those of stellar-mass black holes and ULXs in nearby galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | RYOHEI MIYAWAKI | JAP | 2 | AO2 | HARD X-RAY SPECTRAL STUDY OF M82 X-1 WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702026010/ | Quick Look | ![]() |
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10 | 1H0323+342 | 51.1746 | 34.1741 | 50.388045 | 33.998103 | 57.519907 | 15.008853 | 155.73224486 | -18.75935356 | 251.4848 | 56352.6173611111 | 2013-03-01 14:49:00 | 56354.8078819444 | 2013-03-03 19:23:21 | 707015010 | 101.272 | 100 | 101.288 | 101.272 | 0 | 101.288 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 97.1283 | 97.1283 | 189.2516 | 0 | PROCESSED | 57610.7547916667 | 2016-08-10 18:06:54 | 56739 | 2014-03-23 00:00:00 | 56372.5724189815 | 2013-03-21 13:44:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070088 | We propose to observe a narrow-line radio-loud gamma-ray emitting Seyfert 1 galaxy 1H0323+342, which is the X-ray brightest among a new class of GeV gamma-ray emitting AGNs, first detected by Fermi/LAT. Based on accurate and high-sensitive measurement of X-ray spectra with Suzaku, we study the presence of Fe-K lines and energy-dependence of time variability, in order to constrain the origin of X-ray emission of this object. This leads to understanding the SED of this object and constraining the jet power. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YASUSHI FUKAZAWA | JAP | 7 | AO7 | STUDY OF X-RAY SPECTRAL VARIABILITY OF A NARROW-LINE RADIO-LOUD GAMAM-RAY EMITTING SEYFERT 1 GALAXY 1H0323+342 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707015010/ | Quick Look | ![]() |
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11 | SWIFT J1922.7-1716 | 290.6403 | -17.2233 | 289.918336 | -17.319807 | 289.738469 | 4.813727 | 20.73500926 | -14.48356253 | 80.064 | 54198.231099537 | 2007-04-08 05:32:47 | 54200.4321643518 | 2007-04-10 10:22:19 | 702028010 | 78.6386 | 80 | 78.6386 | 78.6386 | 0 | 78.6386 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61.3533 | 61.3533 | 190.1298 | 0 | PROCESSED | 57538.1728356482 | 2016-05-30 04:08:53 | 54744 | 2008-10-05 00:00:00 | 54206.3754166667 | 2007-04-16 09:00:36 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020097 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many new absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe two of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 2 | AO2 | BROAD BAND SPECTRA OF NEW SWIFT/BAT AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702028010/ | Quick Look | ![]() |
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12 | 2MASX J15115979-2119 | 227.9997 | -21.3083 | 227.279118 | -21.120692 | 231.351076 | -3.323732 | 341.57056512 | 30.81939061 | 105.6253 | 55979.0551388889 | 2012-02-22 01:19:24 | 55980.937650463 | 2012-02-23 22:30:13 | 706010010 | 83.8162 | 80 | 83.8162 | 83.8162 | 0 | 83.8162 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82.2568 | 82.2568 | 162.6359 | 1 | PROCESSED | 57604.7185763889 | 2016-08-04 17:14:45 | 56361 | 2013-03-10 00:00:00 | 55995.1640393518 | 2012-03-09 03:56:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060032 | We propose to observe two hard X-ray bright narrow-line Seyfert 1 galaxies, which are an important class of objects in studying accretion processes under a large mass accretion rate and therefore mass growth of black holes. Our aims are (1) to measure a continuum shape such as spectral slope and high energy cutoff, (2) to compare them with other classes of AGNs, and (3) to search for highly ionized outflows with a large column density. All of these will be a fundamental piece of information to better understand accretion physics and ``feedback'' processes in galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YUICHI TERASHIMA | JAP | 6 | AO6 | ACCRETION AND OUTFLOW IN THE HARD X-RAY SELECTED NARROW-LINE SEYFERT 1S | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706010010/ | Quick Look | ![]() |
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13 | MARKARIAN 3 | 93.9187 | 71.0301 | 92.469282 | 71.045623 | 91.893166 | 47.615546 | 143.30552616 | 22.72176381 | 268.1895 | 57104.2423148148 | 2015-03-23 05:48:56 | 57104.6266550926 | 2015-03-23 15:02:23 | 709022040 | 23.518 | 20 | 23.518 | 23.526 | 0 | 23.526 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8399305556 | 2016-08-17 20:09:30 | 57486 | 2016-04-08 00:00:00 | 57119.4206018518 | 2015-04-07 10:05:40 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092008 | We propose to measure size and distance from the black hole of the optically-thick absorbing and reprocessing system(s) in the heavily obscured Seyfert Galaxy Markarian~3 by means of its known X-ray spectral variability. We aim at simultaneously measuring: the variability timescale of the primary emission, seen in transmission through a photoelectric column density of (0.7--1.1)x10^{24} atoms/cm/cm; the variability timescale of its Compton-reflection, dominating the continuum flux in the 3-10 keV energy band; and the variability timescale of the nuclear obscuration. Only the scientific payload on-board Suzaku possesses the required combination of broadband X-ray coverage, sensitivity, and spectroscopic capabilities to perform this experiment. We request 5 observations of 20 ks each. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MATTEO GUAINAZZI | EUR | 9 | AO9 | MEASURING THE TORUS SPATIAL SCALE(S) IN SEYFERT GALAXIES: A SUZAKU MONITORING OF MARKARIAN 3 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709022040/ | Quick Look | ![]() |
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14 | PKS 1345+12 | 206.9131 | 12.3498 | 206.299989 | 12.598696 | 200.201065 | 21.844458 | 347.38894416 | 70.20282736 | 113.9421 | 54472.3082407407 | 2008-01-07 07:23:52 | 54473.6799768518 | 2008-01-08 16:19:10 | 702053010 | 52.9844 | 50 | 52.9844 | 52.9844 | 0 | 52.9844 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.2034 | 45.2034 | 118.5038 | 4 | PROCESSED | 57541.3141782407 | 2016-06-02 07:32:25 | 54854 | 2009-01-23 00:00:00 | 54483.4984375 | 2008-01-18 11:57:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021341 | We wish to take advantage of the sensitivity of Suzaku above 10 keV to constrain the energy source -- starburst or black-hole driven activity -- in three of the brightest warm transitional ultraluminous infrared galaxies, PKS 1345+12, Mrk 463, and 3C 273. 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 time scale variability, another signature of black-hole driven activity. These data will be combined with our A01 spectra and be part of S. Teng's PhD thesis at UMD. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | SYLVAIN VEILLEUX | USA | 2 | AO2 | SPECTRA OF THE BRIGHTEST WARM ULTRALUMINOUS INFRARED GALAXIES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702053010/ | Quick Look | ![]() |
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15 | NGC 4593 | 189.915 | -5.3482 | 189.270103 | -5.073686 | 191.205514 | -0.992169 | 297.48487911 | 57.39893055 | 292.7762 | 56824.1040972222 | 2014-06-16 02:29:54 | 56824.8563888889 | 2014-06-16 20:33:12 | 709014010 | 29.7616 | 30 | 29.7696 | 29.7616 | 0 | 29.7696 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24.185 | 24.185 | 64.9919 | 1 | PROCESSED | 57615.2408449074 | 2016-08-15 05:46:49 | 57204 | 2015-07-01 00:00:00 | 56835.7291435185 | 2014-06-27 17:29:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090097 | In the AO-8 cycle, we proposed six X-ray and optical simultaneous observations of type I Seyfert galaxy NGC 3516, and now obtaining a good correlation between those wavelengths. In the observations, we confirmed that a hard X-ray primary component (HXPC) found in Noda et al. (2013) was dominant, and its variation is well correlated with an optical one. To verify the probability that a variation of HXPC in other Seyfert also correlates with that in its optical, we propose six X-ray and optical simultaneous observations of NGC 4593, which has an X-ray spectrum dominated by HXPC as well as NGC 3516 in 2013. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 9 | AO9 | X-RAY AND OPTICAL SIMULTANEOUS OBSERVATIONS OF TYPICAL TYPE I SEYFERT NGC 4593 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709014010/ | Quick Look | ![]() |
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16 | AO 0235+164 | 39.665 | 16.613 | 38.972105 | 16.397631 | 42.455706 | 1.088366 | 156.77598662 | -39.11106084 | 252.4352 | 56310.722337963 | 2013-01-18 17:20:10 | 56311.7418634259 | 2013-01-19 17:48:17 | 707021010 | 43.1028 | 40 | 43.1108 | 43.1188 | 0 | 43.1028 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38.3583 | 38.3583 | 88.0698 | 0 | PROCESSED | 57608.5604166667 | 2016-08-08 13:27:00 | 56709 | 2014-02-21 00:00:00 | 56342.5387731482 | 2013-02-19 12:55:50 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071402 | We request observations of the variable blazar AO 0235+164, to be conducted simultaneously with Fermi and optical and radio telescopes, towards a multi-band campaign. This object has complex X-ray spectrum due to absorption by an intervening galaxy, and Suzaku will be essential in unraveling the effects and composition of that absorber, and for the first time, provide a robust measurement of the underlying blazar X-ray continuum, which, together with the Swift UVOT spectrum, will allow to verify the signature of the bulk-Compton component, due to cold electrons propagating in the relativistic jet. At the highest priority, we request 40 ks for a precise spectral measurement; at a lower priority, we wish to monitor the source for the total of 5 days, with the request of additional 160 ks. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GRZEGORZ MADEJSKI | USA | 7 | AO7 | SUZAKU OBSERVATIONS OF THE GAMMA-RAY BLAZAR AO 0235+164 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707021010/ | Quick Look | ![]() |
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17 | NGC 5347 | 208.2716 | 33.4399 | 207.717601 | 33.685673 | 191.037943 | 41.510938 | 62.06849004 | 75.29189994 | 312.225 | 54627.6603703704 | 2008-06-10 15:50:56 | 54628.6064699074 | 2008-06-11 14:33:19 | 703011010 | 42.1611 | 40 | 42.1611 | 42.1611 | 0 | 42.1611 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.1302 | 37.1302 | 81.734 | 1 | PROCESSED | 57542.8072569444 | 2016-06-03 19:22:27 | 55008 | 2009-06-26 00:00:00 | 54637.3250810185 | 2008-06-20 07:48:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030040 | We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YUICHI TERASHIMA | JAP | 3 | AO3 | COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703011010/ | Quick Look | ![]() |
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18 | MARKARIAN 79 | 115.6357 | 49.8015 | 114.696355 | 49.919868 | 108.437878 | 27.988088 | 168.6115046 | 28.38007803 | 283.4884 | 54193.9134953704 | 2007-04-03 21:55:26 | 54195.7655439815 | 2007-04-05 18:22:23 | 702044010 | 83.7038 | 82 | 83.7118 | 83.7038 | 0 | 83.7118 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82.1042 | 82.1042 | 160.0059 | 0 | PROCESSED | 57538.0894444444 | 2016-05-30 02:08:48 | 54695 | 2008-08-17 00:00:00 | 54203.4223842593 | 2007-04-13 10:08:14 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021313 | Recently, deep observations of a number of Seyfert AGN with XMM-Newton and Suzaku have established variable and relativistic iron lines as robust features in roughly half of all deep Seyfert spectra. In these sources, the spin of the black hole can be constrained directly through fits to the relativistic iron line. A sample of excellent spectra from well-chosen AGN will facilitate a better understanding of the innermost regime near to black holes, and make correlations with parameters like radio luminosity, star formation rate, and galaxy and black hole mass possible for the first time. We propose to obtain observations of 4 under-exposed Seyfert AGN with promising evidence for broad lines to robustly constrain their spin parameters. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | JON MILLER | USA | 2 | AO2 | REVEALING BLACK HOLE SPIN IN RELATIVISTIC SEYFERT AGN | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702044010/ | Quick Look | ![]() |
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19 | M106 | 184.7117 | 47.2376 | 184.094273 | 47.515109 | 160.404745 | 44.085185 | 138.43381178 | 68.89762168 | 287.1938 | 53896.5413078704 | 2006-06-10 12:59:29 | 53898.7113425926 | 2006-06-12 17:04:20 | 701095010 | 99.8175 | 100 | 99.8815 | 99.8175 | 99.8815 | 99.8815 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 97.5229 | 97.5229 | 187.4839 | 1 | PROCESSED | 57534.6515393518 | 2016-05-26 15:38:13 | 54401 | 2007-10-28 00:00:00 | 53927.2308449074 | 2006-07-11 05:32:25 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 013151 | We propose observations of the nearby Low Luminosity AGN, M81 and M106, for 100 ks for each target. We aim to detect both targets up to ~200 keV for the first time. We will determine the photon indices of the hard X-ray power-law continuum, with searching for other possible characteristics such as Compton hump around 10-20 keV and cutoff around 100-200 keV which would lead major discoveries. We will study the shape of Fe-K line(s) around 6-7 keV and their time variances. Our goal is to compare their hard X-ray spectra with those of SWG seyfert galaxies, with unprecedented accuracy, to study the accresion mechanism of LLAGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TAKESHI ITOH | CHRISTOPHER REYNOLDS | JUS | 1 | AO1 | OBSERVATIONS OF HARD X-RAYS FROM LOW LUMINOSITY ACTIVE GALACTIC NUCLEI | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701095010/ | Quick Look | ![]() |
20 | IRAS 00182-7112 | 5.1458 | -70.9276 | 4.573856 | -71.205097 | 312.979414 | -61.496651 | 306.55074146 | -45.98323945 | 33.8687 | 56050.171087963 | 2012-05-03 04:06:22 | 56052.8759143518 | 2012-05-05 21:01:19 | 707036010 | 93.959 | 90 | 93.967 | 93.959 | 0 | 93.959 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86.5766 | 86.5766 | 233.6819 | 1 | PROCESSED | 57605.3998263889 | 2016-08-05 09:35:45 | 56435 | 2013-05-23 00:00:00 | 56068.6299537037 | 2012-05-21 15:07:08 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071441 | We propose to observe with the Hard X-ray Detector onboard Suzaku the two Ultraluminous Infrared Galaxies IRAS 00182-7112 and IRAS 12127-1412, both of which are known to harbour very luminous and highly obscured active galactic nuclei (AGN). An AGN reflection component arising from ionized gas is clearly identified at 2 10 keV: the detection of the direct AGN emission above 10 keV and the measure of the reflection efficiency would provide fundamental information on both the physical structure of Compton-thick AGN embedded in a nuclear starburst and their feedback on the surrounding environment. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | EMANUELE NARDINI | USA | 7 | AO7 | THE PHYSICAL STRUCTURE OF COMPTON-THICK AGN/ULIRGS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707036010/ | Quick Look | ![]() |
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21 | E1821+643 | 275.5207 | 64.3306 | 275.456094 | 64.303959 | 318.282096 | 86.807262 | 93.98984501 | 27.40177083 | 228.4067 | 56239.7868981482 | 2012-11-08 18:53:08 | 56241.8217708333 | 2012-11-10 19:43:21 | 707016010 | 100.4132 | 100 | 100.4132 | 100.4132 | 0 | 100.4132 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95.5411 | 95.5411 | 175.7799 | 2 | PROCESSED | 57608.0299421296 | 2016-08-08 00:43:07 | 56631 | 2013-12-05 00:00:00 | 56265.6966319444 | 2012-12-04 16:43:09 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070089 | Central engines of AGN are considered to be generally in Multi-Zone Comptonization (MZC) condition (e.g., Noda et al. 2011a,b). To verify this thing on a high-luminosiy AGN, we suggest to observe Radio-Quiet Quasar E1821+643 By Suzaku. Utilizing a time variability of each Comptonization component, we will resolve spectral variable components, and study whether the central engine of E1821+643 is in MZC condition or not. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | HIROUMI NODA | JAP | 7 | AO7 | SUZAKU STUDY OF MULTI-ZONE COMPTONIZATION PICTURE ON THE CENTRAL ENGINE OF RADIO-QUIET QUASAR E1821+643 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707016010/ | Quick Look | ![]() |
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22 | SWIFT J1200.8+0650 | 180.2185 | 6.7488 | 179.57779 | 7.027186 | 177.502279 | 6.275772 | 270.13481807 | 66.34579154 | 293.0035 | 54617.9027662037 | 2008-05-31 21:39:59 | 54619.9280555556 | 2008-06-02 22:16:24 | 703009010 | 84.4866 | 80 | 84.5106 | 84.4866 | 0 | 84.5106 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71.1109 | 71.1109 | 174.9638 | 3 | PROCESSED | 57542.752037037 | 2016-06-03 18:02:56 | 55003 | 2009-06-21 00:00:00 | 54634.1479282407 | 2008-06-17 03:33:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030034 | The hard X-ray survey with Swift BAT have been finding various types of AGNs. Many buried AGNs with very low scattered X-rays have been discovered, for example. We propose to obtain broad band spectra of Compton-thin buried AGNs in the Swift sample. The data will be used to measure the amount of absoption in the direct and reflected emission and to constrain the structure of the obscuring matter around the AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YUICHI TERASHIMA | JAP | 3 | AO3 | THE STRUCTURE OF BURIED COMPTON-THIN AGNS DISCOVERED BY SWIFT | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703009010/ | Quick Look | ![]() |
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23 | J081618.99+482328.4 | 124.0768 | 48.3841 | 123.174595 | 48.53824 | 114.890427 | 27.844597 | 171.01809871 | 33.69777889 | 298.4793 | 54917.0925462963 | 2009-03-27 02:13:16 | 54919.0946643518 | 2009-03-29 02:16:19 | 703042010 | 90.9224 | 90 | 90.9224 | 90.9224 | 0 | 90.9224 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81.0739 | 81.0739 | 172.9637 | 2 | PROCESSED | 57545.9726736111 | 2016-06-06 23:20:39 | 55329 | 2010-05-13 00:00:00 | 54930.3718055556 | 2009-04-09 08:55:24 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031337 | We have discovered polar broad absorption-line quasars (BALQSOs) from their radio variabilities. We know their inclination angles. Our results derived from the archival Chandra data of one polar BALQSO indicate that the X-ray emissions are from the jet and the X-ray absorbing gas is located at tens of parsecs above the accretion disk corona. We want to confirm these results at high confidence level using better signal to noise ratio data from a big observatory, like SUZAKU. In addition, we propose to observe three more polar BALQSOs, which have wide range of radio/UV/X-ray properties. Our primary science goal of this proposal is to determine the radial distribution of the X-ray absorbing gas in 4 polar BALQSOs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | KAJAL GHOSH | USA | 3 | AO3 | PROBING THE INNER STRUCTURE OF AGNS USING THE POLAR BALQSOS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703042010/ | Quick Look | ![]() |
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24 | QSO 1222+216 | 186.229 | 21.3887 | 185.599657 | 21.665582 | 176.758525 | 22.008941 | 255.03812277 | 81.66761796 | 123.6044 | 56988.9003125 | 2014-11-27 21:36:27 | 56989.2953240741 | 2014-11-28 07:05:16 | 709025010 | 13.4002 | 15 | 0 | 0 | 0 | 13.4002 | 0 | 0 | 0 | 2 | 1 | 0 | 0 | 12.0474 | 12.0474 | 31.4359 | 0 | PROCESSED | 57617.406099537 | 2016-08-17 09:44:47 | 57368 | 2015-12-12 00:00:00 | 57002.0161111111 | 2014-12-11 00:23:12 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092023 | EXTRAGALACTIC COMPACT SOURCES | 7 | C | MARCUS LANGEJAHN | EUR | 9 | AO9 | false | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709025010/ | Quick Look | ![]() |
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25 | EMS0857 | 198.1882 | 0.8497 | 197.548985 | 1.114667 | 196.443673 | 7.917565 | 314.828891 | 63.22804034 | 111.0249 | 55578.1935532407 | 2011-01-17 04:38:43 | 55578.746087963 | 2011-01-17 17:54:22 | 705011010 | 22.07 | 20 | 22.078 | 22.07 | 0 | 22.085 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15.3267 | 15.3267 | 47.7279 | 0 | PROCESSED | 57600.6315046296 | 2016-07-31 15:09:22 | 55962 | 2012-02-05 00:00:00 | 55595.4732986111 | 2011-02-03 11:21:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050050 | We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 5 | AO5 | SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705011010/ | Quick Look | ![]() |
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26 | 3C454.3 | 343.4951 | 16.1379 | 342.877484 | 15.871411 | 351.362437 | 21.321746 | 86.10833014 | -38.194784 | 252.9263 | 55525.0494675926 | 2010-11-25 01:11:14 | 55526.0141087963 | 2010-11-26 00:20:19 | 705021010 | 41.0252 | 40 | 41.0332 | 41.0332 | 0 | 41.0252 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.1412 | 37.1412 | 83.3278 | 0 | PROCESSED | 57554.2391319445 | 2016-06-15 05:44:21 | 55916 | 2011-12-21 00:00:00 | 55550.1355439815 | 2010-12-20 03:15:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050052 | We propose 40 ksec x 2 (at most) Suzaku ToO observations - from a list of five -of GeV-bright flat spectrum radio quasars (FSRQs) that would be triggered by significant flaring (with E>100 MeV flux of 2x10^(-6) photons/cm^2/s or greater) in the Fermi all-sky monitoring. Those observations will be coordinated with optical and Swift XRT observations, with the goal of obtaining broadband spectra and light-curves during a flare gamma-ray activity. Such detailed spectral and variability studies are crucial to discriminate between different radiation scenarios responsible for production of X-rays and gamma-rays, and to constrain the content and by extension, the accelertation process of the jet and energization of the radiating particles. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 5 | AO5-TOO | SUZAKU TOO OBSERVATION OF GIANT FLARE IN FRSQS TRIGGERED BY FERMI-LAT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705021010/ | Quick Look | ![]() |
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27 | SMC X-1 | 19.2828 | -73.4495 | 18.951598 | -73.712645 | 312.330174 | -66.477022 | 300.41169288 | -43.55280074 | 39.2778 | 55706.0851851852 | 2011-05-25 02:02:40 | 55706.6745833333 | 2011-05-25 16:11:24 | 706030050 | 17.8463 | 18 | 17.8463 | 18.1823 | 0 | 18.1001 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 16.6829 | 16.6829 | 50.9139 | 0 | PROCESSED | 57602.111099537 | 2016-08-02 02:39:59 | 56092 | 2012-06-14 00:00:00 | 55725.1651736111 | 2011-06-13 03:57:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JOSEPH NEILSEN | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030050/ | Quick Look | ![]() |
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28 | MRK 766 | 184.6154 | 29.8184 | 183.986779 | 30.095968 | 171.206094 | 28.943476 | 190.63186084 | 82.27243688 | 133.2599 | 54055.0242361111 | 2006-11-16 00:34:54 | 54057.363900463 | 2006-11-18 08:44:01 | 701035010 | 97.8693 | 150 | 98.1756 | 97.8693 | 0 | 98.1676 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 96.8931 | 96.8931 | 202.1299 | 2 | PROCESSED | 57536.189525463 | 2016-05-28 04:32:55 | 54800 | 2008-11-30 00:00:00 | 54132.8396990741 | 2007-02-01 20:09:10 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011328 | X-ray spectroscopy of Mkn 766 has revealed ionised Fe emission that varies with the continuum on 10 ks timescales: direct evidence for ionised reflection from the accretion disk. This bright NLSy1 also shows extreme spectral variability, with the low state being dominated by a hard, constant reflection component, probably from cool distant material. We propose to measure the spectrum above 10 keV; the hot component should vary with the continuum, the cold distant component should be constant, and we can measure their relative contributions to test the predictions of the lower-energy analysis. This source is complex and needs the high-energy spectrum from Suzaku: it seems likely that previous complex behavior of several Seyferts can be described by these components | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TRACEY TURNER | USA | 1 | AO1 | DECOMPOSITION OF SEYFERT SPECTRA: TRACKING THE INNER DISK IN MKN 766 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701035010/ | Quick Look | ![]() |
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29 | MRK 1 | 19.06 | 33.0289 | 18.361574 | 32.765252 | 30.564721 | 23.029207 | 128.90716196 | -29.55492804 | 249.7486 | 54111.5318171296 | 2007-01-11 12:45:49 | 54114.5836111111 | 2007-01-14 14:00:24 | 701047010 | 126.4441 | 120 | 126.4441 | 126.4441 | 0 | 126.4441 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 126.0122 | 126.0122 | 263.6237 | 2 | PROCESSED | 57637.5831944445 | 2016-09-06 13:59:48 | 54702 | 2008-08-24 00:00:00 | 54133.1552314815 | 2007-02-02 03:43:32 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011336 | The supermassive black holes of active galactic nuclei (AGN) are fundamentally connected to the stars of their host galaxies, but it is not clear whether this relationship is evident at X-ray energies. We will test the prediction that prolific star formation is responsible for the soft X-ray emission from a Compton thick AGN that also contains a powerful circumnuclear starburst. The AGN's deep obscuration facilitates the soft X-ray measurements, and Compton thick AGN are generally significant, both as a large fraction of the local AGN population and for their contribution to the X-ray background. Furthermore, we will use the direct measurement of the intrinsic AGN luminosity to test unified AGN models and the validity of indirect luminosity indicators. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | NANCY LEVENSON | USA | 1 | AO1 | TESTING THE STARBURST-AGN CONNECTION AND MEASURING DEEPLY OBSCURED AGN | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701047010/ | Quick Look | ![]() |
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30 | NGC 1365 | 53.3976 | -36.1412 | 52.920229 | -36.30818 | 36.797911 | -53.03906 | 237.95777124 | -54.60123537 | 60.7695 | 55392.8956597222 | 2010-07-15 21:29:45 | 55399.3676273148 | 2010-07-22 08:49:23 | 705031020 | 302.1753 | 450 | 302.1753 | 302.1833 | 0 | 302.1833 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 251.0612 | 251.0612 | 425.5339 | 2 | PROCESSED | 57552.8844791667 | 2016-06-13 21:13:39 | 55287 | 2010-04-01 00:00:00 | 55413.8216435185 | 2010-08-05 19:43:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051112 | We propose 3 observations (~4 days each) of the Seyfert galaxy NGC 1365, at 2-week intervals. We aim to use eclipses to unambiguously identify the broad Fe K line, examine variability of the HXD/PIN excess, and to search for changes in the physical properties of the ionized absorber in this bright, nearby AGN. Shorter observations of this galaxy with XMM-Newton, Chandra and Suzaku showcase several remarkable physical traits: (1) FeXXV and FeXXVI K-shell absorption lines (the highest s/n detection so far among AGN), (2) rapidly varying cold absorption, (3) a highly significant relativistic Fe K emission line, and (4) a factor ~4 excess flux at high energies. The proposed observations will provide legacy spectra for what is arguably the single most physically-revealing obscured AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | LAURA BRENNEMAN | USA | 5 | AO5 | A LONG LOOK AT NGC 1365: DISC TOMOGRAPHY, IONIZED ABSORPTION AND HIGH ENERGY EXCESS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705031020/ | Quick Look | ![]() |
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31 | NGC 7130 | 327.065 | -34.8962 | 326.317147 | -35.128916 | 317.224283 | -20.334869 | 10.02903365 | -50.33744977 | 78.4767 | 54597.5198726852 | 2008-05-11 12:28:37 | 54598.56625 | 2008-05-12 13:35:24 | 703012010 | 44.4931 | 40 | 44.4931 | 44.4931 | 0 | 44.4931 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 36.7677 | 36.7677 | 90.3759 | 1 | PROCESSED | 57542.510474537 | 2016-06-03 12:15:05 | 54975 | 2009-05-24 00:00:00 | 54609.0170949074 | 2008-05-23 00:24:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030040 | We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YUICHI TERASHIMA | JAP | 3 | AO3 | COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703012010/ | Quick Look | ![]() |
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32 | ESO 511-G030 | 214.8456 | -26.6457 | 214.126189 | -26.416188 | 221.40386 | -12.022179 | 326.23004886 | 32.21661925 | 292.391 | 56156.7622337963 | 2012-08-17 18:17:37 | 56157.7960416667 | 2012-08-18 19:06:18 | 707023030 | 51.9172 | 270 | 51.9252 | 51.9252 | 0 | 51.9172 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 52.011 | 52.011 | 89.3158 | 3 | PROCESSED | 57606.8813194444 | 2016-08-06 21:09:06 | 56640 | 2013-12-14 00:00:00 | 56272.6998148148 | 2012-12-11 16:47:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071413 | The study of "bare" Seyfert 1 AGN is essential to measure the true properties of the inner regions of the accretion disk. The nearby Seyfert ESO 511-G30 is a prime candidate for fulfilling this role due to its broad Fe K component and lack of any intrinsic warm absorption. It is also one of the X-ray brightest bare Seyferts featured in the Swift 58 month BAT catalogue as yet unobserved with Suzaku. We propose a 270 ks Suzaku observation of ESO 511-G30 to unambiguously constrain the properties of the accretion disk and subsequently the black hole spin. In addition, the HXD data will allow us to measure the Compton reflection hump, while the excellent soft X-ray spectral resolution of XIS will allow the origin of the soft excess to be determined. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JAMES REEVES | USA | 7 | AO7 | MEASURING THE ACCRETION DISK AND BLACK HOLE PROPERTIES OF ESO 511-G30 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707023030/ | Quick Look | ![]() |
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33 | SWIFT J2052.0-5704 | 312.9788 | -57.0176 | 312.02055 | -57.205734 | 297.951069 | -37.67562 | 340.05945565 | -38.72742848 | 73.9304 | 54945.6280671296 | 2009-04-24 15:04:25 | 54946.6863310185 | 2009-04-25 16:28:19 | 704010010 | 45.16 | 40 | 45.16 | 45.168 | 0 | 45.168 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57.6242 | 57.6242 | 91.4098 | 1 | PROCESSED | 57546.2560416667 | 2016-06-07 06:08:42 | 55339 | 2010-05-23 00:00:00 | 54973.4487152778 | 2009-05-22 10:46:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040059 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright, absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe three of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. With these observations we can make the spectral survey of bright absorbed Swift/BAT AGNs complete. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 4 | AO4 | SPECTRAL SURVEY OF A COMPLETE SAMPLE OF SWIFT/BAT SELECTED AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704010010/ | Quick Look | ![]() |
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34 | SWIFT J1952.4+0237 | 298.0556 | 2.5705 | 297.425623 | 2.440903 | 300.700434 | 23.070542 | 42.31566647 | -12.27488447 | 82.9116 | 54929.8284722222 | 2009-04-08 19:53:00 | 54931.1079166667 | 2009-04-10 02:35:24 | 704011010 | 47.9211 | 40 | 47.9259 | 47.9211 | 0 | 47.9259 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.3044 | 39.3044 | 110.5258 | 2 | PROCESSED | 57546.1208680556 | 2016-06-07 02:54:03 | 55324 | 2010-05-08 00:00:00 | 54949.4878356482 | 2009-04-28 11:42:29 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040059 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright, absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe three of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. With these observations we can make the spectral survey of bright absorbed Swift/BAT AGNs complete. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 4 | AO4 | SPECTRAL SURVEY OF A COMPLETE SAMPLE OF SWIFT/BAT SELECTED AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704011010/ | Quick Look | ![]() |
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35 | NGC1365 | 53.4052 | -36.1452 | 52.927869 | -36.31215 | 36.804669 | -53.045157 | 237.96410536 | -54.59489483 | 47.2005 | 56107.1526041667 | 2012-06-29 03:39:45 | 56107.9972916667 | 2012-06-29 23:56:06 | 707017010 | 30.6949 | 30 | 30.6949 | 30.6949 | 0 | 30.6949 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.8321 | 27.8321 | 72.9738 | 0 | PROCESSED | 57606.5279050926 | 2016-08-06 12:40:11 | 56491 | 2013-07-18 00:00:00 | 56125.2372453704 | 2012-07-17 05:41:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070095 | NGC1365 is one of AGNs which shows the most highly variable spectral change, and furthermore exhibits strong Fe-K absorption lines blue-shifted by 1000--5000 km/s with EW of about 100eV. These absorption lines indicate a massive outflow and are important to consider the AGN feedback to parent galaxies. Currently, there is no other object by which we can measure the Fe-K absorption lines accurately than NGC 1365. Therefore, we propose to monitor a velocity, depth, and ratio of blue-shifted Fe-K absorption lines, hard X-ray flux above 10 keV of NGC1365 every 10 days, in order to probe the massive outflow dynamically and compare the results with the numerical simulation. } | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YASUSHI FUKAZAWA | JAP | 7 | AO7 | MONITOR OF VELOCITY AND STRENGTH OF BLUE-SHIFTED STRONG FE-K ABSORPTION LINES OF NGC 1365 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707017010/ | Quick Look | ![]() |
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36 | NGC 3516 | 166.6957 | 72.5543 | 165.843141 | 72.824666 | 123.386475 | 57.973853 | 133.24670004 | 42.41457084 | 283.0856 | 56435.1473148148 | 2013-05-23 03:32:08 | 56436.2952199074 | 2013-05-24 07:05:07 | 708006070 | 51.4752 | 50 | 51.4772 | 51.4752 | 0 | 51.4792 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53.7203 | 53.7203 | 99.1658 | 1 | PROCESSED | 57611.3639351852 | 2016-08-11 08:44:04 | 56383 | 2013-04-01 00:00:00 | 56449.6609027778 | 2013-06-06 15:51:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080066 | We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 8 | AO8 | THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006070/ | Quick Look | ![]() |
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37 | NGC 4968 | 196.7464 | -23.7282 | 196.071371 | -23.461103 | 204.633939 | -15.321329 | 307.51234678 | 39.00523278 | 298.8345 | 53954.7307523148 | 2006-08-07 17:32:17 | 53955.6822222222 | 2006-08-08 16:22:24 | 701005010 | 39.0508 | 40 | 39.0508 | 39.0508 | 39.0508 | 39.0508 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35.617 | 35.617 | 82.1979 | 1 | PROCESSED | 57535.2527546296 | 2016-05-27 06:03:58 | 54408 | 2007-11-04 00:00:00 | 54020.7898148148 | 2006-10-12 18:57:20 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010037 | We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YUICHI TERASHIMA | JAP | 1 | AO1 | COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701005010/ | Quick Look | ![]() |
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38 | NGC 2992 | 146.4207 | -14.2696 | 145.81924 | -14.038457 | 154.003817 | -26.061971 | 249.65504756 | 28.81616071 | 88.7924 | 53693.8781597222 | 2005-11-19 21:04:33 | 53694.9759722222 | 2005-11-20 23:25:24 | 700005020 | 37.4935 | 120 | 37.6565 | 39.6915 | 37.4935 | 37.8205 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 33.8991 | 33.8991 | 94.8479 | 1 | PROCESSED | 57528.0334490741 | 2016-05-20 00:48:10 | 54247 | 2007-05-27 00:00:00 | 54037.7316087963 | 2006-10-29 17:33:31 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001013 | NGC 2992 is a nearby Seyfert 1.9 galaxy showing long-term (20 yrs) large amplitude (factor of 20) variability. This object showed switching between Compton-thick and -thin. Recent RXTE monitoring has shown that this object is highly variable on shorter time scales (2 weeks). We propose three Suzaku observations to monitor the variability of absorption column, broad band continuum shape, and Fe line intensity to understand the cause of the remarkable variability. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YUICHI TERASHIMA | JAP | 0 | SWG | THE SPECTRAL VARIABILITY IN NGC 2992: FE-LINE, REFLECTION, AND COMPTON-THIN/THICK SWITCHING | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700005020/ | Quick Look | ![]() |
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39 | 3C 236 BACKGROUND | 151.1488 | 34.7362 | 150.413548 | 34.979134 | 140.636655 | 21.408004 | 190.35215815 | 53.68789407 | 299.9977 | 56055.786712963 | 2012-05-08 18:52:52 | 56056.7919444444 | 2012-05-09 19:00:24 | 707006010 | 46.2113 | 40 | 46.2113 | 46.2113 | 0 | 46.2113 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.1095 | 44.1095 | 86.8399 | 0 | PROCESSED | 57605.3836574074 | 2016-08-05 09:12:28 | 56436 | 2013-05-24 00:00:00 | 56070.1639930556 | 2012-05-23 03:56:09 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070014 | Through the Suzaku observations of giant radio galaxies, of which the size is larger than about 1 Mpc, we are going to reveal a picture that the jets in radio galaxies become inactive as they evolve from 500 kpc to 1 Mpc. However, the current Suzaku sample of the giant radio galaxies is far from being satisfactory to make a definite conclusion. Therefore, we propose a Suzaku observation of 3C 236, one of the most giant radio galaxy in the Universe. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NAOKI ISOBE | JAP | 7 | AO7 | INVESTIGATION INTO EVOLUTION OF THE JET ENERGETICS, THROUGH THE SUZAKU OBSERVATION OF THE GIANT RADIO GALAXY 3C 236 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707006010/ | Quick Look | ![]() |
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40 | IRASF01475-0740 | 27.4875 | -7.3766 | 26.863598 | -7.624293 | 22.745573 | -17.452267 | 160.69718538 | -65.86110455 | 68.025 | 54661.0549652778 | 2008-07-14 01:19:09 | 54662.3023032407 | 2008-07-15 07:15:19 | 703065010 | 57.9147 | 50 | 57.9147 | 57.9183 | 0 | 57.9263 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.1257 | 51.1257 | 107.6988 | 0 | PROCESSED | 57543.0527546296 | 2016-06-04 01:15:58 | 55051 | 2009-08-08 00:00:00 | 54683.4056712963 | 2008-08-05 09:44:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032030 | We propose 50ks observations of IRASF01475-0740 and NGC 3147, both of which are Seyfert 2s apparently unobscured in X-rays. Unsatisfied with this apparent contradiction, we seek Suzaku observations with two main aims. First, high energy observations with the HXD can reveal whether a deeply buried AGN is present above 10 keV. Second, the XIS observations will probe sensitively for short time-scale variability below 10 keV, the detection of which would establish unambiguously that the objects have genuinely unobscured nuclei and rule out the alternatives of scattered light or X-ray binaries. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KIRPAL NANDRA | EUR | 3 | AO3 | SOLVING THE MYSTERY OF UNOBSCURED SEYFERT 2 GALAXIES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703065010/ | Quick Look | ![]() |
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41 | 3C120 | 68.2993 | 5.3535 | 67.634764 | 5.249056 | 67.434072 | -16.404208 | 190.3755878 | -27.39480435 | 262.4873 | 53789.4598726852 | 2006-02-23 11:02:13 | 53790.8748958333 | 2006-02-24 20:59:51 | 700001030 | 40.9073 | 160 | 40.9073 | 40.9073 | 40.9073 | 40.9073 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 38.4817 | 38.4817 | 77.876 | 2 | PROCESSED | 57533.073900463 | 2016-05-25 01:46:25 | 54247 | 2007-05-27 00:00:00 | 54041.5149189815 | 2006-11-02 12:21:29 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001003 | Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 0 | SWG | BROAD-BAND MONITORING OF 3C120 IN VARIOUS ACCRETING STATES | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700001030/ | Quick Look | ![]() |
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42 | MCG-6-30-15 | 203.9713 | -34.2978 | 203.254904 | -34.042659 | 215.172989 | -22.546967 | 313.28925681 | 27.67845448 | 102.4359 | 53762.928275463 | 2006-01-27 22:16:43 | 53765.368275463 | 2006-01-30 08:50:19 | 700007030 | 96.6919 | 300 | 96.6919 | 96.6919 | 96.6999 | 96.6999 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 89.8194 | 89.8194 | 210.8019 | 5 | PROCESSED | 57532.8529861111 | 2016-05-24 20:28:18 | 54247 | 2007-05-27 00:00:00 | 54040.8156828704 | 2006-11-01 19:34:35 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001035 | The broad iron line in the Seyfert 1 galaxy MCG-6-30-15 shows that most of the power is released at 2--4 gravitational radii enabling the strong gravity, accretion flow and energy release in that exciting regime to be studied. The spectral variability of the source decomposes into a highly variable power law and a reflection-dominated component, containing the iron line and Compton hump, which varies significantly but with much less amplitude. This can be explained by the extreme gravitational light bending occuring in this region. We propose to observe MCG--6-30-15 for 4 x 50~ks in order to determine for the first time the variability of the reflection over a wide range of energies from below 1 keV to above 40 keV and timescales . | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ANDREW FABIAN | JAP | 0 | SWG | REFLECTION, ABSORPTION AND STRONG GRAVITY AROUND THE SPINNING BLACK HOLE IN MCG--6-30-15 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700007030/ | Quick Look | ![]() |
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43 | 0836+714 | 130.267 | 70.829 | 129.006808 | 71.006559 | 109.318804 | 50.076677 | 143.62710847 | 34.4182022 | 294.8268 | 53809.7578125 | 2006-03-15 18:11:15 | 53810.5836111111 | 2006-03-16 14:00:24 | 700010010 | 55.6261 | 50 | 55.6341 | 55.6341 | 55.6261 | 55.6341 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 47.4058 | 47.4058 | 71.3419 | 1 | PROCESSED | 57533.2238541667 | 2016-05-25 05:22:21 | 54247 | 2007-05-27 00:00:00 | 54041.9651851852 | 2006-11-02 23:09:52 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001061 | We propose two 50 ks observations, one for each of two EGRET blazars, 1510-089 (OR -017) and 0836+710 (4C +71.07). Both objects show extremely hard X-ray spectra, with photon indices about 1.3. The blazar 1510-089 ($z = 0.361$) is among a few OVV quasars showing prominent soft X-ray excess. The blazar 0836+710 ($z = 2.172)$ is the brightest X-ray source among the high redshift ($z>2$) quasars, and its very hard X-ray spectrum extends down to soft X-rays. Studying spectral shape and variability in the soft X-ray band relative to variability in the mid X-ray and optical bands can help to reveal nature of the soft X-ray excess of unknown origin, and multifrequency variability studies can provide constraints on the structure of jets on subparsec scales. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GREG MADEJSKI | JAP | 0 | SWG | TESTING THE SHOCK-IN-JET MODEL FOR NONTHERMAL FLARES IN BLAZARS VIA SUZAKU OBSERVATIONS | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700010010/ | Quick Look | ![]() |
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44 | SWIFT J0746.3+2548 | 116.6142 | 25.8792 | 115.852151 | 26.002245 | 113.853224 | 4.615293 | 194.5201067 | 22.91801121 | 97.0095 | 53678.357974537 | 2005-11-04 08:35:29 | 53680.5862847222 | 2005-11-06 14:04:15 | 700011010 | 99.4284 | 100 | 99.5235 | 100.4524 | 99.4284 | 99.7235 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 87.6995 | 87.6995 | 192.472 | 4 | PROCESSED | 57527.9575694445 | 2016-05-19 22:58:54 | 54247 | 2007-05-27 00:00:00 | 54037.5799074074 | 2006-10-29 13:55:04 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001087 | Recently the BAT gamma-ray detector onboard Swift satellite has discovered very flat hard X-ray sources with photon index ~ 1.5 above 100 keV. The x-ray spectrum obtained with the XRT on Swiftis highly variable on time scales < 90 minutes. This variability and flat continuum spectrum suggests that this source is classified as a blazar. If this association is real, we have a precious chance to obtain spectrum upto several hundred keV in the source frame of the source. This wide range is of particularly importanceto study the blazar spectrum, or the electron distribution. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TADAYUKI TAKAHASHI | JAP | 0 | SWG | SUZAKU OBSERVATION OF A HIGH REDSHIFT BLAZAR RECENTLY DISCOVERED BY THE BAT ON SWIFT | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700011010/ | Quick Look | ![]() |
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45 | PKS 0558-504 | 89.9335 | -50.4395 | 89.62999 | -50.44058 | 89.864093 | -73.881363 | 257.95137808 | -28.57681508 | 212.4401 | 54121.9091203704 | 2007-01-21 21:49:08 | 54122.3529976852 | 2007-01-22 08:28:19 | 701011050 | 19.5154 | 20 | 19.5314 | 19.5154 | 0 | 19.5314 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.1236 | 16.1236 | 38.312 | 0 | PROCESSED | 57536.8983217593 | 2016-05-28 21:33:35 | 54735 | 2008-09-26 00:00:00 | 54137.0453240741 | 2007-02-06 01:05:16 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010057 | Narrow-line Seyfert 1 Galaxies (NLS1s) must have been crucial key to understand the rapid growth of the central supermassive black hole, which may be related to the evolution of the host galaxy. Hence, we propose 20x5 ksec observations of the luminous NLS1 galaxy PKS 0558-504, which is the candidate having the highest mass-accretion rate among the class. Large effective area and good energy resolution of XISs allow us to strictly constrain the temperature and the luminosity of the accretion flow. In addition, Suzaku HXD will detect the significant fraction of hard power law emission in the 10-60 keV band for the first time. From these observations, we expect to derive the new picture of the high mass-accretion mechanism in NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YOSHITO HABA | JAP | 1 | AO1 | SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701011050/ | Quick Look | ![]() |
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46 | SWIFT J0350.1-5019 | 57.6662 | -50.2998 | 57.309175 | -50.449494 | 28.967165 | -67.019674 | 259.65657878 | -48.95336771 | 180.7044 | 54062.0888078704 | 2006-11-23 02:07:53 | 54062.5647453704 | 2006-11-23 13:33:14 | 701017020 | 19.271 | 23 | 19.271 | 19.271 | 0 | 19.271 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.74 | 16.74 | 41.097 | 0 | PROCESSED | 57536.1549768518 | 2016-05-28 03:43:10 | 54750 | 2008-10-11 00:00:00 | 54088.5939583333 | 2006-12-19 14:15:18 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010133 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 1 | AO1 | DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701017020/ | Quick Look | ![]() |
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47 | BO 375 | 11.4476 | 41.6573 | 10.75946 | 41.384162 | 28.671168 | 33.427051 | 121.80050832 | -21.20204189 | 232.9596 | 54135.3691666667 | 2007-02-04 08:51:36 | 54135.7592476852 | 2007-02-04 18:13:19 | 701028010 | 12.7798 | 13 | 12.7798 | 12.7798 | 0 | 12.7798 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.8386 | 12.8386 | 33.664 | 1 | PROCESSED | 57536.9599189815 | 2016-05-28 23:02:17 | 54695 | 2008-08-17 00:00:00 | 54151.4930324074 | 2007-02-20 11:49:58 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011120 | There are over 400 very luminous (Lx > 1e38-1e40 erg/s) globular cluster X-ray sources in nearby galaxies. None are present in our Galaxy, and their nature is unknown. They may be accreting black holes, however, this is quite controversial and it is contrary to theoretical expectations. The distance is too large to make accurate studies of any of them that could reveal their nature. Luckily, there is one such very luminous source, Bo 375, in a globular cluster in M31. We propose to perform ten 10 ksec Suzaku observations of Bo 375. We expect that from the long-term lightcurve, broad-band energy spectra, and power spectra, we will be able to determine the nature of this object and thereby possibly the nature of the many very luminous globular cluster X-ray sources in nearby galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ALBERT KONG | USA | 1 | AO1 | PROBING THE NATURE OF A VERY LUMINOUS GLOBULAR CLUSTER X-RAY SOURCE IN M31 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701028010/ | Quick Look | ![]() |
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48 | BO 375 | 11.4497 | 41.6556 | 10.761554 | 41.382464 | 28.671878 | 33.424815 | 121.80214792 | -21.2037783 | 231.6187 | 54137.6100810185 | 2007-02-06 14:38:31 | 54137.9737731482 | 2007-02-06 23:22:14 | 701028020 | 15.5371 | 13 | 15.5371 | 15.5371 | 0 | 15.5371 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14.942 | 14.942 | 31.4159 | 0 | PROCESSED | 57537.3176967593 | 2016-05-29 07:37:29 | 54695 | 2008-08-17 00:00:00 | 54151.4987731482 | 2007-02-20 11:58:14 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011120 | There are over 400 very luminous (Lx > 1e38-1e40 erg/s) globular cluster X-ray sources in nearby galaxies. None are present in our Galaxy, and their nature is unknown. They may be accreting black holes, however, this is quite controversial and it is contrary to theoretical expectations. The distance is too large to make accurate studies of any of them that could reveal their nature. Luckily, there is one such very luminous source, Bo 375, in a globular cluster in M31. We propose to perform ten 10 ksec Suzaku observations of Bo 375. We expect that from the long-term lightcurve, broad-band energy spectra, and power spectra, we will be able to determine the nature of this object and thereby possibly the nature of the many very luminous globular cluster X-ray sources in nearby galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ALBERT KONG | USA | 1 | AO1 | PROBING THE NATURE OF A VERY LUMINOUS GLOBULAR CLUSTER X-RAY SOURCE IN M31 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701028020/ | Quick Look | ![]() |
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49 | BO 375 | 11.4497 | 41.6556 | 10.761554 | 41.382464 | 28.671878 | 33.424815 | 121.80214792 | -21.2037783 | 231.4176 | 54142.8248032407 | 2007-02-11 19:47:43 | 54143.2167824074 | 2007-02-12 05:12:10 | 701028030 | 15.0878 | 13 | 15.0878 | 15.0878 | 0 | 15.0878 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.7164 | 15.7164 | 33.8379 | 1 | PROCESSED | 57537.3535069444 | 2016-05-29 08:29:03 | 54695 | 2008-08-17 00:00:00 | 54153.1806828704 | 2007-02-22 04:20:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011120 | There are over 400 very luminous (Lx > 1e38-1e40 erg/s) globular cluster X-ray sources in nearby galaxies. None are present in our Galaxy, and their nature is unknown. They may be accreting black holes, however, this is quite controversial and it is contrary to theoretical expectations. The distance is too large to make accurate studies of any of them that could reveal their nature. Luckily, there is one such very luminous source, Bo 375, in a globular cluster in M31. We propose to perform ten 10 ksec Suzaku observations of Bo 375. We expect that from the long-term lightcurve, broad-band energy spectra, and power spectra, we will be able to determine the nature of this object and thereby possibly the nature of the many very luminous globular cluster X-ray sources in nearby galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ALBERT KONG | USA | 1 | AO1 | PROBING THE NATURE OF A VERY LUMINOUS GLOBULAR CLUSTER X-RAY SOURCE IN M31 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701028030/ | Quick Look | ![]() |
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50 | NGC 3783 | 174.7611 | -37.7364 | 174.141196 | -37.45925 | 192.677729 | -36.170962 | 287.45850943 | 22.95048745 | 293.6402 | 53910.7726388889 | 2006-06-24 18:32:36 | 53912.8571412037 | 2006-06-26 20:34:17 | 701033010 | 75.7193 | 75 | 75.7193 | 75.7193 | 75.7193 | 75.7193 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 68.2993 | 68.2993 | 180.0237 | 0 | PROCESSED | 57534.7899652778 | 2016-05-26 18:57:33 | 54401 | 2007-10-28 00:00:00 | 53926.8847453704 | 2006-07-10 21:14:02 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011325 | We propose a 75 ksec Suzaku observation of the bright Seyfert 1 NGC 3783. Absorption due to photo-ionized material in the line of sight is well-established in this source, but can lead to degeneracy during modeling: is 3-6 keV continuum curvature due to photo-ionized absorption or a relativistically broad Fe K component? The simultaneous broadband XIS/HXD coverage is needed to define the continuum emission over a wide bandpass and disentangle the various emitting and absorbing components. We can then study the ionized absorber components, establish whether or not broad Fe K emission exists, and constrain reflection components, including the Compton shoulder. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | ALEX MARKOWITZ | USA | 1 | AO1 | PROBING FE K EMISSION AND IONIZED ABSORPTION IN NGC 3783 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701033010/ | Quick Look | ![]() |
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51 | MRK 273 | 206.1319 | 55.8192 | 205.671114 | 56.069559 | 168.560084 | 59.024421 | 108.09580624 | 59.75355315 | 290.8776 | 53923.3108333333 | 2006-07-07 07:27:36 | 53925.3356481482 | 2006-07-09 08:03:20 | 701050010 | 79.9046 | 80 | 79.9126 | 79.9046 | 79.9206 | 79.9206 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 82.8076 | 82.8076 | 174.9059 | 3 | PROCESSED | 57534.931400463 | 2016-05-26 22:21:13 | 54401 | 2007-10-28 00:00:00 | 53930.7076851852 | 2006-07-14 16:59:04 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011341 | 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 | USA | 1 | AO1 | THE DOMINANT ENERGY SOURCE OF ULTRALUMINOUS INFRARED GALAXIES | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701050010/ | Quick Look | ![]() |
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52 | APM 08279+5255 | 127.9265 | 52.7635 | 126.994318 | 52.932793 | 116.239859 | 32.72128 | 165.74397918 | 36.24189551 | 118.0523 | 54020.1580902778 | 2006-10-12 03:47:39 | 54022.3134143518 | 2006-10-14 07:31:19 | 701057010 | 102.3328 | 100 | 102.3408 | 102.3408 | 102.3328 | 102.3408 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 96.0187 | 96.0187 | 186.1858 | 3 | PROCESSED | 57535.8953125 | 2016-05-27 21:29:15 | 54702 | 2008-08-24 00:00:00 | 54053.9467013889 | 2006-11-14 22:43:15 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011353 | Motivated by the detection of a relativistic outflow of highly ionized gas in previous XMM-Newton and Chandra observations of the lensed quasar APM08279+5255 we propose to monitor this object with three 100ks observations with the aim of improving our understanding of the significance of such outflows in regulating black hole growth and in influencing structure formation. The main scientific goals are : (a) verify the present interpretations of Fe line features in this quasar, (b) monitor the time variability of the Fe absorption features and thus constrain the acceleration mechanism, (c) constrain the kinematic, ionization and absorbing properties of the outflow, and (d) show whether the low-energy ionized absorber is part of the relativistic outflow. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GEORGE CHARTAS | USA | 1 | AO1 | VIEWS OF RELATIVISTIC WINDS THROUGH NATURAL LENSES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701057010/ | Quick Look | ![]() |
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53 | 1ES 1101-232 | 165.8976 | -23.5471 | 165.286971 | -23.277424 | 177.035323 | -27.087344 | 273.21266184 | 33.02701002 | 279.8544 | 53880.6859606482 | 2006-05-25 16:27:47 | 53882.2161921296 | 2006-05-27 05:11:19 | 701071010 | 62.4327 | 55 | 62.4407 | 62.4407 | 62.4407 | 62.4327 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 50.1033 | 50.1033 | 132.1939 | 0 | PROCESSED | 57534.4584027778 | 2016-05-26 11:00:06 | 54401 | 2007-10-28 00:00:00 | 53927.4165393518 | 2006-07-11 09:59:49 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011376 | Detecting absorption effects in TeV blazar spectra from TeV photon collisions on the extragalactic IR background (EBL) is a powerful tool to probe the EBL. It requires a thorough understanding of the intrinsic blazar spectra. We propose XIS and HXD observations, with emphasis on the hard X-rays, for the 3 most distant HESS blazars, coordinated with HESS observations. Thanks to Suzaku's sensitivity in a broad energy range, we expect to set tight limits on the models' parameter space, and constrain emission and acceleration scenarios by studying the shape and evolution of the particle distribution, most sensitively conducted in the important hard X-ray energy range. In coordination with TeV observations, it allows us to disentangle EBL absorption effects from the blazar intrinsic spectra. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ANITA REIMER | USA | 1 | AO1 | CHALLENGING JET MODELS OF THE MOST DISTANT TEV-BLAZARS | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701071010/ | Quick Look | ![]() |
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54 | NGC 4992 | 197.2442 | 11.5776 | 196.620329 | 11.84391 | 191.275652 | 17.435393 | 318.61367169 | 73.91298788 | 297.9177 | 53904.2287615741 | 2006-06-18 05:29:25 | 53905.2112615741 | 2006-06-19 05:04:13 | 701080010 | 38.7886 | 40 | 38.7886 | 38.7886 | 38.7886 | 38.7886 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 33.6179 | 33.6179 | 84.8819 | 1 | PROCESSED | 57534.7313657407 | 2016-05-26 17:33:10 | 54422 | 2007-11-18 00:00:00 | 53926.1865856482 | 2006-07-10 04:28:41 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012016 | The high-energy detectors onboard Swift and INTEGRAL have started to survey the hard X-ray sky above 10 keV. Although limited to bright X-ray fluxes (~10^-11 cgs), the large area surveyed so far has allowed to build up sizable sa mples of hard X-ray selected AGN almost unbiased against X-ray absorption. The AGN content of these surveys is dominated by obscured AGN. We have identified 3 objects which are most likely obscured by Compton-thick matter and very bright above 10 keV. We propose to observe them with Suzaku for 40 ks each to study their broad-band X-ray spectra and unveil previously unknown nearby heavily obscured AGN, with important consequences for the study of the AGN evolution and the synthesis of the X-ray background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ANDREA COMASTRI | EUR | 1 | AO1 | BRIGHT COMPTON THICK GALAXIES IN THE BACKYARD | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701080010/ | Quick Look | ![]() |
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55 | MKN 841 | 226.022 | 10.498 | 225.418561 | 10.69235 | 220.178743 | 26.653826 | 11.31218444 | 54.65057921 | 105.7688 | 54122.3650925926 | 2007-01-22 08:45:44 | 54123.6063541667 | 2007-01-23 14:33:09 | 701084010 | 51.7528 | 50 | 51.7928 | 51.7528 | 0 | 51.7928 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.7077 | 43.7077 | 107.2379 | 1 | PROCESSED | 57536.9356481482 | 2016-05-28 22:27:20 | 54777 | 2008-11-07 00:00:00 | 54139.3030208333 | 2007-02-08 07:16:21 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012028 | We propose to perform two 50 ks Suzaku observations of Mkn 841, at an interval of a few months, in order to elucidate the origin of its different X-ray components. Strong soft excess and complex iron line profile are known to be present in this source and recent XMM observations reveal their extreme and puzzling spectral and temporal behaviors. Nevertheless, while the XMM observations help to better constrain their natures, their physical interpretation strongly suffer from the lack of data above 10 keV. Two dedicated Suzaku observations will provide crucial information for our understanding of these components, allowing 1) to obtain high S/N and striclty simultaneous broad band X-ray spectra from the soft X-ray up to the reflection bump and 2) to study their spectral variability behaviors | EXTRAGALACTIC COMPACT SOURCES | 7 | B | PIERRE-OLIVIER PETRUCCI | EUR | 1 | AO1 | PROBING THE ORIGIN OF THE STRONG SOFT EXCESS AND PUZZLING REFLECTION COMPONENTS IN MKN 841 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701084010/ | Quick Look | ![]() |
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56 | GB1428+4217 | 217.5879 | 42.0673 | 217.100189 | 42.288572 | 194.201902 | 52.635769 | 75.8575282 | 64.90635728 | 315.7011 | 53898.716400463 | 2006-06-12 17:11:37 | 53899.8336111111 | 2006-06-13 20:00:24 | 701092010 | 48.6956 | 50 | 48.6956 | 48.6956 | 48.6956 | 48.6956 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 43.4943 | 43.4943 | 96.5159 | 1 | PROCESSED | 57534.6334259259 | 2016-05-26 15:12:08 | 54394 | 2007-10-21 00:00:00 | 53926.3635069444 | 2006-07-10 08:43:27 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012043 | We propose to observe GB1428+4217 at z=4.72 for 50ks with Suzaku in order to determine its spectrum up to 45 keV, corresponding to a rest-frame energy of ~250 keV. This will allow to robustly model the spectrum in terms of a hard power-law and a Comptonization component from the scattering of `cold' electrons in the jet onto the soft nuclear photon field, as qualitatively hinted by XMM-Newton available data. This would be the first detection of such a feature in blazars and would directly and uniquely give information on the power of the relativistic jets in this source. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ANDREW FABIAN | EUR | 1 | AO1 | JET POWER OF THE DISTANT EXTREME LUMINOSITY BLAZAR GB1428+4217 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701092010/ | Quick Look | ![]() |
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57 | 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 | ![]() |
58 | OJ 287 FLARE | 133.7115 | 20.1695 | 132.996174 | 20.360602 | 130.493887 | 2.661227 | 206.74425687 | 35.84822718 | 98.7868 | 54411.475 | 2007-11-07 11:24:00 | 54413.896099537 | 2007-11-09 21:30:23 | 702008010 | 112.044 | 100 | 112.052 | 112.06 | 0 | 112.044 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102.9238 | 102.9238 | 209.1519 | 3 | PROCESSED | 57540.5116087963 | 2016-06-01 12:16:43 | 54791 | 2008-11-21 00:00:00 | 54423.3848032407 | 2007-11-19 09:14:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020024 | OJ 287 is a promissing candidate of a suppermassive binary black hole, based on its periodic flare with a cycle of about 12 years. The next flare is predicted to take place on the fall, 2007. Therefore, two Suzaku exposures on OJ 287 is proposed, coordinated with radio, optical and very high energy gamma-ray observations. The first observation is on the spring to obtained the multi-wavelength spectrum of the target in its quiescent phase. The second is planned to be in a form of ToO observation on the fall, which will be triggered by an optical flare. The nature of the flare will be extensively investigated in these observatsions. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NAOKI ISOBE | JAP | 2 | AO2-TOO | MULTI-WAVELENGTH OBSERVATION OF PREDICTED FLARE OF SUPERMASSIVE BINARY BLACK HOLE CANDIDATE, OJ 287 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702008010/ | Quick Look | ![]() |
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59 | IC 3639 | 190.1935 | -36.8078 | 189.517353 | -36.533453 | 205.04698 | -29.556314 | 300.55692841 | 26.01476797 | 293.9494 | 54293.1966435185 | 2007-07-12 04:43:10 | 54294.4133564815 | 2007-07-13 09:55:14 | 702011010 | 53.3912 | 50 | 53.3912 | 53.3912 | 0 | 53.3912 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.4852 | 48.4852 | 105.11 | 1 | PROCESSED | 57539.1904050926 | 2016-05-31 04:34:11 | 54709 | 2008-08-31 00:00:00 | 54339.5331365741 | 2007-08-27 12:47:43 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020034 | Seyfert 2 galaxies often have an nucleus obscured by thick matter. Risaliti et al. found that Compton thick Seyfert 2 galaxies may constitute a large fraction of the Seyfert 2 galaxy s population by studying the distribution of absorbing column densities among Seyfert 2 galaxies. This result is important to discuss on the structure and evolution of active galactic nuclei. However, it is difficult to classify Seyfert 2 galaxies into Compton thick and thin objects only by using their X-ray spectra below 10 keV. Therefore, there may be Compton thin objects among Risaliti s Compton thick sample. In order to make the distribuion of the column density more reliable, we propose the Suzaku observations of heavily obscured AGNs with NH >1E25cm-2. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | HISAMITSU AWAKI | JAP | 2 | AO2 | SUZAKU OBSERVATIONS OF THE HEAVILY OBSCURED AGNS WITH NH>1E25 CM-2 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702011010/ | Quick Look | ![]() |
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60 | NGC5548 | 214.4933 | 25.1285 | 213.926392 | 25.358693 | 201.994196 | 36.40686 | 31.9338138 | 70.49848107 | 305.6607 | 54289.4186921296 | 2007-07-08 10:02:55 | 54290.1182175926 | 2007-07-09 02:50:14 | 702042040 | 30.6996 | 30 | 30.6996 | 30.6996 | 0 | 30.6996 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 28.8279 | 28.8279 | 60.4319 | 1 | PROCESSED | 57539.1330324074 | 2016-05-31 03:11:34 | 54695 | 2008-08-17 00:00:00 | 54328.4843402778 | 2007-08-16 11:37:27 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021307 | We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARTIN ELVIS | USA | 2 | AO2 | NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702042040/ | Quick Look | ![]() |
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61 | NGC5548 | 214.4959 | 25.1277 | 213.928994 | 25.357885 | 201.997272 | 36.407089 | 31.932758 | 70.49602002 | 293.6791 | 54296.5817013889 | 2007-07-15 13:57:39 | 54297.4168865741 | 2007-07-16 10:00:19 | 702042050 | 30.0197 | 30 | 30.0277 | 30.0357 | 0 | 30.0197 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.3004 | 26.3004 | 58.971 | 1 | PROCESSED | 57539.274849537 | 2016-05-31 06:35:47 | 54707 | 2008-08-29 00:00:00 | 54340.3894328704 | 2007-08-28 09:20:47 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021307 | We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARTIN ELVIS | USA | 2 | AO2 | NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702042050/ | Quick Look | ![]() |
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62 | NGC5548 | 214.4979 | 25.1264 | 213.930994 | 25.35658 | 201.999984 | 36.406639 | 31.92993093 | 70.49400067 | 281.7605 | 54317.0262268518 | 2007-08-05 00:37:46 | 54318.0211111111 | 2007-08-06 00:30:24 | 702042080 | 38.7757 | 210 | 38.7837 | 38.7917 | 0 | 38.7757 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 32.6497 | 32.6497 | 85.9519 | 0 | PROCESSED | 57539.4187037037 | 2016-05-31 10:02:56 | 54714 | 2008-09-05 00:00:00 | 54347.3528472222 | 2007-09-04 08:28:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021307 | We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARTIN ELVIS | USA | 2 | AO2 | NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702042080/ | Quick Look | ![]() |
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63 | FAIRALL 9 | 20.9481 | -58.8141 | 20.470954 | -59.074601 | 340.57309 | -59.156739 | 295.06951561 | -57.81752905 | 48.1772 | 54258.155462963 | 2007-06-07 03:43:52 | 54260.5766666667 | 2007-06-09 13:50:24 | 702043010 | 167.7983 | 164 | 167.7983 | 167.8063 | 0 | 167.8143 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 136.4834 | 136.4834 | 209.1758 | 2 | PROCESSED | 57538.9238425926 | 2016-05-30 22:10:20 | 54773 | 2008-11-03 00:00:00 | 54265.5470717593 | 2007-06-14 13:07:47 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021313 | Recently, deep observations of a number of Seyfert AGN with XMM-Newton and Suzaku have established variable and relativistic iron lines as robust features in roughly half of all deep Seyfert spectra. In these sources, the spin of the black hole can be constrained directly through fits to the relativistic iron line. A sample of excellent spectra from well-chosen AGN will facilitate a better understanding of the innermost regime near to black holes, and make correlations with parameters like radio luminosity, star formation rate, and galaxy and black hole mass possible for the first time. We propose to obtain observations of 4 under-exposed Seyfert AGN with promising evidence for broad lines to robustly constrain their spin parameters. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JON MILLER | USA | 2 | AO2 | REVEALING BLACK HOLE SPIN IN RELATIVISTIC SEYFERT AGN | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702043010/ | Quick Look | ![]() |
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64 | NGC 1052 | 40.2309 | -8.2134 | 39.616406 | -8.42693 | 35.027708 | -22.668341 | 181.91154484 | -57.92833515 | 49.7745 | 54297.4313888889 | 2007-07-16 10:21:12 | 54299.87875 | 2007-07-18 21:05:24 | 702058010 | 100.6691 | 100 | 100.6691 | 100.6691 | 0 | 100.6691 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 83.4998 | 83.4998 | 211.4278 | 2 | PROCESSED | 57539.327037037 | 2016-05-31 07:50:56 | 54707 | 2008-08-29 00:00:00 | 54339.9136458333 | 2007-08-27 21:55:39 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021355 | Accretion onto supermassive black holes is thought to play a major role in the production of relativistic jets. Our understanding of jet production remains elusive, however, because we cannot image the accretion flow. Fortunately, the Fe K line offers a direct probe of accretion. As part of a multi-mission monitoring program of the radio loud AGN NGC 1052, we propose two 100 ksec Suzaku observations to obtain best-quality X-ray spectra at two epochs to determine the true continuum shape and thus probe the relativistic iron line, determine line and continuum variability patterns and possibly investigate how the structure of the accretion disk changes when there are jet ejection events. Our aim is to determine what leads supermassive black holes to launch powerful jets. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KIMBERLY WEAVER | USA | 2 | AO2 | PROBING THE DISK-JET CONNECTION IN AGN WITH AN INTENSIVE MULTIWAVELENGTH MONITORING CAMPAIGN OF NGC 1052 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702058010/ | Quick Look | ![]() |
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65 | Q1946+7658 | 296.1546 | 77.0965 | 296.596903 | 76.972833 | 64.242641 | 76.919523 | 109.22346589 | 23.50098326 | 3.7704 | 54294.4255902778 | 2007-07-13 10:12:51 | 54294.6432175926 | 2007-07-13 15:26:14 | 702060010 | 13.1636 | 13 | 13.1636 | 13.1636 | 0 | 13.1636 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.9282 | 13.9282 | 18.7759 | 0 | PROCESSED | 57539.2591782407 | 2016-05-31 06:13:13 | 54706 | 2008-08-28 00:00:00 | 54339.4067824074 | 2007-08-27 09:45:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021361 | The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | GEORGE CHARTAS | USA | 2 | AO2 | AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702060010/ | Quick Look | ![]() |
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66 | Q1334-0033 | 204.1954 | -0.819 | 203.55335 | -0.564423 | 202.702904 | 8.620784 | 326.07775276 | 59.99926461 | 306.9566 | 54295.3551736111 | 2007-07-14 08:31:27 | 54295.7084953704 | 2007-07-14 17:00:14 | 702067010 | 13.9621 | 15 | 13.9621 | 13.9621 | 0 | 13.9621 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.0064 | 13.0064 | 30.5199 | 0 | PROCESSED | 57539.262337963 | 2016-05-31 06:17:46 | 54710 | 2008-09-01 00:00:00 | 54340.4777430556 | 2007-08-28 11:27:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021361 | The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | GEORGE CHARTAS | USA | 2 | AO2 | AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702067010/ | Quick Look | ![]() |
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67 | Q1548+0917 | 237.6002 | 9.1581 | 236.997547 | 9.308492 | 232.970531 | 28.527987 | 18.5566992 | 44.16075413 | 106.1242 | 54513.4560763889 | 2008-02-17 10:56:45 | 54514.16 | 2008-02-18 03:50:24 | 702068010 | 32.1133 | 23 | 32.1213 | 32.1213 | 0 | 32.1133 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 29.4756 | 29.4756 | 60.8159 | 0 | PROCESSED | 57541.5745601852 | 2016-06-02 13:47:22 | 54889 | 2009-02-27 00:00:00 | 54522.1462731482 | 2008-02-26 03:30:38 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021361 | The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | GEORGE CHARTAS | USA | 2 | AO2 | AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702068010/ | Quick Look | ![]() |
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68 | MRK 417 | 162.3659 | 22.9016 | 161.688757 | 23.166381 | 154.921054 | 14.241178 | 214.84390845 | 62.11471123 | 281.9359 | 54238.6593402778 | 2007-05-18 15:49:27 | 54239.5730555556 | 2007-05-19 13:45:12 | 702078010 | 41.5066 | 40 | 41.5066 | 41.5066 | 0 | 41.5066 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.3385 | 39.3385 | 78.9239 | 0 | PROCESSED | 57538.6952662037 | 2016-05-30 16:41:11 | 54695 | 2008-08-17 00:00:00 | 54245.0002430556 | 2007-05-25 00:00:21 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021374 | Though Compton thick AGN are expected to constitute a sizable fraction of the Seyfert population (Maiolino et al 1998 and Risaliti et al 1999), the fraction and the signatures of Compton thick AGN is unknown. The SWIFT BAT all-sky AGN survey has detected a complete sample of AGN with flux > 1-3e-11 erg/cm^2/s in the 15-200 keV band. At this energy range, the effects of heavy obscuration are minimal and thus BAT will allow us to determine the true fraction of Compton-thick sources. However, the BAT spectra are not simultaneous with XRT and XRT does not have the spectral resolution (with 10 ks) necessary to characterize a heavily absorbed 0.3-10 keV spectrum. We propose HXD nominal Suzaku observations of 4 possible Compton thick sources for which we recently obtained XMM 10 ks follow-ups. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RICHARD MUSHOTZKY | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF POSSIBLY COMPTON THICK AGN FROM THE SWIFT BAT SURVEY | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702078010/ | Quick Look | ![]() |
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69 | NGC 1142 | 43.7827 | -0.1295 | 43.142852 | -0.331581 | 41.283841 | -16.101856 | 175.79604248 | -49.86350093 | 73.9096 | 54302.4506481482 | 2007-07-21 10:48:56 | 54303.4308333333 | 2007-07-22 10:20:24 | 702079010 | 40.5697 | 40 | 40.5697 | 40.5697 | 0 | 40.5697 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36.5404 | 36.5404 | 84.6799 | 1 | PROCESSED | 57539.2980902778 | 2016-05-31 07:09:15 | 54706 | 2008-08-28 00:00:00 | 54339.1106828704 | 2007-08-27 02:39:23 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021374 | Though Compton thick AGN are expected to constitute a sizable fraction of the Seyfert population (Maiolino et al 1998 and Risaliti et al 1999), the fraction and the signatures of Compton thick AGN is unknown. The SWIFT BAT all-sky AGN survey has detected a complete sample of AGN with flux > 1-3e-11 erg/cm^2/s in the 15-200 keV band. At this energy range, the effects of heavy obscuration are minimal and thus BAT will allow us to determine the true fraction of Compton-thick sources. However, the BAT spectra are not simultaneous with XRT and XRT does not have the spectral resolution (with 10 ks) necessary to characterize a heavily absorbed 0.3-10 keV spectrum. We propose HXD nominal Suzaku observations of 4 possible Compton thick sources for which we recently obtained XMM 10 ks follow-ups. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RICHARD MUSHOTZKY | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF POSSIBLY COMPTON THICK AGN FROM THE SWIFT BAT SURVEY | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702079010/ | Quick Look | ![]() |
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70 | MCG +04-48-002 | 307.1488 | 25.8021 | 306.615298 | 25.635019 | 318.241154 | 43.22286 | 67.06317106 | -7.53431612 | 93.9583 | 54208.4668634259 | 2007-04-18 11:12:17 | 54209.4134143518 | 2007-04-19 09:55:19 | 702081010 | 41.2988 | 40 | 41.3068 | 41.2988 | 0 | 41.3068 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.7466 | 37.7466 | 81.7699 | 2 | PROCESSED | 57538.398275463 | 2016-05-30 09:33:31 | 54695 | 2008-08-17 00:00:00 | 54217.0231712963 | 2007-04-27 00:33:22 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021374 | Though Compton thick AGN are expected to constitute a sizable fraction of the Seyfert population (Maiolino et al 1998 and Risaliti et al 1999), the fraction and the signatures of Compton thick AGN is unknown. The SWIFT BAT all-sky AGN survey has detected a complete sample of AGN with flux > 1-3e-11 erg/cm^2/s in the 15-200 keV band. At this energy range, the effects of heavy obscuration are minimal and thus BAT will allow us to determine the true fraction of Compton-thick sources. However, the BAT spectra are not simultaneous with XRT and XRT does not have the spectral resolution (with 10 ks) necessary to characterize a heavily absorbed 0.3-10 keV spectrum. We propose HXD nominal Suzaku observations of 4 possible Compton thick sources for which we recently obtained XMM 10 ks follow-ups. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RICHARD MUSHOTZKY | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF POSSIBLY COMPTON THICK AGN FROM THE SWIFT BAT SURVEY | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702081010/ | Quick Look | ![]() |
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71 | TYPE2AGN | 216.4026 | 35.2819 | 215.878545 | 35.506676 | 198.09088 | 46.269263 | 60.85487771 | 68.34395808 | 307.3753 | 54292.1781712963 | 2007-07-11 04:16:34 | 54292.6183333333 | 2007-07-11 14:50:24 | 702090010 | 19.8387 | 19 | 19.8467 | 19.8547 | 0 | 19.8387 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.87 | 20.87 | 38.0159 | 0 | PROCESSED | 57539.1533912037 | 2016-05-31 03:40:53 | 54706 | 2008-08-28 00:00:00 | 54339.0120833333 | 2007-08-27 00:17:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021376 | We propose to use Suzaku's large collecting area and excellent energy response to measure accurate X-ray spectra for 9 XBONGs and 8 luminous Type 2 AGN selected from very large samples of identified XBONGs and Type 2 AGN found in our Chandra XBootes survey. We have obtained optical spectra for 258 XBONGs and identified ~700 X-ray luminous Type 2 AGN at z>0.7. With known source positions and X-ray fluxes, we select sources that are relatively bright with little or no contamination from other X-ray sources. Thus we will measure individual spectra for these bright sources. We propose eight 15 ksec Suzaku XIS observations to measure the absorption in 8 luminous z > 0.8 Type 2 AGN and eight 10 ksec observations to measure the absorption and iron emission for nine XBONGs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | CHRISTINE JONES | USA | 2 | AO2 | OBSCURED AGN AND XBONGS IN BOOTES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702090010/ | Quick Look | ![]() |
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72 | IC4329A | 207.3319 | -30.3107 | 206.617741 | -30.062544 | 216.345447 | -17.778019 | 317.49747069 | 30.91844112 | 292.4395 | 54313.2280092593 | 2007-08-01 05:28:20 | 54314.0419444444 | 2007-08-02 01:00:24 | 702113010 | 25.4534 | 25 | 25.4534 | 25.4534 | 0 | 25.4534 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.4422 | 21.4422 | 70.292 | 1 | PROCESSED | 57539.3768287037 | 2016-05-31 09:02:38 | 54710 | 2008-09-01 00:00:00 | 54340.5826273148 | 2007-08-28 13:58:59 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022009 | IC 4329A is the brightest known Seyfert 1 galaxy between ~2-30 keV (F(2-10 keV)~1-2e-10 erg/cm2s). With its clear warm absorber and reflection component, it is often taken as the prototypical Sey 1 galaxy. Its X-ray variability is strong enough (and on a sufficiently long time scale, ideal for Suzaku) to make multiple observations critical for probing the origin of the Compton reflection component, and to attempt measuring variations of the high energy cut-off. We thus propose 5x20 ks observations to monitor i) the correlated variability of the reflection continuum plus FeK line to primary continuum variations, and ii) the variations in the high-E cut-off, and their relation with the power-law, and iii) check the evidence for a blueshifted (v~0.1c) FeK absorption line at ~7.7 keV. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MASSIMO CAPPI | EUR | 2 | AO2 | SUZAKU MULTIPLE OBSERVATIONS OF IC4329A TO PROBE THE ORIGIN OF THE COMPTON REFLECTION COMPONENT AND HIGH-ENERGY CUT-OFF | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702113010/ | Quick Look | ![]() |
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73 | IC4329A | 207.3317 | -30.3084 | 206.617549 | -30.060244 | 216.344382 | -17.775948 | 317.49797139 | 30.92070724 | 297.0437 | 54328.4922106482 | 2007-08-16 11:48:47 | 54329.1612731482 | 2007-08-17 03:52:14 | 702113040 | 24.2194 | 25 | 24.2194 | 24.2194 | 0 | 24.2194 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.2031 | 20.2031 | 57.8 | 1 | PROCESSED | 57539.604537037 | 2016-05-31 14:30:32 | 54730 | 2008-09-21 00:00:00 | 54351.1843171296 | 2007-09-08 04:25:25 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022009 | IC 4329A is the brightest known Seyfert 1 galaxy between ~2-30 keV (F(2-10 keV)~1-2e-10 erg/cm2s). With its clear warm absorber and reflection component, it is often taken as the prototypical Sey 1 galaxy. Its X-ray variability is strong enough (and on a sufficiently long time scale, ideal for Suzaku) to make multiple observations critical for probing the origin of the Compton reflection component, and to attempt measuring variations of the high energy cut-off. We thus propose 5x20 ks observations to monitor i) the correlated variability of the reflection continuum plus FeK line to primary continuum variations, and ii) the variations in the high-E cut-off, and their relation with the power-law, and iii) check the evidence for a blueshifted (v~0.1c) FeK absorption line at ~7.7 keV. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MASSIMO CAPPI | EUR | 2 | AO2 | SUZAKU MULTIPLE OBSERVATIONS OF IC4329A TO PROBE THE ORIGIN OF THE COMPTON REFLECTION COMPONENT AND HIGH-ENERGY CUT-OFF | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702113040/ | Quick Look | ![]() |
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74 | IRAS 10565+2448 | 164.8573 | 24.5988 | 164.182449 | 24.867063 | 156.396321 | 16.702388 | 212.34078465 | 64.72788111 | 119.4619 | 54410.6325 | 2007-11-06 15:10:48 | 54411.4675347222 | 2007-11-07 11:13:15 | 702115010 | 39.4232 | 30 | 39.4232 | 39.4232 | 0 | 39.4232 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.7388 | 35.7388 | 72.1459 | 0 | PROCESSED | 57540.4702893518 | 2016-06-01 11:17:13 | 54791 | 2008-11-21 00:00:00 | 54423.1618518518 | 2007-11-19 03:53:04 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022023 | We propose for 30ks Suzaku observations of two ultra-luminous infrared galaxies that lack sensitive 2keV constraints to provide a complete census of Active Galactic Nuclei (AGN) activity in ULIRGs out to 200Mpc. Six (~75%) of the eight ULIRGs in our sample for which we already have sensitive >2keV constraints host AGN activity, indicating that black-hole growth is ubiqitious in the most luminous local galaxies. Our proposed observations are sensitive enough to identify luminous AGN activity (L_X=3x10^{43} erg/s) out to ~40keV, to accurately quantify the properties of less luminous AGN activity, and to identify and quantify the star-formation activity. In addition the results will be used to better understand the z~2 ULIRG population, the likely progenitors of todays massive galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | DAVID ALEXANDER | EUR | 2 | AO2 | A COMPLETE CENSUS OF AGN ACTIVITY IN ULTRA-LUMINOUS GALAXIES OUT TO 200 MPC | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702115010/ | Quick Look | ![]() |
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75 | AKN 564 | 340.6246 | 29.7785 | 340.037211 | 29.516371 | 355.343017 | 34.767845 | 92.13720271 | -25.27363853 | 56.6178 | 54277.5375694444 | 2007-06-26 12:54:06 | 54279.8002199074 | 2007-06-28 19:12:19 | 702117010 | 99.9781 | 100 | 99.9861 | 99.9861 | 0 | 99.9781 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 87.2253 | 87.2253 | 195.4739 | 1 | PROCESSED | 57539.0843518518 | 2016-05-31 02:01:28 | 54703 | 2008-08-25 00:00:00 | 54333.5152199074 | 2007-08-21 12:21:55 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022024 | Narrow Line Seyfert 1 galaxies show complex X-ray behaviour. At low flux levels their 2-10~keV spectra are hard, with a huge excess at lower energies. Conversely, at high fluxes, the same objects show a soft 2-10 keV spectrum, with moderate soft excess. This behaviour can be explained either by reflection or absorption models. It is important to distinguish between these scenarios as they imply critical differences in the inferred physics of the accretion flow. There is already good Suzaku data on the hard 2-10 keV spectra from a GT observation of NGC4051. We propose to compare this with 100ks of data from Akn564, the brightest NLS1 at 10keV having a soft 2-10keV spectrum, so as to use the full range of spectral behaviour seen in NLS1's to determine the origin of the soft excess. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | CHRIS DONE | EUR | 2 | AO2 | UNDERSTANDING THE ORIGIN OF SPECTRAL COMPLEXITY IN NLS1: AKN564 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702117010/ | Quick Look | ![]() |
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76 | ESO 323-G032 | 193.3499 | -41.5832 | 192.653913 | -41.311875 | 210.129179 | -32.696187 | 303.32560645 | 21.28704922 | 104.5857 | 54456.5856481482 | 2007-12-22 14:03:20 | 54458.1459953704 | 2007-12-24 03:30:14 | 702119010 | 79.2494 | 80 | 80.8178 | 79.2494 | 0 | 80.8014 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86.8967 | 86.8967 | 134.7778 | 1 | PROCESSED | 57540.9568055556 | 2016-06-01 22:57:48 | 54854 | 2009-01-23 00:00:00 | 54483.1116203704 | 2008-01-18 02:40:44 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022033 | The high-energy detectors onboard Swift and INTEGRAL are mapping the hard (>10 keV) X-ray sky. Although limited to bright X-ray fluxes (~1e-11 erg/cm2/s), the large area surveyed so far has allowed to build up sizable samples of hard X-ray selected AGN almost unbiased against X-ray absorption. On the basis of a careful analysis of the available X-ray observations below 10 keV, we identified a sample of relatively bright AGN which are likely to be obscured by Compton-thick (logN_H >24) cold gas. Two of them were observed in EAO-1 and the results confirmed our predictions. We propose further Suzaku observations of 3 bright objects (F(20-40 keV) ~ 0.7-1.4 x 1e-11 erg/cm2/s) which will allow us to unveil previously unknown nearby heavily obscured AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ANDREA COMASTRI | EUR | 2 | AO2 | BRIGHT COMPTON-THICK GALAXIES IN THE BACKYARD - PART II | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702119010/ | Quick Look | ![]() |
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77 | PKS2126-15 | 322.2988 | -15.6437 | 321.609655 | -15.862975 | 319.629627 | -0.752825 | 35.92993079 | -41.86589251 | 72.3882 | 54576.0912384259 | 2008-04-20 02:11:23 | 54578.4238310185 | 2008-04-22 10:10:19 | 703001010 | 81.9214 | 80 | 81.9214 | 81.9364 | 0 | 81.9454 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71.5414 | 71.5414 | 201.5279 | 3 | PROCESSED | 57542.3941087963 | 2016-06-03 09:27:31 | 54961 | 2009-05-10 00:00:00 | 54594.3427777778 | 2008-05-08 08:13:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030003 | We propose intensive Suzaku observations (80ksec each) of two "primitive" blazars at z > 3.3, with a highly unusual SED. ROXA J081009.9 (z=4.0) was recently found by a short Swift/XRT exposure (6 ksec) with a luminosity well in excess of 10^47 ergs/s, but its synchrotron power peaking above 10 keV. This may suggest the bulk Lorentz factor of the jet could reach ~1000 like GRBs, though quite conspicuous among the AGN jets. Meanwhile, unusual SED of PKS2126-15 (z=3.3) , where the synchrotron peaking at GHz and the inverse Compton peaks at ~10 keV, is most likely due to the presence of ultra-massive black hole with 2x10^10 Ms. These new-types are only found in highly distant universe, and maybe categorized as primitive blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | JUN KATAOKA | JAP | 3 | AO3 | UNVEILING NEW-TYPE "PRIMITIVE" BLAZARS WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703001010/ | Quick Look | ![]() |
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78 | SWIFT J2009.0-6103 | 302.158 | -61.0495 | 301.087298 | -61.195509 | 289.575526 | -39.777943 | 335.84532046 | -32.77756596 | 73.0628 | 54563.6948148148 | 2008-04-07 16:40:32 | 54564.600775463 | 2008-04-08 14:25:07 | 703015010 | 43.7268 | 40 | 43.7268 | 43.7268 | 0 | 43.7268 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36.1996 | 36.1996 | 78.268 | 1 | PROCESSED | 57542.2661342593 | 2016-06-03 06:23:14 | 54953 | 2009-05-02 00:00:00 | 54580.2454976852 | 2008-04-24 05:53:31 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030045 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe the remaining four Compton thick AGN candidates in the 2nd BAT catalog with Suzaku to make it complete. To resolve the degeneracy of spectral modeling to the XMM spectra of these sources, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 3 | AO3 | DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703015010/ | Quick Look | ![]() |
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79 | NGC3227 | 155.8768 | 19.8688 | 155.194236 | 20.122176 | 150.387557 | 9.143202 | 216.98485011 | 55.4460253 | 111.8565 | 54790.7083333333 | 2008-11-20 17:00:00 | 54792.374525463 | 2008-11-22 08:59:19 | 703022040 | 64.5679 | 50 | 64.5759 | 64.5679 | 0 | 64.5759 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.622 | 46.622 | 143.9478 | 1 | PROCESSED | 57544.506412037 | 2016-06-05 12:09:14 | 54557 | 2008-04-01 00:00:00 | 54812.4380324074 | 2008-12-12 10:30:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031013 | We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARTIN ELVIS | USA | 3 | AO3 | NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703022040/ | Quick Look | ![]() |
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80 | NGC3227 | 155.8768 | 19.8687 | 155.194236 | 20.122076 | 150.387594 | 9.143109 | 216.98501654 | 55.44599229 | 109.926 | 54802.6028125 | 2008-12-02 14:28:03 | 54803.7231365741 | 2008-12-03 17:21:19 | 703022060 | 51.4105 | 50 | 51.4105 | 51.4105 | 0 | 51.4105 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.6836 | 39.6836 | 96.7818 | 1 | PROCESSED | 57544.6321875 | 2016-06-05 15:10:21 | 54557 | 2008-04-01 00:00:00 | 54812.4432407407 | 2008-12-12 10:38:16 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031013 | We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARTIN ELVIS | USA | 3 | AO3 | NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703022060/ | Quick Look | ![]() |
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81 | SN 2006JD | 120.5331 | 0.8102 | 119.888824 | 0.950282 | 122.553341 | -19.245849 | 220.45612728 | 16.05834455 | 284.354 | 54578.4377777778 | 2008-04-22 10:30:24 | 54579.6807175926 | 2008-04-23 16:20:14 | 703026010 | 54.1968 | 50 | 54.2048 | 54.1968 | 0 | 54.2048 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52.0488 | 52.0488 | 107.3398 | 1 | PROCESSED | 57542.379837963 | 2016-06-03 09:06:58 | 54957 | 2009-05-06 00:00:00 | 54588.1523611111 | 2008-05-02 03:39:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031241 | Supernovae (SNe) 2005kd and 2006jd are some of the brightest SNe ever detected in X-rays. The high X-ray luminosities (>E41 erg/s) are the results of the SN shock interacting with dense material in the environment of the SNe. We propose one Suzaku observation of each SN to obtain high-quality spectra that will be used to measure the temperature of the forward and reverse shock and to establish the rate of decline in comparison with existing Swift, Chandra and XMM-Newton data. The data will further be used to measure the circumstellar matter density and mass-loss rate of the progenitors to probe the nature of the SN progenitors. Our science objectives rely on Suzaku's uniqueness, i.e. the large collecting area, good spectral resolution, and the high sensitivity in the hard X-ray band. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | STEFAN IMMLER | USA | 3 | AO3 | SUZAKU OBSERVATIONS OF X-RAY BRIGHT SUPERNOVAE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703026010/ | Quick Look | ![]() |
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82 | ESO 103- G 035 | 279.5941 | -65.4238 | 278.351287 | -65.467222 | 275.354112 | -42.161198 | 329.78379096 | -23.17817546 | 291.5832 | 54761.6331597222 | 2008-10-22 15:11:45 | 54764.1717476852 | 2008-10-25 04:07:19 | 703031010 | 91.442 | 80 | 91.442 | 91.45 | 0 | 91.45 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81.0096 | 81.0096 | 219.282 | 2 | PROCESSED | 57544.3339467593 | 2016-06-05 08:00:53 | 55148 | 2009-11-13 00:00:00 | 54782.4220023148 | 2008-11-12 10:07:41 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031322 | X-ray observations of Seyfert 2 have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by the AGN Unification Scheme. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (80 ksec each) of three bright Compton-thin Seyfert 2 galaxies, selected from the Swift/BAT survey, with a hard X-ray flux exceeding 9e-11cgs, to form a flux-limited sample. The unprecedented bandpass of Suzaku offers a unique tool to investigate the X-ray emission of these sources, allowing us to put strong constraints on the reprocessing matter in Seyfert 2s. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | VALENTINA BRAITO | USA | 3 | AO3 | THE NATURE OF THE X-RAY ABSORBER IN SEYFERT 2 GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703031010/ | Quick Look | ![]() |
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83 | Q0551-3637 | 88.2027 | -36.6207 | 87.768974 | -36.630505 | 87.117827 | -60.044705 | 242.37463259 | -26.91966553 | 321.5977 | 54600.5596643518 | 2008-05-14 13:25:55 | 54601.2044444444 | 2008-05-15 04:54:24 | 703036020 | 21.6143 | 22 | 21.6143 | 21.6143 | 0 | 21.6183 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.2831 | 18.2831 | 55.684 | 1 | PROCESSED | 57542.5389236111 | 2016-06-03 12:56:03 | 54979 | 2009-05-28 00:00:00 | 54613.0157060185 | 2008-05-27 00:22:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031334 | Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GEORGE CHARTAS | USA | 3 | AO3 | A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703036020/ | Quick Look | ![]() |
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84 | Q0329-385 | 52.7815 | -38.4067 | 52.316664 | -38.576045 | 34.470474 | -54.910107 | 241.941352 | -54.89845774 | 23.7676 | 54633.4249421296 | 2008-06-16 10:11:55 | 54634.1898611111 | 2008-06-17 04:33:24 | 703038010 | 30.203 | 29 | 30.219 | 30.203 | 0 | 30.219 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.2925 | 25.2925 | 66.082 | 1 | PROCESSED | 57542.8370601852 | 2016-06-03 20:05:22 | 55010 | 2009-06-28 00:00:00 | 54644.1762615741 | 2008-06-27 04:13:49 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031334 | Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GEORGE CHARTAS | USA | 3 | AO3 | A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703038010/ | Quick Look | ![]() |
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85 | 1ES1426+428 | 217.0602 | 42.6327 | 216.573667 | 42.855515 | 193.163684 | 52.913705 | 77.47261603 | 64.96709047 | 324.5702 | 54622.8702662037 | 2008-06-05 20:53:11 | 54625.0856944444 | 2008-06-08 02:03:24 | 703063010 | 101.1662 | 100 | 101.1662 | 101.1742 | 0 | 101.1742 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92.1456 | 92.1456 | 191.3937 | 3 | PROCESSED | 57542.7937731482 | 2016-06-03 19:03:02 | 55003 | 2009-06-21 00:00:00 | 54636.5084953704 | 2008-06-19 12:12:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032021 | Simultaneous optical/UV, X-ray and TeV observations are a powerful tool to study the innermost regions of blazar jets, probing the physical state of the jet close to its base. We propose to perform a long SUZAKU observation of the extreme hard-X-ray blazar 1ES 1426+428, simultaneously with MAGIC TeV observations, combined with a series of short Swift observations. With SUZAKU we will study the evolution of the X-ray emission over timescales of minutes-hours, providing important insight into the structure of the emission region and the physical process producing the radiation. We will characterize the synchrotron part of the SED and see how it correlates with the TeV spectrum, disentangling the main physical parameters and probing the still poorly known cosmic IR background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GIANPIERO TAGLIAFERRI | EUR | 3 | AO3 | THE EXTREME BLAZAR 1ES 1426+428: TESTING THE JET | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703063010/ | Quick Look | ![]() |
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86 | 1739+518 | 264.9784 | 52.1719 | 264.694846 | 52.196929 | 257.680013 | 75.396251 | 79.52646168 | 31.85370007 | 22.9152 | 54985.7571759259 | 2009-06-03 18:10:20 | 54986.3641087963 | 2009-06-04 08:44:19 | 704008010 | 22.4868 | 20 | 22.4948 | 22.4948 | 0 | 22.4868 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.2378 | 28.2378 | 52.4319 | 0 | PROCESSED | 57547.4536458333 | 2016-06-08 10:53:15 | 55367 | 2010-06-20 00:00:00 | 54998.1968634259 | 2009-06-16 04:43:29 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040049 | We propose the first X-ray follow-up observations of 4 gamma-ray bright Seyferts and starburst galaxy, recently discovered by Fermi gamma-ray space telescope. The detection of GeV emission provides new evidence for relativistic jets in radio-quiet AGNs, but steep gamma-ray spectrum as well as an exotic spectral energy distribution (where GeV flux is 2-4 orders of magnitude brighter than radio) indicates that non-thermal emission is relatively weak, and less enhanced compared to radio-loud AGNs. Throughout multiwavelength observations including Suzaku and Fermi satellites, we will investigate the jet power, accretion rate and line intensity of these new comers (i.e., gamma-loud Seyferts) towards the unification scheme of radio-loud and radio-quiet AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF GAMMA-LOUD SEYFERTS AND STARBURST GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704008010/ | Quick Look | ![]() |
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87 | CENTAURUS_A | 201.3322 | -43.0688 | 200.598815 | -42.808768 | 217.137097 | -31.383435 | 309.48334217 | 19.37141452 | 298.7164 | 55048.3079513889 | 2009-08-05 07:23:27 | 55049.7029398148 | 2009-08-06 16:52:14 | 704018020 | 51.2787 | 50 | 51.2787 | 51.2947 | 0 | 51.2867 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.7332 | 43.7332 | 120.5059 | 1 | PROCESSED | 57548.0839699074 | 2016-06-09 02:00:55 | 55430 | 2010-08-22 00:00:00 | 55062.3520023148 | 2009-08-19 08:26:53 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040085 | We propose to observe a nearby radio galaxy Centaurus A (Cen A) in order to search for non-thermal X-ray emission associated with a mis-alighned jet. Recently TeV gamma-ray was detected from M87 and nonthermal X-ray emission was detected from 3C120 with Suzaku, where they are not a blazar and harbor a mis-alighned jet. COMPTEL and EGRET reported a hint of gamma-ray emission from Cen A, but it has not been established. So far, only Seyfert-like thermal-Compoton powerlaw has been detected from Cen A. By taking advantage of Suzaku capability, we study a temporal spectral variation to extract nonthermal emission by considering a different variability time scale of accretion disk component and jet one, as demonstrated for 3C120 with Suzaku. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YASUSHI FUKAZAWA | JAP | 4 | AO4 | SEARCH FOR NON-THERMAL X-RAY EMISSION FROM A NEARBY RADIO GALAXY CENTAURUS A | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704018020/ | Quick Look | ![]() |
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88 | ESO 548-G081 | 55.4927 | -21.1949 | 54.941134 | -21.353755 | 46.730142 | -39.596754 | 213.74761618 | -50.8353425 | 69.3236 | 55046.3350462963 | 2009-08-03 08:02:28 | 55047.1946064815 | 2009-08-04 04:40:14 | 704026010 | 39.4112 | 40 | 39.4192 | 39.4192 | 0 | 39.4112 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36.1429 | 36.1429 | 74.2599 | 0 | PROCESSED | 57548.0531481482 | 2016-06-09 01:16:32 | 55427 | 2010-08-19 00:00:00 | 55060.8071875 | 2009-08-17 19:22:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041402 | The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | LISA WINTER | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704026010/ | Quick Look | ![]() |
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89 | MCG +04-22-042 | 140.9461 | 22.9693 | 140.230202 | 23.184366 | 136.125191 | 7.311314 | 205.9821846 | 43.11036681 | 106.3587 | 55157.3309259259 | 2009-11-22 07:56:32 | 55158.2634143518 | 2009-11-23 06:19:19 | 704028010 | 40.962 | 40 | 40.994 | 40.962 | 0 | 40.986 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 35.8969 | 35.8969 | 80.5599 | 0 | PROCESSED | 57549.5187384259 | 2016-06-10 12:26:59 | 55542 | 2010-12-12 00:00:00 | 55176.1858101852 | 2009-12-11 04:27:34 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041402 | The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | LISA WINTER | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704028010/ | Quick Look | ![]() |
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90 | 1H0323+342 | 51.1507 | 34.2411 | 50.363828 | 34.065013 | 57.518057 | 15.07869 | 155.67406743 | -18.71640786 | 76.7168 | 55038.1604513889 | 2009-07-26 03:51:03 | 55040.2084722222 | 2009-07-28 05:00:12 | 704034010 | 84.0884 | 80 | 84.0884 | 84.2404 | 0 | 84.3524 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74.2979 | 74.2979 | 176.9379 | 0 | PROCESSED | 57548.0010532407 | 2016-06-09 00:01:31 | 55419 | 2010-08-11 00:00:00 | 55050.8162847222 | 2009-08-07 19:35:27 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041408 | Recent radio observations reveal blazar-like properties in some radio-loud narrow line Seyfert-1 AGNs. 1H0323+342, classified as this class of AGNs, shows prominent hard X-ray emission with a hard photon index. Since the spectrum in hard X-ray is reminiscent of blazar, its X-ray spectrum seems to have different components originated from disk and jet. Thanks to sensitive X-ray detectors extending to the hard X-ray band, Suzaku observation is expected to resolve a possible multi-component structure in the spectrum. Since beamed radiation from jet is highly variable, spectral temporal behavior is also vital information to distinguish the emission origin. As this source is located relatively nearby (z=0.061), the source is an excellent target to investigate the emission from disk and jet. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MASAAKI HAYASHIDA | USA | 4 | AO4 | SUZAKU OBSERVATION OF 1H0323+342: A PECULIAR SEYFERT-1 --PROBING THE DISK AND JET CONNECTION IN AGN-- | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704034010/ | Quick Look | ![]() |
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91 | MCG0208 | 43.0963 | -8.5129 | 42.484335 | -8.717227 | 37.842662 | -23.868775 | 185.55840319 | -55.88722126 | 57.4541 | 55016.0987037037 | 2009-07-04 02:22:08 | 55017.2134722222 | 2009-07-05 05:07:24 | 704045010 | 42.9115 | 40 | 42.9435 | 42.9115 | 0 | 42.9195 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36.7878 | 36.7878 | 96.286 | 5 | PROCESSED | 57547.7724768518 | 2016-06-08 18:32:22 | 55395 | 2010-07-18 00:00:00 | 55027.1160532407 | 2009-07-15 02:47:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041414 | We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | EZEQUIEL TREISTER | USA | 4 | AO4 | THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704045010/ | Quick Look | ![]() |
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92 | SDSS J1352+4239 | 208.1832 | 42.6476 | 207.663098 | 42.893525 | 184.337785 | 49.439251 | 88.11360974 | 70.09649039 | 316.6443 | 54984.9959375 | 2009-06-02 23:54:09 | 54985.7502199074 | 2009-06-03 18:00:19 | 704050010 | 32.0745 | 30 | 32.0825 | 32.0745 | 0 | 32.0825 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29.5021 | 29.5021 | 65.1639 | 0 | PROCESSED | 57547.4324652778 | 2016-06-08 10:22:45 | 55364 | 2010-06-17 00:00:00 | 54994.4273032407 | 2009-06-12 10:15:19 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041422 | BALQSOs can be used to probe geometric and evolutionary models of quasars and AGN feedback. Recent studies have found larger (~2X) BALQSO fractions in NIR selected samples compared to those in optical samples and have suggested that the NIR samples of BALQSOs better represent the general population of BALQSOs. We propose to observe three bright, red 2MASS selected BALQSOs with Suzaku, to complement archival X-ray observations of BALQSOs that may have been biased by their selection on optical properties only. Combined with the archival sample, we will measure the average X-ray properties of BALQSOs. By comparing the hard X-ray to K_s band flux ratios at a range of optical to infrared colors, we will test the robustness of NIR selection and the origin of the large NIR BALQSO fraction. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | XINYU DAI | USA | 4 | AO4 | X-RAY PROPERTIES OF 2MASS SELECTED BALQSOS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704050010/ | Quick Look | ![]() |
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93 | SDSS J0943+5417 | 145.8252 | 54.2751 | 144.963883 | 54.504193 | 127.754031 | 37.9036 | 161.23003018 | 46.41565232 | 274.2141 | 54975.5889236111 | 2009-05-24 14:08:03 | 54976.3473611111 | 2009-05-25 08:20:12 | 704052010 | 34.2264 | 30 | 34.2264 | 34.2264 | 0 | 34.2264 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.0591 | 32.0591 | 65.5179 | 2 | PROCESSED | 57546.6638773148 | 2016-06-07 15:55:59 | 55358 | 2010-06-11 00:00:00 | 54992.6588888889 | 2009-06-10 15:48:48 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041422 | BALQSOs can be used to probe geometric and evolutionary models of quasars and AGN feedback. Recent studies have found larger (~2X) BALQSO fractions in NIR selected samples compared to those in optical samples and have suggested that the NIR samples of BALQSOs better represent the general population of BALQSOs. We propose to observe three bright, red 2MASS selected BALQSOs with Suzaku, to complement archival X-ray observations of BALQSOs that may have been biased by their selection on optical properties only. Combined with the archival sample, we will measure the average X-ray properties of BALQSOs. By comparing the hard X-ray to K_s band flux ratios at a range of optical to infrared colors, we will test the robustness of NIR selection and the origin of the large NIR BALQSO fraction. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | XINYU DAI | USA | 4 | AO4 | X-RAY PROPERTIES OF 2MASS SELECTED BALQSOS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704052010/ | Quick Look | ![]() |
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94 | MR 2251-178 | 343.5217 | -17.5814 | 342.855263 | -17.84794 | 338.051604 | -9.763358 | 46.19628588 | -61.32288878 | 63.4108 | 54958.1447222222 | 2009-05-07 03:28:24 | 54961.4675231482 | 2009-05-10 11:13:14 | 704055010 | 136.924 | 130 | 136.932 | 136.924 | 0 | 136.9399 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 112.1637 | 112.1637 | 287.0576 | 2 | PROCESSED | 57546.6278009259 | 2016-06-07 15:04:02 | 55343 | 2010-05-27 00:00:00 | 54976.3091782407 | 2009-05-25 07:25:13 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042002 | The bright, nearby (z=0.06398) QSO MR 2251-178 was the first AGN where a warm absorber was detected. There are now thought to be at least two warm absorber components in MR 2251-178; a low ionisation soft X-ray absorber and a putative high velocity (13000 km/s) high ionisation wind, which exhibits absorption lines in the iron K-shell band. We propose a 130 ks observation with Suzaku of MR 2251-178 with the primary goals; (i) to establish the nature of the high ionisation absorber, e.g. an accretion disk wind, through unprecedented high S/N observations in the iron K band with XIS; (ii) to determine the physical parameters of the soft X-ray warm absorber and (iii) to characterise the ionised reflection component and high-energy cut-off thanks to the high energy sensitivity of the HXD. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JAMES REEVES | YASUSHI FUKAZAWA | EUR | 4 | AO4 | PROBING THE OUTFLOWING WIND IN MR 2251-178 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704055010/ | Quick Look | ![]() |
95 | IRAS 04507+0358 | 73.3635 | 4.1233 | 72.703908 | 4.042054 | 72.49644 | -18.313087 | 194.58361833 | -23.84576016 | 98.871 | 55075.0228356482 | 2009-09-01 00:32:53 | 55078.1356481482 | 2009-09-04 03:15:20 | 704058010 | 109.0524 | 100 | 109.0524 | 109.0524 | 0 | 109.0524 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 84.1098 | 84.1098 | 268.9118 | 3 | PROCESSED | 57548.5242939815 | 2016-06-09 12:34:59 | 55476 | 2010-10-07 00:00:00 | 55109.5623842593 | 2009-10-05 13:29:50 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042022 | According to X-ray synthesis models, Compton-thick AGN (NH>1e24 cm-2) should represent 50% of the total absorbed AGN population. Despite their importance in the cosmological context, only a few of them have been found so far. We have selected a well-defined sample of 31 Compton-thick candidates on the basis on their FX/FIR and X-ray colors. Due to the heavy obscuration, data above 10 keV are fundamental to unveil these sources. We ask here deep Suzaku observations (100 ks on each source) for 2 sources of our sample for which data at energy >10keV are not available yet. These observations will allow to complete the physical characterization (NH and LX) of the bright tail (F(2-10 keV)>5e-12 cgs) of our sample and to add more information to test the prediction of the AGN synthesis model. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | PAOLA SEVERGNINI | EUR | 4 | AO4 | SUZAKU OBSERVATIONS OF COMPTON-THICK CANDIDATES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704058010/ | Quick Look | ![]() |
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96 | IGR J22517+2218 | 342.9769 | 22.2871 | 342.369941 | 22.021351 | 353.695074 | 27.113044 | 89.68946946 | -32.75751552 | 253.7359 | 55161.7610648148 | 2009-11-26 18:15:56 | 55163.0086111111 | 2009-11-28 00:12:24 | 704060010 | 52.7265 | 50 | 52.7265 | 52.7265 | 0 | 52.7265 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.1164 | 40.1164 | 107.7779 | 0 | PROCESSED | 57549.6312152778 | 2016-06-10 15:08:57 | 55545 | 2010-12-15 00:00:00 | 55179.2471527778 | 2009-12-14 05:55:54 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042027 | We propose to observe 4 high-z QSOs observed by INTEGRAL, two of which are newly discovered in hard X-rays. The broadband and the good energy resolution will allow to investigate the spectral behaviour at low energies, and in particular to constraint true absorption $vs$ continuum features scenario. Particularly intriguing is the possible presence of a bulk Compton motion component. A self consistent test of this model could be derived by measuring the peak energy of the Inverse Compton component in the SED, a requirement that further strenghtens the need of a broadband observation with Suzaku. Simultaneous optical, hard X and gamma-ray observations available through WEBT, INTEGRAL and AGILE will also improve the feasibility of the proposed program. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | ALESSANDRA DE ROSA | EUR | 4 | AO4 | SUZAKU OBSERVATION A SAMPLE OF FOUR RADIO-LOUD/HIGH REDSHIFT QSOS OBSERVED BY INTEGRAL | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704060010/ | Quick Look | ![]() |
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97 | 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 | ![]() |
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98 | PBC J0216.1+5124 | 34.0954 | 51.5104 | 33.261431 | 51.278784 | 50.779826 | 35.406451 | 136.13174863 | -9.17115539 | 78.3815 | 55421.9728356482 | 2010-08-13 23:20:53 | 55423.4168171296 | 2010-08-15 10:00:13 | 705006010 | 72.7733 | 80 | 72.7964 | 72.7733 | 0 | 72.7964 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 73.5582 | 73.5582 | 124.7258 | 3 | PROCESSED | 57553.114375 | 2016-06-14 02:44:42 | 55804 | 2011-08-31 00:00:00 | 55435.2980092593 | 2010-08-27 07:09:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050024 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Previously, such studies have been limited to AGNs with low to intermediate luminosities. Here we propose to observe two of the most luminous AGNs in the latest BAT catalog to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 5 | AO5 | BROAD BAND SPECTRA OF SWIFT/BAT SELECTED ULTRALUMINOUS AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705006010/ | Quick Look | ![]() |
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99 | EMS1164 | 265.9438 | -76.3446 | 264.162094 | -76.320567 | 268.39939 | -52.925114 | 317.07818058 | -22.45515073 | 114.3984 | 55300.0111689815 | 2010-04-14 00:16:05 | 55300.6980439815 | 2010-04-14 16:45:11 | 705013010 | 42.3783 | 40 | 42.3836 | 42.3783 | 0 | 42.389 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.0487 | 39.0487 | 59.3439 | 1 | PROCESSED | 57551.2223958333 | 2016-06-12 05:20:15 | 55675 | 2011-04-24 00:00:00 | 55309.1947453704 | 2010-04-23 04:40:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050050 | We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 5 | AO5 | SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705013010/ | Quick Look | ![]() |
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100 | EMS1395 | 310.8148 | 17.1786 | 310.239098 | 16.997696 | 318.830842 | 33.961912 | 61.89528011 | -15.30299533 | 74.9546 | 55319.8076736111 | 2010-05-03 19:23:03 | 55320.4342476852 | 2010-05-04 10:25:19 | 705015010 | 23.3002 | 20 | 23.3002 | 23.3002 | 0 | 23.3002 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.4944 | 19.4944 | 54.1299 | 0 | PROCESSED | 57551.3813773148 | 2016-06-12 09:09:11 | 55696 | 2011-05-15 00:00:00 | 55330.2005208333 | 2010-05-14 04:48:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050050 | We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 5 | AO5 | SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705015010/ | Quick Look | ![]() |
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101 | MRK 509 | 311.0469 | -10.7401 | 310.365769 | -10.921688 | 310.545768 | 7.110758 | 35.95684044 | -29.86794514 | 252.3716 | 55521.595625 | 2010-11-21 14:17:42 | 55523.8155092593 | 2010-11-23 19:34:20 | 705025010 | 102.1205 | 100 | 102.1285 | 102.1285 | 0 | 102.1205 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92.0625 | 92.0625 | 191.7697 | 0 | PROCESSED | 57554.2039930556 | 2016-06-15 04:53:45 | 55916 | 2011-12-21 00:00:00 | 55550.2628356482 | 2010-12-20 06:18:29 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050113 | We propose the observation of one of the typical Seyferts I Mrk 509 for 100 ksec to understand how a vry hard component component that varies independently of power-law is created and how the physical structure near SMBH in Seyferts is. The hard component has been found by carrying out timing analysis of hard X-ray band to explain the extremely broad iron line feature of several Seyferts. Taking this component into account, we succeeded to explain the data of MCG 6-30-15 without the extremely broad iron line, though the origin of this component has not been identified yet. Because Mrk 509 has strong flux and large amplitude of hard X-ray variation, we found it is the most suitable object to verify this component and to get alternative interpretation to the extremely broad iron line. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | HIROFUMI NODA | JAP | 5 | AO5 | VERIFICATION OF A HARD COMPONENT THAT VARIES INDEPENDENTLY OF POWER-LAW IN TYPE I SEYFERT MRK 509 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705025010/ | Quick Look | ![]() |
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102 | CEN A S LOBE NO. 2 | 200.3949 | -45.1401 | 199.658837 | -44.878468 | 217.502785 | -33.539168 | 308.49497877 | 17.40582221 | 289.0008 | 55419.7766087963 | 2010-08-11 18:38:19 | 55420.9641087963 | 2010-08-12 23:08:19 | 705033010 | 81.3878 | 80 | 81.3958 | 81.3878 | 0 | 81.4038 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 68.1085 | 68.1085 | 102.5858 | 0 | PROCESSED | 57552.9708564815 | 2016-06-13 23:18:02 | 55812 | 2011-09-08 00:00:00 | 55445.267662037 | 2010-09-06 06:25:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051401 | We propose a set of four pointings (200 ks), to study the X-ray emission from the Southern giant lobe of the radio galaxy Cen A. Those lobes clearly separated from the central source, have been detected as a source of diffuse gamma-ray emission by the Fermi Telescope. The goal of the Suzaku observations is two-fold: first, to measure the diffuse component of the non-thermal X-ray emission with both the XIS and the HXD in order to determine the details of the distribution of the radiating relativistic particles (and B field), and second, to measure the thermal emission from the lobes (using primarily the XIS), to determine temperature and density of the X-ray emitting plasma, which, via consideration of pressure balance, will determine the content of energetic protons (cosmic rays). | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GRZEGORZ MADEJSKI | USA | 5 | AO5 | SUZAKU OBSERVATIONS OF THE SOUTHERN LOBE OF CEN A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705033010/ | Quick Look | ![]() |
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103 | 1RXS J111706.3+20141 | 169.2749 | 20.2432 | 168.614437 | 20.516401 | 162.09404 | 14.35752 | 225.56577108 | 67.37465885 | 120.2309 | 55510.3081944444 | 2010-11-10 07:23:48 | 55511.1543402778 | 2010-11-11 03:42:15 | 705036010 | 34.2125 | 32 | 34.2125 | 34.2125 | 0 | 34.2125 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31.5366 | 31.5366 | 73.0979 | 0 | PROCESSED | 57554.0402199074 | 2016-06-15 00:57:55 | 55903 | 2011-12-08 00:00:00 | 55537.0979050926 | 2010-12-07 02:20:59 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051402 | High frequency peaked BL Lacs are a peculiar subclass of Blazars characterized by non-thermal emission across the whole electromagnetic spectrum. Their spectral energy distributions (SEDs) include two main components: a low-energy component with power peaking in the range from the UV to the X-ray band, and a substantial high-energy component often dominated by gamma-rays. We propose 3 observations (32 ks each) of a selected sample of HBLs to study the behavior of the first component, widely interpreted as synchrotron radiation. First, we will be able to disentangle between different spectral shapes of the synchrotron SED of HBLs. Second, we will use the proposed observations to investigate the properties of the most representative sample of TeV candidate HBLs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | FRANCESCO MASSARO | USA | 5 | AO5 | X-RAY CURVED SPECTRA IN HIGH FREQUENCY PEAKED BL LACS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705036010/ | Quick Look | ![]() |
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104 | 3C111 | 64.5838 | 38.0329 | 63.747646 | 37.911608 | 69.36811 | 16.396021 | 161.66828978 | -8.81804056 | 76.1726 | 55453.9599768518 | 2010-09-14 23:02:22 | 55455.7432986111 | 2010-09-16 17:50:21 | 705040030 | 80.3659 | 80 | 80.3819 | 80.3659 | 0 | 80.3819 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.9533 | 70.9533 | 154.0639 | 2 | PROCESSED | 57553.468599537 | 2016-06-14 11:14:47 | 55835 | 2011-10-01 00:00:00 | 55469.3718287037 | 2010-09-30 08:55:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051412 | Using our Suzaku observations we discovered ultra-fast outflows (UFOs) in radio-loud Broad-Line Radio Galaxies, with velocities v/c~0.04--0.15 and carrying a mass of the same order as the accretion mass. The bright BLRG 3C~111 was selected for an in-depth study of its UFO through its predicted variability on timescales of approximately one week. We propose 3 Suzaku pointings of 80~ks each separated by one week to determine the gas geometrical, physical, and dynamical characteristics and start addressing its role for the jet-disk connection in radio-loud AGN. Additionally, we will obtain a simultaneous radio-to-GeV Spectral Energy Distribution and model the relative contributions of the accretion and non-thermal components. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RITA SAMBRUNA | USA | 5 | AO5 | PROBING THE ULTRA-FAST OUTFLOW IN 3C 111 WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705040030/ | Quick Look | ![]() |
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105 | MKN 590 | 33.6477 | -0.7713 | 33.009436 | -1.003927 | 31.140057 | -13.460103 | 163.51612886 | -56.94122484 | 251.1273 | 55587.0949652778 | 2011-01-26 02:16:45 | 55588.2146990741 | 2011-01-27 05:09:10 | 705043020 | 40.9139 | 150 | 40.9219 | 40.9219 | 0 | 40.9139 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.8699 | 37.8699 | 96.7339 | 1 | PROCESSED | 57600.7810763889 | 2016-07-31 18:44:45 | 55988 | 2012-03-02 00:00:00 | 55621.2137731482 | 2011-03-01 05:07:50 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051433 | We propose a 150 ks Suzaku long-look to study the Compton reflection component, soft excess, ionized emission and possible ionized reflection of the Seyfert 1.2 AGN Mkn 590, which has an unobscured line of sight or "bare nucleus" and as of yet unquantified reflection. We aim to accurately constrain the geometry of the circumnuclear material and determine the ionization states of both the Compton-thin and Compton-thick material surrounding the black hole by studying the origin of the soft excess, determining the likelihood of ionized reflection and accurately measuring the intensity of neutral, H-like and He-like Fe emission lines. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | ELIZABETH RIVERS | USA | 5 | AO5 | QUANTIFYING THE COMPTON REFLECTION AND IONIZED EMISSION IN MKN 590 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705043020/ | Quick Look | ![]() |
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106 | NGC 4945 | 196.3636 | -49.4659 | 195.633608 | -49.198211 | 217.017818 | -38.639251 | 305.27160994 | 13.34216317 | 120.2557 | 55590.0873842593 | 2011-01-29 02:05:50 | 55591.1182175926 | 2011-01-30 02:50:14 | 705047050 | 46.1076 | 40 | 46.1076 | 46.1076 | 0 | 46.1076 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54.0907 | 54.0907 | 89.0518 | 0 | PROCESSED | 57600.8100810185 | 2016-07-31 19:26:31 | 55969 | 2012-02-12 00:00:00 | 55602.2238194445 | 2011-02-10 05:22:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051442 | We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GUIDO RISALITI | USA | 5 | AO5 | HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705047050/ | Quick Look | ![]() |
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107 | SWIFTJ2344.6-424322 | 356.1059 | -42.7624 | 355.44614 | -43.040118 | 336.666972 | -37.094539 | 339.65324523 | -69.27134863 | 225.0657 | 55505.2812731482 | 2010-11-05 06:45:02 | 55506.5570601852 | 2010-11-06 13:22:10 | 705049010 | 61.7416 | 60 | 61.7416 | 61.7416 | 0 | 61.7416 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50.3941 | 50.3941 | 110.2118 | 1 | PROCESSED | 57553.9985532407 | 2016-06-14 23:57:55 | 55885 | 2011-11-20 00:00:00 | 55518.3162847222 | 2010-11-18 07:35:27 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051443 | We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195 keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log(L_x) > 45.5 erg/sec) absorbed type II QSOs in the local universe and the most ripe for study with Suzaku. The newly discovered source SWIFT J2344.6-4233 at a redshift of z=0.6 is the most luminous object in the BAT sample with log(L_x) = 46.5 erg/sec. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | WAYNE BAUMGARTNER | USA | 5 | AO5 | SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705049010/ | Quick Look | ![]() |
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108 | MCG-03-58-007 | 342.3795 | -19.2152 | 341.708645 | -19.480081 | 336.393592 | -10.851288 | 42.20057234 | -60.96689333 | 68.5139 | 55350.7016203704 | 2010-06-03 16:50:20 | 55352.8940046296 | 2010-06-05 21:27:22 | 705052010 | 99.0873 | 100 | 99.0873 | 99.0873 | 0 | 99.0873 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81.42 | 81.42 | 189.406 | 1 | PROCESSED | 57551.8454513889 | 2016-06-12 20:17:27 | 55734 | 2011-06-22 00:00:00 | 55365.563912037 | 2010-06-18 13:32:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052011 | Despite their relevance, less than two dozens of confirmed Compton-thick (CT) AGN have been found so far. We have recently selected a well defined sample of CT AGN candidates using FX/Fir ratios and X-ray colors. Due to their heavy obscuration, good statistics at 6.4 keV and data above 10 keV are needed to assess the real nature of these sources. We propose deep Suzaku observations (100 and 150 ks) for two sources for which data above 10 keV are not available and the quality of XMM data is poor. This request is a continuation of an approved AO4 proposal. These observations will allow us to possibly unveil two more examples of CT AGN, provide a physical characterization of the relatively bright tail of our sample, and estimate the efficiency of our method in selecting CT AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | PAOLA SEVERGNINI | EUR | 5 | AO5 | SUZAKU OBSERVATIONS OF TWO COMPTON-THICK CANDIDATES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705052010/ | Quick Look | ![]() |
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109 | CENTAURUS B | 206.7018 | -60.4061 | 205.845186 | -60.15638 | 231.230588 | -45.191821 | 309.72060452 | 1.73379394 | 97.6796 | 55572.6060763889 | 2011-01-11 14:32:45 | 55572.7919444444 | 2011-01-11 19:00:24 | 705059010 | 8.7611 | 10 | 8.7691 | 8.7691 | 0 | 8.7611 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6.4526 | 6.4526 | 16.0559 | 0 | PROCESSED | 57600.577650463 | 2016-07-31 13:51:49 | 55962 | 2012-02-05 00:00:00 | 55595.2069675926 | 2011-02-03 04:58:02 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052018 | We propose a 100 ks Suzaku observation of 4U 1344-60, a poorly studied (because at low Galactic latitude) but bright (about 2 millicrabs) AGN which showed, in an XMM-Newton observation, a strong relativistic disk iron line. The main aim of the proposal is to determine in detail the parameters of the disk, which is possible only with a high quality broad band observation which permits to control the continuum beneath the line. Presently, only Suzaku has the right combination of sensitivity, energy resolution and broad band coverage to achieve this objective. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | JIRI SVOBODA | EUR | 5 | AO5 | 4U 1344-60: A BRIGHT AGN WITH A STRONG RELATIVISTIC IRON LINE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705059010/ | Quick Look | ![]() |
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110 | 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 | ![]() |
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111 | NGC6251_LOBE_BGD2 | 245.2973 | 82.3586 | 246.565183 | 82.472103 | 101.108878 | 73.211894 | 115.82251183 | 31.60630628 | 26.9772 | 55667.4343981482 | 2011-04-16 10:25:32 | 55667.8230902778 | 2011-04-16 19:45:15 | 706005010 | 12.0103 | 20 | 12.0183 | 12.0103 | 0 | 12.0263 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17.5851 | 17.5851 | 33.5759 | 0 | PROCESSED | 57601.5154976852 | 2016-08-01 12:22:19 | 56058 | 2012-05-11 00:00:00 | 55690.9834490741 | 2011-05-09 23:36:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060004 | We propose a Suzaku observation of "Gamma-ray lobe" accociated with a FR-I/II radio galaxy NGC6251. This is the second discovery next to Cen-A lobe with Fermi-LAT above 100 MeV. Compared to huge angular extent of Cen-A (~10 degree), the lobe of NGC 6251 is comfortably fit within an XIS-FOV, but its physical size is almost the same as Cen-A(~Mpc). We can therefore estimate the total power accumulated in lobe with much less uncertainties, and pressure balance between non-thermal electrons and external thermal cluster medium, that may reveal possible contributions of hidden protons in the lobe. We propose a 40 ksec observation of NGC 6251 centered on the NW-lobe, with additional 20 ksec x 2 observations at "OFF-src" positions to improve the background estimate. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 6 | AO6 | SUZAKU OBSERVATION OF "GAMMA-RAY LOBE'' IN A RADIO GALAXY NGC6251 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706005010/ | Quick Look | ![]() |
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112 | IC 4518A | 224.419 | -43.1269 | 223.597719 | -42.926611 | 234.851401 | -25.085272 | 326.11466585 | 13.99053707 | 102.9822 | 55959.1723263889 | 2012-02-02 04:08:09 | 55961.0002777778 | 2012-02-04 00:00:24 | 706012010 | 64.3986 | 60 | 64.3986 | 64.3986 | 0 | 64.3986 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57.2381 | 57.2381 | 157.9058 | 1 | PROCESSED | 57604.5692708333 | 2016-08-04 13:39:45 | 56434 | 2013-05-22 00:00:00 | 56068.6321064815 | 2012-05-21 15:10:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060040 | We propose to observe the Compton-thin AGN IC 4518A with a very small L_X/L_IR ratio, which has often been employed as an indicator of the presence of a Compton-thick AGN. Our aim is to examine the recent argument that L_X/L_IR is not a good measure of absorption column densities and that this ratio is more dependent on the covering fraction of absorber and intrinsic spectral shape. We measure the spectral slope, covering fraction, and NH, and compare them with the prediction of Monte-Carlo simulations to test the validity of L_X/L_IR as a measure of Compton thickness. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YOSHITAKA HIRATA | JAP | 6 | AO6 | BROAD-BAND SPECTRA OF THE COMPTON-THIN AGN IC 4518A WITH A SMALL L_X/L_IR: TESTING VALIDITY OF A COMPTON-THICK INDICATOR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706012010/ | Quick Look | ![]() |
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113 | RX J1633+4718 | 248.3303 | 47.3072 | 247.970126 | 47.410772 | 228.761848 | 67.666439 | 73.53738657 | 42.62611906 | 329.4078 | 55743.8204050926 | 2011-07-01 19:41:23 | 55744.8460069444 | 2011-07-02 20:18:15 | 706027010 | 39.9916 | 40 | 39.9916 | 39.9916 | 0 | 39.9916 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.6531 | 39.6531 | 88.6059 | 1 | PROCESSED | 57602.4692013889 | 2016-08-02 11:15:39 | 56144 | 2012-08-05 00:00:00 | 55775.3057407407 | 2011-08-02 07:20:16 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060089 | RX J1633+4718 was detected in the ROSAT all sky survey, later identified as a radio loud narrow line Seyfert 1 (NLS1) galaxy. The soft X-ray spectrum of this source was fitted with a blackbody with temperature of 32eV plus a flat power law component. The blackbody temperature is much lower than 100-200eV, typical soft X-ray excess commonly observed in NLS1. Since radio to UV continuum spectrum of this souce resembles those of blazars, the flat power law X-ray component is likely to be a jet origin. The jet might supress accretion corona, and thus the emission from the accretion disk might visible in its bare form. Suzaku observation of this source will give us X-ray spectrum above 2keV and CCD resolution spectrum below 2keV for the 1st time. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KIYOSHI HAYASHIDA | JAP | 6 | AO6 | X-RAY EMISSION FROM DISK AND JET AROUND A SMBH IN RX J1633+4718 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706027010/ | Quick Look | ![]() |
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114 | SMC X-1 | 19.2724 | -73.4484 | 18.941012 | -73.711562 | 312.330249 | -66.473862 | 300.41553375 | -43.55429702 | 25.8573 | 55691.0197337963 | 2011-05-10 00:28:25 | 55691.4064814815 | 2011-05-10 09:45:20 | 706030040 | 17.9054 | 18 | 17.9214 | 17.9214 | 0 | 17.9054 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.8143 | 16.8143 | 33.4079 | 0 | PROCESSED | 57601.9922222222 | 2016-08-01 23:48:48 | 56068 | 2012-05-21 00:00:00 | 55701.1543981482 | 2011-05-20 03:42:20 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JOSEPH NEILSEN | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030040/ | Quick Look | ![]() |
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115 | SMC X-1 | 19.2675 | -73.4407 | 18.935881 | -73.70387 | 312.347206 | -66.469935 | 300.41598527 | -43.56211574 | 204.2035 | 55875.0768055556 | 2011-11-10 01:50:36 | 55875.6182291667 | 2011-11-10 14:50:15 | 706030080 | 19.8598 | 18 | 19.8881 | 19.8961 | 0 | 19.8598 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 19.2508 | 19.2508 | 46.772 | 0 | PROCESSED | 57603.7203587963 | 2016-08-03 17:17:19 | 56260 | 2012-11-29 00:00:00 | 55890.6941203704 | 2011-11-25 16:39:32 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JOSEPH NEILSEN | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030080/ | Quick Look | ![]() |
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116 | SMC X-1 | 19.2681 | -73.4483 | 18.936643 | -73.711469 | 312.329443 | -66.472676 | 300.41718915 | -43.55456404 | 342.3682 | 56005.2598611111 | 2012-03-19 06:14:12 | 56005.8452546296 | 2012-03-19 20:17:10 | 706030100 | 18.5821 | 18 | 18.6263 | 18.6343 | 0 | 18.5821 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 20.3061 | 20.3061 | 50.5719 | 0 | PROCESSED | 57604.9618055556 | 2016-08-04 23:05:00 | 56399 | 2013-04-17 00:00:00 | 56022.2021296296 | 2012-04-05 04:51:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JOSEPH NEILSEN | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030100/ | Quick Look | ![]() |
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117 | III ZW 2 | 2.6244 | 10.9839 | 1.981573 | 10.705729 | 6.801457 | 9.029508 | 106.97577765 | -50.61513425 | 67.4163 | 55726.9877893518 | 2011-06-14 23:42:25 | 55728.9792708333 | 2011-06-16 23:30:09 | 706031010 | 81.466 | 80 | 81.466 | 81.466 | 0 | 81.466 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74.3629 | 74.3629 | 172.0397 | 3 | PROCESSED | 57602.3450925926 | 2016-08-02 08:16:56 | 56127 | 2012-07-19 00:00:00 | 55757.7040046296 | 2011-07-15 16:53:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061411 | Fermi-LAT has revealed gamma-ray emission from Seyfert galaxies in its 1st catalog. Optical and X-ray spectra of Seyferts generally provide important clues to the nature of the accretion process, and thus those objects are promising targets to investigate the connection of the jet to the central source. Here, we propose Suzaku observations of three Seyfert-type AGNs from our gamma-ray candidate list: those objects are also present in the Swift-BAT catalog. Those are III Zw 2, NGC 6814 and ESO 323-G077 and we request pointings of 80 ks, 40 ks and 40 ks respectively. All three candidates appear to be associated with AGN, but show different radio or IR properties. Suzaku data will give us crucial information to investigate the origin of high-energy emission from those Seyfert objects. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MASAAKI HAYASHIDA | USA | 6 | AO6 | SUZAKU OBSERVATIONS OF SEYFERT GALAXIES AS GAMMA-RAY SOURCE CANDIDATES SELECTED FROM THE SWIFT-BAT CATALOG | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706031010/ | Quick Look | ![]() |
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118 | ESO 323-G077 | 196.6073 | -40.4236 | 195.900559 | -40.156267 | 212.090645 | -30.55227 | 306.0162391 | 22.35835315 | 295.8925 | 55762.647337963 | 2011-07-20 15:32:10 | 55763.4168287037 | 2011-07-21 10:00:14 | 706033010 | 44.1222 | 40 | 44.1222 | 44.1222 | 0 | 44.1222 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.9258 | 40.9258 | 66.4819 | 0 | PROCESSED | 57602.6188310185 | 2016-08-02 14:51:07 | 56212 | 2012-10-12 00:00:00 | 55845.2395949074 | 2011-10-11 05:45:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061411 | Fermi-LAT has revealed gamma-ray emission from Seyfert galaxies in its 1st catalog. Optical and X-ray spectra of Seyferts generally provide important clues to the nature of the accretion process, and thus those objects are promising targets to investigate the connection of the jet to the central source. Here, we propose Suzaku observations of three Seyfert-type AGNs from our gamma-ray candidate list: those objects are also present in the Swift-BAT catalog. Those are III Zw 2, NGC 6814 and ESO 323-G077 and we request pointings of 80 ks, 40 ks and 40 ks respectively. All three candidates appear to be associated with AGN, but show different radio or IR properties. Suzaku data will give us crucial information to investigate the origin of high-energy emission from those Seyfert objects. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MASAAKI HAYASHIDA | USA | 6 | AO6 | SUZAKU OBSERVATIONS OF SEYFERT GALAXIES AS GAMMA-RAY SOURCE CANDIDATES SELECTED FROM THE SWIFT-BAT CATALOG | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706033010/ | Quick Look | ![]() |
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119 | 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 | ![]() |
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120 | 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 | ![]() |
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121 | 1622-297 | 246.5282 | -29.8629 | 245.741591 | -29.750241 | 249.573082 | -8.070344 | 348.81494865 | 13.309894 | 287.0011 | 55828.8879166667 | 2011-09-24 21:18:36 | 55829.1800810185 | 2011-09-25 04:19:19 | 706044010 | 8.7781 | 10 | 8.7781 | 8.7781 | 0 | 8.7781 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 8.7513 | 8.7513 | 25.198 | 0 | PROCESSED | 57603.2321064815 | 2016-08-03 05:34:14 | 56236 | 2012-11-05 00:00:00 | 55868.9351851852 | 2011-11-03 22:26:40 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061601 | We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | SVETLANA JORSTAD | USA | 6 | AO6 | EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706044010/ | Quick Look | ![]() |
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122 | 4C38.41 | 248.824 | 38.1186 | 248.386993 | 38.220121 | 236.373082 | 59.10929 | 61.06470824 | 42.32788618 | 255.0463 | 55829.1891666667 | 2011-09-25 04:32:24 | 55829.4148032407 | 2011-09-25 09:57:19 | 706045010 | 8.9239 | 10 | 8.9319 | 8.9319 | 0 | 8.9239 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.5353 | 9.5353 | 19.4719 | 0 | PROCESSED | 57603.2349305556 | 2016-08-03 05:38:18 | 56225 | 2012-10-25 00:00:00 | 55875.6235185185 | 2011-11-10 14:57:52 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061601 | We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | SVETLANA JORSTAD | USA | 6 | AO6 | EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706045010/ | Quick Look | ![]() |
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123 | 3C 236 WEST LOBE | 151.329 | 34.9949 | 150.593371 | 35.23826 | 140.67974 | 21.703249 | 189.91194492 | 53.83302535 | 299.9981 | 56053.9465740741 | 2012-05-06 22:43:04 | 56055.7862384259 | 2012-05-08 18:52:11 | 707005010 | 83.9935 | 80 | 83.9935 | 83.9935 | 0 | 83.9935 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80.4248 | 80.4248 | 158.9318 | 2 | PROCESSED | 57605.4100925926 | 2016-08-05 09:50:32 | 56436 | 2013-05-24 00:00:00 | 56070.2690856482 | 2012-05-23 06:27:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070014 | Through the Suzaku observations of giant radio galaxies, of which the size is larger than about 1 Mpc, we are going to reveal a picture that the jets in radio galaxies become inactive as they evolve from 500 kpc to 1 Mpc. However, the current Suzaku sample of the giant radio galaxies is far from being satisfactory to make a definite conclusion. Therefore, we propose a Suzaku observation of 3C 236, one of the most giant radio galaxy in the Universe. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NAOKI ISOBE | JAP | 7 | AO7 | INVESTIGATION INTO EVOLUTION OF THE JET ENERGETICS, THROUGH THE SUZAKU OBSERVATION OF THE GIANT RADIO GALAXY 3C 236 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707005010/ | Quick Look | ![]() |
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124 | 2FGL J0037.8+1238 | 9.4591 | 12.6426 | 8.808625 | 12.367737 | 13.671851 | 7.875917 | 117.75617703 | -50.09241086 | 67.2998 | 56108.005787037 | 2012-06-30 00:08:20 | 56108.9432523148 | 2012-06-30 22:38:17 | 707010010 | 28.6039 | 30 | 28.6039 | 28.6039 | 0 | 28.6039 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.0977 | 30.0977 | 80.972 | 1 | PROCESSED | 57606.5224768518 | 2016-08-06 12:32:22 | 56493 | 2013-07-20 00:00:00 | 56127.1415625 | 2012-07-19 03:23:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070034 | We propose Suzaku observations of "unusual" Fermi-LAT sources 2FGL J0022.2, J0037.8 and J0157.2, which are yet unidentified in gamma-ray, but their counterparts have already been detected with snapshot (typically 5ksec) Swift XRT observations. Their positions are determined with an excellent accuracy of several arcseconds. Since all three sources are detected both in radio and X-rays, they could be most likely AGN jet sources but their spectral energy distributions are far from what expected from typical blazars, suggesting "new-type" AGN sources. We propose 30 ksec observations of each to investigate temporal variability, as well as to determine wideband XIS/HXD spectra between 0.5-30 keV (J01572.2 is detectable with HXD/PIN). | EXTRAGALACTIC COMPACT SOURCES | 7 | B | JUN KATAOKA | JAP | 7 | AO7 | FURTHER CHALLENGES TO UNUSUAL FERMI-UNIDS WITH SUZAKU X-RAY OBSERVATORY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707010010/ | Quick Look | ![]() |
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125 | NGC1365 | 53.4072 | -36.1471 | 52.929884 | -36.314043 | 36.805891 | -53.04754 | 237.96723255 | -54.59318142 | 57.2979 | 56125.3876273148 | 2012-07-17 09:18:11 | 56125.896087963 | 2012-07-17 21:30:22 | 707017030 | 26.7672 | 30 | 26.7672 | 26.7672 | 0 | 26.7672 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.2112 | 25.2112 | 43.9239 | 1 | PROCESSED | 57606.6299537037 | 2016-08-06 15:07:08 | 56582 | 2013-10-17 00:00:00 | 56212.7663194444 | 2012-10-12 18:23:30 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070095 | NGC1365 is one of AGNs which shows the most highly variable spectral change, and furthermore exhibits strong Fe-K absorption lines blue-shifted by 1000--5000 km/s with EW of about 100eV. These absorption lines indicate a massive outflow and are important to consider the AGN feedback to parent galaxies. Currently, there is no other object by which we can measure the Fe-K absorption lines accurately than NGC 1365. Therefore, we propose to monitor a velocity, depth, and ratio of blue-shifted Fe-K absorption lines, hard X-ray flux above 10 keV of NGC1365 every 10 days, in order to probe the massive outflow dynamically and compare the results with the numerical simulation. } | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YASUSHI FUKAZAWA | JAP | 7 | AO7 | MONITOR OF VELOCITY AND STRENGTH OF BLUE-SHIFTED STRONG FE-K ABSORPTION LINES OF NGC 1365 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707017030/ | Quick Look | ![]() |
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126 | HOLMBERG IX X-1 | 149.4435 | 69.0486 | 148.425456 | 69.287009 | 119.776016 | 51.672601 | 141.95726659 | 41.07139178 | 311.5635 | 56030.7575810185 | 2012-04-13 18:10:55 | 56034.6807175926 | 2012-04-17 16:20:14 | 707019010 | 182.5274 | 500 | 182.5274 | 182.5274 | 0 | 182.5274 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 208.6236 | 208.6236 | 338.9339 | 3 | PROCESSED | 57605.2861342593 | 2016-08-05 06:52:02 | 56018 | 2012-04-01 00:00:00 | 56044.4614699074 | 2012-04-27 11:04:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071251 | Recent X-ray observations have found evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in a super-Eddington state. Current data are unable to deliver a clear answer, but the diagnostics possible in a long observation will be decisive. We request a 500 ks observation of the ULX Holmberg IX X-1 to place crucial constraints on atomic features that would signal a super-Eddington flow. Detecting or ruling out atomic features naturally requires a deep exposure. The strong spectral constraints derived will reveal the nature of the accreting black holes in these systems. A definitive statement on the existence of 100-1000 Msun black holes or extreme accretion states will be an important Suzaku legacy. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JON MILLER | USA | 7 | AO7 | A DECISIVE LEGACY OBSERVATION OF AN ULTRALUMINOUS X-RAY SOURCE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707019010/ | Quick Look | ![]() |
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127 | HOLMBERG IX X-1 | 149.4877 | 69.0751 | 148.469613 | 69.31362 | 119.77363 | 51.703415 | 141.9165022 | 41.0686989 | 124.501 | 56221.770162037 | 2012-10-21 18:29:02 | 56224.1252083333 | 2012-10-24 03:00:18 | 707019020 | 107.4958 | 320 | 107.4958 | 107.4958 | 0 | 107.4958 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 106.8673 | 106.8673 | 203.4479 | 1 | PROCESSED | 57607.8555324074 | 2016-08-07 20:31:58 | 56018 | 2012-04-01 00:00:00 | 56330.5864930556 | 2013-02-07 14:04:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071251 | Recent X-ray observations have found evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in a super-Eddington state. Current data are unable to deliver a clear answer, but the diagnostics possible in a long observation will be decisive. We request a 500 ks observation of the ULX Holmberg IX X-1 to place crucial constraints on atomic features that would signal a super-Eddington flow. Detecting or ruling out atomic features naturally requires a deep exposure. The strong spectral constraints derived will reveal the nature of the accreting black holes in these systems. A definitive statement on the existence of 100-1000 Msun black holes or extreme accretion states will be an important Suzaku legacy. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JON MILLER | USA | 7 | AO7 | A DECISIVE LEGACY OBSERVATION OF AN ULTRALUMINOUS X-RAY SOURCE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707019020/ | Quick Look | ![]() |
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128 | HOLMBERG IX X-1 | 149.4867 | 69.0744 | 148.468616 | 69.312918 | 119.773774 | 51.702635 | 141.91753226 | 41.06881922 | 124.4999 | 56226.4169097222 | 2012-10-26 10:00:21 | 56228.7717708333 | 2012-10-28 18:31:21 | 707019040 | 110.0175 | 500 | 110.0383 | 110.0175 | 0 | 110.0175 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 105.7961 | 105.7961 | 203.426 | 2 | PROCESSED | 57607.8756018518 | 2016-08-07 21:00:52 | 56018 | 2012-04-01 00:00:00 | 56240.5502430556 | 2012-11-09 13:12:21 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071251 | Recent X-ray observations have found evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in a super-Eddington state. Current data are unable to deliver a clear answer, but the diagnostics possible in a long observation will be decisive. We request a 500 ks observation of the ULX Holmberg IX X-1 to place crucial constraints on atomic features that would signal a super-Eddington flow. Detecting or ruling out atomic features naturally requires a deep exposure. The strong spectral constraints derived will reveal the nature of the accreting black holes in these systems. A definitive statement on the existence of 100-1000 Msun black holes or extreme accretion states will be an important Suzaku legacy. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JON MILLER | USA | 7 | AO7 | A DECISIVE LEGACY OBSERVATION OF AN ULTRALUMINOUS X-RAY SOURCE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707019040/ | Quick Look | ![]() |
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129 | NGC 4151 | 182.642 | 39.4132 | 182.010684 | 39.69131 | 164.095796 | 36.629182 | 155.04475012 | 75.06022062 | 134.3454 | 56242.8428472222 | 2012-11-11 20:13:42 | 56245.9599537037 | 2012-11-14 23:02:20 | 707024010 | 150.2669 | 150 | 150.2829 | 150.2669 | 0 | 150.2829 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 150.5465 | 150.5465 | 269.2897 | 4 | PROCESSED | 57608.0679861111 | 2016-08-08 01:37:54 | 56702 | 2014-02-14 00:00:00 | 56330.6348032407 | 2013-02-07 15:14:07 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071417 | We propose simultaneous NuSTAR/Suzaku observations of NGC 4151 and IC 4329A. These pointings will achieve three goals: (1) They will provide the best-ever broad-band X-ray spectra of two of the brightest Seyfert galaxies in the 0.5-80 keV band; (2) They will enable broad-band, time-resolved X-ray spectroscopy of these fascinating and variable sources; (3) They will serve as invaluable calibration targets for the two observatories. The spectral coverage and sensitivity will enable the continuum, absorption and reflection components of each spectrum to be conclusively disentangled, allowing us to determine whether inner disk reflection signatures are present. We will also be able to break the degeneracy between the coronal temperature and optical depth in both AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | LAURA BRENNEMAN | USA | 7 | AO7 | SHEDDING NEW LIGHT ON THE BROAD-BAND X-RAY SPECTRA OF NGC 4151 AND IC 4329A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707024010/ | Quick Look | ![]() |
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130 | NGC 5252 | 204.5663 | 4.5481 | 203.934961 | 4.801923 | 201.032031 | 13.744519 | 331.30380316 | 64.80829028 | 117.6998 | 56287.8794791667 | 2012-12-26 21:06:27 | 56289.0952777778 | 2012-12-28 02:17:12 | 707028010 | 50.2701 | 45 | 50.2701 | 50.2921 | 0 | 50.2766 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.3367 | 43.3367 | 105.0278 | 0 | PROCESSED | 57608.3760300926 | 2016-08-08 09:01:29 | 56687 | 2014-01-30 00:00:00 | 56321.5462268518 | 2013-01-29 13:06:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071424 | A hard X-ray-selected (BAT) AGN sample shows a remarkable 70% of the local population of type 1 AGN to have extreme hard excesses above 20 keV, likely caused by Compton-thick gas in the line-of-sight, covering at least 50% of the source. We request six snapshot observations to complete a Suzaku survey of a BAT-flux-limited sample and make a complete and unbiased measurement of the incidence. Analysis of the new sources will be performed in conjunction with existing exposures, providing exciting new insight into the previously unknown structures in hard X-ray selected AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TRACEY TURNER | USA | 7 | AO7 | INVESTIGATING COMPTON-THICK ABSORBERS IN TYPE 1 AGN: OVERHAULING THE AGN PARADIGM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707028010/ | Quick Look | ![]() |
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131 | PDS 456 | 262.0802 | -14.261 | 261.369515 | -14.22093 | 262.220782 | 8.966234 | 10.39487872 | 11.16781955 | 96.2511 | 56344.8907407407 | 2013-02-21 21:22:40 | 56349.993912037 | 2013-02-26 23:51:14 | 707035010 | 182.299 | 450 | 182.299 | 182.299 | 0 | 182.299 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 160.3071 | 160.3071 | 440.8752 | 4 | PROCESSED | 57610.7549768518 | 2016-08-10 18:07:10 | 56018 | 2012-04-01 00:00:00 | 56363.6993981482 | 2013-03-12 16:47:08 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071431 | PDS 456 is the most luminous nearby (z=0.184) AGN, more typical of quasars at high redshift. A 2007 Suzaku observation resolved iron K absorption at 9 keV in the QSO frame, moving at near relativistic velocities (0.25c). A follow-up 2011 observation was highly absorbed and showed a direct response of the iron K absorber to a decrease in the ionizing flux, while the harder photons lag behind the soft, by 10^4 secs. We propose to monitor the remarkable spectral variability and outflow from PDS 456, through a deep 450ks Suzaku observation. We wish to:- (i) quantify the time lags and determine the location of the reprocessor, (ii) determine the origin and timescale of the absorber variability and (iii) measure the hard X-ray variability from a Compton thick absorber in PDS 456. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | JAMES REEVES | USA | 7 | AO7 | VARIABILITY AND REVERBERATION OF THE QUASAR WIND IN PDS 456 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707035010/ | Quick Look | ![]() |
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132 | PDS 456 | 262.0805 | -14.2617 | 261.369811 | -14.221632 | 262.221115 | 8.965551 | 10.39443055 | 11.16720212 | 96.2512 | 56354.8215972222 | 2013-03-03 19:43:06 | 56359.5001388889 | 2013-03-08 12:00:12 | 707035020 | 164.8107 | 450 | 164.8267 | 164.8107 | 0 | 164.8291 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 147.4496 | 147.4496 | 404.1815 | 2 | PROCESSED | 57610.8342824074 | 2016-08-10 20:01:22 | 56018 | 2012-04-01 00:00:00 | 56373.6804166667 | 2013-03-22 16:19:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071431 | PDS 456 is the most luminous nearby (z=0.184) AGN, more typical of quasars at high redshift. A 2007 Suzaku observation resolved iron K absorption at 9 keV in the QSO frame, moving at near relativistic velocities (0.25c). A follow-up 2011 observation was highly absorbed and showed a direct response of the iron K absorber to a decrease in the ionizing flux, while the harder photons lag behind the soft, by 10^4 secs. We propose to monitor the remarkable spectral variability and outflow from PDS 456, through a deep 450ks Suzaku observation. We wish to:- (i) quantify the time lags and determine the location of the reprocessor, (ii) determine the origin and timescale of the absorber variability and (iii) measure the hard X-ray variability from a Compton thick absorber in PDS 456. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | JAMES REEVES | USA | 7 | AO7 | VARIABILITY AND REVERBERATION OF THE QUASAR WIND IN PDS 456 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707035020/ | Quick Look | ![]() |
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133 | PKS 0548-322 | 87.6707 | -32.2739 | 87.20583 | -32.286363 | 86.511257 | -55.687672 | 237.56869078 | -26.144265 | 287.028 | 56023.6105555556 | 2012-04-06 14:39:12 | 56026.3891435185 | 2012-04-09 09:20:22 | 707040010 | 102.6567 | 100 | 102.6567 | 102.6567 | 0 | 102.6567 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91.5237 | 91.5237 | 240.0558 | 3 | PROCESSED | 57605.1844907407 | 2016-08-05 04:25:40 | 56415 | 2013-05-03 00:00:00 | 56044.314525463 | 2012-04-27 07:32:55 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072006 | We propose Suzaku observations of the two brightest extreme BL Lac objects, PKS 0548-322 and RGB J0710+591 (100 ksec each), whose synchrotron bump peaks in the medium-hard X-ray band. The requested observations, never performed by Suzaku on this two sources, will permit to measure their continuum in the 0.6-70 keV range, fully exploiting the unique capabilities of the Suzaku satellite. With its wide energy coverage and good response, Suzaku will allow us to determine with unprecedented precision the spectral properties of the sources in the hard, medium and soft X-ray ranges, allowing us to measure the physical properties of the emitting relativistic electrons and, complemented by data at other frequencies, to infer the physical conditions in the emitting region. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | FABRIZIO TAVECCHIO | EUR | 7 | AO7 | REVEALING THE HIGH-ENERGY SYNCHROTRON PEAK OF EXTREME BL LACS WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707040010/ | Quick Look | ![]() |
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134 | 0836+710 | 130.3582 | 70.9091 | 129.096 | 71.086996 | 109.311372 | 50.162038 | 143.52368034 | 34.42368753 | 111.9979 | 56213.6030787037 | 2012-10-13 14:28:26 | 56213.8223726852 | 2012-10-13 19:44:13 | 707042010 | 10.613 | 10 | 10.613 | 10.613 | 0 | 10.613 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.866 | 8.866 | 18.9279 | 0 | PROCESSED | 57607.7537615741 | 2016-08-07 18:05:25 | 56598 | 2013-11-02 00:00:00 | 56232.4320717593 | 2012-11-01 10:22:11 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071601 | We propose to perform two 2-week multi-frequency campaigns of observations of a sample of gamma-ray blazars during Fermi Cycle 5. The campaigns will involve: (1) gamma-ray monitoring with the Fermi LAT, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B, V, R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku and Swift; (6) mid-IR measurements with IRTF; and (7) near-IR photometric J, H, and K observations. The research aims i) to search for correlated variability on short timescales; ii) to compile SEDs at different states of gamma-ray and radio jet activitiy; and iii) to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | SVETLANA JORSTAD | USA | 7 | AO7 | MULTI-FREQUENCY CAMPAIGNS TO STUDY RAPID VARIABILITY IN GAMMA_RAY BLAZARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707042010/ | Quick Look | ![]() |
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135 | BL LAC | 330.6707 | 42.2941 | 330.154473 | 42.052039 | 354.261979 | 49.60384 | 92.59387966 | -10.42383814 | 77.7587 | 56431.6193981482 | 2013-05-19 14:51:56 | 56431.8724884259 | 2013-05-19 20:56:23 | 707044010 | 12.7426 | 10 | 12.7506 | 12.7426 | 0 | 12.7506 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.144 | 13.144 | 21.8319 | 0 | PROCESSED | 57611.320625 | 2016-08-11 07:41:42 | 56826 | 2014-06-18 00:00:00 | 56455.7300231482 | 2013-06-12 17:31:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071601 | We propose to perform two 2-week multi-frequency campaigns of observations of a sample of gamma-ray blazars during Fermi Cycle 5. The campaigns will involve: (1) gamma-ray monitoring with the Fermi LAT, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B, V, R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku and Swift; (6) mid-IR measurements with IRTF; and (7) near-IR photometric J, H, and K observations. The research aims i) to search for correlated variability on short timescales; ii) to compile SEDs at different states of gamma-ray and radio jet activitiy; and iii) to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | SVETLANA JORSTAD | USA | 7 | AO7 | MULTI-FREQUENCY CAMPAIGNS TO STUDY RAPID VARIABILITY IN GAMMA_RAY BLAZARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707044010/ | Quick Look | ![]() |
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136 | MARKARIAN 1040 | 37.056 | 31.3166 | 36.314628 | 31.093376 | 44.885956 | 15.789444 | 146.10796909 | -27.16282444 | 69.5695 | 56515.9165740741 | 2013-08-11 21:59:52 | 56519.1681597222 | 2013-08-15 04:02:09 | 707046010 | 137.4353 | 135 | 137.4353 | 137.4353 | 0 | 137.4353 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 136.328 | 136.328 | 280.9053 | 1 | PROCESSED | 57612.3140625 | 2016-08-12 07:32:15 | 56955 | 2014-10-25 00:00:00 | 56587.9502662037 | 2013-10-22 22:48:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072025 | Mrk 1040 is a nearby type-1 Seyfert galaxy where a recent XMM observation revealed the presence of a deep soft X-ray warm absorber. However the current data are unable to resolve the components of the absorber so very little is known about its properties. We propose to obtain a 200 ks definitive Chandra HETG observation of Mrk 1040 from 0.5-9.0 keV where we will resolve the lines for the first time enabling a detailed analysis of the kinematics and energetics to be made. We will also obtain the first high-resolution spectrum > 2 keV in this source allowing us to resolve the narrow Fe K alpha core. Furthermore, through a 125 ks Suzaku observation we will also study the Fe K complex in unprecedented detail while simultaneously determining the origin of the hard excess. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | ANDREW LOBBAN | EUR | 7 | AO7 | A HIGH-RESOLUTION VIEW OF THE WARM ABSORBER AND IRON LINE IN MRK 1040 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707046010/ | Quick Look | ![]() |
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137 | NGC 3516 | 166.6556 | 72.561 | 165.802341 | 72.831319 | 123.361761 | 57.969661 | 133.25565935 | 42.40250412 | 335.7404 | 56391.9675925926 | 2013-04-09 23:13:20 | 56393.0460185185 | 2013-04-11 01:06:16 | 708006010 | 51.386 | 50 | 51.402 | 51.386 | 0 | 51.402 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.1015 | 49.1015 | 93.1638 | 1 | PROCESSED | 57611.0515856482 | 2016-08-11 01:14:17 | 56383 | 2013-04-01 00:00:00 | 56421.6947106482 | 2013-05-09 16:40:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080066 | We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 8 | AO8 | THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006010/ | Quick Look | ![]() |
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138 | NGC 3516 | 166.6684 | 72.5566 | 165.815394 | 72.826934 | 123.372761 | 57.969452 | 133.25443095 | 42.40827092 | 314.5458 | 56409.0119560185 | 2013-04-27 00:17:13 | 56409.446087963 | 2013-04-27 10:42:22 | 708006020 | 19.103 | 50 | 19.119 | 19.103 | 0 | 19.119 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 20.2121 | 20.2121 | 30.7239 | 0 | PROCESSED | 57611.1744907407 | 2016-08-11 04:11:16 | 56383 | 2013-04-01 00:00:00 | 56457.6034375 | 2013-06-14 14:28:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080066 | We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 8 | AO8 | THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006020/ | Quick Look | ![]() |
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139 | NGC 3516 | 166.6764 | 72.5574 | 165.823506 | 72.827743 | 123.374751 | 57.971749 | 133.25110438 | 42.40886909 | 307.603 | 56424.0155555556 | 2013-05-12 00:22:24 | 56425.1044328704 | 2013-05-13 02:30:23 | 708006030 | 50.4283 | 50 | 50.4283 | 50.4283 | 0 | 50.4283 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 57.2275 | 57.2275 | 94.076 | 0 | PROCESSED | 57611.3108680556 | 2016-08-11 07:27:39 | 56383 | 2013-04-01 00:00:00 | 56436.6511805556 | 2013-05-24 15:37:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080066 | We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 8 | AO8 | THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006030/ | Quick Look | ![]() |
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140 | NGC6552 | 270.0757 | 66.6036 | 270.078264 | 66.603205 | 60.706525 | 89.950181 | 96.43339546 | 29.78135373 | 217.6129 | 56610.8399884259 | 2013-11-14 20:09:35 | 56613.0126851852 | 2013-11-17 00:18:16 | 708014010 | 105.7767 | 100 | 105.7767 | 105.7767 | 0 | 105.7767 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102.2797 | 102.2797 | 187.7079 | 1 | PROCESSED | 57613.3907060185 | 2016-08-13 09:22:37 | 57019 | 2014-12-28 00:00:00 | 56653.7413078704 | 2013-12-27 17:47:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080092 | We propose to observe the interesting Seyfert 2 galaxy NGC6552, which has multi fluorescence lines in the X-ray band. There ara only three objects, including NGC6552, which has multi fluorescence lines in the X-ray band. We aim to detect emission lines finely and study the chemical evolution of the galaxy. We also aim measurements of hard X-ray continuum to constrain the reflection component and other nonthermal emission asscciated with jet or starburst activity. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TAKAFUMI KAWANO | JAP | 8 | AO8 | OBSERVATION OF THE MULTI EMISSION LINES FROM SEYFERT 2 GALAXY: NGC6552 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708014010/ | Quick Look | ![]() |
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141 | MKN 335 | 1.5767 | 20.2085 | 0.933785 | 19.930185 | 9.740922 | 17.859652 | 108.75946317 | -41.41793251 | 71.5257 | 56454.1494907407 | 2013-06-11 03:35:16 | 56457.9792824074 | 2013-06-14 23:30:10 | 708016010 | 143.995 | 300 | 144.027 | 143.995 | 0 | 144.027 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 129.5529 | 129.5529 | 330.8674 | 3 | PROCESSED | 57611.6156828704 | 2016-08-11 14:46:35 | 56383 | 2013-04-01 00:00:00 | 56470.7662037037 | 2013-06-27 18:23:20 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081411 | The idea of this proposal is trigger a 300ks observation with Suzaku of the Narrow Line Seyfert 1 Galaxy Mkn 335 during one of its low X-ray flux states. The goal here is to measure its underlying broad-band continuum with Suzaku during a low state and compare it with the 2006 high-state observations. Mkn 335 is one of the best examples of an AGN that went into a deep minimum X-ray flux state. Two competing models can explain these extreme low states: reflection models and partial covering absorber models. Both models still require a variable underlying intrinsic continuum. The science driver is to find out what is causing these low X-ray flux states that have been observed in several NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | DIRK GRUPE | USA | 8 | AO8-TOO | INTRINSIC LOW-STATE X-RAY LUMINOSITY OF THE NLS1 MKN 335 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708016010/ | Quick Look | ![]() |
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142 | MCG-5-23-16 | 146.9232 | -30.945 | 146.373955 | -30.712416 | 162.623211 | -41.142672 | 262.74537578 | 17.2400137 | 295.4404 | 56444.9213194444 | 2013-06-01 22:06:42 | 56448.2467361111 | 2013-06-05 05:55:18 | 708021010 | 159.5262 | 300 | 159.5582 | 159.5262 | 0 | 159.5582 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 155.1267 | 155.1267 | 287.3018 | 1 | PROCESSED | 57611.525787037 | 2016-08-11 12:37:08 | 56383 | 2013-04-01 00:00:00 | 56461.789537037 | 2013-06-18 18:56:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081416 | Significant recent developments in probing environments around AGN black holes has been achieved using X-ray reverberation. They were initially detected in the soft excess of several NLS1s, then recently, the first Fe K reverberation was also seen. In addition to measuring x-rays reverberating a few r_g from the event horizon, short/long delays from different radii have been separated for the first time in NGC4151. Here we propose to observe MCG-5-23-1 for 300 ks in order to study its iron K reverberation. It is optimally one of the brightest and most variable AGN in X-rays. Archival data already show very exciting signatures of Fe K reverberation. With new observations we aim to constrain the emitting region size and study the emission originating at different distances from of the hole. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ABDERAHMEN ZOGHBI | USA | 8 | AO8 | IRON K REVERBERATION IN MCG 5-23-16 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708021010/ | Quick Look | ![]() |
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143 | NGC 235A | 10.7176 | -23.5378 | 10.098982 | -23.81167 | 359.839777 | -25.738096 | 94.13393297 | -85.9211578 | 213.1719 | 56636.0921759259 | 2013-12-10 02:12:44 | 56636.4792939815 | 2013-12-10 11:30:11 | 708026010 | 19.8251 | 20 | 19.8331 | 19.8251 | 0 | 19.8409 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.2251 | 18.2251 | 33.4439 | 1 | PROCESSED | 57613.5511921296 | 2016-08-13 13:13:43 | 56383 | 2013-04-01 00:00:00 | 56646.6871412037 | 2013-12-20 16:29:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081419 | The BAT AGN sample constitutes an unprecedented all-sky hard X-ray survey of the local AGN population. However, to properly model the X-ray absorption & reflection, coverage below 10 keV is needed with CCD spectral resolution and adequate signal-to-noise. We propose to observe 11 AGN with Suzaku, which will increase the completeness of a flux-limited sample with such coverage from 85 to 158 sources. The 11 AGN only have severely underexposed Swift XRT coverage below 10 keV whereas the remaining sources have either Suzaku or XMM coverage. The Suzaku data have the additional advantage of sensitivity above 10 keV that helps to mitigate the long time-baseline of the BAT spectra. The new observations will create a significantly enhanced legacy data set that will provide value for years to come. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TAHIR YAQOOB | USA | 8 | AO8 | ROBUST CHARACTERIZATION OF ABSORPTION AND REFLECTION IN A LOCAL FLUX-LIMITED AGN POPULATION FROM THE SWIFT BAT SURVEY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708026010/ | Quick Look | ![]() |
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144 | CENTAURUS A | 201.3699 | -43.0194 | 200.636516 | -42.759434 | 217.141069 | -31.326977 | 309.51956362 | 19.416494 | 303.7255 | 56519.1824305556 | 2013-08-15 04:22:42 | 56519.4264930556 | 2013-08-15 10:14:09 | 708036010 | 10.6751 | 10 | 10.6751 | 10.6751 | 0 | 10.6911 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.0647 | 10.0647 | 21.0799 | 0 | PROCESSED | 57612.2554050926 | 2016-08-12 06:07:47 | 56954 | 2014-10-24 00:00:00 | 56587.7389351852 | 2013-10-22 17:44:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081433 | We request observations of the nucleus of the radio galaxy Centaurus A to study time variability of its broadband spectral energy distribution (SED) and constrain jet emission models of radio-loud AGN. Due to its proximity, Cen A can be studied in unique detail. Although frequently observed, no time-dependent, simultaneous SEDs covering the spectrum from radio to gamma-rays have been obtained for Cen A so far. Since AGN are highly variable, only quasi-contemporaneous SEDs allow us to constrain parameters of jet emission models. Combining our TANAMI radio Very Long Baseline Interferometry monitoring campaign and Fermi observations with simultaneous Suzaku spectra will fill the gap in energy and address the time-dependent behavior of jet emission and torus absorption with high accuracy. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | ROOPESH OJHA | USA | 8 | AO8 | SIMULTANEOUS SUZAKU AND MULTIWAVELENGTH OBSERVATIONS OF THE NUCLEUS OF CENTAURUS A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708036010/ | Quick Look | ![]() |
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145 | CENTAURUS A | 201.3033 | -43.0014 | 200.570255 | -42.741318 | 217.080563 | -31.331883 | 309.47108059 | 19.44109405 | 111.5377 | 56663.4710763889 | 2014-01-06 11:18:21 | 56663.6613888889 | 2014-01-06 15:52:24 | 708036020 | 7.3652 | 10 | 7.3652 | 7.3732 | 0 | 7.3732 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6.5444 | 6.5444 | 16.4399 | 0 | PROCESSED | 57613.7500462963 | 2016-08-13 18:00:04 | 57086 | 2015-03-05 00:00:00 | 56719.7206944444 | 2014-03-03 17:17:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081433 | We request observations of the nucleus of the radio galaxy Centaurus A to study time variability of its broadband spectral energy distribution (SED) and constrain jet emission models of radio-loud AGN. Due to its proximity, Cen A can be studied in unique detail. Although frequently observed, no time-dependent, simultaneous SEDs covering the spectrum from radio to gamma-rays have been obtained for Cen A so far. Since AGN are highly variable, only quasi-contemporaneous SEDs allow us to constrain parameters of jet emission models. Combining our TANAMI radio Very Long Baseline Interferometry monitoring campaign and Fermi observations with simultaneous Suzaku spectra will fill the gap in energy and address the time-dependent behavior of jet emission and torus absorption with high accuracy. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | ROOPESH OJHA | USA | 8 | AO8 | SIMULTANEOUS SUZAKU AND MULTIWAVELENGTH OBSERVATIONS OF THE NUCLEUS OF CENTAURUS A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708036020/ | Quick Look | ![]() |
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146 | ABELL 998 | 156.5862 | 67.9284 | 155.666008 | 68.182911 | 124.296815 | 52.261797 | 140.87284378 | 43.80315875 | 119.4303 | 56601.7924768518 | 2013-11-05 19:01:10 | 56602.9584722222 | 2013-11-06 23:00:12 | 708041010 | 60.2402 | 60 | 60.2402 | 60.2404 | 0 | 60.2562 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 51.856 | 51.856 | 100.7319 | 2 | PROCESSED | 57613.2563657407 | 2016-08-13 06:09:10 | 56980 | 2014-11-19 00:00:00 | 56614.6831944444 | 2013-11-18 16:23:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081533 | We propose to map out the core of the A981 supercluster with three Suzaku observations. The A981 supercluster contains four Abell richness class 2 clusters within a redshift range of 2,000 km/s. All four clusters also overlap within their virial radii, at least in projection. The low and steady background of the Suzaku telescope is ideal for studying the low surface brightness X-ray emission between the clusters. Such observations will determine if the clusters are interacting via the detection of merger-induced shocks or perturbed features in the outskirts of the individual clusters. Our proposed Suzaku observations will help elucidate the fundamental astrophysics that occurs during the formation of very massive clusters. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | LAURENCE DAVID | USA | 8 | AO8 | MAPPING THE ABELL 981 SUPER CLUSTER WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708041010/ | Quick Look | ![]() |
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147 | FAIRALL 51 | 281.2231 | -62.3584 | 280.059194 | -62.409813 | 276.677853 | -39.177664 | 333.20555808 | -23.08834808 | 251.8035 | 56542.816087963 | 2013-09-07 19:35:10 | 56543.4286689815 | 2013-09-08 10:17:17 | 708046030 | 23.9301 | 30 | 23.9381 | 23.9439 | 0 | 23.9301 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 35.6507 | 35.6507 | 52.9199 | 0 | PROCESSED | 57612.5525694445 | 2016-08-12 13:15:42 | 56990 | 2014-11-29 00:00:00 | 56625.6038078704 | 2013-11-29 14:29:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082016 | Fairall 51 is a variable bright active galaxy (about 1 millicrab), classified as a polar-scattered Seyfert~1 galaxy. It was observed twice with high-quality X-ray spectrometers on-board the XMM-Newton satellite. The two observations are separated by half a year and the spectra significantly differ from each other. The difference can be well explained by a variable covering fraction of a cold (very low-ionised) absorber (Ricci et al., 2010). Two additional Swift data, separated by five days, suggest that the variability may occur at time-scales as short as a few days. The ultimate goal of the proposal is to locate this variable absorber by the determination of the typical time-scale of the variability. We therefore propose a series of observations of Fairall 51 with short exposures. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JIRI SVOBODA | EUR | 8 | AO8 | STUDY OF THE VARIABLE ABSORBER IN A BRIGHT ACTIVE GALAXY FAIRALL 51 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708046030/ | Quick Look | ![]() |
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148 | SN 2006JD | 120.5317 | 0.8109 | 119.887421 | 0.950976 | 122.551734 | -19.245465 | 220.45479917 | 16.05743863 | 101.8795 | 56954.8286458333 | 2014-10-24 19:53:15 | 56958.31125 | 2014-10-28 07:28:12 | 709001010 | 144.4894 | 150 | 144.4894 | 151.0361 | 0 | 151.0521 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7014351852 | 2016-08-16 16:50:04 | 57435 | 2016-02-17 00:00:00 | 57066.4298032407 | 2015-02-13 10:18:55 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090005 | We propose a 150 ks observation of a supernova (SN) 2006jd, a bright SN IIn discovered on October 12, 2006. It is a rare SN that remains bright in X-rays over several years, hence provides us with a rare opportunity to study the dense medium that was ejected by the progenitor star before the SN explosion. Our analysis of archival data taken by Suzaku in 2008 and XMM-Newton in 2009 has indicated interesting spectral evolution, i.e., spectral softening and an increasing centroid of Fe-K lines complex. Our proposed observation will show much clearer spectral variation than that seen in the previous Suzaku and XMM-Newton data, allowing us to understand the details of spectral evolution. The dataset will become a reference for the study of late-time X-ray spectroscopy of SN IIn. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | SATORU KATSUDA | JAP | 9 | AO9 | PROBING LATE-TIME X-RAY SPECTRUM OF SN 2006JD | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709001010/ | Quick Look | ![]() |
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149 | NGC 2655 | 133.9038 | 78.2094 | 132.281402 | 78.399558 | 105.125039 | 57.091904 | 134.93858201 | 32.69360092 | 275.5561 | 56789.4281828704 | 2014-05-12 10:16:35 | 56791.0731712963 | 2014-05-14 01:45:22 | 709003010 | 76.8371 | 80 | 76.8371 | 76.8371 | 0 | 76.8371 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 2.1539 | 0 | PROCESSED | 57615.0904398148 | 2016-08-15 02:10:14 | 57173 | 2015-05-31 00:00:00 | 56807.6198726852 | 2014-05-30 14:52:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090017 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Here we propose to observe two of the lowest luminosity BAT AGNs to measure the amount of the reflection component with unpreceded accuracy, a key parameter to determine the contribution of Compton thick AGNs to the X-ray background. We will also study how the torus structure of low luminosity AGNs differs from that of more luminous AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | BROAD BAND SPECTRA OF HARD X-RAY SELECTED VERY LOW LUMINOSITY AGNS AND THEIR TORUS STRUCTURE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709003010/ | Quick Look | ![]() |
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150 | ARP318 | 32.3792 | -10.1586 | 31.765368 | -10.394539 | 26.44249 | -21.810803 | 173.95964772 | -64.97329044 | 75.9989 | 56873.8890509259 | 2014-08-04 21:20:14 | 56875.8252662037 | 2014-08-06 19:48:23 | 709009010 | 80.2195 | 80 | 80.2195 | 80.2195 | 0 | 80.222 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.3811 | 15.3811 | 43.076 | 0 | PROCESSED | 57616.4808217593 | 2016-08-16 11:32:23 | 57267 | 2015-09-02 00:00:00 | 56898.4603703704 | 2014-08-29 11:02:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090037 | We propose Suzaku/XIS and PIN observations of nearby two radio-quiet AGNs with very weak mid-infrared emission, which might represent a new class of hot dust free AGNs. We found hot dust free AGN candidates by combining the Swift/BAT hard X-ray all-sky AGN catalog with mid-infrared (MIR) all-sky surveys. Three out of 503 sources are not detected in their MIR bands, even in the high sensitivity of WISE. One source is radio-loud AGNs and the other two radio-quiet sources are also observed in 2-10 keV band with Swift/XRT, and no significant Fe Ka line emission is detected. The scientific goal of this proposal is to obtain the first Fe Ka detection or strong constraints of the emission, which will give us a direct evidence that these sources have very small amount or even lack of torus. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | KOHEI ICHIKAWA | JAP | 9 | AO9 | THE FIRST BROADBAND X-RAY OBSERVATIONS OF HOT DUST FREE AGNS IN THE LOCAL UNIVERSE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709009010/ | Quick Look | ![]() |
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151 | HOLMBERG IX X-1 | 149.4663 | 69.0509 | 148.44846 | 69.289367 | 119.784926 | 51.679022 | 141.94846823 | 41.07666025 | 284.4995 | 57158.2357291667 | 2015-05-16 05:39:27 | 57159.0827546296 | 2015-05-17 01:59:10 | 709015040 | 34.12 | 30 | 34.12 | 34.128 | 0 | 34.128 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.6575347222 | 2016-08-18 15:46:51 | 57536 | 2016-05-28 00:00:00 | 57168.6253935185 | 2015-05-26 15:00:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091251 | Broadband X-ray spectroscopy of ultraluminous X-ray sources (ULXs) with NuSTAR and Suzaku has begun to provide important information regarding the nature of these enigmatic sources. Recent NuSTAR observations of the extreme ULX Holmberg IX X-1 revealed unusual spectral variability, and different competing evolutionary scenarios can explain the available data. Resolving this degeneracy is critical to determining the nature of the accretion onto this source, and requires multi-epoch broadband spectroscopy probing a more diverse range of fluxes. We propose to undertake 4x30 ks coordinated Suzaku+NuSTAR observations of Holmberg IX X-1 to provide the additional spectra needed to robustly determine the nature of the observed evolution, providing a vital step in our understanding of extreme ULXs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | DOMINIC WALTON | USA | 9 | AO9 | MULTI-EPOCH BROADBAND X-RAY SPECTROSCOPY OF HOLMBERG IX X-1 WITH SUZAKU AND NUSTAR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709015040/ | Quick Look | ![]() |
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152 | HE0512-3329 | 78.5445 | -33.4308 | 78.084109 | -33.487216 | 72.678048 | -56.186874 | 236.61833373 | -33.85137764 | 251.0519 | 57071.9701388889 | 2015-02-18 23:17:00 | 57072.4937847222 | 2015-02-19 11:51:03 | 709020030 | 25.0955 | 26 | 25.0955 | 25.0955 | 0 | 25.0955 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6171296296 | 2016-08-17 14:48:40 | 57457 | 2016-03-10 00:00:00 | 57087.4623726852 | 2015-03-06 11:05:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091431 | The origin of AGN iron K alpha emission has been debated for two decades. We propose to constrain iron line emission sizes using quasar X-ray microlensing. Our Chandra Cycle 11 observations have shown that the iron line equivalent widths (EWs) in six lensed systems are significantly higher than those measured in local AGNs. This implies that the iron line emission is microlensed more strongly than the X-ray continuum and originates from very compact regions. We propose to confirm the high iron line EWs in lensed quasars by monitoring two more lenses, Q0142-100 and HE0512+3329 using Suzaku, with a total exposure time 115 kilo-seconds. This will provide independent constraints for settling the debate on the origin of the iron line emission. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | BIN CHEN | USA | 9 | AO9 | CONSTRAINING QUASAR IRON LINE EMISSION USING MICROLENSING | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709020030/ | Quick Look | ![]() |
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153 | MARKARIAN 3 | 93.8812 | 71.0496 | 92.43086 | 71.064939 | 91.873944 | 47.634543 | 143.28137914 | 22.71605454 | 71.2169 | 56953.1510532407 | 2014-10-23 03:37:31 | 56953.6731828704 | 2014-10-23 16:09:23 | 709022030 | 22.7461 | 20 | 22.7541 | 22.7541 | 0 | 22.7461 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6616087963 | 2016-08-16 15:52:43 | 57376 | 2015-12-20 00:00:00 | 57010.3833217593 | 2014-12-19 09:11:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092008 | We propose to measure size and distance from the black hole of the optically-thick absorbing and reprocessing system(s) in the heavily obscured Seyfert Galaxy Markarian~3 by means of its known X-ray spectral variability. We aim at simultaneously measuring: the variability timescale of the primary emission, seen in transmission through a photoelectric column density of (0.7--1.1)x10^{24} atoms/cm/cm; the variability timescale of its Compton-reflection, dominating the continuum flux in the 3-10 keV energy band; and the variability timescale of the nuclear obscuration. Only the scientific payload on-board Suzaku possesses the required combination of broadband X-ray coverage, sensitivity, and spectroscopic capabilities to perform this experiment. We request 5 observations of 20 ks each. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MATTEO GUAINAZZI | EUR | 9 | AO9 | MEASURING THE TORUS SPATIAL SCALE(S) IN SEYFERT GALAXIES: A SUZAKU MONITORING OF MARKARIAN 3 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709022030/ | Quick Look | ![]() |
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154 | 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 | ![]() |
155 | SMC X-1 | 19.2661 | -73.446 | 18.934565 | -73.709172 | 312.334379 | -66.471359 | 300.41753301 | -43.55692043 | 64.0051 | 55740.5953819444 | 2011-06-28 14:17:21 | 55741.0960069444 | 2011-06-29 02:18:15 | 706030060 | 18.6682 | 18 | 18.7129 | 18.7049 | 0 | 18.6682 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 20.6764 | 20.6764 | 43.2479 | 0 | PROCESSED | 57602.4222800926 | 2016-08-02 10:08:05 | 56163 | 2012-08-24 00:00:00 | 55775.167974537 | 2011-08-02 04:01:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JOSEPH NEILSEN | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030060/ | Quick Look | ![]() |
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156 | MARKARIAN 509 | 311.0428 | -10.7274 | 310.361715 | -10.908973 | 310.545221 | 7.124071 | 35.9681072 | -29.85888698 | 254.2043 | 54054.375150463 | 2006-11-15 09:00:13 | 54055.0113541667 | 2006-11-16 00:16:21 | 701093030 | 24.4466 | 25 | 24.4466 | 24.4466 | 0 | 24.4466 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.327 | 18.327 | 54.9679 | 1 | PROCESSED | 57536.1015162037 | 2016-05-28 02:26:11 | 54456 | 2007-12-22 00:00:00 | 54088.6171875 | 2006-12-19 14:48:45 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012050 | We propose to perform 4 repeated Suzaku observations of 25 ks each of the Seyfert 1 galaxy MKN 509, the brightest Seyfert galaxy of the Piccinotti sample in the 2-100 keV band that is not strongly affected by neutral or ionized absorbing material. The aim of the study is to disentangle the different physical explanations for the origin of the soft excess looking at the long time--scale correlations between the variations of the emission and shape of the soft excess and the emission at high energy (E > 10 keV). | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GABRIELE PONTI | EUR | 1 | AO1 | SOLVING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701093030/ | Quick Look | ![]() |
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157 | 1H 0707-495 | 107.1586 | -49.5558 | 106.829982 | -49.474426 | 125.752559 | -70.871973 | 260.16951247 | -17.68246857 | 144.7199 | 53707.1759143518 | 2005-12-03 04:13:19 | 53710.0974537037 | 2005-12-06 02:20:20 | 700008010 | 97.2291 | 100 | 97.8529 | 100.3891 | 97.2291 | 97.8149 | 4 | 2 | 4 | 4 | 1 | 0 | 0 | 91.8008 | 91.8008 | 252.3688 | 4 | PROCESSED | 57532.4288194444 | 2016-05-24 10:17:30 | 54247 | 2007-05-27 00:00:00 | 54059.7078472222 | 2006-11-20 16:59:18 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001040 | We propose a 100 ks observation of the NLS1 1H 0707--495 in order to understand its remarkable and puzzling spectral and variability properties. The Suzaku data will help us to disentangle between the two interpretations adopted so far, namely partial covering and relativistically blurred reflection. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GIOVANNI MINIUTTI | JAP | 0 | SWG | THE EXTREME PROPERTIES OF THE NLS1 GALAXY 1H 0707-495 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700008010/ | Quick Look | ![]() |
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158 | MRK 501 | 253.4335 | 39.8281 | 253.015349 | 39.90842 | 242.48193 | 61.693142 | 63.68387876 | 38.89139128 | 70.9919 | 54913.7775347222 | 2009-03-23 18:39:39 | 54915.3328587963 | 2009-03-25 07:59:19 | 703046010 | 72.3342 | 65 | 72.3342 | 72.3342 | 0 | 72.3342 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64.8365 | 64.8365 | 134.3581 | 1 | PROCESSED | 57545.930462963 | 2016-06-06 22:19:52 | 55329 | 2010-05-13 00:00:00 | 54924.366724537 | 2009-04-03 08:48:05 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031343 | We propose to observe two bright TeV blazars with Suzaku, in coordination with VERITAS and MAGIC at TeV energies. The primary objective is to make use of the recently available observational capabilities in collecting the much needed simultaneous X-ray and TeV data on these intriguing sources. The data will be essential for addressing a number of unresolved issues in the study of TeV blazars, such as spectral variability, X-ray/TeV correlation and associated time lags, spectral hysteresis, etc. The results will likely provide insights into the properties of the emitting particles, as well as those of the emitting regions, emission mechanism, composition of the jets, and acceleration energetics. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | WEI CUI | USA | 3 | AO3 | COORDINATED X-RAY/TEV OBSERVATIONS OF TEV BLAZARS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703046010/ | Quick Look | ![]() |
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159 | SWIFT J0601.9-8636 | 91.1523 | -86.6779 | 95.292028 | -86.662252 | 269.78546 | -69.879444 | 299.2555588 | -27.75439578 | 292.1727 | 53838.6834259259 | 2006-04-13 16:24:08 | 53839.0779976852 | 2006-04-14 01:52:19 | 701018010 | 19.7657 | 20 | 19.7817 | 19.7817 | 19.7657 | 19.7737 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 16.6614 | 16.6614 | 34.0599 | 0 | PROCESSED | 57533.4511226852 | 2016-05-25 10:49:37 | 54397 | 2007-10-24 00:00:00 | 53905.4682060185 | 2006-06-19 11:14:13 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010133 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 1 | AO1 | DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701018010/ | Quick Look | ![]() |
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160 | NGC 5506 | 213.3121 | -3.2119 | 212.6632 | -2.97838 | 212.190756 | 9.596557 | 339.14659218 | 53.80640928 | 287.3747 | 53958.1015972222 | 2006-08-11 02:26:18 | 53959.4488425926 | 2006-08-12 10:46:20 | 701030020 | 53.2962 | 63 | 53.3042 | 53.2962 | 53.3042 | 53.3042 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 47.9832 | 47.9832 | 116.386 | 1 | PROCESSED | 57535.2817476852 | 2016-05-27 06:45:43 | 54695 | 2008-08-17 00:00:00 | 54116.3307291667 | 2007-01-16 07:56:15 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011312 | NGC 5506 is one of the brightest Seyferts in the X-ray sky, the second brightest in the PIN bandpass. Obscuring gas has kept the true nature of this AGN secret until recent optical and infrared studies have unmasked the narrow-line-seyfert 1 nucleus. With this knowledge, NGC 5506 is the perfect candidate for confirming the generality of a new result based on a recent XMM observation of Mkn 766, ie that the ionized component of Fe K emission originates from the inner accretion disk and closely tracks the hard X-ray continuum flux. This immediately gives us the ionization-state and size-scale of the inner disk. We request a 150 ks Suzaku observation to see whether a similar result holds for NGC 5506 and, by extension, may be a property of NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TRACEY TURNER | USA | 1 | AO1 | SUZAKU STUDY OF THE BRIGHTEST NARROW LINE SEYFERT 1: NGC 5506 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701030020/ | Quick Look | ![]() |
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161 | MRK 766 | 184.6147 | 29.8197 | 183.986078 | 30.097268 | 171.204802 | 28.944359 | 190.62410896 | 82.27145087 | 134.9989 | 54421.893287037 | 2007-11-17 21:26:20 | 54423.2363310185 | 2007-11-19 05:40:19 | 701035020 | 59.3635 | 50 | 59.3635 | 59.3635 | 0 | 59.3635 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 51.1517 | 51.1517 | 116.0238 | 1 | PROCESSED | 57540.5762384259 | 2016-06-01 13:49:47 | 54800 | 2008-11-30 00:00:00 | 54433.2716666667 | 2007-11-29 06:31:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011328 | X-ray spectroscopy of Mkn 766 has revealed ionised Fe emission that varies with the continuum on 10 ks timescales: direct evidence for ionised reflection from the accretion disk. This bright NLSy1 also shows extreme spectral variability, with the low state being dominated by a hard, constant reflection component, probably from cool distant material. We propose to measure the spectrum above 10 keV; the hot component should vary with the continuum, the cold distant component should be constant, and we can measure their relative contributions to test the predictions of the lower-energy analysis. This source is complex and needs the high-energy spectrum from Suzaku: it seems likely that previous complex behavior of several Seyferts can be described by these components | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TRACEY TURNER | USA | 1 | AO1 | DECOMPOSITION OF SEYFERT SPECTRA: TRACKING THE INNER DISK IN MKN 766 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701035020/ | Quick Look | ![]() |
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162 | RBS 315 | 36.2519 | 18.8398 | 35.555924 | 18.614311 | 40.065414 | 4.223463 | 151.73247281 | -38.74296898 | 76.7825 | 53941.8167013889 | 2006-07-25 19:36:03 | 53943.0404976852 | 2006-07-27 00:58:19 | 701077010 | 47.8309 | 50 | 47.8309 | 47.8309 | 47.8309 | 47.8309 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 43.425 | 43.425 | 105.7299 | 1 | PROCESSED | 57535.0495023148 | 2016-05-27 01:11:17 | 54400 | 2007-10-27 00:00:00 | 53955.7322106482 | 2006-08-08 17:34:23 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012008 | We propose to observe with Suzaku the X-ray bright blazar RBS 315, showing a very hard spectrum (Gamma<1.2) in the 2-10 keV range as determined by XMM. The requested observation will allow us to measure the continuum in the full Suzaku range (0.3-200 keV), fully exploiting the unique capabilities of the satellite. With its wide energy coverage and good response at soft energies, Suzaku will allow to determine with precision the spectral properties of the source in the hard medium and soft X-ray ranges, providing important clues on the physics and the environment of relativistic jets. A good measurement of the continuum will allow us to determine the luminosity emitted via the IC mechanism which usually dominates the radiative output and the total kinetic power carried by the outflow. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | FABRIZIO TAVECCHIO | EUR | 1 | AO1 | SUZAKU OBSERVATION OF THE HARD BROAD BAND CONTINUUM OF THE POWERFUL BLAZAR RBS 315 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701077010/ | Quick Look | ![]() |
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163 | 3C 111 | 64.5741 | 38.0889 | 63.737568 | 37.967565 | 69.370671 | 16.452489 | 161.62276278 | -8.7838332 | 81.5451 | 54700.4141898148 | 2008-08-22 09:56:26 | 54703.1836111111 | 2008-08-25 04:24:24 | 703034010 | 122.378 | 120 | 122.386 | 122.378 | 0 | 122.378 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 109.7067 | 109.7067 | 239.2517 | 1 | PROCESSED | 57543.4018287037 | 2016-06-04 09:38:38 | 55084 | 2009-09-10 00:00:00 | 54713.6361226852 | 2008-09-04 15:16:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031332 | The origin of the high-energy emission from Broad-Line Radio Galaxies is still an open issue. A plausible scenario is reprocessed emission from a cold medium (disk) diluted by variable, non-thermal jet flux. To test this scenario we propose Suzaku observations of the BLRG 3C 111, which exhibits flux variability above 10 keV from available data, suggesting a jet contribution. Moreover, 3C 111 was previously detected with EGRET at GeV energies, and synergy with GLAST will thus be exploited in the proposed program. The coupled timing and spectral information provided by Suzaku are key to disentangle the disk and jet contributions, and determine their respective role for the source energy budget. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RITA SAMBRUNA | USA | 3 | AO3 | SUZAKU OBSERVATIONS OF 3C 111: UNCOVERING THE JET WITHIN | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703034010/ | Quick Look | ![]() |
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164 | 3C 326 | 238.0402 | 20.0989 | 237.485976 | 20.247377 | 230.081092 | 39.212111 | 33.27596058 | 48.22956027 | 119.5805 | 54484.6775 | 2008-01-19 16:15:36 | 54486.215462963 | 2008-01-21 05:10:16 | 702006010 | 61.7381 | 60 | 61.7381 | 61.7381 | 0 | 61.7381 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53.4126 | 53.4126 | 132.8598 | 1 | PROCESSED | 57541.3565162037 | 2016-06-02 08:33:23 | 54888 | 2009-02-26 00:00:00 | 54515.0338078704 | 2008-02-19 00:48:41 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020014 | Suzaku observations of two giant radio galaxies, 3C 326 and 3C 35, are proposed. In 60 ks exposure on the individual targets, inverse Component X-ray emission from their lobes is detected with high signal statistics. As a result, the energy densities of electrons and magnetic fields in these lobesare precisely deteremined. The size of these radio galaxies are significantly larger than that of the previous sample. Therefore, the size dependence of energetics in the lobes will be investigated. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | NAOKI ISOBE | JAP | 2 | AO2 | SUZAKU OBSERVATIONS OF LOBES OF GIANT RADIO GALAXIES, 3C 326 AND 3C 35 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702006010/ | Quick Look | ![]() |
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165 | SDSS J1723+5553 | 260.8912 | 55.8942 | 260.65651 | 55.938805 | 243.54174 | 78.493359 | 83.89291292 | 34.34970174 | 8.0654 | 54986.3677777778 | 2009-06-04 08:49:36 | 54986.8148032407 | 2009-06-04 19:33:19 | 704051010 | 35.9368 | 30 | 35.9448 | 35.9368 | 0 | 35.9528 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 29.0393 | 29.0393 | 38.6159 | 0 | PROCESSED | 57547.4618865741 | 2016-06-08 11:05:07 | 55364 | 2010-06-17 00:00:00 | 54998.1759722222 | 2009-06-16 04:13:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041422 | BALQSOs can be used to probe geometric and evolutionary models of quasars and AGN feedback. Recent studies have found larger (~2X) BALQSO fractions in NIR selected samples compared to those in optical samples and have suggested that the NIR samples of BALQSOs better represent the general population of BALQSOs. We propose to observe three bright, red 2MASS selected BALQSOs with Suzaku, to complement archival X-ray observations of BALQSOs that may have been biased by their selection on optical properties only. Combined with the archival sample, we will measure the average X-ray properties of BALQSOs. By comparing the hard X-ray to K_s band flux ratios at a range of optical to infrared colors, we will test the robustness of NIR selection and the origin of the large NIR BALQSO fraction. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | XINYU DAI | USA | 4 | AO4 | X-RAY PROPERTIES OF 2MASS SELECTED BALQSOS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704051010/ | Quick Look | ![]() |
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166 | PBC J0839.7-1214 | 129.9392 | -12.3029 | 129.345024 | -12.125278 | 136.15221 | -29.568931 | 237.21342575 | 17.37856511 | 291.8979 | 55324.6892824074 | 2010-05-08 16:32:34 | 55326.4896990741 | 2010-05-10 11:45:10 | 705007010 | 80.5643 | 80 | 80.5643 | 80.5643 | 0 | 80.5643 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.7418 | 70.7418 | 155.5358 | 1 | PROCESSED | 57551.4721759259 | 2016-06-12 11:19:56 | 55707 | 2011-05-26 00:00:00 | 55341.5690856482 | 2010-05-25 13:39:29 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050024 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Previously, such studies have been limited to AGNs with low to intermediate luminosities. Here we propose to observe two of the most luminous AGNs in the latest BAT catalog to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 5 | AO5 | BROAD BAND SPECTRA OF SWIFT/BAT SELECTED ULTRALUMINOUS AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705007010/ | Quick Look | ![]() |
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167 | NGC 3147 | 154.2433 | 73.3869 | 153.186306 | 73.636446 | 117.480978 | 56.071635 | 136.29780832 | 39.47682975 | 262.9224 | 55340.8248611111 | 2010-05-24 19:47:48 | 55343.2925231482 | 2010-05-27 07:01:14 | 705054010 | 150.0476 | 150 | 150.0476 | 150.0556 | 0 | 150.0556 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 132.9136 | 132.9136 | 213.1818 | 2 | PROCESSED | 57553.0649074074 | 2016-06-14 01:33:28 | 55765 | 2011-07-23 00:00:00 | 55393.4710648148 | 2010-07-16 11:18:20 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052013 | NGC3147 is the best candidate to be a true Seyfert 2, i.e., with no BLR. We propose a 150 ks observation with Suzaku to study the Fe line profile which in the short XMM-Newton observation shows some structure. If the iron line will turn out to be originated from the accretion disc, the lack of the BLR cannot be attributed to the lack of ionizing photons; if originated from the torus, this would put constraints on models assuming a common origin for the torus and the BLR; if the presence of an ionized iron line is confirmed, a BLR might exist but so highly ionized to be invisible at optical/UV wavelengths. An important added value of this observation is to confirm NGC3147 as a true Seyfert 2 by ruling out a Compton-thick nature, which only Suzaku can do thanks to its hard X-ray coverage. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GIORGIO MATT | EUR | 5 | AO5 | SUZAKU OBSERVATION OF THE BEST ``TRUE SEYFERT 2'' GALAXY CANDIDATE, NGC 3147 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705054010/ | Quick Look | ![]() |
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168 | NGC 7603 | 349.73 | 0.2557 | 349.089402 | -0.017972 | 350.656446 | 4.302592 | 80.07171077 | -54.72674929 | 67.5296 | 56080.5080208333 | 2012-06-02 12:11:33 | 56082.6598726852 | 2012-06-04 15:50:13 | 707003010 | 101.2567 | 100 | 101.2602 | 101.2657 | 0 | 101.2567 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 96.0023 | 96.0023 | 185.9037 | 2 | PROCESSED | 57605.6196875 | 2016-08-05 14:52:21 | 56464 | 2013-06-21 00:00:00 | 56096.2688541667 | 2012-06-18 06:27:09 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070010 | X-ray spectra from Seyfert galaxies often consist of various emission components such as from an accretion disk and dusty torus. Because of this complexity, interpretation of reprocessed feature (Fe lines and reflection continuum) in X-ray spectra is often ambiguous. We selected a Seyfert 1 with very weak mid infrared emission from the putative torus relative to X-rays from an accretin disk bu using AKARI IR and XMM X-ray catalogs. We will measure a ``pure'' accretion disk spectrum without contamination of reprocessed emission from the torus, and castrain extent of an accretion disk, which is expected to depend on an Eddington ratio, from the reprocessed X-ray emission. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YUICHI TERASHIMA | JAP | 7 | AO7 | PURE ACCRETION DISK SPECTRUM OF THE SEYFERT 1 NGC 7603 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707003010/ | Quick Look | ![]() |
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169 | LMC X-4 | 83.1804 | -66.3624 | 83.172059 | -66.39551 | 0.975905 | -87.276392 | 276.32693529 | -32.54034863 | 209.1491 | 54480.3607175926 | 2008-01-15 08:39:26 | 54480.7919560185 | 2008-01-15 19:00:25 | 702038010 | 21.6579 | 20 | 21.6726 | 21.6579 | 0 | 21.6726 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.8837 | 22.8837 | 37.252 | 0 | PROCESSED | 57541.3108796296 | 2016-06-02 07:27:40 | 54860 | 2009-01-29 00:00:00 | 54490.3089236111 | 2008-01-25 07:24:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021127 | We propose for a series of three 20ks observations of the binary X-ray pulsar LMC X-4. This source shows 13.5 s pulsations, a 1.4 d orbital period, and a long-period (~30 d) variability due to a warped, precessing accretion disk. The proposed analysis will use pulse-phase spectroscopy with XIS to explore changes in the X-ray pulses and spectra at three different phases in the disk precession. This work will give us a detailed picture of the accretion flow, particularly for the inner regions of the accretion disk that are illuminated by the X-rays from the neutron star. This project takes advantage of the strengths of the XIS, particularly its excellent spectral resolution, sufficient (1s) time resolution in Window mode, and wide PSF that limits pile-up effects. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RYAN HICKOX | USA | 2 | AO2 | SUPERORBITAL VARIATION OF LMC X-4: EXPLORING THE ACCRETION FLOW | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702038010/ | Quick Look | ![]() |
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170 | NGC5548 | 214.4969 | 25.1266 | 213.929993 | 25.356783 | 201.998856 | 36.406453 | 31.93001973 | 70.4949274 | 285.8791 | 54310.1810648148 | 2007-07-29 04:20:44 | 54311.0209953704 | 2007-07-30 00:30:14 | 702042070 | 31.8099 | 30 | 31.8099 | 31.8099 | 0 | 31.8099 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 29.503 | 29.503 | 72.5279 | 1 | PROCESSED | 57539.3547569444 | 2016-05-31 08:30:51 | 54706 | 2008-08-28 00:00:00 | 54339.4245486111 | 2007-08-27 10:11:21 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021307 | We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARTIN ELVIS | USA | 2 | AO2 | NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702042070/ | Quick Look | ![]() |
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171 | NGC 1365 | 53.3968 | -36.1347 | 52.919388 | -36.301683 | 36.801187 | -53.032832 | 237.94662462 | -54.6022242 | 221.6565 | 54486.2300578704 | 2008-01-21 05:31:17 | 54490.0002083333 | 2008-01-25 00:00:18 | 702047010 | 160.5057 | 150 | 160.5057 | 160.5137 | 0 | 160.5137 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 146.8139 | 146.8139 | 325.6768 | 4 | PROCESSED | 57541.4786342593 | 2016-06-02 11:29:14 | 54883 | 2009-02-21 00:00:00 | 54515.5847800926 | 2008-02-19 14:02:05 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021314 | We propose a 150 ksec observation of the Seyfert Galaxy NGC 1365. This galaxy have a unique set of properties: FeXXV and FeXXVI Kalpha and Kbeta absorption lines (the highest S/N detection so far among AGNs), rapidly varying cold absorber (nH variations of ~10^23/cm^2 in a few hours, changes from Compton-thick to Compton-thin in two days), a relativistic iron emission line. This new long observation will use at best the unique capabilities of Suzaku to constrain the dimensions of the absorbers, and, for the first time, will investigate the dynamics and physical conditions of the hot absorber responsible of the iron absorption lines. It is likely that an occultation will occur during the observation. This occultation would directly set the dimension of the X-ray source. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | GUIDO RISALITI | USA | 2 | AO2 | BLACK HOLE OCCULTATION AND OUTFLOW VARIABILITY IN NGC 1365 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702047010/ | Quick Look | ![]() |
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172 | NGC 6300 | 259.2549 | -62.8185 | 258.083078 | -62.76377 | 263.641528 | -39.613132 | 328.49505458 | -14.05378352 | 296.7285 | 54390.5141087963 | 2007-10-17 12:20:19 | 54392.375162037 | 2007-10-19 09:00:14 | 702049010 | 82.577 | 80 | 82.577 | 82.577 | 0 | 82.577 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 105.5127 | 105.5127 | 160.7798 | 1 | PROCESSED | 57540.3276041667 | 2016-06-01 07:51:45 | 54770 | 2008-10-31 00:00:00 | 54403.3802083333 | 2007-10-30 09:07:30 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021331 | Recent X-ray observations of Seyfert 2 galaxies have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by AGN Unified Schemes. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (60 ksec each) of four local bright Compton-thin Seyfert2s, selected from the Swift/BAT survey with a hard X-ray flux exceeding 1e-10 cgs to form a flux-limited sample. The unprecedented broad bandpass of Suzaku offers a unique tool to investigate the X-ray emission, placing strong constraints on the geometry and location of the reprocessing matter. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | JAMES REEVES | USA | 2 | AO2 | REVEALING THE REPROCESSING MATTER IN SEYFERT 2 GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702049010/ | Quick Look | ![]() |
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173 | PKS1127-145 | 172.5274 | -14.8245 | 171.896651 | -14.548647 | 179.186436 | -16.542663 | 275.2785401 | 43.63731171 | 115.9184 | 54799.7571180556 | 2008-11-29 18:10:15 | 54800.9523611111 | 2008-11-30 22:51:24 | 703004010 | 55.5451 | 40 | 55.5511 | 55.5451 | 0 | 55.5511 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31.0123 | 31.0123 | 103.2488 | 0 | PROCESSED | 57544.5555208333 | 2016-06-05 13:19:57 | 54557 | 2008-04-01 00:00:00 | 54809.1987152778 | 2008-12-09 04:46:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030004 | We propose intensive Suzaku observations of 11 "VIP" blazars with 40ksec each, as a long-category project. We stress that all of the sources will be monitored simultaneously by GLAST (GeV), Swift XRT/UVOT (UV to X-ray), as well as ground-based radio-to-optical telescopes. We will obtain the broadband spectra and light-curves from 10^9 Hz to 10^25 Hz, which reveals for the first time the nature of gamma-loud blazars in their quiescent states. The proposed 40ksec x 11 Suzaku observations will allow us to investigate | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 3 | AO3 | REVEALING THE NATURE OF GAMMA-LOUD BLAZARS VIA SUZAKU/GLAST AND WORLD-WIDE GROUND-BASED OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703004010/ | Quick Look | ![]() |
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174 | ESO 506-G027 | 189.6943 | -27.3584 | 189.030338 | -27.083667 | 200.074921 | -21.229266 | 299.48164005 | 35.42851647 | 302.0467 | 54314.0460300926 | 2007-08-02 01:06:17 | 54315.2572222222 | 2007-08-03 06:10:24 | 702080010 | 41.7453 | 40 | 41.7533 | 41.7613 | 0 | 41.7453 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 38.2828 | 38.2828 | 104.6399 | 2 | PROCESSED | 57539.3906134259 | 2016-05-31 09:22:29 | 54710 | 2008-09-01 00:00:00 | 54340.5553125 | 2007-08-28 13:19:39 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021374 | Though Compton thick AGN are expected to constitute a sizable fraction of the Seyfert population (Maiolino et al 1998 and Risaliti et al 1999), the fraction and the signatures of Compton thick AGN is unknown. The SWIFT BAT all-sky AGN survey has detected a complete sample of AGN with flux > 1-3e-11 erg/cm^2/s in the 15-200 keV band. At this energy range, the effects of heavy obscuration are minimal and thus BAT will allow us to determine the true fraction of Compton-thick sources. However, the BAT spectra are not simultaneous with XRT and XRT does not have the spectral resolution (with 10 ks) necessary to characterize a heavily absorbed 0.3-10 keV spectrum. We propose HXD nominal Suzaku observations of 4 possible Compton thick sources for which we recently obtained XMM 10 ks follow-ups. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RICHARD MUSHOTZKY | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF POSSIBLY COMPTON THICK AGN FROM THE SWIFT BAT SURVEY | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702080010/ | Quick Look | ![]() |
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175 | NGC 788 | 30.262 | -6.7593 | 29.638132 | -7.000547 | 25.672425 | -17.884233 | 165.15039638 | -63.76864601 | 77.358 | 54660.0353819444 | 2008-07-13 00:50:57 | 54661.0516666667 | 2008-07-14 01:14:24 | 703032010 | 45.9073 | 40 | 45.9153 | 45.9073 | 0 | 45.9153 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 39.594 | 39.594 | 87.7999 | 0 | PROCESSED | 57543.0405902778 | 2016-06-04 00:58:27 | 55048 | 2009-08-05 00:00:00 | 54682.1458564815 | 2008-08-04 03:30:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031323 | The classical unified model predicts only one type of Seyfert II (Sy2). Recent observations of SWIFT BAT-detected AGN found at least 4 classes of Sy2s: (1) objects with high column density and scattered soft x-rays, (2) Compton thick objects, (3) `hidden' AGN (Ueda et al. 2007), and (4) the `changing look' objects (Risaliti et al. 2006). The nature of these sources can only be revealed with high quality broad-band X-ray spectra from Suzaku. Thus, we are proposing 40ks observations for 2 of the brightest BAT AGN without high quality data, NGC 788, a type (3) object showing polarized optical broad lines, and NGC 3281, a classified (2) object. Such observations are necessary to build a reasonably large sample of high-quality, broad-band Sy2 spectra covering the range of X-ray/optical types. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RICHARD MUSHOTZKY | USA | 3 | AO3 | SUZAKU OBSERVATIONS OF X-RAY BRIGHT TYPE II AGN | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703032010/ | Quick Look | ![]() |
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176 | Q0122-380 | 21.0759 | -37.7461 | 20.512127 | -38.006435 | 1.342949 | -42.439189 | 271.91657466 | -77.33125236 | 48.7944 | 54615.4511921296 | 2008-05-29 10:49:43 | 54616.2009722222 | 2008-05-30 04:49:24 | 703035010 | 28.481 | 25 | 28.481 | 28.489 | 0 | 28.497 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.8107 | 26.8107 | 64.7699 | 1 | PROCESSED | 57542.6524421296 | 2016-06-03 15:39:31 | 54999 | 2009-06-17 00:00:00 | 54633.6971759259 | 2008-06-16 16:43:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031334 | Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GEORGE CHARTAS | USA | 3 | AO3 | A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703035010/ | Quick Look | ![]() |
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177 | Q0551-3637 | 88.2026 | -36.6158 | 87.768837 | -36.625605 | 87.11791 | -60.039805 | 242.36930247 | -26.91846995 | 296.4731 | 54575.4385763889 | 2008-04-19 10:31:33 | 54575.6251041667 | 2008-04-19 15:00:09 | 703036010 | 3.8954 | 22 | 3.8954 | 3.8954 | 0 | 3.8954 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3.773 | 3.773 | 16.0959 | 0 | PROCESSED | 57542.3345601852 | 2016-06-03 08:01:46 | 54979 | 2009-05-28 00:00:00 | 54588.1227314815 | 2008-05-02 02:56:44 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031334 | Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GEORGE CHARTAS | USA | 3 | AO3 | A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703036010/ | Quick Look | ![]() |
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178 | Q0109-3518 | 17.9376 | -35.0527 | 17.356449 | -35.318066 | 0.204002 | -38.849268 | 275.45528409 | -80.96443984 | 40.3411 | 54606.0677199074 | 2008-05-20 01:37:31 | 54606.6772453704 | 2008-05-20 16:15:14 | 703037010 | 29.9585 | 18 | 29.9665 | 29.9585 | 0 | 29.9665 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22.8339 | 22.8339 | 52.6559 | 1 | PROCESSED | 57542.5808101852 | 2016-06-03 13:56:22 | 54982 | 2009-05-31 00:00:00 | 54616.3810300926 | 2008-05-30 09:08:41 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031334 | Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GEORGE CHARTAS | USA | 3 | AO3 | A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703037010/ | Quick Look | ![]() |
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179 | IRASF11223-1244 | 171.2239 | -12.9662 | 170.593283 | -12.69128 | 177.194404 | -15.365769 | 272.54538498 | 44.73919633 | 107.3062 | 54064.7275347222 | 2006-11-25 17:27:39 | 54065.5709953704 | 2006-11-26 13:42:14 | 701008010 | 40.9415 | 40 | 41.1015 | 40.9415 | 0 | 41.1095 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 37.6804 | 37.6804 | 72.8639 | 1 | PROCESSED | 57536.1775925926 | 2016-05-28 04:15:44 | 54735 | 2008-09-26 00:00:00 | 54088.8556828704 | 2006-12-19 20:32:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010038 | The source of huge energy output from ultraluminous infrared galaxies (ULIRGs) is still under debate. We propose to search for a hidden QSO as the energy source by observing ULIRGs with high luminosity optical emission lines classified as a Seyfert 2. The data will be used to constrain the power of the central AGN and to study the nature of infrared selected type 2 QSOs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YUICHI TERASHIMA | JAP | 1 | AO1 | A SEARCH FOR HIDDEN QSO IN ULTRALUMINOUS INFRARED GALAXIES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701008010/ | Quick Look | ![]() |
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180 | MRK 0359 | 21.8893 | 19.1757 | 21.213343 | 18.916781 | 27.368924 | 9.282102 | 134.6025573 | -42.87605962 | 244.6178 | 54137.9789699074 | 2007-02-06 23:29:43 | 54140.3738078704 | 2007-02-09 08:58:17 | 701082010 | 107.507 | 100 | 107.507 | 107.507 | 0 | 107.507 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102.5761 | 102.5761 | 206.8678 | 2 | PROCESSED | 57537.3689930556 | 2016-05-29 08:51:21 | 54735 | 2008-09-26 00:00:00 | 54151.5150925926 | 2007-02-20 12:21:44 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012023 | Markarian 359 was the first source to be identified as a Narrow Line Seyfert 1 (NLS1) AGN, and its importance as an unusual source has been recognised for a long time. In the optical, it has unusually narrow lines for a NLS1. X-ray observations of the source are rare, but based on an XMM-Newton observation a strong reflection 'hump' is predicted. The source is therefore a critical one in the investigation of relativistically blurred photoionized disc reflection models. A detailed Suzaku observation will provide improved data quality in the XIS waveband, allow investigation of spectral variability in this waveband, and constrain the amount of reflection independently by using the HXD. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | JAMIE CRUMMY | EUR | 1 | AO1 | NVESTIGATING REFLECTION IN MARKARIAN 359 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701082010/ | Quick Look | ![]() |
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181 | IC1586 | 11.9805 | 22.3783 | 11.316843 | 22.105657 | 19.903516 | 15.841027 | 121.86323541 | -40.48615304 | 70.9045 | 55006.4686458333 | 2009-06-24 11:14:51 | 55007.0280555556 | 2009-06-25 00:40:24 | 704005010 | 23.5306 | 20 | 23.5306 | 24.3466 | 0 | 24.3546 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.2778 | 22.2778 | 48.3259 | 0 | PROCESSED | 57547.6510648148 | 2016-06-08 15:37:32 | 55385 | 2010-07-08 00:00:00 | 55019.1259259259 | 2009-07-07 03:01:20 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040049 | We propose the first X-ray follow-up observations of 4 gamma-ray bright Seyferts and starburst galaxy, recently discovered by Fermi gamma-ray space telescope. The detection of GeV emission provides new evidence for relativistic jets in radio-quiet AGNs, but steep gamma-ray spectrum as well as an exotic spectral energy distribution (where GeV flux is 2-4 orders of magnitude brighter than radio) indicates that non-thermal emission is relatively weak, and less enhanced compared to radio-loud AGNs. Throughout multiwavelength observations including Suzaku and Fermi satellites, we will investigate the jet power, accretion rate and line intensity of these new comers (i.e., gamma-loud Seyferts) towards the unification scheme of radio-loud and radio-quiet AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF GAMMA-LOUD SEYFERTS AND STARBURST GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704005010/ | Quick Look | ![]() |
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182 | 3C120 | 68.2984 | 5.3555 | 67.633855 | 5.251051 | 67.433469 | -16.402094 | 190.37315865 | -27.39441526 | 237.4585 | 53775.1527199074 | 2006-02-09 03:39:55 | 53776.2433217593 | 2006-02-10 05:50:23 | 700001010 | 41.9321 | 160 | 41.9321 | 41.9321 | 41.9321 | 41.9321 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 34.0941 | 34.0941 | 94.2219 | 1 | PROCESSED | 57532.9769791667 | 2016-05-24 23:26:51 | 54247 | 2007-05-27 00:00:00 | 53906.2470601852 | 2006-06-20 05:55:46 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001003 | Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 0 | SWG | BROAD-BAND MONITORING OF 3C120 IN VARIOUS ACCRETING STATES | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700001010/ | Quick Look | ![]() |
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183 | PKS2155-304 | 329.7191 | -30.2247 | 328.99529 | -30.464273 | 321.189186 | -16.770975 | 17.73226544 | -52.24760927 | 254.1358 | 53704.7749884259 | 2005-11-30 18:35:59 | 53706.3613888889 | 2005-12-02 08:40:24 | 700012010 | 63.9114 | 80 | 63.9194 | 63.9114 | 63.9194 | 63.9166 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 58.0114 | 58.0114 | 137.0498 | 3 | PROCESSED | 57532.3797685185 | 2016-05-24 09:06:52 | 54247 | 2007-05-27 00:00:00 | 54038.8920138889 | 2006-10-30 21:24:30 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001100 | Jets in blazars are believed to be a powerful site of particle acceleration. TeV emitting blazars are very important, because we can study very end of electron distribution near the maximum energy by using X-ray spectrum, because X-ray emission is believed to be due to synchrotron emission from the higher energy electron. Comparison of spectral index between X-ray and TeV gives us a crucial information on these source, because this is very sensitive to the particle injection and rapid cooling. In order to maximize the capability of sensitive hard X-ray observations of Suzaku, we propose reserved TOO observations for the next six months of PV phase from the TeV emitting blazars established by HESS, selected from five candidates. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TADAYUKI TAKAHASHI | JAP | 0 | SWG-TOO | RESERVED TOO OBSERVATIONS OF SELECTED TEV-BRIGHT BLAZARS | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700012010/ | Quick Look | ![]() |
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184 | PKS 0558-504 | 89.9324 | -50.4401 | 89.628897 | -50.441186 | 89.861567 | -73.881962 | 257.95192858 | -28.57760064 | 211.3321 | 54120.8400925926 | 2007-01-20 20:09:44 | 54121.3279976852 | 2007-01-21 07:52:19 | 701011040 | 19.7381 | 20 | 19.7541 | 19.7381 | 0 | 19.7541 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17.175 | 17.175 | 42.1359 | 0 | PROCESSED | 57536.8909953704 | 2016-05-28 21:23:02 | 54735 | 2008-09-26 00:00:00 | 54137.1036921296 | 2007-02-06 02:29:19 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010057 | Narrow-line Seyfert 1 Galaxies (NLS1s) must have been crucial key to understand the rapid growth of the central supermassive black hole, which may be related to the evolution of the host galaxy. Hence, we propose 20x5 ksec observations of the luminous NLS1 galaxy PKS 0558-504, which is the candidate having the highest mass-accretion rate among the class. Large effective area and good energy resolution of XISs allow us to strictly constrain the temperature and the luminosity of the accretion flow. In addition, Suzaku HXD will detect the significant fraction of hard power law emission in the 10-60 keV band for the first time. From these observations, we expect to derive the new picture of the high mass-accretion mechanism in NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YOSHITO HABA | JAP | 1 | AO1 | SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701011040/ | Quick Look | ![]() |
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185 | SWIFT J0255.2-0011 | 43.8161 | -0.2397 | 43.176621 | -0.441669 | 41.282729 | -16.217011 | 175.95402612 | -49.91735431 | 256.3177 | 54123.6209490741 | 2007-01-23 14:54:10 | 54126.2294560185 | 2007-01-26 05:30:25 | 701013010 | 101.6321 | 100 | 101.6321 | 101.6321 | 0 | 101.6321 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86.2824 | 86.2824 | 225.3379 | 3 | PROCESSED | 57536.9811342593 | 2016-05-28 23:32:50 | 54735 | 2008-09-26 00:00:00 | 54137.3009027778 | 2007-02-06 07:13:18 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010122 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of type-2 AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many new type-2 AGNs that can be best followed-up with Suzaku. Here we propose to observe two of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. This proposal is complementary to our separate proposal entitled "direct determination of the fraction of Compton-thick AGNs in the local universe". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 1 | AO1 | BROAD BAND SPECTRA OF NEW SWIFT/BAT AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701013010/ | Quick Look | ![]() |
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186 | ESO 428-G014 | 109.1256 | -29.3248 | 108.632746 | -29.234716 | 116.992827 | -50.987581 | 241.87528565 | -7.96864273 | 123.1273 | 55516.1372569445 | 2010-11-16 03:17:39 | 55518.5508680556 | 2010-11-18 13:13:15 | 705008010 | 82.8873 | 80 | 82.9033 | 82.8873 | 0 | 82.9033 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 68.4518 | 68.4518 | 208.5016 | 2 | PROCESSED | 57554.1967361111 | 2016-06-15 04:43:18 | 55898 | 2011-12-03 00:00:00 | 55530.4256597222 | 2010-11-30 10:12:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050031 | Non-Hidden Broad Line Region Seyfert 2 galaxies (NHBLR Sey2s) are classified as Seyfert 2 galaxies without broad Balmer lines even in the polarized light. One possible interpretation for the absence of broad lines is that NHBLR Sey2s are viewed from an extreme edge-on direction, so that the scattered light is obscured by the accretion torus. Hence observation of NHBLR Sey2s provides us the unique opportunity to investigate the densest region of the torus. We, therefore, propose 80 ksec observation of NHBLR Sey2 ESO 428-G014. High sensitivity throughout the 0.5-70 keV wide energy band of Suzaku allows us to strictly constrain the intrinsic X-ray luminosity and column density of the obscuring material. From our observation, we expect to derive more complete unified picture of AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YOSHITO HABA | JAP | 5 | AO5 | SUZAKU VIEW OF NON-HIDDEN BROAD LINE REGION SEYFERT 2 GALAXY ESO 428-G014 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705008010/ | Quick Look | ![]() |
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187 | SWIFT J0505.7-2348 | 76.4285 | -23.9055 | 75.907939 | -23.972083 | 71.84647 | -46.496539 | 225.00444872 | -33.15769393 | 284.9903 | 53826.9254166667 | 2006-04-01 22:12:36 | 53829.1216898148 | 2006-04-04 02:55:14 | 701014010 | 78.5544 | 80 | 78.5544 | 78.5544 | 78.5544 | 78.5544 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 53.4937 | 53.4937 | 189.6979 | 1 | PROCESSED | 57533.4023726852 | 2016-05-25 09:39:25 | 54439 | 2007-12-05 00:00:00 | 53945.2822569444 | 2006-07-29 06:46:27 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010122 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of type-2 AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many new type-2 AGNs that can be best followed-up with Suzaku. Here we propose to observe two of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. This proposal is complementary to our separate proposal entitled "direct determination of the fraction of Compton-thick AGNs in the local universe". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 1 | AO1 | BROAD BAND SPECTRA OF NEW SWIFT/BAT AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701014010/ | Quick Look | ![]() |
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188 | IRAS 01250+2832 | 21.9819 | 28.787 | 21.285155 | 28.528242 | 31.216552 | 18.139977 | 132.5132824 | -33.40495941 | 250.843 | 55571.3211805556 | 2011-01-10 07:42:30 | 55572.5926388889 | 2011-01-11 14:13:24 | 705024010 | 57.5829 | 50 | 57.5829 | 57.5829 | 0 | 57.5829 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54.8082 | 54.8082 | 109.8299 | 1 | PROCESSED | 57600.6088194444 | 2016-07-31 14:36:42 | 55962 | 2012-02-05 00:00:00 | 55595.2272569444 | 2011-02-03 05:27:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050074 | We propose Suzaku XIS and HXD/PIN observations of two buried Active Galactic Nuclei(AGNs) at z=0.04 which are discovered by the AKARI mid-infrared all-sky survey. Both objects only show AGN features in AKARI near- and mid-infrared obsevations, while there are no clues of AGN presence in previous X-ray survey of ROSAT, radio 20cm, near-infrared photometries of 2MASS and detail optical spectroscopic data. These results indicate that a central engine of the AGN is completely buried and the nature of this population of AGNs is only poorly understood. Therefore, the hard X-ray observations is needed in order to confirm the AGN presence as well as to estimate the amount of absorption component and the AGN energy. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | SHINKI OYABU | JAP | 5 | AO5 | SUZAKU SEARCH FOR DIRECT EVIDENCE OF SUPER MASSIVE BLACK HOLES IN BURIED ACTIVE GALACTIC NUCLEI DISCOVERED BY AKARI | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705024010/ | Quick Look | ![]() |
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189 | IRAS 00521-7054 | 13.5029 | -70.6421 | 13.04558 | -70.91316 | 316.631077 | -63.690795 | 302.62218098 | -46.48460341 | 40.2116 | 56431.8840740741 | 2013-05-19 21:13:04 | 56434.2543287037 | 2013-05-22 06:06:14 | 708005010 | 103.045 | 100 | 103.053 | 103.045 | 0 | 103.053 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 87.3405 | 87.3405 | 204.7697 | 1 | PROCESSED | 57611.3837152778 | 2016-08-11 09:12:33 | 56809 | 2014-06-01 00:00:00 | 56443.6034259259 | 2013-05-31 14:28:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080036 | The existence of a broad iron line in AGN is still very debated. Amongst the several claims of detection of broad iron lines performed in the last decade, that of IRAS 00521-7054 is one of the most surprising. This type-2 object appears to show in fact an extremely broadened iron line, which would require a maximally rotating supermassive black hole and the presence of light bending. However, due to the lack of high-quality broadband studies, alternative explanations, as a clumpy-absorbers scenario, cannot be ruled out. The aim of this proposal is to perform a 100ks observation of IRAS 00521-7054. Thanks to its large band coverage and its good sensitivity in the iron-line region, Suzaku will allow us to clearly understand the origin of the intriguing spectral features of IRAS 00521-7054. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | CLAUDIO RICCI | JAP | 8 | AO8 | UNDERSTANDING THE ORIGIN OF THE PECULIAR X-RAY SPECTRAL FEATURES OF THE SEYFERT 2 IRAS 00521-7054 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708005010/ | Quick Look | ![]() |
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190 | NGC 526A | 20.9794 | -35.0729 | 20.408158 | -35.333404 | 3.010528 | -40.076485 | 263.77547728 | -79.45131683 | 257.0195 | 55578.7592939815 | 2011-01-17 18:13:23 | 55580.6404050926 | 2011-01-19 15:22:11 | 705044010 | 72.9346 | 70 | 72.9346 | 72.9346 | 0 | 72.9346 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 63.1372 | 63.1372 | 162.4977 | 2 | PROCESSED | 57600.6980324074 | 2016-07-31 16:45:10 | 55961 | 2012-02-04 00:00:00 | 55595.4905671296 | 2011-02-03 11:46:25 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051434 | The Compton-thin NELG NGC 526a has large hard X-ray variability and likely an abnormally flat photon index, Gamma near 1.6. We request two observations of 70 ks each, spaced six months apart, to accurately constrain Compton reflection and obtain geometrical constraints on the accreting material to test Seyfert unification schemes, as well as constrain coronal power law parameters. Importantly, we will track long-term spectral variability to constrain the location and nature of the reflecting material. We also will resolve the moderately broad Fe K alpha line, which may indicate the presence of a truncated accretion disk, and thus constrain the amount of reflection off an accretion disk versus that from a torus. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | ALEX MARKOWITZ | USA | 5 | AO5 | COMPTON REFLECTION AND LONG-TERM SPECTRAL VARIABILITY IN THE SEYFERT AGN NGC 526A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705044010/ | Quick Look | ![]() |
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191 | SWIFT J0138.6-4001 | 24.6022 | -39.9757 | 24.058156 | -40.229446 | 3.045259 | -45.758208 | 268.75310615 | -73.8819888 | 44.7851 | 53890.7590740741 | 2006-06-04 18:13:04 | 53891.2085532407 | 2006-06-05 05:00:19 | 701015010 | 21.1979 | 20 | 21.2139 | 21.1979 | 21.2139 | 21.2139 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 17.4771 | 17.4771 | 38.8319 | 1 | PROCESSED | 57534.4839814815 | 2016-05-26 11:36:56 | 54394 | 2007-10-21 00:00:00 | 53926.7722337963 | 2006-07-10 18:32:01 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010133 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 1 | AO1 | DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701015010/ | Quick Look | ![]() |
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192 | SWIFT J0350.1-5019 | 57.5863 | -50.3518 | 57.229549 | -50.501821 | 28.784936 | -67.035424 | 259.75531799 | -48.98660415 | 277.9348 | 54162.2927777778 | 2007-03-03 07:01:36 | 54162.5036921296 | 2007-03-03 12:05:19 | 701017030 | 8.1487 | 10 | 8.1567 | 8.1487 | 0 | 8.1567 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.0597 | 7.0597 | 18.2159 | 0 | PROCESSED | 57537.5866898148 | 2016-05-29 14:04:50 | 54750 | 2008-10-11 00:00:00 | 54167.6235763889 | 2007-03-08 14:57:57 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010133 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 1 | AO1 | DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701017030/ | Quick Look | ![]() |
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193 | TON S180 | 14.333 | -22.3803 | 13.720307 | -22.650448 | 3.73482 | -26.131336 | 138.98529016 | -85.06726133 | 237.1425 | 54078.5680671296 | 2006-12-09 13:38:01 | 54081.3584953704 | 2006-12-12 08:36:14 | 701021010 | 120.6609 | 120 | 120.6849 | 120.6609 | 0 | 120.6769 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 109.3128 | 109.3128 | 241.052 | 3 | PROCESSED | 57536.3458680556 | 2016-05-28 08:18:03 | 54735 | 2008-09-26 00:00:00 | 54094.4773958333 | 2006-12-25 11:27:27 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010141 | TON S180 is a luminous Narrow Line Seyfert 1 galaxy, chracterizing enhanced Soft X-ray emission component without complex absorption/emission structures. The source is considered to be at super Eddington accretion rate. We aim to track change (or no change) in soft X-ray spectrum of this source according to factor of two ,rapid flux variation this source show. We partciularly focus on the slim disk model propsed for super Eddington accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | KIYOSHI HAYASHIDA | JAP | 1 | AO1 | SOFT X-RAY EMISSION FROM SUPER-EDDINGTON ACCRETION DISK IN TON S180 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701021010/ | Quick Look | ![]() |
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194 | MARKARIAN 335 | 1.5539 | 20.2624 | 0.911019 | 19.984083 | 9.744165 | 17.917566 | 108.74842011 | -41.36053721 | 68.4831 | 53907.0624537037 | 2006-06-21 01:29:56 | 53910.7585532407 | 2006-06-24 18:12:19 | 701031010 | 151.2884 | 150 | 151.2964 | 151.2884 | 151.2964 | 151.2964 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 140.9812 | 140.9812 | 319.3028 | 4 | PROCESSED | 57534.8340046296 | 2016-05-26 20:00:58 | 54401 | 2007-10-28 00:00:00 | 53928.5392361111 | 2006-07-12 12:56:30 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011323 | We propose to observe the two Seyfert 1 galaxies Mrk 335 and ESO198-G024 for a total exposure of 150 ks each with the high sensitivity and broad band coverage of the Suzaku satellite. Both sources show a broad Fe K line and a strong soft excess. One appealing explanation for the nature of the soft excess is reflection. Fundamental to this hypothesis is the assumption that the same self-consistent reflection spectrum explains the Fe K line (including its shape), the soft excess, and also the Compton reflection hump above 20 keV. Suzaku's ability to measure all three reflection components simultaneously enables the different spectral models to be disentangled and reflection to be strongly tested. Understanding black hole accretion is fundamental to NASA's "SEU" theme. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | JON MILLER | USA | 1 | AO1 | REVEALING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701031010/ | Quick Look | ![]() |
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195 | NGC 1068 | 40.6928 | -0.0667 | 40.052721 | -0.278811 | 38.248989 | -15.097296 | 172.18986515 | -51.95763403 | 248.588 | 54141.0038078704 | 2007-02-10 00:05:29 | 54141.9168287037 | 2007-02-10 22:00:14 | 701039010 | 41.6229 | 35 | 41.6309 | 41.6309 | 0 | 41.6229 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.8024 | 41.8024 | 78.8839 | 0 | PROCESSED | 57537.346875 | 2016-05-29 08:19:30 | 54525 | 2008-02-29 00:00:00 | 54151.5012962963 | 2007-02-20 12:01:52 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011333 | The majority of accretion onto supermassive black holes in the local Universe occurs in obscured Seyferts. At moderate redshifts, the optical narrow emission-lines used to identify Seyfert 2s become difficult to isolate from the host galaxy's emission, resulting in an underestimate of the numbers of Seyfert 2s. Seyfert 2s are a critical component of AGN synthesis models of the Cosmic X-ray Background (CXB), as these sources are likely responsible for the unresolved component of the 2-8 keV background and may also contribute significantly to the 30 keV background. We propose to use Suzaku observations of ten local Seyfert 2s to measure their ultrahard (>10 keV) emission and examine how Seyfert 2s at moderate redshifts contribute to the CXB. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | AARON STEFFEN | USA | 1 | AO1 | MEASURING THE ULTRAHARD X-RAY EMISSION OF A LOCAL POPULATION OF SEYFERT 2S | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701039010/ | Quick Look | ![]() |
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196 | MARKARIAN 509 | 311.0427 | -10.7271 | 310.361616 | -10.908673 | 310.545205 | 7.124386 | 35.96837179 | -29.85867019 | 254.3019 | 54022.3263888889 | 2006-10-14 07:50:00 | 54023.0856365741 | 2006-10-15 02:03:19 | 701093020 | 25.9298 | 25 | 25.9618 | 25.9298 | 25.9538 | 25.9618 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 23.4497 | 23.4497 | 65.5899 | 1 | PROCESSED | 57535.8399305556 | 2016-05-27 20:09:30 | 54526 | 2008-03-01 00:00:00 | 54053.6032638889 | 2006-11-14 14:28:42 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012050 | We propose to perform 4 repeated Suzaku observations of 25 ks each of the Seyfert 1 galaxy MKN 509, the brightest Seyfert galaxy of the Piccinotti sample in the 2-100 keV band that is not strongly affected by neutral or ionized absorbing material. The aim of the study is to disentangle the different physical explanations for the origin of the soft excess looking at the long time--scale correlations between the variations of the emission and shape of the soft excess and the emission at high energy (E > 10 keV). | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GABRIELE PONTI | EUR | 1 | AO1 | SOLVING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701093020/ | Quick Look | ![]() |
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197 | MARKARIAN 509 | 311.0451 | -10.7278 | 310.364015 | -10.909382 | 310.547312 | 7.12309 | 35.96880101 | -29.86110163 | 254.2048 | 54066.1625810185 | 2006-11-27 03:54:07 | 54067.12875 | 2006-11-28 03:05:24 | 701093040 | 33.0944 | 32 | 33.0944 | 33.0944 | 0 | 33.0944 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29.4544 | 29.4544 | 83.4659 | 1 | PROCESSED | 57536.2044212963 | 2016-05-28 04:54:22 | 54456 | 2007-12-22 00:00:00 | 54088.5895023148 | 2006-12-19 14:08:53 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012050 | We propose to perform 4 repeated Suzaku observations of 25 ks each of the Seyfert 1 galaxy MKN 509, the brightest Seyfert galaxy of the Piccinotti sample in the 2-100 keV band that is not strongly affected by neutral or ionized absorbing material. The aim of the study is to disentangle the different physical explanations for the origin of the soft excess looking at the long time--scale correlations between the variations of the emission and shape of the soft excess and the emission at high energy (E > 10 keV). | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GABRIELE PONTI | EUR | 1 | AO1 | SOLVING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701093040/ | Quick Look | ![]() |
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198 | PKS 1510-089 | 228.2108 | -9.1043 | 227.537329 | -8.917552 | 228.287746 | 8.492539 | 351.2856545 | 40.1353659 | 286.8003 | 53949.3968634259 | 2006-08-02 09:31:29 | 53952.2544444445 | 2006-08-05 06:06:24 | 701094010 | 119.1577 | 120 | 119.1577 | 119.1577 | 119.1657 | 119.1657 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 106.2588 | 106.2588 | 246.8638 | 5 | PROCESSED | 57535.1605208333 | 2016-05-27 03:51:09 | 54394 | 2007-10-21 00:00:00 | 54018.7363194444 | 2006-10-10 17:40:18 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 013016 | It has been a long mystery (i) how the relativistic jets are formed, and (ii) what is the composition of a jet. In the theoretical view, strong magnetic field (u_B >> u_e) is necessary to produce such outflows with baryonic matters, but observations favor opposite scenario, namely particle dominated (u_e >> u_B), leptonic jet. Such discrepancies can be resolved if moderate numbers of protons (n_e/n_p > 50) are mixed in the non-tnermal pair populations. This can be easily tested if we can observe characteristic "soft X-ray bump" produced by the bulk-Comptonization of UV photons emitted from an accretion disk. We propose a deep observation (40ksec x3) of an EGRET quasar PKS 1510-089, which shows a clear sign of soft X-ray bump in BeppoSAX, ROSAT and ASCA observations. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | JUN KATAOKA | GRZEGORZ MADEJSKI | JUS | 1 | AO1 | DIRECT TESTING THE JET COMPOSITION IN A POWERFUL EGRET QUASAR PKS 1510-089 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701094010/ | Quick Look | ![]() |
199 | NGC5135 | 201.4174 | -29.8897 | 200.719488 | -29.629866 | 211.188294 | -19.343803 | 311.72101463 | 32.39717213 | 286.1252 | 54284.2497800926 | 2007-07-03 05:59:41 | 54285.3057175926 | 2007-07-04 07:20:14 | 702005010 | 52.4964 | 50 | 52.4964 | 52.4964 | 0 | 52.4964 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.7837 | 49.7837 | 91.2209 | 2 | PROCESSED | 57539.1022222222 | 2016-05-31 02:27:12 | 54696 | 2008-08-18 00:00:00 | 54328.4497453704 | 2007-08-16 10:47:38 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020005 | Compton thick Seyfert 2 galaxies may constitute a large fraction of the Seyfert 2 galaxy's population. However, the nature of the Compton-thick objects is still unclear due to the heavy obscuration of the nuclear emission. The wide-band spectroscopy with Suzaku is crucial to expose their nature hidden by thick matter. In order to reveal their nature in the local Universe, we propose Suzaku observations of Risaliti's Compton-thick objects. These observations will also bring us important results to study the structure and evolution of active galactic nuclei. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HISAMITSU AWAKI | JAP | 2 | AO2 | REVEAL THE NATURE OF COMPTON THICK SEYFERT 2 GALAXIES WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702005010/ | Quick Look | ![]() |
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200 | NGC5643 | 218.1422 | -44.2268 | 217.336243 | -44.006582 | 230.485298 | -27.635672 | 321.40267054 | 14.9878026 | 293.4229 | 54331.8795023148 | 2007-08-19 21:06:29 | 54332.9724421296 | 2007-08-20 23:20:19 | 702010010 | 42.8823 | 50 | 42.8903 | 42.8903 | 0 | 42.8823 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.8685 | 40.8685 | 94.386 | 2 | PROCESSED | 57539.6330902778 | 2016-05-31 15:11:39 | 54770 | 2008-10-31 00:00:00 | 54402.2016782407 | 2007-10-29 04:50:25 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020034 | Seyfert 2 galaxies often have an nucleus obscured by thick matter. Risaliti et al. found that Compton thick Seyfert 2 galaxies may constitute a large fraction of the Seyfert 2 galaxy s population by studying the distribution of absorbing column densities among Seyfert 2 galaxies. This result is important to discuss on the structure and evolution of active galactic nuclei. However, it is difficult to classify Seyfert 2 galaxies into Compton thick and thin objects only by using their X-ray spectra below 10 keV. Therefore, there may be Compton thin objects among Risaliti s Compton thick sample. In order to make the distribuion of the column density more reliable, we propose the Suzaku observations of heavily obscured AGNs with NH >1E25cm-2. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | HISAMITSU AWAKI | JAP | 2 | AO2 | SUZAKU OBSERVATIONS OF THE HEAVILY OBSCURED AGNS WITH NH>1E25 CM-2 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702010010/ | Quick Look | ![]() |
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201 | NGC 7314 | 338.9055 | -25.9984 | 338.214858 | -26.257583 | 330.662233 | -15.873025 | 27.22535085 | -59.7013223 | 59.6979 | 54215.4316319444 | 2007-04-25 10:21:33 | 54217.9516666667 | 2007-04-27 22:50:24 | 702015010 | 109.0198 | 100 | 109.0198 | 109.0198 | 0 | 109.0198 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92.2408 | 92.2408 | 217.7139 | 2 | PROCESSED | 57538.5280439815 | 2016-05-30 12:40:23 | 54744 | 2008-10-05 00:00:00 | 54230.4096527778 | 2007-05-10 09:49:54 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020037 | We propose a Suzaku observation of the highly variable Seyfert 1.9 NGC 7314. The Fe K line in this object varies on a very short time scale (<10 keV) in contrast to Seyferts observed with Suzaku in the SWG time. The data will be used to search for a weak broad Fe K line to constrain the inner radius of an optically thick disk and to study the spectral variation on short time scales to elucidate the fundamental processes producing X-rays in the vicinity of the central black hole. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YUICHI TERASHIMA | JAP | 2 | AO2 | RAPID SPECTRAL X-RAY VARIABILITY IN THE SEYFERT GALAXY NGC 7314: UNDERSTANDING ENERGY RELEASE PROCESSES IN AGN | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702015010/ | Quick Look | ![]() |
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202 | IGR J21247+5058 | 321.1969 | 51.0428 | 320.772046 | 50.826527 | 353.918258 | 60.483587 | 93.38215801 | 0.42876214 | 108.8126 | 54206.5871759259 | 2007-04-16 14:05:32 | 54208.4613888889 | 2007-04-18 11:04:24 | 702027010 | 85.0319 | 80 | 85.0319 | 85.0399 | 0 | 85.0479 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.9709 | 70.9709 | 161.8949 | 2 | PROCESSED | 57538.4530671296 | 2016-05-30 10:52:25 | 54744 | 2008-10-05 00:00:00 | 54214.1071412037 | 2007-04-24 02:34:17 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020097 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many new absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe two of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 2 | AO2 | BROAD BAND SPECTRA OF NEW SWIFT/BAT AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702027010/ | Quick Look | ![]() |
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203 | MRK 1239 | 148.0816 | -1.6118 | 147.44487 | -1.376316 | 150.825441 | -13.652204 | 239.27134701 | 38.21950621 | 286.5242 | 54226.0919907407 | 2007-05-06 02:12:28 | 54227.5973726852 | 2007-05-07 14:20:13 | 702031010 | 63.128 | 80 | 63.128 | 63.128 | 0 | 63.128 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53.5944 | 53.5944 | 130.0619 | 2 | PROCESSED | 57615.5991435185 | 2016-08-15 14:22:46 | 54744 | 2008-10-05 00:00:00 | 54235.4602662037 | 2007-05-15 11:02:47 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020127 | X-ray observations of "Hidden" narrow-line Seyfert 1 galaxies (NLS1s) have never been performed effectively, in spite of the fact that both obscuring material and nucleus of NLS1s are thought to be a crucial key to understand the fueling and accretion mechanisms, which may be directly related to the evolution of supermassive black holes and host galaxies. Hence,we propose 80 ksec observation of the candidates of hidden NLS1s Mrk 1239. Large effective area and unprecedented wide energy band of Suzaku allows us to strictly constrain the column density and covering fraction of obscuring matter, intrinsic power law slope, and its luminosity. From these observations, we expect to derive more complete unified picture of AGNs | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YOSHITO HABA | JAP | 2 | AO2 | SUZAKU VIEW OF "HIDDEN" NARROW-LINE SEYFERT 1 GALAXY MRK 1239 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702031010/ | Quick Look | ![]() |
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204 | NGC 4593 | 189.9131 | -5.3426 | 189.268208 | -5.068085 | 191.201579 | -0.987759 | 297.48049807 | 57.40434975 | 112.24 | 54449.1962384259 | 2007-12-15 04:42:35 | 54451.972349537 | 2007-12-17 23:20:11 | 702040010 | 118.8415 | 107 | 118.8415 | 118.8415 | 0 | 118.8415 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 108.976 | 108.976 | 239.7899 | 6 | PROCESSED | 57540.92 | 2016-06-01 22:04:48 | 54829 | 2008-12-29 00:00:00 | 54462.4425462963 | 2007-12-28 10:37:16 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021302 | We propose a 80 ksec observation of the bright Seyfert 1 NGC 4593 to resolve the moderately relativistic Fe K line, and test for a truncated or ionized accretion disk. To achieve accurate modeling of the broad Fe line, Suzaku's broad bandpass is required to deconvolve the broadband emitting component and accurately constrain the continuum. NGC 4593 is one of the few Seyferts to also show evidence for Fe XXVI emission at 6.9 keV; we will use the XIS to confirm the line and constrain its origin. If the thin accretion disk is truncated or transitions to an ADAF, it would reveal NGC 4593 to be an analogue of low/hard-state X-ray Binaries. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | ALEX MARKOWITZ | USA | 2 | AO2 | DOES THE SEYFERT AGN NGC 4593 HAVE A TRUNCATED OR IONIZED ACCRETION DISK? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702040010/ | Quick Look | ![]() |
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205 | NGC7582 | 349.5472 | -42.3304 | 348.858747 | -42.603943 | 331.723267 | -34.368393 | 348.20905034 | -65.68466064 | 49.5845 | 54221.7937384259 | 2007-05-01 19:02:59 | 54222.3176273148 | 2007-05-02 07:37:23 | 702052010 | 23.9412 | 25 | 23.9572 | 23.9412 | 0 | 23.9572 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.5816 | 21.5816 | 45.256 | 0 | PROCESSED | 57538.5368402778 | 2016-05-30 12:53:03 | 54695 | 2008-08-17 00:00:00 | 54228.073275463 | 2007-05-08 01:45:31 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021332 | We propose to perform 4 Suzaku observations of 25 ks each (for a total of 100 ks) of the bright Seyfert 2 galaxy,NGC 7582.The aim of this proposal is to measure the distance of the gas that absorbs the nuclear radiation, by analyzing the pattern of variability of its column density.NGC7582 is the ideal target for this kind of analysis, because it already showed large variations of the column density of the absorber between X-ray observations taken a few years apart.With the present proposal, we intend to probe a wider range of timescales, from a week to about six months, in order to measure the distance of the absorber from the nucleus. This measure is crucial to understand the nature of the absorber in type 2 objects and the validity of the torus paradigm. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARCO CHIABERGE | USA | 2 | AO2 | MEASURING THE DISTANCE OF THE ABSORBER IN NGC 7582 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702052010/ | Quick Look | ![]() |
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206 | NGC7582 | 349.6446 | -42.4137 | 348.956435 | -42.687331 | 331.752163 | -34.475865 | 347.94526846 | -65.70277041 | 233.1822 | 54413.9093981482 | 2007-11-09 21:49:32 | 54414.6459490741 | 2007-11-10 15:30:10 | 702052030 | 29.3538 | 25 | 29.3538 | 29.3538 | 0 | 29.3538 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24.4331 | 24.4331 | 63.6319 | 1 | PROCESSED | 57540.4723842593 | 2016-06-01 11:20:14 | 54790 | 2008-11-20 00:00:00 | 54423.1929398148 | 2007-11-19 04:37:50 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021332 | We propose to perform 4 Suzaku observations of 25 ks each (for a total of 100 ks) of the bright Seyfert 2 galaxy,NGC 7582.The aim of this proposal is to measure the distance of the gas that absorbs the nuclear radiation, by analyzing the pattern of variability of its column density.NGC7582 is the ideal target for this kind of analysis, because it already showed large variations of the column density of the absorber between X-ray observations taken a few years apart.With the present proposal, we intend to probe a wider range of timescales, from a week to about six months, in order to measure the distance of the absorber from the nucleus. This measure is crucial to understand the nature of the absorber in type 2 objects and the validity of the torus paradigm. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARCO CHIABERGE | USA | 2 | AO2 | MEASURING THE DISTANCE OF THE ABSORBER IN NGC 7582 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702052030/ | Quick Look | ![]() |
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207 | NGC7582 | 349.6411 | -42.4153 | 348.952917 | -42.688928 | 331.748482 | -34.476047 | 347.94523476 | -65.69973119 | 236.7954 | 54420.0722337963 | 2007-11-16 01:44:01 | 54420.8960532407 | 2007-11-16 21:30:19 | 702052040 | 31.8955 | 25 | 31.8955 | 31.8955 | 0 | 31.8955 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.7806 | 25.7806 | 71.1719 | 0 | PROCESSED | 57540.5407060185 | 2016-06-01 12:58:37 | 54797 | 2008-11-27 00:00:00 | 54430.3041203704 | 2007-11-26 07:17:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021332 | We propose to perform 4 Suzaku observations of 25 ks each (for a total of 100 ks) of the bright Seyfert 2 galaxy,NGC 7582.The aim of this proposal is to measure the distance of the gas that absorbs the nuclear radiation, by analyzing the pattern of variability of its column density.NGC7582 is the ideal target for this kind of analysis, because it already showed large variations of the column density of the absorber between X-ray observations taken a few years apart.With the present proposal, we intend to probe a wider range of timescales, from a week to about six months, in order to measure the distance of the absorber from the nucleus. This measure is crucial to understand the nature of the absorber in type 2 objects and the validity of the torus paradigm. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARCO CHIABERGE | USA | 2 | AO2 | MEASURING THE DISTANCE OF THE ABSORBER IN NGC 7582 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702052040/ | Quick Look | ![]() |
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208 | 3C 33 | 17.2445 | 13.2796 | 16.584921 | 13.013252 | 20.958615 | 5.507742 | 129.4936436 | -49.368548 | 249.2604 | 54460.3029282407 | 2007-12-26 07:16:13 | 54463.6390509259 | 2007-12-29 15:20:14 | 702059010 | 127.3677 | 100 | 127.3757 | 127.3757 | 0 | 127.3677 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 106.5885 | 106.5885 | 288.2036 | 7 | PROCESSED | 57541.0545833333 | 2016-06-02 01:18:36 | 54854 | 2009-01-23 00:00:00 | 54483.4886458333 | 2008-01-18 11:43:39 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021356 | We propose a 100 ks Suzaku observation of the nucleus of the nearby (z=0.0597) FRII radio galaxy 3C 33, to constrain the nature of its Compton reflection component, and make an accurate measurement of its Fe Ka emission line. 3C 33 (awarded category-C time in Suzaku AO-1, not observed) is the only radio-loud AGN with evidence of Compton reflection in its low-energy (< 10 keV) spectrum, and so offers a unique opportunity to study both the soft- and hard-band properties of reflection. The HXD will allow us, for the first time, to constrain the nature of the Compton reflection component in 3C 33 and, when combined with the superb sensitivity of the XIS, will enable us to determine the line-of-sight geometry and structure of the reflecting region. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | DANIEL EVANS | USA | 2 | AO2 | CONSTRAINING THE REFLECTION PROPERTIES OF THE NARROW-LINE RADIO GALAXY 3C 33 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702059010/ | Quick Look | ![]() |
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209 | Q1017+1055 | 155.041 | 10.671 | 154.377707 | 10.922699 | 152.99156 | 0.282434 | 230.36219873 | 50.83483368 | 121.1263 | 54431.9135185185 | 2007-11-27 21:55:28 | 54432.4376851852 | 2007-11-28 10:30:16 | 702064010 | 18.0486 | 20 | 18.0486 | 18.0486 | 0 | 18.0486 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.0316 | 15.0316 | 45.2819 | 0 | PROCESSED | 57540.6059606482 | 2016-06-01 14:32:35 | 54805 | 2008-12-05 00:00:00 | 54438.285150463 | 2007-12-04 06:50:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021361 | The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | GEORGE CHARTAS | USA | 2 | AO2 | AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702064010/ | Quick Look | ![]() |
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210 | 3C 273 | 187.2559 | 1.9961 | 186.616492 | 2.272457 | 185.868054 | 4.712799 | 289.92713501 | 64.30042167 | 293.1671 | 54281.0022569444 | 2007-06-30 00:03:15 | 54282.2661342593 | 2007-07-01 06:23:14 | 702070010 | 54.8927 | 67 | 54.8927 | 54.8927 | 0 | 54.8927 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.2592 | 51.2592 | 109.1439 | 1 | PROCESSED | 57539.0801388889 | 2016-05-31 01:55:24 | 54695 | 2008-08-17 00:00:00 | 54322.4904166667 | 2007-08-10 11:46:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021364 | We propose a Suzaku campaign on the bright z=0.158 quasar 3C 273. The source exhibits a Seyfert-like X-ray spectrum when the luminosity is low but is dominated by emission from the jet in a high state. Suzaku will be able to measure the broadband spectrum, especially X-ray reprocessed features, with greater sensitivity than ever before. Decoupling and monitoring of the disk and jet components will enable detailed spectroscopy to help understand the disk-jet connection and the wider implications for AGN physics in general. The target is bright and well-suited because for most AGN either the disk or jet component dominates. For this pilot study we propose two 50 ks observations, one in each visibility window. The science goals cannot be achieved with existing data or other missions. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TAHIR YAQOOB | USA | 2 | AO2 | EXPLORING THE ACCRETION DISK AND JET CONNECTION IN 3C 273 WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702070010/ | Quick Look | ![]() |
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211 | SWIFT J0318.7+6828 | 49.4315 | 68.5395 | 48.26024 | 68.35635 | 69.167768 | 48.016071 | 135.6962435 | 9.37350025 | 42.3301 | 54365.4488078704 | 2007-09-22 10:46:17 | 54367.125162037 | 2007-09-24 03:00:14 | 702075010 | 77.1156 | 53 | 77.1396 | 77.1156 | 0 | 77.1396 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.6855 | 70.6855 | 144.7978 | 1 | PROCESSED | 57540.0779513889 | 2016-06-01 01:52:15 | 54770 | 2008-10-31 00:00:00 | 54403.1984490741 | 2007-10-30 04:45:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021372 | The nature and even the existence of type II quasars is highly controversial. Due to their highly obscured nature, very hard (> 15 keV) observations are needed to probe their properties. With the 9-month SWIFT BAT all-sky AGN survey, detection of heavily obscured sources is now possible. Indeed, 6 type II quasars have been identified. Their properties, however, are a challenge to standard AGN models e.g., all but one of these sources are strong radio sources and several have optical spectra indicative of an un-absorbed source. We propose Suzaku observations of the 5 without broadband high signal to noise x-ray data to perform a detailed analysis of their x-ray properties and to understand their relationship to the lower luminosity well studied Seyfert IIs. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RICHARD MUSHOTZKY | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF SWIFT BAT TYPE II QUASARS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702075010/ | Quick Look | ![]() |
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212 | PHOENIX GALAXY | 120.9921 | 5.0644 | 120.329999 | 5.206365 | 122.073674 | -14.991802 | 216.72692126 | 18.43029643 | 304.6737 | 54222.3296296296 | 2007-05-02 07:54:40 | 54223.9585069445 | 2007-05-03 23:00:15 | 702111010 | 58.8677 | 50 | 58.8677 | 58.8677 | 0 | 58.8677 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.6978 | 49.6978 | 140.7239 | 5 | PROCESSED | 57538.5788078704 | 2016-05-30 13:53:29 | 54744 | 2008-10-05 00:00:00 | 54230.3771527778 | 2007-05-10 09:03:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022002 | We propose a 50 ks Suzaku observation of the Seyfert galaxy UGC4203 (a.k.a. Mrk 1210), the ``Phoenix Galaxy''. It is one of the sources which have been discovered to change from Compton-thin to reflection-dominated states. The aim of the proposal is to understand the origin of this variation (i.e. as either due to flux or to NH variations) by measuring its column density and compare it to previous observations. Suzaku is unique for this task, because thanks to its broad band it may probe column densities up to several times 10^24 cm^-2 in this source, which has never been observed above 10 keV. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GIORGIO MATT | EUR | 2 | AO2 | THE NATURE OF THE VARIATIONS OF STATE IN THE PHOENIX GALAXY | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702111010/ | Quick Look | ![]() |
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213 | IC4329A | 207.3329 | -30.3099 | 206.618741 | -30.061746 | 216.345977 | -17.776956 | 317.49868436 | 30.91898994 | 293.8517 | 54318.0289930556 | 2007-08-06 00:41:45 | 54318.8786226852 | 2007-08-06 21:05:13 | 702113020 | 30.6233 | 25 | 30.6233 | 30.6233 | 0 | 30.6233 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.7461 | 25.7461 | 73.384 | 3 | PROCESSED | 57539.4343287037 | 2016-05-31 10:25:26 | 54730 | 2008-09-21 00:00:00 | 54347.5971180556 | 2007-09-04 14:19:51 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022009 | IC 4329A is the brightest known Seyfert 1 galaxy between ~2-30 keV (F(2-10 keV)~1-2e-10 erg/cm2s). With its clear warm absorber and reflection component, it is often taken as the prototypical Sey 1 galaxy. Its X-ray variability is strong enough (and on a sufficiently long time scale, ideal for Suzaku) to make multiple observations critical for probing the origin of the Compton reflection component, and to attempt measuring variations of the high energy cut-off. We thus propose 5x20 ks observations to monitor i) the correlated variability of the reflection continuum plus FeK line to primary continuum variations, and ii) the variations in the high-E cut-off, and their relation with the power-law, and iii) check the evidence for a blueshifted (v~0.1c) FeK absorption line at ~7.7 keV. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MASSIMO CAPPI | EUR | 2 | AO2 | SUZAKU MULTIPLE OBSERVATIONS OF IC4329A TO PROBE THE ORIGIN OF THE COMPTON REFLECTION COMPONENT AND HIGH-ENERGY CUT-OFF | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702113020/ | Quick Look | ![]() |
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214 | IRAS18325-5926 | 279.2243 | -59.4565 | 278.116624 | -59.498471 | 275.782962 | -36.20075 | 335.92469241 | -21.3483138 | 281.9669 | 54399.3814699074 | 2007-10-26 09:09:19 | 54401.4169444444 | 2007-10-28 10:00:24 | 702118010 | 78.4348 | 80 | 78.4348 | 78.4428 | 0 | 78.4428 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74.2917 | 74.2917 | 175.8357 | 0 | PROCESSED | 57540.4011458333 | 2016-06-01 09:37:39 | 54777 | 2008-11-07 00:00:00 | 54409.305474537 | 2007-11-05 07:19:53 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022025 | We propose a 80 ks observation of the Seyfert galaxy IRAS 18325-5926. Previous observations show evidence for reflection from highly ionized matter, absorption features in the 8-10 keV band, and a possible roll-over of the continuum spectrum at around 30 keV. The observation goal is to elucidate the continuum roll-over and to investigate variability of the spectral features, which would have many important implications for the physical condition and the geometry of the accretion disc and the illuminating source. This study will provide crucial keys to understand the geometry of primary X-ray source and immediate surroundings. The broad-band coverage and the high sensitivity at the hard X-ray band provided by Suzaku are ideally suited to study this unique AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | KAZUTAMI MISAKI | EUR | 2 | AO2 | HARD X-RAY SPECTRUM OF IRAS 18325-5926: REFLECTION FROM AN IONIZED DISC AND CONTINUUM ROLL-OVER | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702118010/ | Quick Look | ![]() |
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215 | PKS0208-512 | 32.6864 | -51.0102 | 32.231145 | -51.245187 | 0.269734 | -58.029766 | 276.09849974 | -61.78596913 | 230.2146 | 54814.3149074074 | 2008-12-14 07:33:28 | 54815.4793171296 | 2008-12-15 11:30:13 | 703002010 | 51.9594 | 40 | 51.9834 | 51.9594 | 0 | 51.9834 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.559 | 42.559 | 100.5999 | 0 | PROCESSED | 57544.9648032407 | 2016-06-05 23:09:19 | 54557 | 2008-04-01 00:00:00 | 54826.3087268518 | 2008-12-26 07:24:34 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030004 | We propose intensive Suzaku observations of 11 "VIP" blazars with 40ksec each, as a long-category project. We stress that all of the sources will be monitored simultaneously by GLAST (GeV), Swift XRT/UVOT (UV to X-ray), as well as ground-based radio-to-optical telescopes. We will obtain the broadband spectra and light-curves from 10^9 Hz to 10^25 Hz, which reveals for the first time the nature of gamma-loud blazars in their quiescent states. The proposed 40ksec x 11 Suzaku observations will allow us to investigate | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 3 | AO3 | REVEALING THE NATURE OF GAMMA-LOUD BLAZARS VIA SUZAKU/GLAST AND WORLD-WIDE GROUND-BASED OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703002010/ | Quick Look | ![]() |
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216 | 4C73.08 | 147.4414 | 73.2521 | 146.291521 | 73.485172 | 114.906674 | 54.77086 | 138.04435007 | 38.07252036 | 100.3847 | 54786.9238888889 | 2008-11-16 22:10:24 | 54788.4946643518 | 2008-11-18 11:52:19 | 703018010 | 81.3752 | 80 | 81.3752 | 81.3752 | 0 | 81.3752 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 72.4533 | 72.4533 | 135.692 | 0 | PROCESSED | 57544.4300694444 | 2016-06-05 10:19:18 | 55164 | 2009-11-29 00:00:00 | 54798.0487152778 | 2008-11-28 01:10:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030063 | Suzaku observation of two giant radio galaxies, 4C 73.08 and 3C 35, are proposed. In 80 ks exposure on the individual target, inverse Compton X-ray emission from their lobes is detected with high signal statistics. As a result, the energy densities of electrons and magnetic field in these lobesare precisely determined. The size of these radio galaxies are significantly lager than that of the previous sample. Therefore, the size dependence of energetics in the lobes will be investigated | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YUICHI YAJI | JAP | 3 | AO3 | SUZAKU OBSERVATION OF LOBES OF GIANT RADIO GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703018010/ | Quick Look | ![]() |
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217 | NGC 4051 | 180.7952 | 44.5393 | 180.156844 | 44.817625 | 159.255387 | 40.346248 | 148.86124636 | 70.08047443 | 126.4079 | 54793.7 | 2008-11-23 16:48:00 | 54795.572025463 | 2008-11-25 13:43:43 | 703023020 | 78.3855 | 70 | 78.3935 | 78.3855 | 0 | 78.3939 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 62.7604 | 62.7604 | 161.7358 | 0 | PROCESSED | 57544.5729513889 | 2016-06-05 13:45:03 | 54557 | 2008-04-01 00:00:00 | 54811.74875 | 2008-12-11 17:58:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031014 | The powerful combination of Principal Components Analysis with time-resolved X-ray spectroscopy of Seyfert AGN has shown strong evidence that changes in a complex absorber are the origin of much of observed AGN spectral and flux variability. Large column, high ionization layers of gas may arise in a disk wind, representing a significant new, and possibly dominant, component, responsible for shaping the X-ray spectrum of AGN. The broad bandpass of Suzaku gives us a unique opportunity to model primary and reflected continua and the effects of variable absorbing zones, and test wind and other models. We propose a long 340 ks exposure on the NLSy1 NGC 4051 whose large amplitude of variability and well-studied complex absorption will test those models to the limit | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TRACEY TURNER | USA | 3 | AO3 | DECONSTRUCTING SEYFERT SPECTRA - TIME FOR A PARADIGM SHIFT? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703023020/ | Quick Look | ![]() |
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218 | SMC X-1 | 19.2829 | -73.4465 | 18.951639 | -73.709645 | 312.337269 | -66.476032 | 300.41108523 | -43.55576838 | 356.8796 | 55658.8646759259 | 2011-04-07 20:45:08 | 55659.2447106482 | 2011-04-08 05:52:23 | 706030010 | 18.4662 | 18 | 18.4662 | 18.55 | 0 | 18.5448 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15.5577 | 15.5577 | 32.8239 | 0 | PROCESSED | 57601.4235185185 | 2016-08-01 10:09:52 | 56040 | 2012-04-23 00:00:00 | 55673.2343055556 | 2011-04-22 05:37:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JOSEPH NEILSEN | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030010/ | Quick Look | ![]() |
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219 | SMC X-1 | 19.2476 | -73.446 | 18.915775 | -73.709202 | 312.329896 | -66.466401 | 300.42473809 | -43.55764171 | 6.4299 | 55669.2561805556 | 2011-04-18 06:08:54 | 55669.705775463 | 2011-04-18 16:56:19 | 706030020 | 17.2769 | 18 | 17.2769 | 17.2849 | 0 | 17.4844 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 17.6646 | 17.6646 | 38.8159 | 0 | PROCESSED | 57601.5313657407 | 2016-08-01 12:45:10 | 56058 | 2012-05-11 00:00:00 | 55691.1543171296 | 2011-05-10 03:42:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JOSEPH NEILSEN | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030020/ | Quick Look | ![]() |
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220 | NGC 7172 | 330.5062 | -31.8708 | 329.778877 | -32.112297 | 321.223494 | -18.549637 | 15.12698367 | -53.06449716 | 59.7356 | 54611.0658680556 | 2008-05-25 01:34:51 | 54612.8558217593 | 2008-05-26 20:32:23 | 703030010 | 82.2797 | 80 | 82.2797 | 82.2877 | 0 | 82.2877 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71.7465 | 71.7465 | 154.6338 | 0 | PROCESSED | 57542.6661805556 | 2016-06-03 15:59:18 | 54999 | 2009-06-17 00:00:00 | 54633.7016203704 | 2008-06-16 16:50:20 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031322 | X-ray observations of Seyfert 2 have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by the AGN Unification Scheme. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (80 ksec each) of three bright Compton-thin Seyfert 2 galaxies, selected from the Swift/BAT survey, with a hard X-ray flux exceeding 9e-11cgs, to form a flux-limited sample. The unprecedented bandpass of Suzaku offers a unique tool to investigate the X-ray emission of these sources, allowing us to put strong constraints on the reprocessing matter in Seyfert 2s. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | VALENTINA BRAITO | USA | 3 | AO3 | THE NATURE OF THE X-RAY ABSORBER IN SEYFERT 2 GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703030010/ | Quick Look | ![]() |
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221 | NGC 3281 | 157.9591 | -34.9074 | 157.391937 | -34.649823 | 175.881528 | -40.345828 | 273.03211125 | 19.73409342 | 278.2413 | 54607.8508449074 | 2008-05-21 20:25:13 | 54609.2287615741 | 2008-05-23 05:29:25 | 703033010 | 46.234 | 40 | 46.242 | 46.25 | 0 | 46.234 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.4549 | 41.4549 | 119.038 | 0 | PROCESSED | 57542.6257175926 | 2016-06-03 15:01:02 | 54988 | 2009-06-06 00:00:00 | 54620.2890162037 | 2008-06-03 06:56:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031323 | The classical unified model predicts only one type of Seyfert II (Sy2). Recent observations of SWIFT BAT-detected AGN found at least 4 classes of Sy2s: (1) objects with high column density and scattered soft x-rays, (2) Compton thick objects, (3) `hidden' AGN (Ueda et al. 2007), and (4) the `changing look' objects (Risaliti et al. 2006). The nature of these sources can only be revealed with high quality broad-band X-ray spectra from Suzaku. Thus, we are proposing 40ks observations for 2 of the brightest BAT AGN without high quality data, NGC 788, a type (3) object showing polarized optical broad lines, and NGC 3281, a classified (2) object. Such observations are necessary to build a reasonably large sample of high-quality, broad-band Sy2 spectra covering the range of X-ray/optical types. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RICHARD MUSHOTZKY | USA | 3 | AO3 | SUZAKU OBSERVATIONS OF X-RAY BRIGHT TYPE II AGN | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703033010/ | Quick Look | ![]() |
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222 | 3C279 | 194.0699 | -5.7328 | 193.422743 | -5.462367 | 195.164566 | 0.26232 | 305.15066173 | 57.11808922 | 113.6425 | 54854.8772222222 | 2009-01-23 21:03:12 | 54856.125162037 | 2009-01-25 03:00:14 | 703049020 | 56.937 | 200 | 56.937 | 56.937 | 0 | 56.937 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.6263 | 12.6263 | 107.7799 | 2 | PROCESSED | 57545.3327777778 | 2016-06-06 07:59:12 | 55328 | 2010-05-12 00:00:00 | 54880.5584259259 | 2009-02-18 13:24:08 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031346 | We propose a 200 ks observation of 3C279, the archetypal EGRET blazar to be conducted simultaneously with GLAST as well as many other facilities, with the goal of obtaining broadband spectra and light-curves. The flux in all observable bands is known to be rapidly variable, but the information regarding the correlation between the time history of flux in various bands is limited, and the proposed observations are designed to remedy this shortcoming. Such detailed spectral and variability studies are crucial to discriminate between different radiation scenarios responsible for production of X-rays and gamma-rays, and to constrain the matter content and by extension, the formation process of the jet, dissipation of the jet energy, and energization of the radiating particles. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GRZEGORZ MADEJSKI | USA | 3 | AO3 | SUZAKU AND GLAST OBSERVATIONS OF 3C279 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703049020/ | Quick Look | ![]() |
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223 | PKS1549-79 | 239.2836 | -79.2302 | 237.405254 | -79.084019 | 259.929288 | -56.865354 | 311.18735019 | -19.47008602 | 310.7048 | 54752.6495833333 | 2008-10-13 15:35:24 | 54754.9009375 | 2008-10-15 21:37:21 | 703059010 | 82.1755 | 80 | 82.197 | 82.1835 | 0 | 82.1755 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79.9736 | 79.9736 | 194.4977 | 2 | PROCESSED | 57544.1654398148 | 2016-06-05 03:58:14 | 55148 | 2009-11-13 00:00:00 | 54780.6256597222 | 2008-11-10 15:00:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032005 | Galaxy merger models predict rapid black hole growth and strong outflows late in the merger as the accretion rate increases. PKS1549-79 is a powerful, low redshift, high accretion rate active galaxy which has undergone a recent merger. It is therefore an ideal object to test our understanding of galaxy activity and mergers and for studying feedback between AGN and their host galaxies. We propose an 80 ksec Suzaku observation to: (i) determine the amount and ionisation state of the nuclear obscuring material in PKS1549-79 and hence confirm its status as a local proto-quasar; (ii) search for the massive, probably highly ionised, outflowing wind predicted by galaxy evolution models and hence complete a census of outflow components in this object; and (iii) quantify the high energy spectrum. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | PAUL O'BRIEN | EUR | 3 | AO3 | UNVEILING PKS 1549-79 WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703059010/ | Quick Look | ![]() |
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224 | MRK 573 | 26.0161 | 2.2904 | 25.370891 | 2.039517 | 24.959775 | -7.914401 | 148.3199793 | -57.9636564 | 249.71 | 55217.5861226852 | 2010-01-21 14:04:01 | 55219.0328587963 | 2010-01-23 00:47:19 | 704002010 | 64.3118 | 60 | 64.3118 | 64.3118 | 0 | 64.3118 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53.7471 | 53.7471 | 124.992 | 0 | PROCESSED | 57550.3256944445 | 2016-06-11 07:49:00 | 55612 | 2011-02-20 00:00:00 | 55245.753599537 | 2010-02-18 18:05:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040017 | Monte Carlo simulation is one of the best tools to study the complex spectra of Compton-thick AGNs and to figure out the relation between their nuclear structures and X-ray spectra. We have simulated X-ray spectra of Compton-thick AGNs obscured by an accretion torus, and found that observed spectra of Compton thick objects, Mrk 3 and NGC 2273 are well reproduced by the simulated X-ray spectra. Furthermore, our simulation predicts that there are many obscured AGNs with a heavily absorbed reflection component. Their spectra are similar to that predicted from synthesis modeling of the Cosmic X-ray Background. We propose Suzaku observations of candidates of the Compton thick AGNs, Mrk 573 and Mrk 78. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | HISAMITSU AWAKI | JAP | 4 | AO4 | SEARCH FOR COMPTON THICK AGNS WITH A HEAVILY ABSORBED REFLECTION COMPONENT | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704002010/ | Quick Look | ![]() |
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225 | SWIFT J2248.8+1725 | 342.1903 | 17.444 | 341.576565 | 17.179413 | 350.711211 | 23.025613 | 85.72592105 | -36.41328844 | 248.2402 | 56997.6938888889 | 2014-12-06 16:39:12 | 56999.668287037 | 2014-12-08 16:02:20 | 709004010 | 78.0938 | 80 | 78.0938 | 78.0938 | 0 | 78.0938 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 68.8266 | 68.8266 | 170.56 | 1 | PROCESSED | 57617.5240046296 | 2016-08-17 12:34:34 | 57460 | 2016-03-13 00:00:00 | 57092.3224652778 | 2015-03-11 07:44:21 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090018 | We propose to observe two hard X-ray bright Seyfert galaxies with a highly accreting small BH. This class of objects is of importance in studying accretion processes under a large mass accretion rate and therefore mass growth of black holes. Our aims are (1) to measure a continuum shape such as spectral slope and high energy cutoff, (2) to compare them with other classes of AGNs, and (3) to search for highly ionized outflows with a large column density. All of these will be fundamental pieces of information to better understand accretion physics and ``feedback'' processes in galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YUICHI TERASHIMA | JAP | 9 | AO9 | ACCRETION AND OUTFLOW IN THE HARD X-RAY SELECTED LOW-MASS SEYFERTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709004010/ | Quick Look | ![]() |
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226 | 1216-015 | 184.787 | -1.8118 | 184.145709 | -1.534245 | 185.108736 | 0.239101 | 286.61259693 | 60.03288042 | 293.8466 | 55010.1063773148 | 2009-06-28 02:33:11 | 55010.6043287037 | 2009-06-28 14:30:14 | 704006010 | 20.7779 | 20 | 20.7779 | 20.7859 | 0 | 20.7859 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57547.6897337963 | 2016-06-08 16:33:13 | 55388 | 2010-07-11 00:00:00 | 55020.3653009259 | 2009-07-08 08:46:02 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040049 | We propose the first X-ray follow-up observations of 4 gamma-ray bright Seyferts and starburst galaxy, recently discovered by Fermi gamma-ray space telescope. The detection of GeV emission provides new evidence for relativistic jets in radio-quiet AGNs, but steep gamma-ray spectrum as well as an exotic spectral energy distribution (where GeV flux is 2-4 orders of magnitude brighter than radio) indicates that non-thermal emission is relatively weak, and less enhanced compared to radio-loud AGNs. Throughout multiwavelength observations including Suzaku and Fermi satellites, we will investigate the jet power, accretion rate and line intensity of these new comers (i.e., gamma-loud Seyferts) towards the unification scheme of radio-loud and radio-quiet AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF GAMMA-LOUD SEYFERTS AND STARBURST GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704006010/ | Quick Look | ![]() |
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227 | UGC 12741 | 355.4449 | 30.6414 | 354.81812 | 30.364038 | 9.270542 | 29.65828 | 105.65559107 | -29.88276227 | 64.429 | 54989.5219560185 | 2009-06-07 12:31:37 | 54990.6711111111 | 2009-06-08 16:06:24 | 704014010 | 47.9458 | 40 | 47.9538 | 47.9458 | 0 | 47.9458 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 41.5244 | 41.5244 | 99.2799 | 0 | PROCESSED | 57547.5132060185 | 2016-06-08 12:19:01 | 55367 | 2010-06-20 00:00:00 | 55001.0091435185 | 2009-06-19 00:13:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040060 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe three Compton thick AGN candidates in the 22 months BAT catalog with Suzaku. To resolve the degeneracy of spectral modeling, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 4 | AO4 | DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704014010/ | Quick Look | ![]() |
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228 | NGC985 | 38.6279 | -8.738 | 38.014145 | -8.956444 | 33.218289 | -22.635173 | 180.72422437 | -59.4803664 | 62.3866 | 55027.6174884259 | 2009-07-15 14:49:11 | 55028.5925231482 | 2009-07-16 14:13:14 | 704042010 | 31.9969 | 30 | 31.9969 | 32.0063 | 0 | 32.0063 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.7241 | 25.7241 | 84.2379 | 1 | PROCESSED | 57547.8515856482 | 2016-06-08 20:26:17 | 55406 | 2010-07-29 00:00:00 | 55040.2752430556 | 2009-07-28 06:36:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041414 | We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | EZEQUIEL TREISTER | USA | 4 | AO4 | THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704042010/ | Quick Look | ![]() |
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229 | NGC 3431 | 162.8114 | -17.015 | 162.196181 | -16.749458 | 171.110311 | -22.386386 | 266.03803779 | 37.10135134 | 298.5009 | 56089.5660648148 | 2012-06-11 13:35:08 | 56091.5571412037 | 2012-06-13 13:22:17 | 707012010 | 65.6756 | 70 | 65.6756 | 65.6756 | 0 | 65.6756 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 59.8819 | 59.8819 | 171.9959 | 2 | PROCESSED | 57605.6909259259 | 2016-08-05 16:34:56 | 56473 | 2013-06-30 00:00:00 | 56106.3662384259 | 2012-06-28 08:47:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070067 | The nature of the hard X-ray emission of many AGN remains ill-understood. Using the latest 70 month Swift/BAT sky survey, we have selected optically-classified Seyfert 2s with a very hard BAT photon index (Gamma<1.4). The BAT energy range is not strongly affected by obscuration unless the column is Compton-thick. The selected sources are radio-quiet, arguing against jet-dominated non-thermal spectra. The cause of a low Gamma is unknown, but may include high or atypical obscuration, non-thermal X-ray emission without associated radio/optical jets or the presence of electron coronae with temperatures or optical depths higher than average. Our aim is to observe two of the hardest Seyfert 2s (neither of which has prior pointed observations below 10 keV) with Suzaku to elucidate their nature. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | POSHAK GANDHI | JAP | 7 | AO7 | WHAT IS THE NATURE OF SWIFT/BAT HARD-SPECTRUM SEYFERT 2S? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707012010/ | Quick Look | ![]() |
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230 | NGC4102 | 181.5322 | 52.6534 | 180.899339 | 52.931664 | 153.57589 | 47.373492 | 138.20676485 | 63.11040703 | 305.2196 | 54981.0678009259 | 2009-05-30 01:37:38 | 54983.4203009259 | 2009-06-01 10:05:14 | 704057010 | 105.5579 | 100 | 105.5819 | 105.5579 | 0 | 105.5659 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 97.2802 | 97.2802 | 203.2139 | 2 | PROCESSED | 57547.4983912037 | 2016-06-08 11:57:41 | 55363 | 2010-06-16 00:00:00 | 54994.4413541667 | 2009-06-12 10:35:33 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042014 | The nature of Low Ionization Nuclear Emission-line Region (LINER) galaxies has been the subject of a strong controversy. The distinction between LINER nuclei and other families of Active Galactic Nuclei (AGN) can be due to different amounts and/or properties of the obscuring material. A high population of LINERs are Compton-thick candidates. However the Equivalent Width (EW) of the FeKa emission line are lower than those measured for Compton-thick AGN. We propose to use the unprecedented sensitivity of HXD and XIS on board Suzaku to study NGC4102, one of the brightest LINER in the 36-month Swift/BAT survey. NGC4102 is a Compton-thick LINER candidate with EW(FeKa)<500keV, it is therefore an ideal case to investigate the properties of absorption and the FeKa emission line. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | OMAIRA GONZALEZ-MARTIN | EUR | 4 | AO4 | PROBING COMPTON-THICK OBSCURATION AND LOW EW(FEKA) OF LINERS: THE CASE OF NGC4102 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704057010/ | Quick Look | ![]() |
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231 | 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 | ![]() |
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232 | ARK 347 | 181.0952 | 20.2476 | 180.45595 | 20.52594 | 172.634722 | 18.942585 | 243.01628342 | 77.22827936 | 294.4295 | 55377.99625 | 2010-06-30 23:54:36 | 55378.8668171296 | 2010-07-01 20:48:13 | 705002010 | 38.9726 | 40 | 38.9886 | 38.9726 | 0 | 38.9886 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.9876 | 35.9876 | 75.2099 | 0 | PROCESSED | 57552.4401851852 | 2016-06-13 10:33:52 | 55772 | 2011-07-30 00:00:00 | 55404.2387268518 | 2010-07-27 05:43:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050003 | We propose to observe two Swift/BAT selected obscured AGNs with significant scattered emission, Mrk 18 and Ark 347. Hard X-ray selected AGNs show some peculiar characteristics compared to optically selected ones such as weak scattering emission from the opening part of the putative torus and weak plasma emission in the soft X-ray band. The targets are Swift/BAT selected AND show significant scattered emission, which are poorly explored with Suzaku so far. Our aims are to constrain the geometrical structure of the obscuring matter based on broad-band X-ray spectra and compare them with other hard X-ray or optically selected obscured AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YUICHI TERASHIMA | JAP | 5 | AO5 | THE STRUCTURE OF COMPTON-THIN AGNS WITH SIGNIFICANT SCATTERED EMISSION SELECTED BY SWIFT/BAT | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705002010/ | Quick Look | ![]() |
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233 | EMS0873 | 200.796 | 29.7234 | 200.211284 | 29.984115 | 186.018841 | 35.27496 | 55.1881509 | 82.55574598 | 136.0743 | 55527.7704976852 | 2010-11-27 18:29:31 | 55528.2800231482 | 2010-11-28 06:43:14 | 705029010 | 22.7849 | 20 | 22.7849 | 22.7849 | 0 | 22.7849 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20.8106 | 20.8106 | 44.0079 | 2 | PROCESSED | 57554.227974537 | 2016-06-15 05:28:17 | 55903 | 2011-12-08 00:00:00 | 55536.9832523148 | 2010-12-06 23:35:53 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050126 | Fermi Gamma-ray Space Telescope has detected a lot of unidentified GeV sources in high latitude. Among these, we focus on five Fermi unIDs whose error circles contain ROSAT faint X-ray sources and propose an X-ray follow-up observation with Suzaku. From an X-ray spectral and variability information, we identify these objects, as well as find new class of GeV emitters. We also aim to study emission and particle acceleration mechanism of these objects. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YASUYUKI TANAKA | JAP | 5 | AO5 | SEARCH FOR X-RAY COUNTERPARTS OF FERMI HIGH-LATITUDE UNIDENTIFIED GEV SOURCES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705029010/ | Quick Look | ![]() |
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234 | CEN A S LOBE NO. 4 | 196.751 | -45.1436 | 196.031726 | -44.876448 | 214.740849 | -34.712794 | 305.81117883 | 17.64110832 | 288.0039 | 55421.3479282407 | 2010-08-13 08:21:01 | 55421.67375 | 2010-08-13 16:10:12 | 705035010 | 20.642 | 20 | 20.642 | 20.65 | 0 | 20.658 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.9643 | 18.9643 | 28.1439 | 0 | PROCESSED | 57552.9465277778 | 2016-06-13 22:43:00 | 55803 | 2011-08-30 00:00:00 | 55435.1577314815 | 2010-08-27 03:47:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051401 | We propose a set of four pointings (200 ks), to study the X-ray emission from the Southern giant lobe of the radio galaxy Cen A. Those lobes clearly separated from the central source, have been detected as a source of diffuse gamma-ray emission by the Fermi Telescope. The goal of the Suzaku observations is two-fold: first, to measure the diffuse component of the non-thermal X-ray emission with both the XIS and the HXD in order to determine the details of the distribution of the radiating relativistic particles (and B field), and second, to measure the thermal emission from the lobes (using primarily the XIS), to determine temperature and density of the X-ray emitting plasma, which, via consideration of pressure balance, will determine the content of energetic protons (cosmic rays). | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GRZEGORZ MADEJSKI | USA | 5 | AO5 | SUZAKU OBSERVATIONS OF THE SOUTHERN LOBE OF CEN A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705035010/ | Quick Look | ![]() |
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235 | IRAS 00397-1312 | 10.5707 | -12.9503 | 9.941553 | -13.224287 | 4.464578 | -16.066781 | 113.89016485 | -75.66108211 | 246.4295 | 55558.1361342593 | 2010-12-28 03:16:02 | 55560.2501388889 | 2010-12-30 06:00:12 | 705046010 | 83.7928 | 90 | 83.7928 | 83.7928 | 0 | 83.7928 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71.9314 | 71.9314 | 182.6317 | 1 | PROCESSED | 57632.5965856482 | 2016-09-01 14:19:05 | 56040 | 2012-04-23 00:00:00 | 55670.3615046296 | 2011-04-19 08:40:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051441 | We propose two Suzaku-HXD observations of two ULIRGs hosting a deeply buried AGN. These two objects are expected to host a powerful AGN in the luminosity range of quasars, based on solid evidence from mid-IR Spitzer spectroscopy. However, these sources are completely buried behind a screen of dust with column density in excess of 10^24 cm^-2, so not only the primary emission below 10 keV is obscured, but the reflected emission, usually ascribed to a circumnuclear "torus", is also absent. This suggests a complete spherical coverage of the X-ray source along all directions. The unique capabilities of Suzaku at high energies will allow to confirm the existence of these objects, representing the most extreme examples of buried AGNs, both in terms of obscuration and of intrinsic luminosity. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | GUIDO RISALITI | USA | 5 | AO5 | BURIED QUASAR 2S INSIDE ULIRGS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705046010/ | Quick Look | ![]() |
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236 | NGC 4945 | 196.3415 | -49.5274 | 195.611435 | -49.259681 | 217.040288 | -38.699914 | 305.25336122 | 13.28155854 | 286.7821 | 55386.9936226852 | 2010-07-09 23:50:49 | 55388.2626388889 | 2010-07-11 06:18:12 | 705047020 | 44.1517 | 40 | 44.1517 | 44.1597 | 0 | 44.1517 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.1612 | 40.1612 | 109.434 | 0 | PROCESSED | 57552.6167824074 | 2016-06-13 14:48:10 | 55777 | 2011-08-04 00:00:00 | 55411.4916898148 | 2010-08-03 11:48:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051442 | We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GUIDO RISALITI | USA | 5 | AO5 | HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705047020/ | Quick Look | ![]() |
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237 | NGC 4945 | 196.2918 | -49.5144 | 195.562046 | -49.246615 | 216.996084 | -38.704359 | 305.2209968 | 13.29631795 | 319.7988 | 55438.8990277778 | 2010-08-30 21:34:36 | 55439.9896990741 | 2010-08-31 23:45:10 | 705047040 | 39.3859 | 40 | 39.3859 | 39.3859 | 0 | 39.3859 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.7823 | 35.7823 | 94.2239 | 0 | PROCESSED | 57553.267962963 | 2016-06-14 06:25:52 | 55815 | 2011-09-11 00:00:00 | 55449.2596296296 | 2010-09-10 06:13:52 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051442 | We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GUIDO RISALITI | USA | 5 | AO5 | HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705047040/ | Quick Look | ![]() |
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238 | ESP 39607 | 11.5922 | -40.0968 | 10.997666 | -40.369881 | 351.254657 | -40.701682 | 307.24150307 | -76.98900447 | 243.1952 | 55549.7680208333 | 2010-12-19 18:25:57 | 55551.3175810185 | 2010-12-21 07:37:19 | 705048010 | 60.6687 | 60 | 60.6927 | 60.6687 | 0 | 60.6847 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.9555 | 48.9555 | 133.8399 | 3 | PROCESSED | 57554.5018402778 | 2016-06-15 12:02:39 | 55960 | 2012-02-03 00:00:00 | 55593.2278472222 | 2011-02-01 05:28:06 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051443 | We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195 keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log(L_x) > 45.5 erg/sec) absorbed type II QSOs in the local universe and the most ripe for study with Suzaku. The newly discovered source SWIFT J2344.6-4233 at a redshift of z=0.6 is the most luminous object in the BAT sample with log(L_x) = 46.5 erg/sec. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | WAYNE BAUMGARTNER | USA | 5 | AO5 | SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705048010/ | Quick Look | ![]() |
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239 | 3C 433 | 320.9422 | 25.055 | 320.383545 | 24.83969 | 333.197862 | 37.998992 | 74.46917661 | -17.70913692 | 252.1178 | 55506.5663310185 | 2010-11-06 13:35:31 | 55508.0953472222 | 2010-11-08 02:17:18 | 705050010 | 62.5009 | 60 | 62.54 | 62.5009 | 0 | 62.54 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.4271 | 44.4271 | 132.0698 | 0 | PROCESSED | 57554.0198958333 | 2016-06-15 00:28:39 | 55890 | 2011-11-25 00:00:00 | 55524.1485416667 | 2010-11-24 03:33:54 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051443 | We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195 keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log(L_x) > 45.5 erg/sec) absorbed type II QSOs in the local universe and the most ripe for study with Suzaku. The newly discovered source SWIFT J2344.6-4233 at a redshift of z=0.6 is the most luminous object in the BAT sample with log(L_x) = 46.5 erg/sec. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | WAYNE BAUMGARTNER | USA | 5 | AO5 | SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705050010/ | Quick Look | ![]() |
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240 | 4U 1344-60 | 206.8966 | -60.619 | 206.036622 | -60.369696 | 231.500761 | -45.327278 | 309.76861534 | 1.50528265 | 97.6008 | 55572.7924189815 | 2011-01-11 19:01:05 | 55575.4751273148 | 2011-01-14 11:24:11 | 705058010 | 93.8773 | 100 | 93.9013 | 93.8933 | 0 | 93.8773 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79.5617 | 79.5617 | 231.7537 | 3 | PROCESSED | 57600.6768865741 | 2016-07-31 16:14:43 | 55975 | 2012-02-18 00:00:00 | 55607.6933333333 | 2011-02-15 16:38:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052018 | We propose a 100 ks Suzaku observation of 4U 1344-60, a poorly studied (because at low Galactic latitude) but bright (about 2 millicrabs) AGN which showed, in an XMM-Newton observation, a strong relativistic disk iron line. The main aim of the proposal is to determine in detail the parameters of the disk, which is possible only with a high quality broad band observation which permits to control the continuum beneath the line. Presently, only Suzaku has the right combination of sensitivity, energy resolution and broad band coverage to achieve this objective. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | JIRI SVOBODA | EUR | 5 | AO5 | 4U 1344-60: A BRIGHT AGN WITH A STRONG RELATIVISTIC IRON LINE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705058010/ | Quick Look | ![]() |
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241 | MRK 205 | 185.2459 | 75.2485 | 184.69782 | 75.525765 | 124.91832 | 63.698525 | 125.52269394 | 41.72619699 | 309.3435 | 55338.764849537 | 2010-05-22 18:21:23 | 55340.8203125 | 2010-05-24 19:41:15 | 705062010 | 100.9605 | 126 | 100.9685 | 100.9605 | 0 | 100.9685 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91.9525 | 91.9525 | 177.5778 | 0 | PROCESSED | 57551.6334606482 | 2016-06-12 15:12:11 | 55723 | 2011-06-11 00:00:00 | 55355.4313773148 | 2010-06-08 10:21:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052026 | Mrk 205 (z=0.071) is a ``bare'' radio-quiet quasar, showing a peculiar continuum and FeK complex. From our analysis of past XMM-Newton observations, it shows a prominent and variable soft excess down to a two-day timescale. In 2000, an unusual FeK profile was found with an unresolved narrow line at 6.4keV and a broadened line centered at 6.7keV; while in 2006 a broad line has been observed near 6.4keV with a visible energy shift to 6.5keV occurring when the source flux increased. Our aims are to: (i) determine the FeK origin from its profile, and its possible variability on sub-orbital time-scales, (ii) to obtain an unprecedented simultaneous measurement of the Compton hump which is critical for modelling the true FeK profile (iii) and hence to infer a global picture of this object. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | DELPHINE PORQUET | EUR | 5 | AO5 | PROBING THE ORIGIN OF THE FEK COMPLEX IN THE ``BARE'' NUCLEUS OF MRK205. | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705062010/ | Quick Look | ![]() |
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242 | WISE J1819+4532 | 274.9137 | 45.5584 | 274.555701 | 45.535406 | 279.54226 | 68.836144 | 73.38480627 | 24.31157427 | 77.6532 | 56020.3333333333 | 2012-04-03 08:00:00 | 56021.0070833333 | 2012-04-04 00:10:12 | 707038010 | 30.8819 | 30 | 30.8819 | 30.8819 | 0 | 30.8819 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.564 | 27.564 | 58.2039 | 0 | PROCESSED | 57605.0974537037 | 2016-08-05 02:20:20 | 56399 | 2013-04-17 00:00:00 | 56033.2380787037 | 2012-04-16 05:42:50 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071443 | We request a 30-ks observation of WISE J1819+4532, an extreme WISE-selected AGN at z=2.031. This source stands out even amongst the rare WISE-selected sources we have been targeting: at mid-IR wavelengths, WISE J1819+4532 is ~10x brighter than similarly selected WISE sources, and more than 50x brighter than extreme Spitzer-selected sources. Assuming the local mid-IR to hard X-ray correlations, the implied intrinsic hard X-ray luminosity is L(2-10)~3e46 erg/s. WISE J1819+4532 is optically faint and the optical spectrum shows a typical obscured AGN with narrow emission lines. However, the object is infrared bright and the near-IR spectrum shows broad H-alpha emission. This implies that WISE J1819+4532 is a rare example of a an extremely luminous, semi-obscured AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | DANIEL STERN | USA | 7 | AO7 | WISE J1819+4532: AN OBSCURED, HYPERLUMINOUS ULIRG/AGN AT Z~2 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707038010/ | Quick Look | ![]() |
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243 | NGC 4785 | 193.3693 | -48.746 | 192.657492 | -48.474679 | 214.374181 | -38.980118 | 303.27856941 | 14.12437615 | 296.8629 | 56495.4767013889 | 2013-07-22 11:26:27 | 56496.6341782407 | 2013-07-23 15:13:13 | 708003010 | 79.3882 | 70 | 79.3882 | 79.3962 | 0 | 79.3882 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.777 | 70.777 | 99.994 | 0 | PROCESSED | 57611.9465972222 | 2016-08-11 22:43:06 | 56876 | 2014-08-07 00:00:00 | 56509.7469907407 | 2013-08-05 17:55:40 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080027 | At faint fluxes, the Swift/BAT AGN survey is uncovering sources with very hard photon indices (Gamma) above 10 keV. The origin of a low Gamma in the hard band is ill-understood, but may include high/atypical obscuration, non-thermal X-rays without radio jets, or electron coronae with high temperatures or optical depths. In AO7, we observed two such Seyfert 2s and discovered Compton-thick obscuration in one source, and a buried AGN spectrum with no reflection or high-energy cutoff in the other. The hard BAT Gamma values thus have a variety of origins, and our strategy is very effective in selecting objects with interesting spectra. Here, we propose to observe two hardest sources (Gamma<~1) with no prior X-ray observations below 10 keV in order to shed light on the nature of this population. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | POSHAK GANDHI | JAP | 8 | AO8 | THE VARIED NATURE OF SWIFT/BAT HARD-SPECTRUM SEYFERT 2S | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708003010/ | Quick Look | ![]() |
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244 | 1FGL J1311.7-3429 | 197.9423 | -34.512 | 197.244044 | -34.24657 | 210.304099 | -24.759106 | 307.68226276 | 28.17214982 | 298.263 | 55774.7002314815 | 2011-08-01 16:48:20 | 55776.7362847222 | 2011-08-03 17:40:15 | 706001010 | 82.4771 | 80 | 82.4771 | 82.4771 | 0 | 82.4771 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.3737 | 70.3737 | 175.8638 | 2 | PROCESSED | 57602.7690046296 | 2016-08-02 18:27:22 | 56219 | 2012-10-19 00:00:00 | 55851.4595601852 | 2011-10-17 11:01:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060003 | We propose Suzaku observations of "unusual" Fermi-LAT sources 1FGL J1311.7 and 1FGL J2339.7, which are extremely bright in gamma-ray (> 30 sigma detection), but are as-yet unidentified even after two-year accumulation of Fermi-LAT data. Previous Suzaku observation revealed a highly variable X-ray source at the position of 1FGL J1311.7, but both spectral and temporal features do not resemble that of blazars or the gamma-ray pulsars. Meanwhile, an X-ray counterpart of 1FGL J2339.7 shows extremely hard spectrum with its photon index 1.1, which seems to connect smoothly with a bump feature around 2GeV. We will characterize variability and spectral properties of these peculiar X-ray counterparts and firmly understand the nature/origin of "new-type" GeV gamma-ray sources. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | JUN KATAOKA | JAP | 6 | AO6 | SUZAKU OBSERVATIONS OF "NEW-TYPE'' GAMMA-RAY SOURCES DETECTED WITH FERMI-LAT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706001010/ | Quick Look | ![]() |
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245 | 1FGL J1946.7-5404 | 296.6052 | -54.0506 | 295.618874 | -54.173159 | 288.105396 | -32.270844 | 343.89458124 | -29.55670998 | 268.6577 | 55865.7799074074 | 2011-10-31 18:43:04 | 55866.783599537 | 2011-11-01 18:48:23 | 706026010 | 42.3959 | 40 | 42.3959 | 42.3988 | 0 | 42.3988 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54.8833 | 54.8833 | 86.7079 | 0 | PROCESSED | 57603.6796990741 | 2016-08-03 16:18:46 | 56246 | 2012-11-15 00:00:00 | 55879.1861574074 | 2011-11-14 04:28:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060084 | In this proposal, we'd like to make a suggestion of 2 "steady" unassociated Fermi-LAT gamma-ray sources with Suzaku. 2-year Fermi-LAT observation detected 2412 sources, but 1194 sources are still unassociated. Proposed objects are located at high Galactic latitude, and selected not likely to be associated with blazar(AGN) and pulsar. These lightcurves do not show the significant temporal variability. To confirm their stability, we checked Test Statistic Value of 1FGL and 2-year Fermi observation. Deep Observation with Suzaku (1FGLJ0103: 80ks, 1FGL1946:40ks) is expected to reveal the nature of these unassociated objects, or at least impose strict limits at 2-10keV. Of course, it is necessary that multi-wavelength observation. We'll plan to arrange tie-ups with other wavelength researcher. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | KOTO MAEDA | JAP | 6 | AO6 | SUZAKU OBSERVATION OF "STEADY" UNASSOCIATED FERMI-LAT GAMMA-RAY SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706026010/ | Quick Look | ![]() |
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246 | RX J1633+4718 | 248.3342 | 47.2989 | 247.973952 | 47.402455 | 228.776709 | 67.659807 | 73.52584527 | 42.62417772 | 308.6809 | 55760.5047916667 | 2011-07-18 12:06:54 | 55761.4376388889 | 2011-07-19 10:30:12 | 706027020 | 37.51 | 40 | 37.51 | 37.51 | 0 | 37.51 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57602.5962847222 | 2016-08-02 14:18:39 | 56152 | 2012-08-13 00:00:00 | 55830.7262268518 | 2011-09-26 17:25:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060089 | RX J1633+4718 was detected in the ROSAT all sky survey, later identified as a radio loud narrow line Seyfert 1 (NLS1) galaxy. The soft X-ray spectrum of this source was fitted with a blackbody with temperature of 32eV plus a flat power law component. The blackbody temperature is much lower than 100-200eV, typical soft X-ray excess commonly observed in NLS1. Since radio to UV continuum spectrum of this souce resembles those of blazars, the flat power law X-ray component is likely to be a jet origin. The jet might supress accretion corona, and thus the emission from the accretion disk might visible in its bare form. Suzaku observation of this source will give us X-ray spectrum above 2keV and CCD resolution spectrum below 2keV for the 1st time. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KIYOSHI HAYASHIDA | JAP | 6 | AO6 | X-RAY EMISSION FROM DISK AND JET AROUND A SMBH IN RX J1633+4718 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706027020/ | Quick Look | ![]() |
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247 | ZW229-15 | 286.3333 | 42.4706 | 285.936982 | 42.393229 | 298.560222 | 64.301193 | 73.09172558 | 15.5517204 | 34.6696 | 55715.0128356482 | 2011-06-03 00:18:29 | 55719.6251736111 | 2011-06-07 15:00:15 | 706035010 | 167.0838 | 165 | 168.6766 | 167.0838 | 0 | 168.6846 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 218.1832 | 218.1832 | 398.4357 | 2 | PROCESSED | 57602.3250694445 | 2016-08-02 07:48:06 | 56127 | 2012-07-19 00:00:00 | 55757.7055671296 | 2011-07-15 16:56:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061414 | The optical emission from AGN is though to be a combination of direct radiation from an accretion disk and reprocessed x-ray emission. Separating these components requires simultaneous high-precision x-ray/optical monitoring, which has heretofore not been achieved. We propose to gather this necessary data via simultaneous optical and x-ray monitoring of the Sy 1 galaxy Zw 229-15. Kepler is monitoring Zw 229-15 every 30 minutes with unprecedented 99% duty cycle and 0.1% repeatability. The key missing data is an appropriate x-ray campaign. We propose a 64-orbit (165 ks) Suzaku long-look combined with a series of 48 Swift visits to probe lags of 0.1-10 days. This will be the first experiment sensitive to such short lags and thus will critically test the present disc/reprocessing paradigm | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RICHARD MUSHOTZKY | USA | 6 | AO6 | SIMULTANEOUS SUZAKU/SWIFT/ KEPLER MONITORING OF ZW 229-15 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706035010/ | Quick Look | ![]() |
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248 | IRAS 09104+4109 | 138.3378 | 40.9513 | 137.53478 | 41.157946 | 128.03448 | 23.67766 | 180.99146588 | 43.55010524 | 90.0004 | 55883.9878356482 | 2011-11-18 23:42:29 | 55885.7675694444 | 2011-11-20 18:25:18 | 706038010 | 81.3276 | 80 | 81.3356 | 81.3276 | 0 | 81.3356 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 76.5883 | 76.5883 | 153.73 | 2 | PROCESSED | 57603.9341203704 | 2016-08-03 22:25:08 | 56264 | 2012-12-03 00:00:00 | 55895.209849537 | 2011-11-30 05:02:11 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062009 | We propose to observe IRAS 09104+4109 for 80 ks with Suzaku in order to confirm the ~3 sigma BeppoSAX PDS detection of the source and increase the detection significance with the HXD/PIN to 10 sigma in the 10--80 keV band, allowing the detailed spectral shape to be determined. IRAS 09104+4109 is a hyperluminous Type 2 quasar embedded in a central cluster galaxy at redshift 0.442. It is likely to be the hard-X-ray-brightest such object observed with Suzaku and could well be the prototype Compton-thick Type 2 quasar. The Suzaku observation, especially above 10 keV will most likely reveal one of the most luminous Compton--thick Type 2 QSO to date. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | CHIA-YING CHIANG | EUR | 6 | AO6 | THE TYPE 2 HYPERLUMINOUS QUASAR IRAS 09104+4109 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706038010/ | Quick Look | ![]() |
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249 | 0528+134 | 82.7323 | 13.541 | 82.025359 | 13.504077 | 82.83368 | -9.719507 | 191.35839601 | -11.00951452 | 89.1633 | 55832.6802314815 | 2011-09-28 16:19:32 | 55833.0119444444 | 2011-09-29 00:17:12 | 706043010 | 14.7892 | 10 | 14.7892 | 14.7892 | 0 | 14.7892 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.8659 | 15.8659 | 28.6359 | 0 | PROCESSED | 57603.2623032407 | 2016-08-03 06:17:43 | 56225 | 2012-10-25 00:00:00 | 55875.6223958333 | 2011-11-10 14:56:15 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061601 | We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | SVETLANA JORSTAD | USA | 6 | AO6 | EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706043010/ | Quick Look | ![]() |
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250 | 3C 227 | 146.9365 | 7.4245 | 146.275614 | 7.656926 | 146.610705 | -5.546093 | 228.57888407 | 42.2858038 | 108.3139 | 56237.0794675926 | 2012-11-06 01:54:26 | 56239.0279513889 | 2012-11-08 00:40:15 | 707004010 | 82.5325 | 80 | 82.5405 | 82.5325 | 0 | 82.5405 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71.4299 | 71.4299 | 168.3338 | 0 | PROCESSED | 57608.0036342593 | 2016-08-08 00:05:14 | 56631 | 2013-12-05 00:00:00 | 56264.6488773148 | 2012-12-03 15:34:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070012 | Radio galaxies are a key class to understand the origin and effects of AGN feedback to the surroundings. However, the fundamental question, how the structure of the nucleus is different between AGNs with and without jets, is not resolved yet. A key parameter to understand the accretion flow is the Eddington ratio. BLRGs of 4C 50.55 and 3C 120 are rare objects having high Eddington ratio (L_bol/L_Edd~0.4) compared with Seyferts and typical BLRGs (< 0.1). Though the accretion disks in many BLRGs are known to be truncated and/or inner parts covered by corona, unified picture of accretion flows over a wide range of accretion rate is far from established. Therefore we propose observing a BLRG of 3C 227, which has the highest Eddington ratio in the hard X-ray luminous BLRGs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | FUMIE TAZAKI | JAP | 7 | AO7 | STUDY OF NUCLEAR STRUCTURE OF BLRGS WITH HIGH ACCRETION RATE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707004010/ | Quick Look | ![]() |
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251 | 2FGL J1502.1+5548 | 225.5826 | 55.8575 | 225.235279 | 56.052883 | 185.603435 | 66.74758 | 92.73148616 | 52.90392629 | 345.2903 | 56069.912974537 | 2012-05-22 21:54:41 | 56070.8342824074 | 2012-05-23 20:01:22 | 707008010 | 62.8733 | 60 | 62.8813 | 62.8813 | 0 | 62.8733 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 56.167 | 56.167 | 79.5899 | 1 | PROCESSED | 57605.4999652778 | 2016-08-05 11:59:57 | 56449 | 2013-06-06 00:00:00 | 56083.096875 | 2012-06-05 02:19:30 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070024 | We propose X-ray follow up observations of two high redshift blazar candidates in the Fermi/LAT unidentified sources. The aim of this proposal is to detect X-ray emissions from high redshift blazars (z >> 3) buried in unidentified Fermi/LAT sources and to find the most distant LAT detected blazar. Gamma-ray photons above 10 GeV are attenuated by interactions with UV photons which result in creating electron-positron pairs. Therefore, attenuation signatures are predicted to be observed in gamma-ray spectra and such attenuation of high redshift blazars with redshift up to z ~ 6 provide information about UV background out to the epoch of cosmological reionization. By utilizing the attenuation, we can investigate the UV radiation state of the early universe. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YOSUKE TAKAHASHI | JAP | 7 | AO7 | SUZAKU OBSERVATIONS OF HIGH REDSHIFT BLAZAR CANDIDATES IN THE FERMI UNIDENTIFIED SOURCE SAMPLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707008010/ | Quick Look | ![]() |
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252 | 2FGL J0157.2-5259 | 29.3567 | -53.0295 | 28.896901 | -53.272777 | 354.834799 | -58.248558 | 282.0695167 | -61.34394411 | 33.9769 | 56075.6946064815 | 2012-05-28 16:40:14 | 56076.2565162037 | 2012-05-29 06:09:23 | 707011010 | 32.0753 | 30 | 32.0753 | 32.0753 | 0 | 32.0753 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31.7784 | 31.7784 | 48.5239 | 1 | PROCESSED | 57605.5386458333 | 2016-08-05 12:55:39 | 56527 | 2013-08-23 00:00:00 | 56161.0508449074 | 2012-08-22 01:13:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070034 | We propose Suzaku observations of "unusual" Fermi-LAT sources 2FGL J0022.2, J0037.8 and J0157.2, which are yet unidentified in gamma-ray, but their counterparts have already been detected with snapshot (typically 5ksec) Swift XRT observations. Their positions are determined with an excellent accuracy of several arcseconds. Since all three sources are detected both in radio and X-rays, they could be most likely AGN jet sources but their spectral energy distributions are far from what expected from typical blazars, suggesting "new-type" AGN sources. We propose 30 ksec observations of each to investigate temporal variability, as well as to determine wideband XIS/HXD spectra between 0.5-30 keV (J01572.2 is detectable with HXD/PIN). | EXTRAGALACTIC COMPACT SOURCES | 7 | B | JUN KATAOKA | JAP | 7 | AO7 | FURTHER CHALLENGES TO UNUSUAL FERMI-UNIDS WITH SUZAKU X-RAY OBSERVATORY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707011010/ | Quick Look | ![]() |
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253 | NGC1365 | 53.4038 | -36.1454 | 52.926467 | -36.312356 | 36.802809 | -53.044895 | 237.96455345 | -54.59601318 | 66.4692 | 56137.3445138889 | 2012-07-29 08:16:06 | 56138.1030208333 | 2012-07-30 02:28:21 | 707017040 | 31.3603 | 30 | 31.3683 | 31.3683 | 0 | 31.3603 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 28.2314 | 28.2314 | 65.5279 | 2 | PROCESSED | 57606.7020717593 | 2016-08-06 16:50:59 | 56528 | 2013-08-24 00:00:00 | 56162.0367361111 | 2012-08-23 00:52:54 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070095 | NGC1365 is one of AGNs which shows the most highly variable spectral change, and furthermore exhibits strong Fe-K absorption lines blue-shifted by 1000--5000 km/s with EW of about 100eV. These absorption lines indicate a massive outflow and are important to consider the AGN feedback to parent galaxies. Currently, there is no other object by which we can measure the Fe-K absorption lines accurately than NGC 1365. Therefore, we propose to monitor a velocity, depth, and ratio of blue-shifted Fe-K absorption lines, hard X-ray flux above 10 keV of NGC1365 every 10 days, in order to probe the massive outflow dynamically and compare the results with the numerical simulation. } | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YASUSHI FUKAZAWA | JAP | 7 | AO7 | MONITOR OF VELOCITY AND STRENGTH OF BLUE-SHIFTED STRONG FE-K ABSORPTION LINES OF NGC 1365 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707017040/ | Quick Look | ![]() |
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254 | SWIFT J164449.3+1573 | 251.1623 | 57.5874 | 250.936922 | 57.677768 | 216.812116 | 77.507745 | 86.72267547 | 39.46447046 | 15.8437 | 56064.7296064815 | 2012-05-17 17:30:38 | 56066.0522106482 | 2012-05-19 01:15:11 | 707018010 | 80.8141 | 80 | 80.8221 | 80.8141 | 0 | 80.8221 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74.3379 | 74.3379 | 114.2699 | 0 | PROCESSED | 57605.4610648148 | 2016-08-05 11:03:56 | 56442 | 2013-05-30 00:00:00 | 56076.0214351852 | 2012-05-29 00:30:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070096 | We propose a 80 ks observation of a tidal disruption event Swift J164449.3+1573451 one year after its onset. In this event, a star was presumably disrupted by a strong tidal force of a massive black hole at the center of a galaxy at z=0.35, releasing a relativistic jet that emitted intense X-rays. In this proposal, we attempt to detect the non-thermal emission from the relativistic jet and the fluorescent Fe K line from its surrounding material. With these results we study the driving mechanism of the jet and to test the tidal disruption model. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RYUICHI USUI | JAP | 7 | AO7 | ONE YEAR AFTER THE TIDAL DISRUPTION OF SWIFT J164449.3+1573451 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707018010/ | Quick Look | ![]() |
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255 | MCG-03-34-64 | 200.5996 | -16.727 | 199.930176 | -16.465808 | 205.288367 | -7.470033 | 313.53711237 | 45.50625694 | 110.133 | 56296.8837384259 | 2013-01-04 21:12:35 | 56301.1737384259 | 2013-01-09 04:10:11 | 707027010 | 155.7127 | 150 | 155.7367 | 155.7127 | 0 | 155.7287 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 135.0516 | 135.0516 | 370.6038 | 4 | PROCESSED | 57608.5292824074 | 2016-08-08 12:42:10 | 56018 | 2012-04-01 00:00:00 | 56336.6958680556 | 2013-02-13 16:42:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071423 | Analysis of Suzaku observations selected from the BAT 58-month catalog has shown extreme hard X-ray excesses to exist in ~70% of type 1 AGN, and these can be modeled by partial-covering of Compton-thick gas. This new result shows the importance of broad X-ray coverage, currently available only with Suzaku. The most extreme of the sample sources, MCG-03-34-64 and NGC 1194, show significant spectral and flux variability above 10 keV, likely attributable to changes in the Compton-thick absorber. We request new observations of MCG-03-34-64 (150 ks) and NGC 1194 (200 ks) to study the X-ray reprocessor in these extreme systems, confirm the high-energy spectral variability and constrain the nature and location of the Compton-thick absorber. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TRACEY TURNER | USA | 7 | AO7 | THE CASE FOR VARIATIONS IN COMPTON-THICK ABSORPTION: MCG-03-34-64 AND NGC 1194 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707027010/ | Quick Look | ![]() |
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256 | NGC 1667 | 72.1445 | -6.2644 | 71.533156 | -6.35119 | 69.717897 | -28.457954 | 203.99435404 | -30.10712566 | 81.9813 | 53964.3614814815 | 2006-08-17 08:40:32 | 53965.2536805556 | 2006-08-18 06:05:18 | 701006010 | 39.253 | 40 | 39.253 | 39.261 | 39.261 | 39.261 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35.7281 | 35.7281 | 77.0759 | 0 | PROCESSED | 57535.2875578704 | 2016-05-27 06:54:05 | 54526 | 2008-03-01 00:00:00 | 54020.7803009259 | 2006-10-12 18:43:38 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010037 | We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YUICHI TERASHIMA | JAP | 1 | AO1 | COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701006010/ | Quick Look | ![]() |
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257 | H1821+643 | 275.4669 | 64.3595 | 275.403094 | 64.333117 | 318.334051 | 86.844268 | 94.01942058 | 27.4280098 | 65.0004 | 56402.5419444444 | 2013-04-20 13:00:24 | 56404.6925462963 | 2013-04-22 16:37:16 | 708037020 | 128.2485 | 400 | 128.2703 | 128.2485 | 0 | 128.2485 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 132.8215 | 132.8215 | 185.8058 | 2 | PROCESSED | 57611.1374884259 | 2016-08-11 03:17:59 | 56383 | 2013-04-01 00:00:00 | 56425.6256712963 | 2013-05-13 15:00:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081436 | H1821+643 (z=0.297) is not "just another quasar". This luminous active galactic nucleus (AGN) is an extremely rare example of a powerful quasar at the center of a rich, cooling-core cluster of galaxies. As such, it may represent a key evolutionary stage in the complex interplay between AGN and the core regions of the intracluster medium (ICM). Our analysis of archival XMM-Newton data has found evidence for a relativistically broad iron line. Here, we build on this request deep (400ks) Suzaku spectroscopy of H1821+643 to (1) measure the spin of this supermassive black hole and (2) search for powerful highly ionized outflows. In addition to measuring spin in the most luminous and distant object yet, this will enable us to test key predictions of recent models for AGN feedback. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | CHRISTOPHER REYNOLDS | USA | 8 | AO8 | THE BLACK HOLE SPIN AND IONIZED OUTFLOWS IN THE COOLING-FLOW QUASAR H1821+643 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708037020/ | Quick Look | ![]() |
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258 | IRAS F11119+3257 | 168.6582 | 32.6829 | 167.981225 | 32.955487 | 156.042952 | 25.438757 | 192.21056175 | 68.35212615 | 301.5808 | 56425.1110185185 | 2013-05-13 02:39:52 | 56431.3329050926 | 2013-05-19 07:59:23 | 708038010 | 252.2992 | 250 | 252.3232 | 252.2992 | 0 | 252.3232 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 220.3036 | 220.3036 | 400.8599 | 10 | PROCESSED | 57611.4720717593 | 2016-08-11 11:19:47 | 56858 | 2014-07-20 00:00:00 | 56491.9181828704 | 2013-07-18 22:02:11 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081441 | Recent Herschel observations provided a breakthrough in identifying powerful, large-scale molecular outflows in ULIRGs, indicating that AGN feedback can indeed have a strong impact on star formation and galaxy evolution, in accordance with theoretical models. However, observational evidence for the connection between the putative fast nuclear AGN winds required for the formation of these large-scale outflows is missing. X-ray observations of blue-shifted Fe K absorption lines directly probe ultra-fast outflows (UFOs) ejected from the AGN accretion disk with v>10,000km/s. A 250ks Suzaku exposure of the ULIRG F11119+3257 with observed extreme molecular/neutral/ionized outflows would allow to characterize the expected UFO, providing the "smoking gun" evidence for feedback driven by AGN winds. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | FRANCESCO TOMBESI | USA | 8 | AO8 | IRAS F11119+3257: THE "SMOKING GUN" EVIDENCE FOR AGN FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708038010/ | Quick Look | ![]() |
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259 | UGC 03142 | 70.9469 | 28.9681 | 70.161272 | 28.87543 | 73.291585 | 6.626144 | 172.09277202 | -10.99747628 | 264.8107 | 56335.692349537 | 2013-02-12 16:36:59 | 56336.9946296296 | 2013-02-13 23:52:16 | 707032010 | 51.2847 | 50 | 51.2847 | 51.2927 | 0 | 51.3007 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.5632 | 47.5632 | 112.51 | 1 | PROCESSED | 57610.6216898148 | 2016-08-10 14:55:14 | 56721 | 2014-03-05 00:00:00 | 56349.5963541667 | 2013-02-26 14:18:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071424 | A hard X-ray-selected (BAT) AGN sample shows a remarkable 70% of the local population of type 1 AGN to have extreme hard excesses above 20 keV, likely caused by Compton-thick gas in the line-of-sight, covering at least 50% of the source. We request six snapshot observations to complete a Suzaku survey of a BAT-flux-limited sample and make a complete and unbiased measurement of the incidence. Analysis of the new sources will be performed in conjunction with existing exposures, providing exciting new insight into the previously unknown structures in hard X-ray selected AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TRACEY TURNER | USA | 7 | AO7 | INVESTIGATING COMPTON-THICK ABSORBERS IN TYPE 1 AGN: OVERHAULING THE AGN PARADIGM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707032010/ | Quick Look | ![]() |
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260 | FAIRALL 51 | 281.2285 | -62.3615 | 280.064534 | -62.412939 | 276.680669 | -39.180999 | 333.20299178 | -23.09155943 | 253.9697 | 56548.4894444445 | 2013-09-13 11:44:48 | 56549.3146990741 | 2013-09-14 07:33:10 | 708046040 | 30.1926 | 30 | 30.2006 | 30.1926 | 0 | 30.1926 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.1812 | 37.1812 | 71.2679 | 1 | PROCESSED | 57612.6129050926 | 2016-08-12 14:42:35 | 56990 | 2014-11-29 00:00:00 | 56625.6172337963 | 2013-11-29 14:48:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082016 | Fairall 51 is a variable bright active galaxy (about 1 millicrab), classified as a polar-scattered Seyfert~1 galaxy. It was observed twice with high-quality X-ray spectrometers on-board the XMM-Newton satellite. The two observations are separated by half a year and the spectra significantly differ from each other. The difference can be well explained by a variable covering fraction of a cold (very low-ionised) absorber (Ricci et al., 2010). Two additional Swift data, separated by five days, suggest that the variability may occur at time-scales as short as a few days. The ultimate goal of the proposal is to locate this variable absorber by the determination of the typical time-scale of the variability. We therefore propose a series of observations of Fairall 51 with short exposures. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JIRI SVOBODA | EUR | 8 | AO8 | STUDY OF THE VARIABLE ABSORBER IN A BRIGHT ACTIVE GALAXY FAIRALL 51 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708046040/ | Quick Look | ![]() |
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261 | MCG -5-23-16 | 146.9445 | -30.9023 | 146.395049 | -30.669659 | 162.619875 | -41.096298 | 262.72964912 | 17.28396386 | 118.3849 | 53711.9526388889 | 2005-12-07 22:51:48 | 53714.4939699074 | 2005-12-10 11:51:19 | 700002010 | 95.6774 | 100 | 95.6774 | 95.7174 | 95.7174 | 95.6854 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 85.5647 | 85.5647 | 219.5251 | 3 | PROCESSED | 57532.4508680556 | 2016-05-24 10:49:15 | 54247 | 2007-05-27 00:00:00 | 54039.1988310185 | 2006-10-31 04:46:19 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001006 | We request a 100ks Suzaku observation of the bright Seyfert galaxy, MCG -5-23-16 simultaneously with approved XMM-Newton and Chandra HETG observations in December 2005. MCG -5-23-16 has one of the best known examples of a relativistically broadened iron K line. With a Swift-BAT flux of 1.6e-10 cgs (15-100 keV), it is one of the brightest AGN above 10 keV. The simultaneous observations will allow us to determine the shape of the broad relativistic Fe line after subtracting the narrow line components measured by HETG. Importantly, Suzaku's wide bandpass will accurately measure the broad-band continuum and reflection component of MCG -5-23-16, essential for constraining the broad iron line. These observations will also allow us to determine the temperature of the high energy cut-off. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JAMES REEVES | JAP | 0 | SWG | PROBING THE BROAD IRON LINE AND HIGH ENERGY CONTINUUM OF MCG -5-23-16 SIMULTANEOUSLY WITH SUZAKU, XMM-NEWTON AND CHANDRA | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700002010/ | Quick Look | ![]() |
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262 | IRAS 12127-1412 | 183.8305 | -14.4966 | 183.185484 | -14.2187 | 189.338442 | -11.765951 | 289.94461652 | 47.46236248 | 294.8513 | 56113.7580671296 | 2012-07-05 18:11:37 | 56115.2862615741 | 2012-07-07 06:52:13 | 707037010 | 63.6095 | 60 | 63.6095 | 63.6095 | 0 | 63.6095 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57.584 | 57.584 | 132.012 | 2 | PROCESSED | 57606.6111342593 | 2016-08-06 14:40:02 | 56508 | 2013-08-04 00:00:00 | 56142.1406018518 | 2012-08-03 03:22:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071441 | We propose to observe with the Hard X-ray Detector onboard Suzaku the two Ultraluminous Infrared Galaxies IRAS 00182-7112 and IRAS 12127-1412, both of which are known to harbour very luminous and highly obscured active galactic nuclei (AGN). An AGN reflection component arising from ionized gas is clearly identified at 2 10 keV: the detection of the direct AGN emission above 10 keV and the measure of the reflection efficiency would provide fundamental information on both the physical structure of Compton-thick AGN embedded in a nuclear starburst and their feedback on the surrounding environment. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | EMANUELE NARDINI | USA | 7 | AO7 | THE PHYSICAL STRUCTURE OF COMPTON-THICK AGN/ULIRGS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707037010/ | Quick Look | ![]() |
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263 | PG 1211+143 | 183.6045 | 14.1097 | 182.967898 | 14.387617 | 177.569786 | 14.352789 | 267.53559231 | 74.37841457 | 120.7913 | 53698.7348263889 | 2005-11-24 17:38:09 | 53701.3397453704 | 2005-11-27 08:09:14 | 700009010 | 96.3241 | 100 | 96.59 | 97.5802 | 96.3241 | 96.3241 | 3 | 2 | 3 | 3 | 1 | 0 | 0 | 84.0087 | 84.0087 | 225.0438 | 2 | PROCESSED | 57528.1616203704 | 2016-05-20 03:52:44 | 54247 | 2007-05-27 00:00:00 | 54038.7422106482 | 2006-10-30 17:48:47 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001041 | A 100ks Suzaku observation of the NLS1, PG 1211+143 is proposed. Previous XMM-Newton and Chandra observation claimed both blue-shifted (0.1c) and redshifted (0.26c-0.40c) iron Kalpha absorption lines. The redshifted iron K lines may originate from matter falling onto the supermassive black hole. The high effective area and low background of Suzaku XIS above 5 keV will enable us to measure these relativistically shifted iron lines in PG 1211+143 with great accuracy. Constraining the time variability of the lines will allow us to determine the physical origins of the absorption, e.g. failed jet/outflow or gravitational redshift from a Kerr black hole. The excellent broadband capabilities of Suzaku will accurately determine the continuum, essential for modeling the iron K band. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JAMES REEVES | JAP | 0 | SWG | EXPLORING THE RELATIVISTICALLY SHIFTED IRON LINES IN PG 1211+143 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700009010/ | Quick Look | ![]() |
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264 | NGC4418 | 186.7074 | -0.9383 | 186.066307 | -0.661629 | 186.526079 | 1.80107 | 290.03230216 | 61.31559989 | 292.8039 | 53929.4791898148 | 2006-07-13 11:30:02 | 53931.280775463 | 2006-07-15 06:44:19 | 701001010 | 68.3485 | 70 | 68.3485 | 68.3485 | 68.3485 | 68.3485 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 57.1103 | 57.1103 | 155.634 | 1 | PROCESSED | 57534.9858564815 | 2016-05-26 23:39:38 | 54408 | 2007-11-04 00:00:00 | 53942.4601388889 | 2006-07-26 11:02:36 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010001 | We propose Suzaku observations at E > 10 keV of nearby ultraluminous infrared galaxies (ULIRGs), for which our infrared spectroscopy has strongly suggested the presence of luminous AGNs deeply buried in gas and dust. However, extreme starbursts are still a possibility. Through the proposed X-ray observations using Suzaku, we aim to distinguish clearly between buried AGNs (strong X-ray emitters) and extreme starbursts (weak X-ray emitters), and to obtain convincing evidence for luminous buried AGNs. Since buried AGNs in these ULIRGs' cores are likely to suffer from Compton-thick X-ray absorption, the high sensitivity at E > 10 keV achieved by Suzaku HXD PIN is crucial for the success of this experiment. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MASATOSHI IMANISHI | JAP | 1 | AO1 | COMPTON THICK BURIED AGNS IN NEARBY ULTRALUMINOUS INFRARED GALAXIES | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701001010/ | Quick Look | ![]() |
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265 | 3C345 | 250.7487 | 39.7945 | 250.326948 | 39.887223 | 238.332578 | 61.133151 | 63.43440525 | 40.94504508 | 267.732 | 56181.2697453704 | 2012-09-11 06:28:26 | 56181.4772337963 | 2012-09-11 11:27:13 | 707043010 | 12.7008 | 10 | 12.7088 | 12.7168 | 0 | 12.7008 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.7314 | 10.7314 | 17.9199 | 0 | PROCESSED | 57606.986412037 | 2016-08-06 23:40:26 | 56582 | 2013-10-17 00:00:00 | 56212.7656712963 | 2012-10-12 18:22:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071601 | We propose to perform two 2-week multi-frequency campaigns of observations of a sample of gamma-ray blazars during Fermi Cycle 5. The campaigns will involve: (1) gamma-ray monitoring with the Fermi LAT, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B, V, R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku and Swift; (6) mid-IR measurements with IRTF; and (7) near-IR photometric J, H, and K observations. The research aims i) to search for correlated variability on short timescales; ii) to compile SEDs at different states of gamma-ray and radio jet activitiy; and iii) to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | SVETLANA JORSTAD | USA | 7 | AO7 | MULTI-FREQUENCY CAMPAIGNS TO STUDY RAPID VARIABILITY IN GAMMA_RAY BLAZARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707043010/ | Quick Look | ![]() |
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266 | PKS 0558-504 | 89.9338 | -50.4417 | 89.630316 | -50.442779 | 89.864771 | -73.883563 | 257.95388656 | -28.57696937 | 207.8266 | 54117.4686226852 | 2007-01-17 11:14:49 | 54118.1127777778 | 2007-01-18 02:42:24 | 701011010 | 20.6207 | 20 | 20.6207 | 20.6207 | 0 | 20.6207 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.914 | 18.914 | 55.6479 | 0 | PROCESSED | 57536.8527777778 | 2016-05-28 20:28:00 | 54735 | 2008-09-26 00:00:00 | 54133.0355787037 | 2007-02-02 00:51:14 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010057 | Narrow-line Seyfert 1 Galaxies (NLS1s) must have been crucial key to understand the rapid growth of the central supermassive black hole, which may be related to the evolution of the host galaxy. Hence, we propose 20x5 ksec observations of the luminous NLS1 galaxy PKS 0558-504, which is the candidate having the highest mass-accretion rate among the class. Large effective area and good energy resolution of XISs allow us to strictly constrain the temperature and the luminosity of the accretion flow. In addition, Suzaku HXD will detect the significant fraction of hard power law emission in the 10-60 keV band for the first time. From these observations, we expect to derive the new picture of the high mass-accretion mechanism in NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YOSHITO HABA | JAP | 1 | AO1 | SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701011010/ | Quick Look | ![]() |
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267 | PKS 0558-504 | 89.9338 | -50.4409 | 89.630307 | -50.441979 | 89.864775 | -73.882763 | 257.95298672 | -28.57684464 | 209.1054 | 54118.6998032407 | 2007-01-18 16:47:43 | 54119.2654976852 | 2007-01-19 06:22:19 | 701011020 | 18.8753 | 20 | 18.8753 | 18.8753 | 0 | 18.8753 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.0497 | 18.0497 | 48.87 | 1 | PROCESSED | 57536.8739814815 | 2016-05-28 20:58:32 | 54735 | 2008-09-26 00:00:00 | 54133.3967361111 | 2007-02-02 09:31:18 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010057 | Narrow-line Seyfert 1 Galaxies (NLS1s) must have been crucial key to understand the rapid growth of the central supermassive black hole, which may be related to the evolution of the host galaxy. Hence, we propose 20x5 ksec observations of the luminous NLS1 galaxy PKS 0558-504, which is the candidate having the highest mass-accretion rate among the class. Large effective area and good energy resolution of XISs allow us to strictly constrain the temperature and the luminosity of the accretion flow. In addition, Suzaku HXD will detect the significant fraction of hard power law emission in the 10-60 keV band for the first time. From these observations, we expect to derive the new picture of the high mass-accretion mechanism in NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YOSHITO HABA | JAP | 1 | AO1 | SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701011020/ | Quick Look | ![]() |
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268 | NGC 5273 | 205.535 | 35.6446 | 204.979886 | 35.89633 | 186.960858 | 42.373618 | 74.3162813 | 76.25118024 | 278.9999 | 56489.1929976852 | 2013-07-16 04:37:55 | 56491.0543171296 | 2013-07-18 01:18:13 | 708001010 | 81.7709 | 80 | 81.7709 | 81.7949 | 0 | 81.7789 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79.0981 | 79.0981 | 160.8018 | 3 | PROCESSED | 57612.0002546296 | 2016-08-12 00:00:22 | 56890 | 2014-08-21 00:00:00 | 56523.6749537037 | 2013-08-19 16:11:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080015 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Here we propose to observe two of the lowest luminosity BAT AGNs to measure the amount of the reflection component with unpreceded accuracy, a key parameter to determine the contribution of Compton thick AGNs to the X-ray background. We will also study how the torus structure of low luminosity AGNs differs from that of more luminous AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 8 | AO8 | BROAD BAND SPECTRA OF HARD X-RAY SELECTED VERY LOW LUMINOSITY AGNS AND THEIR TORUS STRUCTURE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708001010/ | Quick Look | ![]() |
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269 | NGC 3516 | 166.6694 | 72.5588 | 165.816381 | 72.829135 | 123.37012 | 57.971175 | 133.25250212 | 42.40656753 | 323.9054 | 56754.7044675926 | 2014-04-07 16:54:26 | 56755.5002777778 | 2014-04-08 12:00:24 | 708006080 | 51.539 | 50 | 51.539 | 51.547 | 0 | 51.555 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.0472 | 46.0472 | 68.752 | 1 | PROCESSED | 57614.1922800926 | 2016-08-14 04:36:53 | 56383 | 2013-04-01 00:00:00 | 56817.774849537 | 2014-06-09 18:35:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080066 | We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 8 | AO8 | THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006080/ | Quick Look | ![]() |
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270 | HOLMBERG II X-1 | 124.8874 | 70.7162 | 123.586257 | 70.872801 | 106.845907 | 49.308193 | 144.27230635 | 32.72696637 | 127.9069 | 56552.1954398148 | 2013-09-17 04:41:26 | 56553.2994212963 | 2013-09-18 07:11:10 | 708015010 | 52.19 | 50 | 52.19 | 52.19 | 0 | 52.19 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.9852 | 48.9852 | 95.376 | 0 | PROCESSED | 57612.6731481482 | 2016-08-12 16:09:20 | 56954 | 2014-10-24 00:00:00 | 56588.6670717593 | 2013-10-23 16:00:35 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081251 | Recent X-ray observations have produced evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in an unusual super-Eddington state. Current data are unable to deliver a clear answer, as attempts to model the 0.5-10keV spectra have been plagued by degeneracies resulting from the limited bandpass, owing to the previous lack of focusing hard X-ray telescopes. Combined, Suzaku and NuSTAR will obtain high-quality spectra covering 0.5-30keV, providing powerful probes for understanding the accretion modes and nature of the central BHs. A definitive statement on the existence of either 100-1000Msun black holes or extreme accretion states will be an important legacy of both missions. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | DOMINIC WALTON | USA | 8 | AO8 | COORDINATED SUZAKU AND NUSTAR OBSERVATIONS OF HOLMBERG II X-1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708015010/ | Quick Look | ![]() |
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271 | KAZ 102 | 270.6661 | 67.6374 | 270.701804 | 67.634057 | 77.059679 | 88.893324 | 97.62313354 | 29.55178422 | 2.066 | 53895.6833101852 | 2006-06-09 16:23:58 | 53896.5343055556 | 2006-06-10 12:49:24 | 701012010 | 41.454 | 40 | 41.454 | 41.462 | 41.47 | 41.47 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 40.9507 | 40.9507 | 73.5199 | 2 | PROCESSED | 57534.6269328704 | 2016-05-26 15:02:47 | 54394 | 2007-10-21 00:00:00 | 53928.2501157407 | 2006-07-12 06:00:10 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010112 | We propose to make a detailed broad-band X-ray spectroscopic study of the radio quiet QSO (RQQ) Kaz 102. This RQQ had a power-law spectrum with a photon index ~ 1 with our ASCA observation. We also found a spectral variability over the time scale of years, from ~ 2.2 during the ROSAT All Sky Survey to ~ 1 during the Einstein / ASCA observations. From our ASCA spectra, we couldn't discriminate whether the apparently unusual hard spectrum was caused by warm absorber, Compton reflection, or a simple featureless power-law continuum. High quality and wide-band spectroscopy with Suzaku is essential to unveil the physical nature of the enigmatic hardness and spectral variability of Kaz 102. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YOSHITAKA ISHISAKI | JAP | 1 | AO1 | WHAT IS THE PHYSICAL NATURE OF KAZ 102: AN ENIGMATIC X-RAY HARD RADIO QUIET QSO? | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701012010/ | Quick Look | ![]() |
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272 | 1ES1218+304 | 185.3064 | 30.1169 | 184.679878 | 30.394195 | 171.661841 | 29.481192 | 186.88913956 | 82.72978014 | 298.9428 | 53874.8006365741 | 2006-05-19 19:12:55 | 53876.706412037 | 2006-05-21 16:57:14 | 701025010 | 79.8692 | 80 | 79.8852 | 79.8692 | 79.8852 | 79.8772 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 70.5118 | 70.5118 | 164.6379 | 2 | PROCESSED | 57534.4292013889 | 2016-05-26 10:18:03 | 54398 | 2007-10-25 00:00:00 | 53927.8564930556 | 2006-07-11 20:33:21 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010157 | We propose to conduct a series of simultaneous X-ray/VHE (very high energy) gamma-ray observations of northern TeV Blazars (Mkn 421, Mkn 501, 1ES1218+304, and 1ES1426+428) with Suzaku XIS and HXD in conjunction with the HESS (High Energy Stereoscopic System) and MAGIC ground based gamma-ray observatories. The goal of these observations is to study the spectral energy distribution of these highly variable objects for the first time simultaneously in the soft to hard X-ray (0.3 keV-100 keV) | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | SIMULTANEOUS X-RAY/VHE GAMMA-RAY OBSERVATIONS OF NORTHERN BLAZARS WITH SUZAKU AND HESS/MAGIC | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701025010/ | Quick Look | ![]() |
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273 | 1ES1426+428 | 217.0716 | 42.6249 | 216.585066 | 42.847682 | 193.182318 | 52.911489 | 77.44668506 | 64.96380656 | 316.1862 | 53902.7388310185 | 2006-06-16 17:43:55 | 53904.2225 | 2006-06-18 05:20:24 | 701026010 | 60.9149 | 60 | 60.9149 | 60.9149 | 60.9149 | 60.9149 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 54.0911 | 54.0911 | 128.16 | 1 | PROCESSED | 57534.6747800926 | 2016-05-26 16:11:41 | 54400 | 2007-10-27 00:00:00 | 53928.3009143518 | 2006-07-12 07:13:19 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010157 | We propose to conduct a series of simultaneous X-ray/VHE (very high energy) gamma-ray observations of northern TeV Blazars (Mkn 421, Mkn 501, 1ES1218+304, and 1ES1426+428) with Suzaku XIS and HXD in conjunction with the HESS (High Energy Stereoscopic System) and MAGIC ground based gamma-ray observatories. The goal of these observations is to study the spectral energy distribution of these highly variable objects for the first time simultaneously in the soft to hard X-ray (0.3 keV-100 keV) | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | SIMULTANEOUS X-RAY/VHE GAMMA-RAY OBSERVATIONS OF NORTHERN BLAZARS WITH SUZAKU AND HESS/MAGIC | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701026010/ | Quick Look | ![]() |
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274 | MRK 501 | 253.4 | 39.7089 | 252.98087 | 39.789378 | 242.4893 | 61.571247 | 63.52834502 | 38.90621529 | 316.9908 | 53934.7872569444 | 2006-07-18 18:53:39 | 53935.7272916667 | 2006-07-19 17:27:18 | 701027010 | 42.4271 | 40 | 42.4389 | 42.4389 | 42.4271 | 42.4351 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39.9711 | 39.9711 | 81.2099 | 0 | PROCESSED | 57534.9978587963 | 2016-05-26 23:56:55 | 54408 | 2007-11-04 00:00:00 | 53971.6784259259 | 2006-08-24 16:16:56 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010157 | We propose to conduct a series of simultaneous X-ray/VHE (very high energy) gamma-ray observations of northern TeV Blazars (Mkn 421, Mkn 501, 1ES1218+304, and 1ES1426+428) with Suzaku XIS and HXD in conjunction with the HESS (High Energy Stereoscopic System) and MAGIC ground based gamma-ray observatories. The goal of these observations is to study the spectral energy distribution of these highly variable objects for the first time simultaneously in the soft to hard X-ray (0.3 keV-100 keV) | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | SIMULTANEOUS X-RAY/VHE GAMMA-RAY OBSERVATIONS OF NORTHERN BLAZARS WITH SUZAKU AND HESS/MAGIC | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701027010/ | Quick Look | ![]() |
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275 | MKN 335 | 1.5763 | 20.2091 | 0.933386 | 19.930785 | 9.740827 | 17.860354 | 108.75916207 | -41.41726175 | 71.5255 | 56457.9792939815 | 2013-06-14 23:30:11 | 56461.868287037 | 2013-06-18 20:50:20 | 708016020 | 154.8168 | 300 | 154.8648 | 154.8168 | 0 | 154.8568 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 141.5908 | 141.5908 | 335.8944 | 3 | PROCESSED | 57611.6590162037 | 2016-08-11 15:48:59 | 56383 | 2013-04-01 00:00:00 | 56512.7189467593 | 2013-08-08 17:15:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081411 | The idea of this proposal is trigger a 300ks observation with Suzaku of the Narrow Line Seyfert 1 Galaxy Mkn 335 during one of its low X-ray flux states. The goal here is to measure its underlying broad-band continuum with Suzaku during a low state and compare it with the 2006 high-state observations. Mkn 335 is one of the best examples of an AGN that went into a deep minimum X-ray flux state. Two competing models can explain these extreme low states: reflection models and partial covering absorber models. Both models still require a variable underlying intrinsic continuum. The science driver is to find out what is causing these low X-ray flux states that have been observed in several NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | DIRK GRUPE | USA | 8 | AO8-TOO | INTRINSIC LOW-STATE X-RAY LUMINOSITY OF THE NLS1 MKN 335 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708016020/ | Quick Look | ![]() |
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276 | NGC5929 | 231.5229 | 41.6989 | 231.07632 | 41.872918 | 210.309469 | 57.436696 | 67.89643134 | 55.30533508 | 120.4869 | 56651.8033217593 | 2013-12-25 19:16:47 | 56652.6042824074 | 2013-12-26 14:30:10 | 708022010 | 24.649 | 30 | 24.649 | 24.6689 | 0 | 24.6565 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.1767 | 25.1767 | 69.1919 | 0 | PROCESSED | 57613.6825925926 | 2016-08-13 16:22:56 | 56383 | 2013-04-01 00:00:00 | 56700.6301388889 | 2014-02-12 15:07:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081418 | Using Suzaku's sensitivity in the 2-50keV range, we propose to obtain broad-band spectral fits to the X-ray emission from five Seyfert galaxies which have nuclei that are likely to be Compton-thick. We will thereby derive estimates of their absorbing column densities (hitherto unknown), Fe line widths and equivalent widths, absorption-corrected nuclear X-ray emission and the reprocessed components. With these new estimates we will have complete measurements for a rigorously selected sample of 20 Seyferts that are matched in orientation-independent parameters. The sample selection enables us to account for orientation effects which dominate in them, and investigate the AGN evolution, AGN-star burst connection, and host galaxy evolution. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | PRAJVAL SHASTRI | USA | 8 | AO8 | COMPTON-THICK SEYFERT NUCLEI AND SEYFERT UNIFICATION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708022010/ | Quick Look | ![]() |
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277 | MRK533 | 351.9889 | 8.7759 | 351.354325 | 8.500435 | 356.155514 | 11.232339 | 90.62800693 | -48.78900326 | 248.1747 | 56634.8830671296 | 2013-12-08 21:11:37 | 56636.0847569444 | 2013-12-10 02:02:03 | 708023010 | 52.194 | 50 | 52.194 | 52.194 | 0 | 52.194 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.5617 | 48.5617 | 103.8059 | 0 | PROCESSED | 57613.5724421296 | 2016-08-13 13:44:19 | 56383 | 2013-04-01 00:00:00 | 56646.7358449074 | 2013-12-20 17:39:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081418 | Using Suzaku's sensitivity in the 2-50keV range, we propose to obtain broad-band spectral fits to the X-ray emission from five Seyfert galaxies which have nuclei that are likely to be Compton-thick. We will thereby derive estimates of their absorbing column densities (hitherto unknown), Fe line widths and equivalent widths, absorption-corrected nuclear X-ray emission and the reprocessed components. With these new estimates we will have complete measurements for a rigorously selected sample of 20 Seyferts that are matched in orientation-independent parameters. The sample selection enables us to account for orientation effects which dominate in them, and investigate the AGN evolution, AGN-star burst connection, and host galaxy evolution. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | PRAJVAL SHASTRI | USA | 8 | AO8 | COMPTON-THICK SEYFERT NUCLEI AND SEYFERT UNIFICATION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708023010/ | Quick Look | ![]() |
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278 | NGC 4552 | 188.9456 | 12.612 | 188.314388 | 12.887225 | 183.105993 | 15.109639 | 287.9907408 | 75.02773792 | 120.0696 | 54072.312974537 | 2006-12-03 07:30:41 | 54072.8405092593 | 2006-12-03 20:10:20 | 701037010 | 20.4398 | 20 | 20.4398 | 20.4398 | 0 | 20.4398 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.553 | 16.553 | 45.5439 | 0 | PROCESSED | 57536.226875 | 2016-05-28 05:26:42 | 54455 | 2007-12-21 00:00:00 | 54088.5410069444 | 2006-12-19 12:59:03 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011333 | The majority of accretion onto supermassive black holes in the local Universe occurs in obscured Seyferts. At moderate redshifts, the optical narrow emission-lines used to identify Seyfert 2s become difficult to isolate from the host galaxy's emission, resulting in an underestimate of the numbers of Seyfert 2s. Seyfert 2s are a critical component of AGN synthesis models of the Cosmic X-ray Background (CXB), as these sources are likely responsible for the unresolved component of the 2-8 keV background and may also contribute significantly to the 30 keV background. We propose to use Suzaku observations of ten local Seyfert 2s to measure their ultrahard (>10 keV) emission and examine how Seyfert 2s at moderate redshifts contribute to the CXB. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | AARON STEFFEN | USA | 1 | AO1 | MEASURING THE ULTRAHARD X-RAY EMISSION OF A LOCAL POPULATION OF SEYFERT 2S | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701037010/ | Quick Look | ![]() |
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279 | PDS 456 | 262.0807 | -14.2604 | 261.370018 | -14.220332 | 262.221238 | 8.96686 | 10.39565911 | 11.16772638 | 98.239 | 54155.7486574074 | 2007-02-24 17:58:04 | 54160.0355787037 | 2007-03-01 00:51:14 | 701056010 | 190.6002 | 188 | 190.6082 | 190.6002 | 0 | 190.6142 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 176.4708 | 176.4708 | 370.3428 | 4 | PROCESSED | 57537.5850578704 | 2016-05-29 14:02:29 | 54757 | 2008-10-18 00:00:00 | 54168.6244560185 | 2007-03-09 14:59:13 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011351 | A long 150ks Suzaku observation of the most luminous nearby quasar, PDS 456, is proposed. In the X-ray band, PDS 456 shows a deep iron K absorption trough. One possibility is that the absorption arises from a massive 0.1c outflow, of column density 10^24 cm^-2. Such an outflow would represent a significant fraction of the quasar energy budget. A deep Suzaku observation is proposed to test this outflow model, in particular the high energy bandpass of Suzaku is essential for measuring the profile of the absorption feature and determining the kinematics of the outflow. It is also possible to differentiate between competing models for the iron K feature, most notably between an outflow and a strong reflection component from the innermost radii around a Kerr black hole. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JAMES REEVES | USA | 1 | AO1 | SOLVING THE ORIGIN OF THE DEEP IRON K ABSORPTION IN PDS 456 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701056010/ | Quick Look | ![]() |
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280 | ABELL 1005 | 156.925 | 68.2013 | 156.004708 | 68.456472 | 124.194907 | 52.556114 | 140.47803773 | 43.70739533 | 119.4313 | 56609.4953819444 | 2013-11-13 11:53:21 | 56610.8334490741 | 2013-11-14 20:00:10 | 708042010 | 61.3496 | 60 | 61.3496 | 61.3496 | 0 | 61.3496 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 58.9645 | 58.9645 | 115.5998 | 2 | PROCESSED | 57613.3284722222 | 2016-08-13 07:53:00 | 56994 | 2014-12-03 00:00:00 | 56625.7198611111 | 2013-11-29 17:16:36 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081533 | We propose to map out the core of the A981 supercluster with three Suzaku observations. The A981 supercluster contains four Abell richness class 2 clusters within a redshift range of 2,000 km/s. All four clusters also overlap within their virial radii, at least in projection. The low and steady background of the Suzaku telescope is ideal for studying the low surface brightness X-ray emission between the clusters. Such observations will determine if the clusters are interacting via the detection of merger-induced shocks or perturbed features in the outskirts of the individual clusters. Our proposed Suzaku observations will help elucidate the fundamental astrophysics that occurs during the formation of very massive clusters. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | LAURENCE DAVID | USA | 8 | AO8 | MAPPING THE ABELL 981 SUPER CLUSTER WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708042010/ | Quick Look | ![]() |
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281 | BL LACERTAE | 330.6466 | 42.3471 | 330.130697 | 42.105096 | 354.282545 | 49.658149 | 92.61224541 | -10.37092111 | 71.9797 | 53882.2303703704 | 2006-05-27 05:31:44 | 53883.305775463 | 2006-05-28 07:20:19 | 701073010 | 48.5294 | 50 | 48.5454 | 48.5454 | 48.5294 | 48.5374 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35.5443 | 35.5443 | 92.902 | 1 | PROCESSED | 57534.4514236111 | 2016-05-26 10:50:03 | 54401 | 2007-10-28 00:00:00 | 53926.2373032407 | 2006-07-10 05:41:43 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011377 | We propose two 50 ks Suzaku observations, one for each of gamma-ray bright blazars PKS 1510-089 and BL Lacertae, to be coordinated with optical and radio observations. The goal is to obtain broadband spectra and light-curves. The X-ray fluxes are known to be rapidly variable, but there is no information about the correlation between the spectral shape and flux, which is necessary to establish the origin of previously detected prominent soft X-ray excesses. They are crucial to discriminate between different radiation scenarios responsible for production of hard X-rays and gamma-rays, and to constrain the content and by extension, the acceleration process of the jet. These observations will be ingredients of a "pilot" campaigns for the future joint Suzaku-GLAST investigations. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GRZEGORZ MADEJSKI | USA | 1 | AO1 | SUZAKU OBSERVATIONS OF GAMMA-RAY BRIGHT BLAZARS BL LACERTAE AND PKS 1510-089 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701073010/ | Quick Look | ![]() |
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282 | NGC 2788A | 135.6754 | -68.2181 | 135.519975 | -68.019146 | 206.346244 | -72.761691 | 284.17134554 | -14.14937336 | 282.2863 | 57157.0478819444 | 2015-05-15 01:08:57 | 57158.2230324074 | 2015-05-16 05:21:10 | 710007010 | 42.2339 | 40 | 42.2339 | 42.2339 | 0 | 42.2339 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.6656828704 | 2016-08-18 15:58:35 | 57591 | 2016-07-22 00:00:00 | 57224.447650463 | 2015-07-21 10:44:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 100009 | Swift/BAT extragalactic survey above E >15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe four Compton thick AGN candidates in the 70 month BAT catalog with Suzaku. Since their spectra below 10 keV are likely reflection dominated, joint analysis of Suzaku/XIS and Swift/BAT can constrain the absorption and intrinsic luminosity without being much affected by time variability. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep survey. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YOSHIHIRO UEDA | JAP | 10 | AO10 | DETERMINATION OF NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710007010/ | Quick Look | ![]() |
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283 | MARKARIAN 509 | 311.0194 | -10.6637 | 310.338544 | -10.845188 | 310.53976 | 7.19158 | 36.02321332 | -29.81091499 | 73.1708 | 53850.7831481482 | 2006-04-25 18:47:44 | 53851.5252199074 | 2006-04-26 12:36:19 | 701093010 | 24.5756 | 25 | 24.5756 | 24.5756 | 24.5916 | 24.5916 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 15.407 | 15.407 | 64.0979 | 1 | PROCESSED | 57533.5586342593 | 2016-05-25 13:24:26 | 54394 | 2007-10-21 00:00:00 | 53907.6894560185 | 2006-06-21 16:32:49 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012050 | We propose to perform 4 repeated Suzaku observations of 25 ks each of the Seyfert 1 galaxy MKN 509, the brightest Seyfert galaxy of the Piccinotti sample in the 2-100 keV band that is not strongly affected by neutral or ionized absorbing material. The aim of the study is to disentangle the different physical explanations for the origin of the soft excess looking at the long time--scale correlations between the variations of the emission and shape of the soft excess and the emission at high energy (E > 10 keV). | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GABRIELE PONTI | EUR | 1 | AO1 | SOLVING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701093010/ | Quick Look | ![]() |
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284 | NGC 4395 | 186.4111 | 33.4884 | 185.79012 | 33.76517 | 170.810459 | 32.904029 | 162.54122992 | 81.55189464 | 303.1476 | 54253.6042013889 | 2007-06-02 14:30:03 | 54256.2981944444 | 2007-06-05 07:09:24 | 702001010 | 101.5075 | 100 | 101.5155 | 101.5075 | 0 | 101.5155 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 101.9292 | 101.9292 | 232.7198 | 4 | PROCESSED | 57538.8900694444 | 2016-05-30 21:21:42 | 54745 | 2008-10-06 00:00:00 | 54263.5438194445 | 2007-06-12 13:03:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020001 | We propose a 100 ks observation of the intermediate mass black hole (IMBH) active nucleus in the dwarf Seyfert galaxy NGC 4395. Utilising the high-energy sensitivity of Suzaku will enable us to determine the shape of the intrinsic continuum, which is significantly absorbed below 10 keV. Constraining the shape of the continuum will allow us to investigate the more general problem of the relationship between AGN flux and apparent spectral slope. In addition, with a firm grasp of the intrinsic continuum properties, we can accurately determine the physical conditions of the warm absorber in NGC 4395. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YASUO TANAKA | JAP | 2 | AO2 | UNCOVERING THE IMBH ACTIVE NUCLEUS IN THE DWARF SEYFERT GALAXY NGC 4395 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702001010/ | Quick Look | ![]() |
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285 | M33 X8 | 23.4834 | 30.5892 | 22.778431 | 30.333215 | 33.223542 | 19.296261 | 133.64723816 | -31.39681198 | 258.5185 | 55207.0743865741 | 2010-01-11 01:47:07 | 55209.5626157407 | 2010-01-13 13:30:10 | 704016010 | 106.1036 | 100 | 106.1036 | 106.1061 | 0 | 106.1061 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 6.1053 | 6.1053 | 214.9577 | 1 | PROCESSED | 57550.3046412037 | 2016-06-11 07:18:41 | 55587 | 2011-01-26 00:00:00 | 55218.6414930556 | 2010-01-22 15:23:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040067 | The nature of ultraluminous X-ray sources (ULXs) is one of the important unresolved issues in the modern astrophysics. In order to solve the problem, it is of crucial importance to observe X-ray spectra above 10 keV from ULXs, which enables us to determine precisely their spectral states. Therefore, Suzaku observations of two bright ULX, M33 X8 and IC 342 X2, are proposed. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | NAOKI ISOBE | JAP | 4 | AO4 | HARD X-RAY STUDY OF ULTRALUMINOUS X-RAY SOURCES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704016010/ | Quick Look | ![]() |
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286 | ARK 564 | 340.6583 | 29.7351 | 340.07073 | 29.472916 | 355.35057 | 34.71587 | 92.13955378 | -25.32593551 | 75.7895 | 57167.0898842593 | 2015-05-25 02:09:26 | 57168.4029282407 | 2015-05-26 09:40:13 | 710018010 | 52.5104 | 50 | 52.5104 | 53.9344 | 0 | 53.9344 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.9802 | 27.9802 | 100.9477 | 2 | PROCESSED | 57618.7636921296 | 2016-08-18 18:19:43 | 57548 | 2016-06-09 00:00:00 | 57178.248587963 | 2015-06-05 05:57:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 102721 | A NuSTAR legacy is emerging through long observations of bare Seyfert galaxies that reveal an unprecedented look at relativistic reflection off an ionized accretion disc. We propose now to look at the Seyfert galaxy Ark 564 for 200 ks with NuSTAR and 50 ks with Suzaku in order to understand the reflection in this bright source. Ark 564 has been well-studied in the soft band, revealing a steep spectrum, strong soft excess, broad iron K emission line and dramatic variability on the order of hours. It is very akin to two other well-known bare Seyferts, 1H0707-405 and IRAS 13224-3809, except it is an order of magnitude brighter. With this 200 ks observation, we will probe the geometry of the corona, through a complete spectral and timing analysis. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | ERIN KARA | EUR | 10 | AO10 | UNDERSTANDING REFLECTION IN THE BARE SEYFERT I ARK 564 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710018010/ | Quick Look | ![]() |
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287 | B2 1023+25 | 156.5986 | 25.7113 | 155.903697 | 25.966089 | 148.79406 | 14.812793 | 207.05661505 | 57.60744793 | 288.3095 | 56442.6428125 | 2013-05-30 15:25:39 | 56444.9133449074 | 2013-06-01 21:55:13 | 708044010 | 100.8874 | 100 | 100.8954 | 100.8874 | 0 | 100.8954 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 96.5787 | 96.5787 | 196.1298 | 2 | PROCESSED | 57611.461099537 | 2016-08-11 11:03:59 | 56821 | 2014-06-13 00:00:00 | 56455.8205324074 | 2013-06-12 19:41:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082005 | We propose a deep (100 ksec) Suzaku observation of the recently discovered high redshift blazar candidate B2 1023+25 (z=5.3). A very hard (Gamma <2) spectrum would confirm its blazar nature, allowing to study the physical properties of the relativistic jet in this extremely powerful and very high redshift source. The proposed observation will yield an X-ray spectrum of sufficient quality to determine the X-ray shape. The confirmation of a second blazar at this redshift has profound cosmological implications, placing stronger constraints on the number density of high mass BH at high z | EXTRAGALACTIC COMPACT SOURCES | 7 | A | VALENTINA BRAITO | EUR | 8 | AO8 | THE HIGH-REDSHIFT BLAZAR CANDIDATE B2 1023+25 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708044010/ | Quick Look | ![]() |
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288 | OJ 287 QUIESCENT | 133.689 | 20.0482 | 132.974133 | 20.239223 | 130.506959 | 2.538802 | 206.87650629 | 35.78772906 | 283.9125 | 54200.8243055556 | 2007-04-10 19:47:00 | 54203.4654976852 | 2007-04-13 11:10:19 | 702009010 | 102.8441 | 100 | 102.8441 | 102.8441 | 0 | 102.8441 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93.6244 | 93.6244 | 228.1859 | 12 | PROCESSED | 57538.2031018518 | 2016-05-30 04:52:28 | 54744 | 2008-10-05 00:00:00 | 54210.7303587963 | 2007-04-20 17:31:43 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020024 | OJ 287 is a promissing candidate of a suppermassive binary black hole, based on its periodic flare with a cycle of about 12 years. The next flare is predicted to take place on the fall, 2007. Therefore, two Suzaku exposures on OJ 287 is proposed, coordinated with radio, optical and very high energy gamma-ray observations. The first observation is on the spring to obtained the multi-wavelength spectrum of the target in its quiescent phase. The second is planned to be in a form of ToO observation on the fall, which will be triggered by an optical flare. The nature of the flare will be extensively investigated in these observatsions. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NAOKI ISOBE | JAP | 2 | AO2-TOO | MULTI-WAVELENGTH OBSERVATION OF PREDICTED FLARE OF SUPERMASSIVE BINARY BLACK HOLE CANDIDATE, OJ 287 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702009010/ | Quick Look | ![]() |
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289 | SWIFT J0714.2+3518 | 108.5168 | 35.2792 | 107.688726 | 35.365694 | 105.421903 | 12.82422 | 182.49455345 | 19.57130625 | 283.6115 | 57116.9939814815 | 2015-04-04 23:51:20 | 57118.9043634259 | 2015-04-06 21:42:17 | 709007010 | 79.2471 | 80 | 79.2471 | 79.2471 | 0 | 79.2471 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.9309027778 | 2016-08-17 22:20:30 | 57565 | 2016-06-26 00:00:00 | 57198.4724074074 | 2015-06-25 11:20:16 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090019 | Swift/BAT extragalactic survey above E >15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe two Compton thick AGN candidates in the 70 month BAT catalog with Suzaku. To resolve the degeneracy of spectral modeling, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | DETERMINATION OF NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709007010/ | Quick Look | ![]() |
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290 | KUV 00311-1938 | 8.3907 | -19.361 | 7.763877 | -19.636683 | 359.653009 | -21.03622 | 94.15504043 | -81.21658968 | 60.8243 | 56821.2581481482 | 2014-06-13 06:11:44 | 56822.2384606482 | 2014-06-14 05:43:23 | 709013010 | 41.8926 | 40 | 41.8926 | 41.9006 | 0 | 41.9006 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.9853 | 35.9853 | 84.6858 | 0 | PROCESSED | 57615.2401851852 | 2016-08-15 05:45:52 | 57200 | 2015-06-27 00:00:00 | 56833.588900463 | 2014-06-25 14:08:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090088 | Extreme HBL objects are BL Lac objects characterized by their hard TeV gamma-ray spectra, by which the sources are considered as excellent targets to study secondary cascade gamma-ray emission induced by very-high-energy photons or protons from the sources. We propose Suzaku observations of 1ES 0347-121 and KUV 00311-1938 for 60 ks and 40 ks, respectively. The observations can reveal detailed spectral structure around synchrotron peak in the extreme HBLs, which are essential to derive physical parameters such as electron spectrum, magnetic filed strength in the jet. The results will help understating gamma-ray components of both intrinsic jet emission and the secondary cascade emission. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | MASAAKI HAYASHIDA | JAP | 9 | AO9 | SUZAKU OBSERVATIONS OF EXTREME HIGH-FREQUENCY PEAKED BL LAC OBJECTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709013010/ | Quick Look | ![]() |
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291 | NGC 4593 | 189.9133 | -5.3412 | 189.268409 | -5.066685 | 191.201213 | -0.986393 | 297.4806457 | 57.40576161 | 111.8999 | 57017.6624421296 | 2014-12-26 15:53:55 | 57021.7640740741 | 2014-12-30 18:20:16 | 709014040 | 130.3584 | 30 | 130.3904 | 130.3584 | 0 | 130.3824 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5950810185 | 2016-08-17 14:16:55 | 57415 | 2016-01-28 00:00:00 | 57049.4551851852 | 2015-01-27 10:55:28 | 3.0.22.44 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090097 | In the AO-8 cycle, we proposed six X-ray and optical simultaneous observations of type I Seyfert galaxy NGC 3516, and now obtaining a good correlation between those wavelengths. In the observations, we confirmed that a hard X-ray primary component (HXPC) found in Noda et al. (2013) was dominant, and its variation is well correlated with an optical one. To verify the probability that a variation of HXPC in other Seyfert also correlates with that in its optical, we propose six X-ray and optical simultaneous observations of NGC 4593, which has an X-ray spectrum dominated by HXPC as well as NGC 3516 in 2013. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 9 | AO9 | X-RAY AND OPTICAL SIMULTANEOUS OBSERVATIONS OF TYPICAL TYPE I SEYFERT NGC 4593 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709014040/ | Quick Look | ![]() |
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292 | LMC X-4 | 83.221 | -66.3591 | 83.212611 | -66.392014 | 1.088478 | -87.292124 | 276.32094979 | -32.52452295 | 284.2438 | 54561.5523842593 | 2008-04-05 13:15:26 | 54562.3058333333 | 2008-04-06 07:20:24 | 702036020 | 25.3397 | 20 | 25.3425 | 25.3425 | 0 | 25.3397 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24.502 | 24.502 | 65.07 | 0 | PROCESSED | 57542.2490046296 | 2016-06-03 05:58:34 | 54943 | 2009-04-22 00:00:00 | 54574.4237152778 | 2008-04-18 10:10:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021127 | We propose for a series of three 20ks observations of the binary X-ray pulsar LMC X-4. This source shows 13.5 s pulsations, a 1.4 d orbital period, and a long-period (~30 d) variability due to a warped, precessing accretion disk. The proposed analysis will use pulse-phase spectroscopy with XIS to explore changes in the X-ray pulses and spectra at three different phases in the disk precession. This work will give us a detailed picture of the accretion flow, particularly for the inner regions of the accretion disk that are illuminated by the X-rays from the neutron star. This project takes advantage of the strengths of the XIS, particularly its excellent spectral resolution, sufficient (1s) time resolution in Window mode, and wide PSF that limits pile-up effects. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RYAN HICKOX | USA | 2 | AO2 | SUPERORBITAL VARIATION OF LMC X-4: EXPLORING THE ACCRETION FLOW | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702036020/ | Quick Look | ![]() |
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293 | NGC5548 | 214.4955 | 25.1272 | 213.928592 | 25.357387 | 201.997114 | 36.406484 | 31.93108614 | 70.4962838 | 289.7815 | 54303.4447337963 | 2007-07-22 10:40:25 | 54304.2711111111 | 2007-07-23 06:30:24 | 702042060 | 28.9178 | 30 | 28.9258 | 28.9258 | 0 | 28.9178 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24.8181 | 24.8181 | 71.3839 | 1 | PROCESSED | 57539.29125 | 2016-05-31 06:59:24 | 54706 | 2008-08-28 00:00:00 | 54339.5363310185 | 2007-08-27 12:52:19 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021307 | We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARTIN ELVIS | USA | 2 | AO2 | NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702042060/ | Quick Look | ![]() |
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294 | NGC 4507 | 188.8987 | -39.9119 | 188.223538 | -39.636542 | 205.656728 | -32.779926 | 299.63576127 | 22.85843053 | 109.5879 | 54454.5145717593 | 2007-12-20 12:20:59 | 54456.5835532407 | 2007-12-22 14:00:19 | 702048010 | 103.626 | 80 | 103.634 | 103.626 | 0 | 103.634 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 110.9021 | 110.9021 | 178.7279 | 0 | PROCESSED | 57540.963900463 | 2016-06-01 23:08:01 | 54829 | 2008-12-29 00:00:00 | 54462.288287037 | 2007-12-28 06:55:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021331 | Recent X-ray observations of Seyfert 2 galaxies have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by AGN Unified Schemes. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (60 ksec each) of four local bright Compton-thin Seyfert2s, selected from the Swift/BAT survey with a hard X-ray flux exceeding 1e-10 cgs to form a flux-limited sample. The unprecedented broad bandpass of Suzaku offers a unique tool to investigate the X-ray emission, placing strong constraints on the geometry and location of the reprocessing matter. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | JAMES REEVES | USA | 2 | AO2 | REVEALING THE REPROCESSING MATTER IN SEYFERT 2 GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702048010/ | Quick Look | ![]() |
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295 | HOLMBERG IX X-1 | 149.4756 | 69.0751 | 148.45738 | 69.31359 | 119.76782 | 51.701026 | 141.91985765 | 41.06519535 | 104.8942 | 56976.7425347222 | 2014-11-15 17:49:15 | 56977.5230787037 | 2014-11-16 12:33:14 | 709015020 | 34.1281 | 30 | 34.1281 | 34.1281 | 0 | 34.1281 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7878240741 | 2016-08-16 18:54:28 | 57359 | 2015-12-03 00:00:00 | 56993.4304513889 | 2014-12-02 10:19:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091251 | Broadband X-ray spectroscopy of ultraluminous X-ray sources (ULXs) with NuSTAR and Suzaku has begun to provide important information regarding the nature of these enigmatic sources. Recent NuSTAR observations of the extreme ULX Holmberg IX X-1 revealed unusual spectral variability, and different competing evolutionary scenarios can explain the available data. Resolving this degeneracy is critical to determining the nature of the accretion onto this source, and requires multi-epoch broadband spectroscopy probing a more diverse range of fluxes. We propose to undertake 4x30 ks coordinated Suzaku+NuSTAR observations of Holmberg IX X-1 to provide the additional spectra needed to robustly determine the nature of the observed evolution, providing a vital step in our understanding of extreme ULXs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | DOMINIC WALTON | USA | 9 | AO9 | MULTI-EPOCH BROADBAND X-RAY SPECTROSCOPY OF HOLMBERG IX X-1 WITH SUZAKU AND NUSTAR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709015020/ | Quick Look | ![]() |
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296 | I ZW 18 | 143.5064 | 55.23 | 142.623877 | 55.452479 | 125.705805 | 38.222173 | 160.54065348 | 44.84408453 | 279.2158 | 56792.4911111111 | 2014-05-15 11:47:12 | 56792.8568402778 | 2014-05-15 20:33:51 | 709021010 | 17.2612 | 100 | 17.2612 | 17.2612 | 0 | 17.2612 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.549 | 16.549 | 31.1279 | 0 | PROCESSED | 57615.102650463 | 2016-08-15 02:27:49 | 57358 | 2015-12-02 00:00:00 | 56818.6775347222 | 2014-06-10 16:15:39 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091441 | The source of energetic photons that reionized and heated the early universe remains uncertain. Early galaxies had low metallicity and the best local analogs are blue compact dwarf galaxies (BCDs) with low metallicity. We propose to observe two such galaxies known to be luminous in X-rays and accurately measure their spectrum with the Suzaku XIS. These observations are important to our understanding of the heating of the universe during the epoch of reionization. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | PHILIP KAARET | USA | 9 | AO9 | X-RAYS FROM LOW-METALLICITY BLUE COMPACT DWARF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709021010/ | Quick Look | ![]() |
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297 | MARKARIAN 3 | 93.8907 | 71.0457 | 92.440546 | 71.061085 | 91.87875 | 47.630769 | 143.28642165 | 22.71781378 | 80.3638 | 56937.8059953704 | 2014-10-07 19:20:38 | 56938.0751967593 | 2014-10-08 01:48:17 | 709022020 | 17.7277 | 20 | 17.7357 | 17.7357 | 0 | 17.7277 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6163078704 | 2016-08-16 14:47:29 | 57358 | 2015-12-02 00:00:00 | 56992.4094560185 | 2014-12-01 09:49:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092008 | We propose to measure size and distance from the black hole of the optically-thick absorbing and reprocessing system(s) in the heavily obscured Seyfert Galaxy Markarian~3 by means of its known X-ray spectral variability. We aim at simultaneously measuring: the variability timescale of the primary emission, seen in transmission through a photoelectric column density of (0.7--1.1)x10^{24} atoms/cm/cm; the variability timescale of its Compton-reflection, dominating the continuum flux in the 3-10 keV energy band; and the variability timescale of the nuclear obscuration. Only the scientific payload on-board Suzaku possesses the required combination of broadband X-ray coverage, sensitivity, and spectroscopic capabilities to perform this experiment. We request 5 observations of 20 ks each. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MATTEO GUAINAZZI | EUR | 9 | AO9 | MEASURING THE TORUS SPATIAL SCALE(S) IN SEYFERT GALAXIES: A SUZAKU MONITORING OF MARKARIAN 3 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709022020/ | Quick Look | ![]() |
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298 | QSO 1222+216 | 186.2289 | 21.3877 | 185.599556 | 21.664582 | 176.758894 | 22.007996 | 255.04256268 | 81.66684682 | 123.6039 | 56989.2953356482 | 2014-11-28 07:05:17 | 56989.4064583333 | 2014-11-28 09:45:18 | 709025020 | 0.5272 | 15 | 0.5352 | 0.5272 | 0 | 0.8088 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4022222222 | 2016-08-17 09:39:12 | 57368 | 2015-12-12 00:00:00 | 57002.4417361111 | 2014-12-11 10:36:06 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092023 | EXTRAGALACTIC COMPACT SOURCES | 7 | C | MARCUS LANGEJAHN | EUR | 9 | AO9 | false | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709025020/ | Quick Look | ![]() |
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299 | XBONGBLUE1 | 217.1061 | 32.8569 | 216.573655 | 33.079659 | 200.393656 | 44.372245 | 54.10325006 | 68.28811801 | 132.8525 | 54453.8528587963 | 2007-12-19 20:28:07 | 54454.166875 | 2007-12-20 04:00:18 | 702082010 | 15.1725 | 13 | 15.1725 | 15.1725 | 0 | 15.1725 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.6996 | 15.6996 | 27.1259 | 0 | PROCESSED | 57540.9008217593 | 2016-06-01 21:37:11 | 54828 | 2008-12-28 00:00:00 | 54461.0450231482 | 2007-12-27 01:04:50 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021376 | We propose to use Suzaku's large collecting area and excellent energy response to measure accurate X-ray spectra for 9 XBONGs and 8 luminous Type 2 AGN selected from very large samples of identified XBONGs and Type 2 AGN found in our Chandra XBootes survey. We have obtained optical spectra for 258 XBONGs and identified ~700 X-ray luminous Type 2 AGN at z>0.7. With known source positions and X-ray fluxes, we select sources that are relatively bright with little or no contamination from other X-ray sources. Thus we will measure individual spectra for these bright sources. We propose eight 15 ksec Suzaku XIS observations to measure the absorption in 8 luminous z > 0.8 Type 2 AGN and eight 10 ksec observations to measure the absorption and iron emission for nine XBONGs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | CHRISTINE JONES | USA | 2 | AO2 | OBSCURED AGN AND XBONGS IN BOOTES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702082010/ | Quick Look | ![]() |
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300 | 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 | ![]() |
301 | IGR J12391-1612 | 189.807 | -16.1292 | 189.153193 | -15.854578 | 195.389743 | -10.939243 | 298.65896251 | 46.64122293 | 122.9437 | 54818.9051273148 | 2008-12-18 21:43:23 | 54822.2910648148 | 2008-12-22 06:59:08 | 703007010 | 130.274 | 120 | 130.274 | 130.274 | 0 | 130.274 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 111.0893 | 111.0893 | 292.4838 | 2 | PROCESSED | 57545.0634953704 | 2016-06-06 01:31:26 | 55206 | 2010-01-10 00:00:00 | 54840.5288425926 | 2009-01-09 12:41:32 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030012 | We propose a Suzaku observation of a Compton thick candidate, IGR J12391-1612. This source is a bright Seyfert 2 galaxy in the INTEGRAL AGN catalog by Beckman et al. 2006. By a follow-up observation in the optical band, this source was classified as an X-ray luminous type 2 Seyfert galaxy. A Chandra follow-up observation was also performed, but the shape of the X-ray spectrum was not well determined due to a short exposure of 3.5ks. Thank to the wide-band spectroscopy of Suzaku, we can obtain an X-ray spectrum in the 0.5-100 keV band. We will reveal the nature of this Compton thick Seyfert in a spectral analysis. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HISAMITSU AWAKI | JAP | 3 | AO3 | X-RAY OBSERVATION OF A COMPTON THICK CANDIDATE, IGR J12391-1612 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703007010/ | Quick Look | ![]() |
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302 | NGC 1313 | 49.5565 | -66.5364 | 49.405687 | -66.717354 | 341.391654 | -74.190914 | 283.40259478 | -44.62074971 | 201.281 | 54805.9606828704 | 2008-12-05 23:03:23 | 54808.2814699074 | 2008-12-08 06:45:19 | 703010010 | 91.4661 | 100 | 91.4981 | 91.4661 | 0 | 91.4981 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 78.7593 | 78.7593 | 200.4937 | 1 | PROCESSED | 57544.7004861111 | 2016-06-05 16:48:42 | 55188 | 2009-12-23 00:00:00 | 54822.6519328704 | 2008-12-22 15:38:47 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030038 | The nature of ultra luminous X-ray sources (ULX) is one of the most important unresolved issue in the modern astrophysics. We propose a 100 ks observation of an famous ULX, NGC 1313 X1, in order to search for Fe-K absorption lines, which are important spectral feature of Galactic black holes. Through the absorption feature, we will examine the nature of the ULX. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | KEN OHSUGA | JAP | 3 | AO3 | EXPLORING FE K-LINE ABSORPTION FEATURES FROM AN ULTRALUMINOUS X-RAY SOURCE, NGC 1313 X1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703010010/ | Quick Look | ![]() |
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303 | NGC 454 | 18.511 | -55.3853 | 17.99732 | -55.649778 | 343.260726 | -55.777074 | 296.21074431 | -61.44696878 | 18.3891 | 54950.2291782407 | 2009-04-29 05:30:01 | 54953.4023032407 | 2009-05-02 09:39:19 | 704009010 | 128.9562 | 120 | 128.9562 | 128.9562 | 0 | 128.9562 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 114.5969 | 114.5969 | 274.1296 | 0 | PROCESSED | 57546.5592361111 | 2016-06-07 13:25:18 | 55342 | 2010-05-26 00:00:00 | 54973.5148842593 | 2009-05-22 12:21:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040050 | Seyfert galaxies with a low-mass central black hole are a key class of objects to study the growth phase of supermassive black holes. We propose to observe the hard X-ray brightest and low-mass (1.6e6 Msolar) Seyfert 2 galaxy NGC 454 selected from the Swift BAT survey. The data will be used (1) to measure broad-band X-ray spectrum and its variability, (2) to compare them with properties of known Seyferts, and (3) to search for variation of absorption to constrain the structure and origin of obscuring matter. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YUICHI TERASHIMA | JAP | 4 | AO4 | X-RAY SPECTRAL VARIABILITY OF THE HARD X-RAY BRIGHTEST LOW-MASS SEYFERT 2 NGC 454 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704009010/ | Quick Look | ![]() |
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304 | MRK 18 | 135.5092 | 60.0703 | 134.525486 | 60.267174 | 118.140543 | 40.9961 | 155.86471567 | 39.40052697 | 266.8203 | 55330.5025810185 | 2010-05-14 12:03:43 | 55331.3772106482 | 2010-05-15 09:03:11 | 705001010 | 37.9667 | 40 | 37.9747 | 37.9747 | 0 | 37.9667 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.667 | 34.667 | 75.5539 | 1 | PROCESSED | 57551.5224074074 | 2016-06-12 12:32:16 | 55769 | 2011-07-27 00:00:00 | 55403.0749768518 | 2010-07-26 01:47:58 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050003 | We propose to observe two Swift/BAT selected obscured AGNs with significant scattered emission, Mrk 18 and Ark 347. Hard X-ray selected AGNs show some peculiar characteristics compared to optically selected ones such as weak scattering emission from the opening part of the putative torus and weak plasma emission in the soft X-ray band. The targets are Swift/BAT selected AND show significant scattered emission, which are poorly explored with Suzaku so far. Our aims are to constrain the geometrical structure of the obscuring matter based on broad-band X-ray spectra and compare them with other hard X-ray or optically selected obscured AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YUICHI TERASHIMA | JAP | 5 | AO5 | THE STRUCTURE OF COMPTON-THIN AGNS WITH SIGNIFICANT SCATTERED EMISSION SELECTED BY SWIFT/BAT | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705001010/ | Quick Look | ![]() |
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305 | NGC3227 | 155.8772 | 19.8684 | 155.194638 | 20.121777 | 150.38806 | 9.142968 | 216.98573476 | 55.44624837 | 110.6974 | 54797.8953703704 | 2008-11-27 21:29:20 | 54799.750162037 | 2008-11-29 18:00:14 | 703022050 | 79.4298 | 50 | 79.4298 | 79.4339 | 0 | 79.4378 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.8439 | 39.8439 | 160.2418 | 1 | PROCESSED | 57544.6203819444 | 2016-06-05 14:53:21 | 54557 | 2008-04-01 00:00:00 | 54809.8059490741 | 2008-12-09 19:20:34 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031013 | We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARTIN ELVIS | USA | 3 | AO3 | NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703022050/ | Quick Look | ![]() |
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306 | CENTAURUS_A | 201.3411 | -43.072 | 200.607667 | -42.811983 | 217.145584 | -31.383496 | 309.48969514 | 19.36734145 | 290.0008 | 55032.3718634259 | 2009-07-20 08:55:29 | 55033.7683333333 | 2009-07-21 18:26:24 | 704018010 | 62.4328 | 50 | 62.4328 | 62.6888 | 0 | 62.7076 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 55.45 | 55.45 | 120.6499 | 3 | PROCESSED | 57547.9397569444 | 2016-06-08 22:33:15 | 55415 | 2010-08-07 00:00:00 | 55048.3403356482 | 2009-08-05 08:10:05 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040085 | We propose to observe a nearby radio galaxy Centaurus A (Cen A) in order to search for non-thermal X-ray emission associated with a mis-alighned jet. Recently TeV gamma-ray was detected from M87 and nonthermal X-ray emission was detected from 3C120 with Suzaku, where they are not a blazar and harbor a mis-alighned jet. COMPTEL and EGRET reported a hint of gamma-ray emission from Cen A, but it has not been established. So far, only Seyfert-like thermal-Compoton powerlaw has been detected from Cen A. By taking advantage of Suzaku capability, we study a temporal spectral variation to extract nonthermal emission by considering a different variability time scale of accretion disk component and jet one, as demonstrated for 3C120 with Suzaku. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YASUSHI FUKAZAWA | JAP | 4 | AO4 | SEARCH FOR NON-THERMAL X-RAY EMISSION FROM A NEARBY RADIO GALAXY CENTAURUS A | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704018010/ | Quick Look | ![]() |
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307 | MKN 279 | 208.2253 | 69.3021 | 207.933654 | 69.547649 | 144.919228 | 67.626916 | 115.05735618 | 46.87522986 | 345.4595 | 54965.2632407407 | 2009-05-14 06:19:04 | 54968.6668287037 | 2009-05-17 16:00:14 | 704031010 | 160.3514 | 150 | 160.3594 | 160.3514 | 0 | 160.3594 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 150.386 | 150.386 | 293.9979 | 3 | PROCESSED | 57546.636099537 | 2016-06-07 15:15:59 | 55345 | 2010-05-29 00:00:00 | 54978.3987152778 | 2009-05-27 09:34:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041403 | We aim to test if the high-luminosity Seyfert 1.5 Mkn 279 contains an ionized inner accretion disk by using Suzaku to spectroscopically separate the ionized and neutral reflectors. This source is relatively unobscured, allowing clear modeling of the shape of the strong soft excess; we will also test for a Fe K diskline component, which may be missing if the disk is ionized or truncated. Only a broadband X-ray spectrum, including simultaneous > 10 keV coverage to constrain Compton reflection, will allow us to thoroughly test blurred, ionized disk reflection models and constrain the nature of the reflector(s). | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ALEX MARKOWITZ | USA | 4 | AO4 | DOES THE LOW-OBSCURATION, LOW-REFLECTION, HIGH-LUMINOSITY SEYFERT MKN279 CONTAIN AN IONIZED OR TRUNCATED ACCRETION DISK? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704031010/ | Quick Look | ![]() |
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308 | NGC1194 | 45.9522 | -1.1044 | 45.31576 | -1.299082 | 43.150403 | -17.672733 | 179.17914291 | -48.96176874 | 76.9913 | 55044.6911689815 | 2009-08-01 16:35:17 | 55045.8141087963 | 2009-08-02 19:32:19 | 704046010 | 50.3161 | 50 | 50.3161 | 50.5961 | 0 | 50.5961 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.4268 | 48.4268 | 97.0038 | 1 | PROCESSED | 57548.0499074074 | 2016-06-09 01:11:52 | 55427 | 2010-08-19 00:00:00 | 55061.5275115741 | 2009-08-18 12:39:37 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041414 | We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | EZEQUIEL TREISTER | USA | 4 | AO4 | THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704046010/ | Quick Look | ![]() |
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309 | IC 2497 | 145.222 | 34.6799 | 144.47003 | 34.907483 | 135.80747 | 19.598067 | 190.267728 | 48.8163504 | 306.2341 | 54939.6906365741 | 2009-04-18 16:34:31 | 54941.5550810185 | 2009-04-20 13:19:19 | 704053010 | 76.4837 | 75 | 76.4837 | 76.4837 | 0 | 76.4837 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 63.948 | 63.948 | 161.0478 | 2 | PROCESSED | 57546.2140046296 | 2016-06-07 05:08:10 | 55318 | 2010-05-02 00:00:00 | 54952.1320717593 | 2009-05-01 03:10:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041432 | The discovery of `Hanny's Voorwerp' near IC 2497 opens an unprecedented window into the time evolution of a single AGN on timescales up to 100,000 years. Based on its properties, the Voorwerp was illuminated by a luminous AGN ~100,000 years ago, but the AGN host galaxy - IC 2497 - does not seem to host a sufficiently luminous AGN. Thus, IC 2497 either hosts a highly obscured AGN only detectable in hard X-rays, or it has dropped in luminosity by a factor of 10-1000. We propose to observe IC 2497 with Suzaku for 75 ksec to determine the hard X-ray luminosity and spectrum to measure the amount of obscuration and the current intrinsic luminosity of its AGN. Only with hard X-ray observations can we break the degeneracy between obscuration and decrease in luminosity. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KEVIN SCHAWINSKI | USA | 4 | AO4 | HOW FAST CAN AN AGN SHUT DOWN? - SUZAKU OBSERVATION OF IC 2497 AND `HANNY'S VOORWERP' | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704053010/ | Quick Look | ![]() |
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310 | IC 342 X2 | 56.516 | 68.1498 | 55.302778 | 67.99381 | 72.573568 | 46.727351 | 138.08335694 | 10.57829767 | 91.9969 | 55415.9786689815 | 2010-08-07 23:29:17 | 55417.3765625 | 2010-08-09 09:02:15 | 705009010 | 74.379 | 80 | 74.379 | 74.379 | 0 | 74.379 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64.1316 | 64.1316 | 120.7679 | 0 | PROCESSED | 57552.9205671296 | 2016-06-13 22:05:37 | 55794 | 2011-08-21 00:00:00 | 55428.1624537037 | 2010-08-20 03:53:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050041 | The nature of ultraluminous X-ray sources (ULXs) is one of the important unresolved issues in the modern astrophysics. A Suzaku HXD spectrum above 10 keV and its variation, in combination with those with XIS, provide us with an unique opportunity to determine unambiguously the physical state of ULXs, which is a key information to solve their nature. Here, two 80 ks Suzaku exposures are proposed on a bright ULX IC 342 X2, one of the most promising candidates for hard X-ray detection. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NAOKI ISOBE | JAP | 5 | AO5 | HARD X-RAY STUDY OF ULTRALUMINOUS X-RAY SOURCES WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705009010/ | Quick Look | ![]() |
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311 | LEDA 84274 | 220.5853 | 66.0952 | 220.354238 | 66.306919 | 158.410677 | 70.66779 | 106.75984756 | 47.40039166 | 359.2838 | 55331.3858333333 | 2010-05-15 09:15:36 | 55332.0542824074 | 2010-05-16 01:18:10 | 705023010 | 49.465 | 50 | 49.465 | 49.465 | 0 | 49.465 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.8385 | 40.8385 | 57.7519 | 1 | PROCESSED | 57551.5334143518 | 2016-06-12 12:48:07 | 55769 | 2011-07-27 00:00:00 | 55403.1228125 | 2010-07-26 02:56:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050074 | We propose Suzaku XIS and HXD/PIN observations of two buried Active Galactic Nuclei(AGNs) at z=0.04 which are discovered by the AKARI mid-infrared all-sky survey. Both objects only show AGN features in AKARI near- and mid-infrared obsevations, while there are no clues of AGN presence in previous X-ray survey of ROSAT, radio 20cm, near-infrared photometries of 2MASS and detail optical spectroscopic data. These results indicate that a central engine of the AGN is completely buried and the nature of this population of AGNs is only poorly understood. Therefore, the hard X-ray observations is needed in order to confirm the AGN presence as well as to estimate the amount of absorption component and the AGN energy. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | SHINKI OYABU | JAP | 5 | AO5 | SUZAKU SEARCH FOR DIRECT EVIDENCE OF SUPER MASSIVE BLACK HOLES IN BURIED ACTIVE GALACTIC NUCLEI DISCOVERED BY AKARI | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705023010/ | Quick Look | ![]() |
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312 | CEN A S LOBE NO. 1 | 200.8664 | -45.1602 | 200.128121 | -44.89936 | 217.870253 | -33.408756 | 308.83796576 | 17.34395301 | 288.0039 | 55418.6612962963 | 2010-08-10 15:52:16 | 55419.7758101852 | 2010-08-11 18:37:10 | 705032010 | 75.1654 | 80 | 75.1654 | 75.1654 | 0 | 75.1654 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64.2728 | 64.2728 | 96.2818 | 0 | PROCESSED | 57552.9742476852 | 2016-06-13 23:22:55 | 55803 | 2011-08-30 00:00:00 | 55428.1537152778 | 2010-08-20 03:41:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051401 | We propose a set of four pointings (200 ks), to study the X-ray emission from the Southern giant lobe of the radio galaxy Cen A. Those lobes clearly separated from the central source, have been detected as a source of diffuse gamma-ray emission by the Fermi Telescope. The goal of the Suzaku observations is two-fold: first, to measure the diffuse component of the non-thermal X-ray emission with both the XIS and the HXD in order to determine the details of the distribution of the radiating relativistic particles (and B field), and second, to measure the thermal emission from the lobes (using primarily the XIS), to determine temperature and density of the X-ray emitting plasma, which, via consideration of pressure balance, will determine the content of energetic protons (cosmic rays). | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GRZEGORZ MADEJSKI | USA | 5 | AO5 | SUZAKU OBSERVATIONS OF THE SOUTHERN LOBE OF CEN A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705032010/ | Quick Look | ![]() |
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313 | CEN A S LOBE NO. 3 | 205.7514 | -45.1409 | 204.991343 | -44.889287 | 221.546575 | -31.897052 | 312.39292182 | 16.78143613 | 279.0007 | 55420.9668981482 | 2010-08-12 23:12:20 | 55421.3452777778 | 2010-08-13 08:17:12 | 705034010 | 20.0575 | 20 | 20.0815 | 20.0735 | 0 | 20.0575 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 18.9436 | 18.9436 | 32.6879 | 1 | PROCESSED | 57552.9389467593 | 2016-06-13 22:32:05 | 55803 | 2011-08-30 00:00:00 | 55435.169537037 | 2010-08-27 04:04:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051401 | We propose a set of four pointings (200 ks), to study the X-ray emission from the Southern giant lobe of the radio galaxy Cen A. Those lobes clearly separated from the central source, have been detected as a source of diffuse gamma-ray emission by the Fermi Telescope. The goal of the Suzaku observations is two-fold: first, to measure the diffuse component of the non-thermal X-ray emission with both the XIS and the HXD in order to determine the details of the distribution of the radiating relativistic particles (and B field), and second, to measure the thermal emission from the lobes (using primarily the XIS), to determine temperature and density of the X-ray emitting plasma, which, via consideration of pressure balance, will determine the content of energetic protons (cosmic rays). | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GRZEGORZ MADEJSKI | USA | 5 | AO5 | SUZAKU OBSERVATIONS OF THE SOUTHERN LOBE OF CEN A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705034010/ | Quick Look | ![]() |
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314 | IGR J19378-0617 | 294.4023 | -6.2869 | 293.733278 | -6.400449 | 295.156006 | 15.047751 | 32.53385066 | -13.11752642 | 260.9167 | 55485.0705324074 | 2010-10-16 01:41:34 | 55487.3016087963 | 2010-10-18 07:14:19 | 705055010 | 77.8014 | 80 | 77.8174 | 77.8014 | 0 | 77.8174 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.5712 | 70.5712 | 192.7439 | 1 | PROCESSED | 57553.8036226852 | 2016-06-14 19:17:13 | 55867 | 2011-11-02 00:00:00 | 55498.2386805556 | 2010-10-29 05:43:42 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052014 | We propose to observe with Suzaku three Narrow Line Seyfert 1 galaxies detected by INTEGRAL/IBIS and/or Swift/BAT with a flux in excess of 1.5e-11 cgs in the 15-50keV band (corresponding to the HXD/PIN band). The proposed observations will provide rare high quality spectra of NLS1s in the 0.5-50keV band. The good quality data above 10keV will dramatically help us removing the spectral degeneracies inherent to limited bandpass analysis (such as that with XMM-Newton and Chandra) and the ambiguities between the different proposed models invoked to explain the unique spectral and variability properties of these most extreme class of high accretion rate sources. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GIOVANNI MINIUTTI | EUR | 5 | AO5 | BROADBAND X-RAY PROPERTIES OF HARD-X-RAY-BRIGHT NLS1 GALAXIES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705055010/ | Quick Look | ![]() |
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315 | SMC X-1 | 19.2337 | -73.4445 | 18.901627 | -73.707724 | 312.330059 | -66.462167 | 300.42986971 | -43.55966827 | 9.1005 | 55673.6490625 | 2011-04-22 15:34:39 | 55674.1112037037 | 2011-04-23 02:40:08 | 706030030 | 15.6526 | 18 | 15.6526 | 15.6526 | 0 | 15.871 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 21.2614 | 21.2614 | 39.9199 | 1 | PROCESSED | 57601.5606597222 | 2016-08-01 13:27:21 | 56067 | 2012-05-20 00:00:00 | 55692.2968634259 | 2011-05-11 07:07:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JOSEPH NEILSEN | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030030/ | Quick Look | ![]() |
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316 | 1ES 1927+654 | 291.8157 | 65.5862 | 291.743016 | 65.482913 | 3.782751 | 81.150517 | 97.0030083 | 20.97400385 | 83.4311 | 55667.8280092593 | 2011-04-16 19:52:20 | 55669.2425115741 | 2011-04-18 05:49:13 | 706006010 | 71.8889 | 100 | 71.9129 | 71.8889 | 0 | 71.9129 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79.6647 | 79.6647 | 122.1919 | 0 | PROCESSED | 57601.5407986111 | 2016-08-01 12:58:45 | 56059 | 2012-05-12 00:00:00 | 55691.2683912037 | 2011-05-10 06:26:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060008 | 1ES 1927+654, an X-ray unabsorbed optically classified type-2 AGN, challenges the standard unified model. What is known about its X-ray characteristics suggest it can provide tremendous insight. It is extremely bright and will render close to 20 ct/s in the combined XIS providing sufficient data to unambiguously detect features in the Fe~K region, distinguish absorption and reflection models, and study its rapid variability. Even in the most conservative estimates a PIN detection is expected. It is persistently variable on short time scales and in combination with the long duration of Suzaku observations, the proposed observationswill yield fruitful variability studies. It has never been observed by Suzaku thus guaranteeing significant opportunity for discovery. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | LUIGI GALLO | JAP | 6 | AO6 | REVEALING THE NATURE OF AN X-RAY ABSORBED SEYFERT 2 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706006010/ | Quick Look | ![]() |
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317 | PG 1626+554 | 247.0224 | 55.3701 | 246.753118 | 55.479335 | 214.524979 | 74.372261 | 84.50112094 | 42.16849703 | 200.5289 | 55876.6090046296 | 2011-11-11 14:36:58 | 55877.9341550926 | 2011-11-12 22:25:11 | 706017010 | 60.8488 | 60 | 60.8488 | 60.8488 | 0 | 60.8488 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 56.1328 | 56.1328 | 114.4639 | 2 | PROCESSED | 57603.7696412037 | 2016-08-03 18:28:17 | 56256 | 2012-11-25 00:00:00 | 55890.6981828704 | 2011-11-25 16:45:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060069 | Measurement of iron abundance in active galactic nuclei (AGN) relative to that of alpha-elements possesses potential of elucidating the cosmic chemical evolution, in particular, when the formation of the first stars initiated. However, it has been found that iron abundances estimated from FeII(opt) and FeII(UV) in the broad line region (BLR) do not agree and their ratio is dependent on the BLR cloud column densities. Thus, in order to derive precise AGN iron abundances, independent measurement of the BLR cloud column densities is required. Here we propose to obtain precise X-ray energy spectra of several AGNs, of which FeII(opt)/FeII(UV) values we have already measured. By combining the optical and X-ray spectra, we can estimate iron abundances of these targets more precisely than ever. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | HIROAKI SAMESHIMA | JAP | 6 | AO6 | X-RAY MEASUREMENTS OF COLUMN DENSITIES OF THE BROAD LINE REGION CLOUDS TO CONSTRAIN THE COSMIC CHEMICAL EVOLUTION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706017010/ | Quick Look | ![]() |
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318 | MRK 841 | 226.0091 | 10.4587 | 225.405512 | 10.653095 | 220.178836 | 26.612533 | 11.24319757 | 54.63999984 | 112.9994 | 55931.8646180556 | 2012-01-05 20:45:03 | 55937.1896990741 | 2012-01-11 04:33:10 | 706029010 | 244.3518 | 350 | 244.3518 | 244.3518 | 0 | 244.3598 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 229.726 | 229.726 | 419.686 | 4 | PROCESSED | 57604.4310648148 | 2016-08-04 10:20:44 | 55652 | 2011-04-01 00:00:00 | 55946.5082407407 | 2012-01-20 12:11:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061119 | 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-LP | A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706029010/ | Quick Look | ![]() |
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319 | NGC 2110 | 88.0457 | -7.4586 | 87.441571 | -7.469572 | 87.744639 | -30.884812 | 212.92775975 | -16.54787795 | 79.201 | 56170.1053009259 | 2012-08-31 02:31:38 | 56172.5412268518 | 2012-09-02 12:59:22 | 707034010 | 103.2595 | 100 | 103.2595 | 103.2595 | 0 | 103.2595 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102.8063 | 102.8063 | 210.4361 | 1 | PROCESSED | 57607.0102199074 | 2016-08-07 00:14:43 | 56667 | 2014-01-10 00:00:00 | 56301.6411458333 | 2013-01-09 15:23:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071426 | We request two 100 ks | EXTRAGALACTIC COMPACT SOURCES | 7 | B | ELIZABETH RIVERS | USA | 7 | AO7 | TRACKING THE PARTIAL COVERING ABSORBERS IN NGC 2110: CONSTRAINTS FOR CLUMPY ABSORBER MODELS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707034010/ | Quick Look | ![]() |
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320 | MRK 478 | 220.4959 | 35.3708 | 219.98335 | 35.583266 | 202.392109 | 47.875746 | 59.0913373 | 65.0766343 | 294.6097 | 55756.9652777778 | 2011-07-14 23:10:00 | 55758.8334837963 | 2011-07-16 20:00:13 | 706041010 | 85.3236 | 80 | 85.3316 | 85.3396 | 0 | 85.3236 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 77.6366 | 77.6366 | 161.3897 | 1 | PROCESSED | 57602.6370601852 | 2016-08-02 15:17:22 | 56151 | 2012-08-12 00:00:00 | 55783.7198842593 | 2011-08-10 17:16:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062028 | The NLS1 galaxy Mrk 478 has exceptionally unusual properties. It shows up to a factor of five variability while keeping its spectral shape constant. Previous short XMM-Newton observations show that it is probably reflection-dominated, where light-bending effects are at their extreme. This is the only known object that shows such high variability while remaining in a reflection-dominated state. All other known objects show reflection-dominated spectra only when in a faint state, making their study very difficult. This object is reflection-dominated yet bright enough to study with relatively short exposures.Here we propose to observe this object for 80 ks. The goal is to detect the reflection hump using Suzaku capabilities above 10 keV and probe light-bending around this black hole. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ABDERAHMEN ZOGHBI | EUR | 6 | AO6 | PROBING EXTREME RELATIVISITC LIGHT-BENDING IN MRK 478 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706041010/ | Quick Look | ![]() |
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321 | 1730-130 | 263.2641 | -13.0933 | 262.559168 | -13.058946 | 263.324851 | 10.191548 | 12.02258907 | 10.80244107 | 271.1606 | 55829.6599537037 | 2011-09-25 15:50:20 | 55830.0946643518 | 2011-09-26 02:16:19 | 706046010 | 11.0858 | 10 | 11.0938 | 11.0938 | 0 | 11.0858 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.8811 | 9.8811 | 37.5359 | 1 | PROCESSED | 57603.2457407407 | 2016-08-03 05:53:52 | 56225 | 2012-10-25 00:00:00 | 55875.6203703704 | 2011-11-10 14:53:20 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061601 | We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | SVETLANA JORSTAD | USA | 6 | AO6 | EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706046010/ | Quick Look | ![]() |
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322 | ESO 565-G019 | 143.6802 | -21.9346 | 143.106087 | -21.711094 | 154.563677 | -34.141633 | 253.87283017 | 21.67453181 | 298.0016 | 56067.8709259259 | 2012-05-20 20:54:08 | 56069.9022222222 | 2012-05-22 21:39:12 | 707013010 | 78.9239 | 80 | 78.9239 | 78.9319 | 0 | 78.9319 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71.1211 | 71.1211 | 175.4878 | 2 | PROCESSED | 57605.5328935185 | 2016-08-05 12:47:22 | 56448 | 2013-06-05 00:00:00 | 56079.3396643518 | 2012-06-01 08:09:07 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070067 | The nature of the hard X-ray emission of many AGN remains ill-understood. Using the latest 70 month Swift/BAT sky survey, we have selected optically-classified Seyfert 2s with a very hard BAT photon index (Gamma<1.4). The BAT energy range is not strongly affected by obscuration unless the column is Compton-thick. The selected sources are radio-quiet, arguing against jet-dominated non-thermal spectra. The cause of a low Gamma is unknown, but may include high or atypical obscuration, non-thermal X-ray emission without associated radio/optical jets or the presence of electron coronae with temperatures or optical depths higher than average. Our aim is to observe two of the hardest Seyfert 2s (neither of which has prior pointed observations below 10 keV) with Suzaku to elucidate their nature. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | POSHAK GANDHI | JAP | 7 | AO7 | WHAT IS THE NATURE OF SWIFT/BAT HARD-SPECTRUM SEYFERT 2S? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707013010/ | Quick Look | ![]() |
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323 | ESO 511-G030 | 214.8452 | -26.646 | 214.125789 | -26.416487 | 221.403618 | -12.022581 | 326.22952078 | 32.2164843 | 286.9689 | 56130.0282407407 | 2012-07-22 00:40:40 | 56136.3340856482 | 2012-07-28 08:01:05 | 707023020 | 224.0255 | 270 | 224.0255 | 224.0255 | 0 | 224.0335 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 195.6334 | 195.6334 | 410.8958 | 3 | PROCESSED | 57606.8434606482 | 2016-08-06 20:14:35 | 56646 | 2013-12-20 00:00:00 | 56279.0046064815 | 2012-12-18 00:06:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071413 | The study of "bare" Seyfert 1 AGN is essential to measure the true properties of the inner regions of the accretion disk. The nearby Seyfert ESO 511-G30 is a prime candidate for fulfilling this role due to its broad Fe K component and lack of any intrinsic warm absorption. It is also one of the X-ray brightest bare Seyferts featured in the Swift 58 month BAT catalogue as yet unobserved with Suzaku. We propose a 270 ks Suzaku observation of ESO 511-G30 to unambiguously constrain the properties of the accretion disk and subsequently the black hole spin. In addition, the HXD data will allow us to measure the Compton reflection hump, while the excellent soft X-ray spectral resolution of XIS will allow the origin of the soft excess to be determined. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JAMES REEVES | USA | 7 | AO7 | MEASURING THE ACCRETION DISK AND BLACK HOLE PROPERTIES OF ESO 511-G30 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707023020/ | Quick Look | ![]() |
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324 | SNR 1987A | 83.833 | -69.2775 | 83.924877 | -69.307216 | 307.543742 | -86.433259 | 279.71430694 | -31.94790633 | 135.9732 | 56233.5143981482 | 2012-11-02 12:20:44 | 56234.854375 | 2012-11-03 20:30:18 | 707020010 | 81.2764 | 80 | 81.2764 | 81.2844 | 0 | 81.2924 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 78.5842 | 78.5842 | 115.7599 | 0 | PROCESSED | 57607.9555439815 | 2016-08-07 22:55:59 | 56611 | 2013-11-15 00:00:00 | 56245.4956365741 | 2012-11-14 11:53:43 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071331 | Despite extensive observations of supernova remnant (SNR) 1987A with Chandra and XMM-Newton, the origin of the hard band (3-10 keV) X-ray emission is elusive (thermal vs nonthermal). A straightforward way to discriminate the thermal and nonthermal origins of the hard X-rays is to detect Fe K lines. The Suzaku XIS provides a uniquely efficient opportunity for a sensitive search for the Fe K lines, which is an excellent complement to the existing Chandra and XMM-Newton studies of SNR 1987A. Thus, we propose an 80 ks Suzaku observation of SNR 1987A. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | SANGWOOK PARK | USA | 7 | AO7 | X-RAY EMISSION FROM SUPERNOVA REMNANT 1987A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707020010/ | Quick Look | ![]() |
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325 | RE J1034+396 | 158.663 | 39.6488 | 157.936699 | 39.907419 | 144.538164 | 28.290615 | 180.26295059 | 59.06449262 | 115.7032 | 56245.9648726852 | 2012-11-14 23:09:25 | 56248.0689583333 | 2012-11-17 01:39:18 | 707039010 | 99.9113 | 100 | 99.9193 | 99.9113 | 0 | 99.9193 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93.446 | 93.446 | 181.7639 | 3 | PROCESSED | 57608.0485416667 | 2016-08-08 01:09:54 | 56640 | 2013-12-14 00:00:00 | 56274.6249884259 | 2012-12-13 14:59:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072005 | Understanding the nature of the emission from the extreme active galaxy, RE J1034+396 can help us to unravel the properties of accretion as the Eddington limit is reached. A fleeting glimpse of the unique quasi-periodic oscillation (QPO) in this source has shown a complex timing behaviour with the emission below ~2 keV apparently crucial to its presence. Thus by understanding the origin and properties of the soft emission we can probe the physical mechanism of signals that cannot be resolved in stellar mass X-ray binaries but must be associated with the regions closest to the black hole. A new observation with Suzaku will allow a much deeper analysis of the soft emission and will shed light on how its changing properties can trigger such unique behaviour as the QPO. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | MATTHEW MIDDLETON | EUR | 7 | AO7 | REVEALING THE NATURE OF RE J1034+396 AND THE EXTREME SOFT EXCESS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707039010/ | Quick Look | ![]() |
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326 | CTA102 | 338.1458 | 11.7401 | 337.526658 | 11.482274 | 344.409824 | 19.371456 | 77.43997335 | -38.57166798 | 72.4263 | 56431.345462963 | 2013-05-19 08:17:28 | 56431.6134606482 | 2013-05-19 14:43:23 | 707045010 | 9.5626 | 10 | 9.5706 | 9.5626 | 0 | 9.5706 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.283 | 7.283 | 23.1439 | 0 | PROCESSED | 57611.3187847222 | 2016-08-11 07:39:03 | 56809 | 2014-06-01 00:00:00 | 56443.5010069444 | 2013-05-31 12:01:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071601 | We propose to perform two 2-week multi-frequency campaigns of observations of a sample of gamma-ray blazars during Fermi Cycle 5. The campaigns will involve: (1) gamma-ray monitoring with the Fermi LAT, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B, V, R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku and Swift; (6) mid-IR measurements with IRTF; and (7) near-IR photometric J, H, and K observations. The research aims i) to search for correlated variability on short timescales; ii) to compile SEDs at different states of gamma-ray and radio jet activitiy; and iii) to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | SVETLANA JORSTAD | USA | 7 | AO7 | MULTI-FREQUENCY CAMPAIGNS TO STUDY RAPID VARIABILITY IN GAMMA_RAY BLAZARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707045010/ | Quick Look | ![]() |
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327 | ESO 119-G008 | 72.2547 | -57.6544 | 72.033322 | -57.73981 | 38.878903 | -77.915205 | 266.66680471 | -38.87724734 | 324.43 | 56411.0111458333 | 2013-04-29 00:16:03 | 56413.2355787037 | 2013-05-01 05:39:14 | 708004010 | 100.5873 | 100 | 100.5953 | 100.5953 | 0 | 100.5873 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 103.7614 | 103.7614 | 192.1719 | 3 | PROCESSED | 57611.2384375 | 2016-08-11 05:43:21 | 56837 | 2014-06-29 00:00:00 | 56475.7648611111 | 2013-07-02 18:21:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080027 | At faint fluxes, the Swift/BAT AGN survey is uncovering sources with very hard photon indices (Gamma) above 10 keV. The origin of a low Gamma in the hard band is ill-understood, but may include high/atypical obscuration, non-thermal X-rays without radio jets, or electron coronae with high temperatures or optical depths. In AO7, we observed two such Seyfert 2s and discovered Compton-thick obscuration in one source, and a buried AGN spectrum with no reflection or high-energy cutoff in the other. The hard BAT Gamma values thus have a variety of origins, and our strategy is very effective in selecting objects with interesting spectra. Here, we propose to observe two hardest sources (Gamma<~1) with no prior X-ray observations below 10 keV in order to shed light on the nature of this population. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | POSHAK GANDHI | JAP | 8 | AO8 | THE VARIED NATURE OF SWIFT/BAT HARD-SPECTRUM SEYFERT 2S | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708004010/ | Quick Look | ![]() |
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328 | NGC 3516 | 166.7239 | 72.5839 | 165.871383 | 72.854298 | 123.356587 | 58.000243 | 133.21571384 | 42.39397937 | 129.7498 | 56600.2605671296 | 2013-11-04 06:15:13 | 56601.215474537 | 2013-11-05 05:10:17 | 708006060 | 46.2 | 50 | 46.2 | 46.2 | 0 | 46.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.1764 | 45.1764 | 82.502 | 1 | PROCESSED | 57613.2009722222 | 2016-08-13 04:49:24 | 56383 | 2013-04-01 00:00:00 | 56646.7076041667 | 2013-12-20 16:58:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080066 | We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 8 | AO8 | THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006060/ | Quick Look | ![]() |
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329 | LEDA 168563 | 73.0158 | 49.5506 | 72.064208 | 49.467096 | 77.740518 | 26.831198 | 157.24701812 | 3.42018054 | 86.3166 | 56536.8773611111 | 2013-09-01 21:03:24 | 56539.0592708333 | 2013-09-04 01:25:21 | 708017010 | 100.011 | 100 | 100.035 | 100.011 | 0 | 100.035 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 92.947 | 92.947 | 188.5018 | 1 | PROCESSED | 57612.530162037 | 2016-08-12 12:43:26 | 56383 | 2013-04-01 00:00:00 | 56608.7327893518 | 2013-11-12 17:35:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081413 | We propose to carry out Suzaku observations, a 100 ks each, of three Seyfert I nuclei hard X-ray selected by Swift. Our goal is to distinguish between various competing models proposed for the X-ray spectra of Seyfert I nuclei. Especially we will test, by observing these targets, the ionized relativistic reflection (hereafter IRR). We will take advantage of Suzaku s unique capability of detecting hard X-rays beyond 10 keV by its HXD-PIN, simultaneously with X-rays in lower to medium energy bands by its XIS on board. With our proposed studies we will gain deeper understanding of accretion-powered AGN in general. Since the IRR takes place close to the black hole we will test the effects of strong gravity, such as the black hole spin. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | SACHIKO TSURUTA | USA | 8 | AO8 | SPECTRAL STUDIES OF SOME HARD X-RAY SELECTED SEYFERT NUCLEI | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708017010/ | Quick Look | ![]() |
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330 | IGR J09026-4812 | 135.6468 | -48.2323 | 135.224236 | -48.033912 | 164.675258 | -60.400706 | 268.86967218 | -1.09239209 | 115.8572 | 56622.3203356482 | 2013-11-26 07:41:17 | 56622.9521990741 | 2013-11-26 22:51:10 | 708031010 | 37.7924 | 35 | 37.8244 | 37.8164 | 0 | 37.7924 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.2029 | 35.2029 | 54.5859 | 1 | PROCESSED | 57613.429212963 | 2016-08-13 10:18:04 | 56383 | 2013-04-01 00:00:00 | 56632.5852777778 | 2013-12-06 14:02:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081419 | The BAT AGN sample constitutes an unprecedented all-sky hard X-ray survey of the local AGN population. However, to properly model the X-ray absorption & reflection, coverage below 10 keV is needed with CCD spectral resolution and adequate signal-to-noise. We propose to observe 11 AGN with Suzaku, which will increase the completeness of a flux-limited sample with such coverage from 85 to 158 sources. The 11 AGN only have severely underexposed Swift XRT coverage below 10 keV whereas the remaining sources have either Suzaku or XMM coverage. The Suzaku data have the additional advantage of sensitivity above 10 keV that helps to mitigate the long time-baseline of the BAT spectra. The new observations will create a significantly enhanced legacy data set that will provide value for years to come. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TAHIR YAQOOB | USA | 8 | AO8 | ROBUST CHARACTERIZATION OF ABSORPTION AND REFLECTION IN A LOCAL FLUX-LIMITED AGN POPULATION FROM THE SWIFT BAT SURVEY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708031010/ | Quick Look | ![]() |
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331 | ABELL 981 | 156.0884 | 68.0988 | 155.16023 | 68.352315 | 123.8863 | 52.287736 | 140.87577234 | 43.55064218 | 119.4308 | 56601.2179398148 | 2013-11-05 05:13:50 | 56601.7917708333 | 2013-11-05 19:00:09 | 708040010 | 27.5945 | 30 | 27.6025 | 27.5945 | 0 | 27.5945 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.286 | 25.286 | 49.574 | 1 | PROCESSED | 57613.2182060185 | 2016-08-13 05:14:13 | 56980 | 2014-11-19 00:00:00 | 56614.6564583333 | 2013-11-18 15:45:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081533 | We propose to map out the core of the A981 supercluster with three Suzaku observations. The A981 supercluster contains four Abell richness class 2 clusters within a redshift range of 2,000 km/s. All four clusters also overlap within their virial radii, at least in projection. The low and steady background of the Suzaku telescope is ideal for studying the low surface brightness X-ray emission between the clusters. Such observations will determine if the clusters are interacting via the detection of merger-induced shocks or perturbed features in the outskirts of the individual clusters. Our proposed Suzaku observations will help elucidate the fundamental astrophysics that occurs during the formation of very massive clusters. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | LAURENCE DAVID | USA | 8 | AO8 | MAPPING THE ABELL 981 SUPER CLUSTER WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708040010/ | Quick Look | ![]() |
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332 | PG 1404+226 | 211.5907 | 22.3868 | 211.009924 | 22.624644 | 200.393386 | 32.82418 | 21.44706338 | 72.36251102 | 287.2346 | 56486.8565972222 | 2013-07-13 20:33:30 | 56489.1889583333 | 2013-07-16 04:32:06 | 708045010 | 102.3327 | 100 | 102.3704 | 102.3327 | 0 | 102.3625 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95.3407 | 95.3407 | 201.5059 | 2 | PROCESSED | 57612.0131828704 | 2016-08-12 00:18:59 | 56872 | 2014-08-03 00:00:00 | 56503.7358796296 | 2013-07-30 17:39:40 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082010 | Suzaku observations reveal evidence of relativistically-broadened emission lines from the inner regions of supermassive black holes, providing a unique tool for studying accreting systems. It is understood that the X-ray source is compact at low-fluxes, and increases in size at higher fluxes. Thus variable sources are essential for probing the physics of the innermost regions. Previous studies of the low-flux 'state' have been limited by low count rates. We propose to observe PG 1404+226, which shares many properties of other AGN showing reverberation, but even at low-fluxes, it is a factor of three brighter than similar objects. This source, never before observed with Suzaku, provides a unique opportunity for probing strong-field accretion because of its high luminosity and variability. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | ERIN KARA | EUR | 8 | AO8 | MAPPING THE X-RAY EMISSION IN THE VICINITY OF THE BLACK HOLE PG 1404+226 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708045010/ | Quick Look | ![]() |
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333 | FAIRALL 51 | 281.2261 | -62.3592 | 280.062181 | -62.410627 | 276.679536 | -39.178599 | 333.20510197 | -23.08989761 | 251.799 | 56540.8073958333 | 2013-09-05 19:22:39 | 56541.1744212963 | 2013-09-06 04:11:10 | 708046020 | 30.958 | 30 | 30.958 | 30.958 | 0 | 30.9646 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 23.2171 | 23.2171 | 31.7039 | 0 | PROCESSED | 57612.5333333333 | 2016-08-12 12:48:00 | 56956 | 2014-10-26 00:00:00 | 56588.7741319444 | 2013-10-23 18:34:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082016 | Fairall 51 is a variable bright active galaxy (about 1 millicrab), classified as a polar-scattered Seyfert~1 galaxy. It was observed twice with high-quality X-ray spectrometers on-board the XMM-Newton satellite. The two observations are separated by half a year and the spectra significantly differ from each other. The difference can be well explained by a variable covering fraction of a cold (very low-ionised) absorber (Ricci et al., 2010). Two additional Swift data, separated by five days, suggest that the variability may occur at time-scales as short as a few days. The ultimate goal of the proposal is to locate this variable absorber by the determination of the typical time-scale of the variability. We therefore propose a series of observations of Fairall 51 with short exposures. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JIRI SVOBODA | EUR | 8 | AO8 | STUDY OF THE VARIABLE ABSORBER IN A BRIGHT ACTIVE GALAXY FAIRALL 51 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708046020/ | Quick Look | ![]() |
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334 | NGC 3998 | 179.4698 | 55.4443 | 178.823114 | 55.722594 | 149.626555 | 48.892783 | 138.19460038 | 60.06850959 | 319.2188 | 56780.8797569445 | 2014-05-03 21:06:51 | 56782.5966898148 | 2014-05-05 14:19:14 | 709002010 | 80.6754 | 80 | 80.6754 | 80.6754 | 0 | 80.6754 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 76.8901 | 76.8901 | 148.2858 | 0 | PROCESSED | 57615.0693981482 | 2016-08-15 01:39:56 | 57159 | 2015-05-17 00:00:00 | 56793.5775 | 2014-05-16 13:51:36 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090017 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Here we propose to observe two of the lowest luminosity BAT AGNs to measure the amount of the reflection component with unpreceded accuracy, a key parameter to determine the contribution of Compton thick AGNs to the X-ray background. We will also study how the torus structure of low luminosity AGNs differs from that of more luminous AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | BROAD BAND SPECTRA OF HARD X-RAY SELECTED VERY LOW LUMINOSITY AGNS AND THEIR TORUS STRUCTURE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709002010/ | Quick Look | ![]() |
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335 | NGC2110 | 88.0489 | -7.4533 | 87.444745 | -7.464256 | 87.748433 | -30.879563 | 212.92425635 | -16.54269345 | 269.0605 | 57101.7987152778 | 2015-03-20 19:10:09 | 57103.3044328704 | 2015-03-22 07:18:23 | 709011010 | 45.6257 | 50 | 45.6257 | 49.4936 | 0 | 49.5096 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8483564815 | 2016-08-17 20:21:38 | 57558 | 2016-06-19 00:00:00 | 57190.4658333333 | 2015-06-17 11:10:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090062 | We propose to observe the Seyfert galaxy NGC2110 twice every half year, which showed a big flare by a factor of around 5 against the normal state around 2012 December. We can observe the echo history following the flare in a time scale of years, and then measure the reflection spectrum very accurately to constrain the geometry of the reflection torus. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YASUSHI FUKAZAWA | JAP | 9 | AO9 | X-RAY ECHO OF THE BIG FLARE OF SEYFERT GALAXY NGC2110 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709011010/ | Quick Look | ![]() |
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336 | HOLMBERG IX X-1 | 149.4572 | 69.0544 | 148.43919 | 69.292844 | 119.777434 | 51.680142 | 141.94722641 | 41.07197433 | 311.5038 | 57118.9110416667 | 2015-04-06 21:51:54 | 57119.5667708333 | 2015-04-07 13:36:09 | 709015030 | 31.5263 | 30 | 31.5263 | 31.5263 | 0 | 31.5263 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.9243402778 | 2016-08-17 22:11:03 | 57513 | 2016-05-05 00:00:00 | 57129.4193171296 | 2015-04-17 10:03:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091251 | Broadband X-ray spectroscopy of ultraluminous X-ray sources (ULXs) with NuSTAR and Suzaku has begun to provide important information regarding the nature of these enigmatic sources. Recent NuSTAR observations of the extreme ULX Holmberg IX X-1 revealed unusual spectral variability, and different competing evolutionary scenarios can explain the available data. Resolving this degeneracy is critical to determining the nature of the accretion onto this source, and requires multi-epoch broadband spectroscopy probing a more diverse range of fluxes. We propose to undertake 4x30 ks coordinated Suzaku+NuSTAR observations of Holmberg IX X-1 to provide the additional spectra needed to robustly determine the nature of the observed evolution, providing a vital step in our understanding of extreme ULXs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | DOMINIC WALTON | USA | 9 | AO9 | MULTI-EPOCH BROADBAND X-RAY SPECTROSCOPY OF HOLMBERG IX X-1 WITH SUZAKU AND NUSTAR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709015030/ | Quick Look | ![]() |
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337 | OJ 287 | 133.705 | 20.1043 | 132.989927 | 20.295379 | 130.505973 | 2.596868 | 206.81753743 | 35.82068078 | 285.8744 | 57148.4467708333 | 2015-05-06 10:43:21 | 57151.4189351852 | 2015-05-09 10:03:16 | 710011020 | 110.2819 | 323 | 110.2819 | 112.3099 | 0 | 112.3099 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.1271643518 | 2016-08-18 03:03:07 | 57113 | 2015-04-01 00:00:00 | 57164.5272337963 | 2015-05-22 12:39:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 101431 | Kepler will observe OJ 287 with 1 min sampling and >90% duty cycle for ~75 days in 2015, providing an unprecedented opportunity to quantitatively compare optical and X-ray variations in one of the brightest and most active blazars in the sky. We request continuous Suzaku coverage for 128 orbits (323 ks) in a simultaneous campaign including XMM, Swift, radio and multi-color optical monitoring. Suzaku samples key intermediate timescales of hours-days, allowing measurement of CCFs and PSDs spanning a wide range of temporal frequencies. These will be used to test models and determine source parameters e.g. if the X-rays are due to synchrotron-self Compton the optical should lead the X-rays by ~1 day, but if they are "synchrotron flashes" the bands should vary nearly simultaneously. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RICK EDELSON | USA | 10 | AO10 | SIMULTANEOUS SUZAKU/KEPLER/MULTIWAVELENGTH MONITORING OF OJ 287 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710011020/ | Quick Look | ![]() |
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338 | OJ 287 | 133.7049 | 20.1044 | 132.989827 | 20.295479 | 130.505855 | 2.596938 | 206.81738245 | 35.82062575 | 285.8744 | 57151.4189467593 | 2015-05-09 10:03:17 | 57154.3266666667 | 2015-05-12 07:50:24 | 710011030 | 107.7143 | 323 | 107.7143 | 107.7143 | 0 | 107.7143 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.6879166667 | 2016-08-18 16:30:36 | 57113 | 2015-04-01 00:00:00 | 57164.5596527778 | 2015-05-22 13:25:54 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 101431 | Kepler will observe OJ 287 with 1 min sampling and >90% duty cycle for ~75 days in 2015, providing an unprecedented opportunity to quantitatively compare optical and X-ray variations in one of the brightest and most active blazars in the sky. We request continuous Suzaku coverage for 128 orbits (323 ks) in a simultaneous campaign including XMM, Swift, radio and multi-color optical monitoring. Suzaku samples key intermediate timescales of hours-days, allowing measurement of CCFs and PSDs spanning a wide range of temporal frequencies. These will be used to test models and determine source parameters e.g. if the X-rays are due to synchrotron-self Compton the optical should lead the X-rays by ~1 day, but if they are "synchrotron flashes" the bands should vary nearly simultaneously. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RICK EDELSON | USA | 10 | AO10 | SIMULTANEOUS SUZAKU/KEPLER/MULTIWAVELENGTH MONITORING OF OJ 287 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710011030/ | Quick Look | ![]() |
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339 | MRK421 | 166.1418 | 38.2711 | 165.447021 | 38.540933 | 151.207571 | 29.566146 | 179.67525089 | 65.03258412 | 111.0988 | 54803.7278240741 | 2008-12-03 17:28:04 | 54805.9480324074 | 2008-12-05 22:45:10 | 703020010 | 101.3075 | 100 | 101.3315 | 101.3075 | 0 | 101.3315 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 65.5148 | 65.5148 | 191.7877 | 3 | PROCESSED | 57544.7029398148 | 2016-06-05 16:52:14 | 55188 | 2009-12-23 00:00:00 | 54818.7659837963 | 2008-12-18 18:23:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030119 | Mrk421 provides our best opportunity to understand the high-energy emission of blazar jets, because it has produced the largest observed flux. Suzaku HXD has proved that spectum upto 40 keV can be measured only with an exposure of 1 ks from Mrk 421. Hard X-ray region is very crucial to study particle acceleration in the jet, since it corresponds to high energy end of electron distribution. Cooling and Acceleration phenomena will appear in this energy band. Here we will propose to monitor Mrk 421 for 200 ks, in which we can expect at least four or five flares. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TADAYUKI TAKAHASHI | JAP | 3 | AO3 | STUDY OF HARD X-RAY EVOLUTION FROM THE BRIGHTEST BLAZAR JET. | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703020010/ | Quick Look | ![]() |
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340 | I ZW 18 | 143.5151 | 55.2494 | 142.632451 | 55.471905 | 125.701519 | 38.241912 | 160.51246258 | 44.84288886 | 130.2629 | 56934.0191666667 | 2014-10-04 00:27:36 | 56935.6258680556 | 2014-10-05 15:01:15 | 709021020 | 82.0708 | 70 | 82.0708 | 82.0868 | 0 | 82.0868 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6143865741 | 2016-08-16 14:44:43 | 57358 | 2015-12-02 00:00:00 | 56989.5111689815 | 2014-11-28 12:16:05 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091441 | The source of energetic photons that reionized and heated the early universe remains uncertain. Early galaxies had low metallicity and the best local analogs are blue compact dwarf galaxies (BCDs) with low metallicity. We propose to observe two such galaxies known to be luminous in X-rays and accurately measure their spectrum with the Suzaku XIS. These observations are important to our understanding of the heating of the universe during the epoch of reionization. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | PHILIP KAARET | USA | 9 | AO9 | X-RAYS FROM LOW-METALLICITY BLUE COMPACT DWARF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709021020/ | Quick Look | ![]() |
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341 | 3C279 | 194.0685 | -5.7338 | 193.421343 | -5.463366 | 195.163667 | 0.26086 | 305.14803375 | 57.11713803 | 113.6423 | 54850.9795833333 | 2009-01-19 23:30:36 | 54853.9391203704 | 2009-01-22 22:32:20 | 703049010 | 134.1106 | 200 | 134.1106 | 134.1106 | 0 | 134.1106 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82.8563 | 82.8563 | 255.689 | 7 | PROCESSED | 57545.3939351852 | 2016-06-06 09:27:16 | 55328 | 2010-05-12 00:00:00 | 54880.5781365741 | 2009-02-18 13:52:31 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031346 | We propose a 200 ks observation of 3C279, the archetypal EGRET blazar to be conducted simultaneously with GLAST as well as many other facilities, with the goal of obtaining broadband spectra and light-curves. The flux in all observable bands is known to be rapidly variable, but the information regarding the correlation between the time history of flux in various bands is limited, and the proposed observations are designed to remedy this shortcoming. Such detailed spectral and variability studies are crucial to discriminate between different radiation scenarios responsible for production of X-rays and gamma-rays, and to constrain the matter content and by extension, the formation process of the jet, dissipation of the jet energy, and energization of the radiating particles. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GRZEGORZ MADEJSKI | USA | 3 | AO3 | SUZAKU AND GLAST OBSERVATIONS OF 3C279 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703049010/ | Quick Look | ![]() |
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342 | NGC 4258 | 184.7518 | 47.3153 | 184.134648 | 47.592794 | 160.376562 | 44.164981 | 138.28789039 | 68.83430148 | 139.1798 | 55511.1601388889 | 2010-11-11 03:50:36 | 55512.7112615741 | 2010-11-12 17:04:13 | 705051010 | 103.8332 | 100 | 103.8332 | 103.8412 | 0 | 103.837 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86.2257 | 86.2257 | 133.9688 | 1 | PROCESSED | 57554.0812384259 | 2016-06-15 01:56:59 | 55903 | 2011-12-08 00:00:00 | 55537.1754398148 | 2010-12-07 04:12:38 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051451 | We request a 100 ksec observation of the Low Luminosity AGN NGC 4258. This observation is meant to complement our existing 100 ksec Suzaku observation (Reynolds et al. 2009), and our 320 ksec Chandra-HETG observation (Murphy et al., in prep.). The goal is to further characterize the observed variability of the Fe Kalpha line and any associated changes in the continuum and/or absorption of NGC 4258. Given the unique constraints that we have on the mass, distance and accretion flow geometry in NGC 4258, as well as its role as a bridge between the most quiescent nuclei and powerful AGN, further Suzaku studies of NGC 4258 are clearly warranted. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | MICHAEL NOWAK | USA | 5 | AO5 | HUNTING FOR THE VARIABLE IRON LINE IN NGC 4258 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705051010/ | Quick Look | ![]() |
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343 | MCG-6-30-15 | 203.9717 | -34.2976 | 203.255303 | -34.04246 | 215.173232 | -22.546653 | 313.28966663 | 27.67858669 | 102.4356 | 53758.5062962963 | 2006-01-23 12:09:04 | 53761.0835648148 | 2006-01-26 02:00:20 | 700007020 | 98.4834 | 300 | 98.4834 | 98.4834 | 98.4834 | 98.4834 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 81.8922 | 81.8922 | 222.6497 | 3 | PROCESSED | 57532.8430902778 | 2016-05-24 20:14:03 | 54247 | 2007-05-27 00:00:00 | 54059.5463773148 | 2006-11-20 13:06:47 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001035 | The broad iron line in the Seyfert 1 galaxy MCG-6-30-15 shows that most of the power is released at 2--4 gravitational radii enabling the strong gravity, accretion flow and energy release in that exciting regime to be studied. The spectral variability of the source decomposes into a highly variable power law and a reflection-dominated component, containing the iron line and Compton hump, which varies significantly but with much less amplitude. This can be explained by the extreme gravitational light bending occuring in this region. We propose to observe MCG--6-30-15 for 4 x 50~ks in order to determine for the first time the variability of the reflection over a wide range of energies from below 1 keV to above 40 keV and timescales . | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ANDREW FABIAN | JAP | 0 | SWG | REFLECTION, ABSORPTION AND STRONG GRAVITY AROUND THE SPINNING BLACK HOLE IN MCG--6-30-15 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700007020/ | Quick Look | ![]() |
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344 | UGC5101 | 144.0189 | 61.4178 | 143.073331 | 61.641673 | 122.524313 | 43.933823 | 152.38145034 | 42.89433298 | 112.6892 | 54039.7635300926 | 2006-10-31 18:19:29 | 54040.396087963 | 2006-11-01 09:30:22 | 701002020 | 42.166 | 35 | 42.166 | 42.174 | 42.182 | 42.182 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 33.5589 | 33.5589 | 54.6519 | 0 | PROCESSED | 57536.0043518518 | 2016-05-28 00:06:16 | 54735 | 2008-09-26 00:00:00 | 54063.3945949074 | 2006-11-24 09:28:13 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010001 | We propose Suzaku observations at E > 10 keV of nearby ultraluminous infrared galaxies (ULIRGs), for which our infrared spectroscopy has strongly suggested the presence of luminous AGNs deeply buried in gas and dust. However, extreme starbursts are still a possibility. Through the proposed X-ray observations using Suzaku, we aim to distinguish clearly between buried AGNs (strong X-ray emitters) and extreme starbursts (weak X-ray emitters), and to obtain convincing evidence for luminous buried AGNs. Since buried AGNs in these ULIRGs' cores are likely to suffer from Compton-thick X-ray absorption, the high sensitivity at E > 10 keV achieved by Suzaku HXD PIN is crucial for the success of this experiment. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MASATOSHI IMANISHI | JAP | 1 | AO1 | COMPTON THICK BURIED AGNS IN NEARBY ULTRALUMINOUS INFRARED GALAXIES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701002020/ | Quick Look | ![]() |
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345 | PKS 0558-504 | 89.9334 | -50.4402 | 89.629898 | -50.441281 | 89.86386 | -73.882062 | 257.95215413 | -28.57698713 | 210.2147 | 54119.7661805556 | 2007-01-19 18:23:18 | 54120.3203009259 | 2007-01-20 07:41:14 | 701011030 | 21.2563 | 20 | 21.2563 | 21.2563 | 0 | 21.2563 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.1145 | 19.1145 | 47.87 | 0 | PROCESSED | 57536.8847916667 | 2016-05-28 21:14:06 | 54735 | 2008-09-26 00:00:00 | 54133.3934259259 | 2007-02-02 09:26:32 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010057 | Narrow-line Seyfert 1 Galaxies (NLS1s) must have been crucial key to understand the rapid growth of the central supermassive black hole, which may be related to the evolution of the host galaxy. Hence, we propose 20x5 ksec observations of the luminous NLS1 galaxy PKS 0558-504, which is the candidate having the highest mass-accretion rate among the class. Large effective area and good energy resolution of XISs allow us to strictly constrain the temperature and the luminosity of the accretion flow. In addition, Suzaku HXD will detect the significant fraction of hard power law emission in the 10-60 keV band for the first time. From these observations, we expect to derive the new picture of the high mass-accretion mechanism in NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YOSHITO HABA | JAP | 1 | AO1 | SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701011030/ | Quick Look | ![]() |
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346 | SWIFT J1628.1+5145 | 246.9541 | 51.8388 | 246.639575 | 51.948443 | 220.797096 | 71.358115 | 79.81767806 | 42.92326404 | 60.2479 | 53840.7843518518 | 2006-04-15 18:49:28 | 53841.3904976852 | 2006-04-16 09:22:19 | 701016010 | 23.589 | 20 | 23.605 | 23.597 | 23.589 | 23.597 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 20.6261 | 20.6261 | 52.3599 | 2 | PROCESSED | 57533.4625231482 | 2016-05-25 11:06:02 | 54394 | 2007-10-21 00:00:00 | 53905.7494444444 | 2006-06-19 17:59:12 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010133 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 1 | AO1 | DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701016010/ | Quick Look | ![]() |
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347 | NGC 4151 | 182.6375 | 39.4139 | 182.006166 | 39.692011 | 164.091601 | 36.628069 | 155.05374688 | 75.05753801 | 112.1087 | 54087.8369097222 | 2006-12-18 20:05:09 | 54090.3848726852 | 2006-12-21 09:14:13 | 701034010 | 124.9796 | 125 | 124.9796 | 124.9796 | 0 | 124.9796 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 131.2741 | 131.2741 | 220.1059 | 3 | PROCESSED | 57536.4582060185 | 2016-05-28 10:59:49 | 54702 | 2008-08-24 00:00:00 | 54132.849537037 | 2007-02-01 20:23:20 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011327 | We propose a 100 ks Suzaku observation of the brightest Seyfert Galaxy in the sky. Given the broad band-pass, and high sensitivity, the proposed observations will provide a high-quality spectrum which will allow us to search for variability in the high-ionized absorber (compared to previous observations). We will be able to obtain stringent constraints on the "Reflection Hump" and compare it to the strength of the Fe Kalpha emission line - thus providing a direct test of Reflection models. The proposed program will also complement observations of fainter and more exotic Seyferts likely to be observed during AO-1. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | IAN GEORGE | USA | 1 | AO1 | DECOUPLING THE COMPONENTS IN THE BRIGHTEST SEYFERT: NGC 4151 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701034010/ | Quick Look | ![]() |
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348 | NGC1386 | 54.1629 | -35.9533 | 53.686009 | -36.117288 | 37.868182 | -53.108166 | 237.58696036 | -53.99184818 | 64.5172 | 54309.0884259259 | 2007-07-28 02:07:20 | 54310.1668402778 | 2007-07-29 04:00:15 | 702002010 | 55.5226 | 50 | 55.5226 | 55.5306 | 0 | 55.5306 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.5213 | 47.5213 | 93.1439 | 1 | PROCESSED | 57539.3619907407 | 2016-05-31 08:41:16 | 54707 | 2008-08-29 00:00:00 | 54339.0775115741 | 2007-08-27 01:51:37 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020005 | Compton thick Seyfert 2 galaxies may constitute a large fraction of the Seyfert 2 galaxy's population. However, the nature of the Compton-thick objects is still unclear due to the heavy obscuration of the nuclear emission. The wide-band spectroscopy with Suzaku is crucial to expose their nature hidden by thick matter. In order to reveal their nature in the local Universe, we propose Suzaku observations of Risaliti's Compton-thick objects. These observations will also bring us important results to study the structure and evolution of active galactic nuclei. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HISAMITSU AWAKI | JAP | 2 | AO2 | REVEAL THE NATURE OF COMPTON THICK SEYFERT 2 GALAXIES WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702002010/ | Quick Look | ![]() |
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349 | APM 08279+5255 | 127.9229 | 52.7639 | 126.990699 | 52.933179 | 116.237243 | 32.72103 | 165.74356471 | 36.23970609 | 100.0676 | 54040.3996643518 | 2006-11-01 09:35:31 | 54041.9690277778 | 2006-11-02 23:15:24 | 701057020 | 102.295 | 100 | 102.303 | 102.311 | 102.311 | 102.295 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 95.624 | 95.624 | 135.5778 | 1 | PROCESSED | 57536.0492592593 | 2016-05-28 01:10:56 | 54695 | 2008-08-17 00:00:00 | 54088.5241782407 | 2006-12-19 12:34:49 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011353 | Motivated by the detection of a relativistic outflow of highly ionized gas in previous XMM-Newton and Chandra observations of the lensed quasar APM08279+5255 we propose to monitor this object with three 100ks observations with the aim of improving our understanding of the significance of such outflows in regulating black hole growth and in influencing structure formation. The main scientific goals are : (a) verify the present interpretations of Fe line features in this quasar, (b) monitor the time variability of the Fe absorption features and thus constrain the acceleration mechanism, (c) constrain the kinematic, ionization and absorbing properties of the outflow, and (d) show whether the low-energy ionized absorber is part of the relativistic outflow. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GEORGE CHARTAS | USA | 1 | AO1 | VIEWS OF RELATIVISTIC WINDS THROUGH NATURAL LENSES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701057020/ | Quick Look | ![]() |
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350 | NGC 5728 | 220.5794 | -17.3095 | 219.88301 | -17.096936 | 223.49481 | -1.485509 | 337.26599487 | 38.0606459 | 290.4081 | 53935.7359143518 | 2006-07-19 17:39:43 | 53936.6264930556 | 2006-07-20 15:02:09 | 701079010 | 41.3077 | 40 | 41.3077 | 41.3077 | 41.3077 | 41.3077 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39.569 | 39.569 | 76.9419 | 0 | PROCESSED | 57535.0121064815 | 2016-05-27 00:17:26 | 54400 | 2007-10-27 00:00:00 | 53943.5061111111 | 2006-07-27 12:08:48 | 3.0.22.43 | 6 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012016 | The high-energy detectors onboard Swift and INTEGRAL have started to survey the hard X-ray sky above 10 keV. Although limited to bright X-ray fluxes (~10^-11 cgs), the large area surveyed so far has allowed to build up sizable sa mples of hard X-ray selected AGN almost unbiased against X-ray absorption. The AGN content of these surveys is dominated by obscured AGN. We have identified 3 objects which are most likely obscured by Compton-thick matter and very bright above 10 keV. We propose to observe them with Suzaku for 40 ks each to study their broad-band X-ray spectra and unveil previously unknown nearby heavily obscured AGN, with important consequences for the study of the AGN evolution and the synthesis of the X-ray background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ANDREA COMASTRI | EUR | 1 | AO1 | BRIGHT COMPTON THICK GALAXIES IN THE BACKYARD | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701079010/ | Quick Look | ![]() |
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351 | NGC3393 | 162.075 | -25.2139 | 161.475136 | -24.949432 | 174.292392 | -30.103718 | 270.6699706 | 29.83420275 | 292.9271 | 54243.7827662037 | 2007-05-23 18:47:11 | 54245.1876041667 | 2007-05-25 04:30:09 | 702004010 | 55.227 | 50 | 55.227 | 55.227 | 0 | 55.227 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.255 | 48.255 | 121.3699 | 4 | PROCESSED | 57538.7560416667 | 2016-05-30 18:08:42 | 54745 | 2008-10-06 00:00:00 | 54255.6532986111 | 2007-06-04 15:40:45 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020005 | Compton thick Seyfert 2 galaxies may constitute a large fraction of the Seyfert 2 galaxy's population. However, the nature of the Compton-thick objects is still unclear due to the heavy obscuration of the nuclear emission. The wide-band spectroscopy with Suzaku is crucial to expose their nature hidden by thick matter. In order to reveal their nature in the local Universe, we propose Suzaku observations of Risaliti's Compton-thick objects. These observations will also bring us important results to study the structure and evolution of active galactic nuclei. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HISAMITSU AWAKI | JAP | 2 | AO2 | REVEAL THE NATURE OF COMPTON THICK SEYFERT 2 GALAXIES WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702004010/ | Quick Look | ![]() |
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352 | LMC X-4 | 83.1883 | -66.3595 | 83.179882 | -66.392572 | 1.044909 | -87.279168 | 276.32310713 | -32.53751505 | 226.9099 | 54507.0294560185 | 2008-02-11 00:42:25 | 54507.6043287037 | 2008-02-11 14:30:14 | 702037010 | 23.3814 | 20 | 23.3894 | 23.3974 | 0 | 23.3814 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20.047 | 20.047 | 49.662 | 1 | PROCESSED | 57541.5628356482 | 2016-06-02 13:30:29 | 54883 | 2009-02-21 00:00:00 | 54515.5898842593 | 2008-02-19 14:09:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021127 | We propose for a series of three 20ks observations of the binary X-ray pulsar LMC X-4. This source shows 13.5 s pulsations, a 1.4 d orbital period, and a long-period (~30 d) variability due to a warped, precessing accretion disk. The proposed analysis will use pulse-phase spectroscopy with XIS to explore changes in the X-ray pulses and spectra at three different phases in the disk precession. This work will give us a detailed picture of the accretion flow, particularly for the inner regions of the accretion disk that are illuminated by the X-rays from the neutron star. This project takes advantage of the strengths of the XIS, particularly its excellent spectral resolution, sufficient (1s) time resolution in Window mode, and wide PSF that limits pile-up effects. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RYAN HICKOX | USA | 2 | AO2 | SUPERORBITAL VARIATION OF LMC X-4: EXPLORING THE ACCRETION FLOW | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702037010/ | Quick Look | ![]() |
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353 | 3C 445 | 335.9528 | -2.0995 | 335.30761 | -2.353112 | 336.949965 | 7.376595 | 61.86726076 | -46.70852053 | 68.9567 | 54245.2015046296 | 2007-05-25 04:50:10 | 54248.9169444444 | 2007-05-28 22:00:24 | 702056010 | 139.7691 | 125 | 139.7691 | 139.7691 | 0 | 139.7691 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 117.2412 | 117.2412 | 320.9918 | 4 | PROCESSED | 57538.8276967593 | 2016-05-30 19:51:53 | 54702 | 2008-08-24 00:00:00 | 54256.717662037 | 2007-06-05 17:13:26 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021352 | It is well known that the circum-black hole environ of Seyferts contain warm, photoionized gas responsible for complex absorption/emission at X-rays. Evidence for such components in radio-loud AGN is, instead, rare. And yet, presence of an ionized, scattering medium is postulated by unification models for these sources, and some models for jet formation. Here we tackle this problem by proposing sensitive Suzaku observations of 3C445, the only Broad-Line Radio Galaxy exhibiting soft X-ray emission lines from 0.4-3 keV in an archival EPIC spectrum. We will: 1) Determine the broad-band continuum; 2) Study the properties of the soft emission lines, determining the gas density and location, and thus its role in jet collimation; and 3) Confirm the strong reflection component suggested by EPIC. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RITA SAMBRUNA | USA | 2 | AO2 | WARM GAS IN THE INNER REGIONS OF RADIO-LOUD AGN: THE CASE OF 3C445 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702056010/ | Quick Look | ![]() |
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354 | Q0450-1310 | 73.3011 | -13.0912 | 72.722633 | -13.172561 | 69.927484 | -35.377207 | 211.74785299 | -32.06702416 | 263.6423 | 54535.8878240741 | 2008-03-10 21:18:28 | 54536.2502314815 | 2008-03-11 06:00:20 | 702062010 | 15.5102 | 13 | 15.5102 | 15.5102 | 0 | 15.5102 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.9887 | 14.9887 | 31.3059 | 0 | PROCESSED | 57541.8181828704 | 2016-06-02 19:38:11 | 54916 | 2009-03-26 00:00:00 | 54550.1640277778 | 2008-03-25 03:56:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021361 | The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | GEORGE CHARTAS | USA | 2 | AO2 | AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702062010/ | Quick Look | ![]() |
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355 | XBONGBLUE2 | 217.7653 | 34.3413 | 217.240861 | 34.56211 | 200.146538 | 45.945194 | 57.71878971 | 67.47993323 | 130.3787 | 54454.1686921296 | 2007-12-20 04:02:55 | 54454.5050694445 | 2007-12-20 12:07:18 | 702084010 | 14.8162 | 13 | 14.8162 | 14.8162 | 0 | 14.8162 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14.5794 | 14.5794 | 29.0559 | 0 | PROCESSED | 57540.9126851852 | 2016-06-01 21:54:16 | 54828 | 2008-12-28 00:00:00 | 54460.6654398148 | 2007-12-26 15:58:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021376 | We propose to use Suzaku's large collecting area and excellent energy response to measure accurate X-ray spectra for 9 XBONGs and 8 luminous Type 2 AGN selected from very large samples of identified XBONGs and Type 2 AGN found in our Chandra XBootes survey. We have obtained optical spectra for 258 XBONGs and identified ~700 X-ray luminous Type 2 AGN at z>0.7. With known source positions and X-ray fluxes, we select sources that are relatively bright with little or no contamination from other X-ray sources. Thus we will measure individual spectra for these bright sources. We propose eight 15 ksec Suzaku XIS observations to measure the absorption in 8 luminous z > 0.8 Type 2 AGN and eight 10 ksec observations to measure the absorption and iron emission for nine XBONGs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | CHRISTINE JONES | USA | 2 | AO2 | OBSCURED AGN AND XBONGS IN BOOTES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702084010/ | Quick Look | ![]() |
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356 | IRAS 05262+4432 | 82.4599 | 44.6406 | 81.547278 | 44.601887 | 84.24873 | 21.350791 | 165.01766257 | 5.72021917 | 78.2999 | 54721.6357523148 | 2008-09-12 15:15:29 | 54723.406412037 | 2008-09-14 09:45:14 | 703019010 | 82.086 | 80 | 82.0975 | 82.094 | 0 | 82.086 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.9075 | 70.9075 | 152.9541 | 0 | PROCESSED | 57543.8409490741 | 2016-06-04 20:10:58 | 55148 | 2009-11-13 00:00:00 | 54780.4562037037 | 2008-11-10 10:56:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030085 | X-ray observations of obscured narrow-line Seyfert 1 galaxies (NLS1s) have never been performed effectively, in spite of the fact that absorbing material and nuclear emission of NLS1s are thought to be a crucial key to understand the fueling and accretion mechanisms, which may be directly related to the rapid evolution of supermassive black holes. We, therefore, propose 80 ksec observation of the candidate of an obscured NLS1 IRAS 05262+4432. High sensitivity throughout the 0.3-70 keV wide energy band of Suzaku allows us to strictly constrain the X-ray luminosity of primary emission and the geometry of the surrounding matter. From our observation, we expect to derive more complete unified picture of AGNs | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHITO HABA | JAP | 3 | AO3 | SUZAKU VIEW OF OBSCURED NARROW-LINE SEYFERT 1 GALAXY IRAS 05262+4432 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703019010/ | Quick Look | ![]() |
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357 | MRK 421 | 166.1081 | 38.2021 | 165.413329 | 38.471893 | 151.215505 | 29.492571 | 179.85015534 | 65.02934628 | 313.5582 | 54591.1196527778 | 2008-05-05 02:52:18 | 54595.3502199074 | 2008-05-09 08:24:19 | 703043010 | 180.7851 | 150 | 180.7931 | 180.7851 | 0 | 180.7931 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 163.5507 | 163.5507 | 343.6517 | 9 | PROCESSED | 57542.5998842593 | 2016-06-03 14:23:50 | 54972 | 2009-05-21 00:00:00 | 54606.5618287037 | 2008-05-20 13:29:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031341 | We propose one 150 ksec Suzaku ToO observations of one of the three strong GeV-TeV gamma-ray blazars Mrk 421, Mrk 501, or 1ES 1959+650 during a 10 day multiwavelength campaign with coverage from radio to gamma-rays. The proposal is submitted by the VERITAS collaboration, assuring excellent TeV gamma-ray coverage. The Suzaku observations will play a key-role in interpreting the multiwavelength data set, allowing us to measure the time lag between the X-ray and gamma-ray flux variability and to scrutinize the correlation of the X-ray and gamma-ray spectral indices. The Suzaku and gamma-ray energy spectra will allow us to constrain the intensity of the IR Diffuse Extragalactic Background Radiation which absorbs TeV gamma-rays in extragalactic pairproduction processes. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HENRIC KRAWCZYNSKI | USA | 3 | AO3-TOO | TARGET OF OPPORTUNITY OBSERVATIONS OF THE BLAZARS MRK 421, MRK 501, AND 1ES 1959+650 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703043010/ | Quick Look | ![]() |
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358 | NGC 4686 | 191.5508 | 54.5121 | 190.986823 | 54.785056 | 159.09559 | 52.489361 | 124.58283765 | 62.59936814 | 342.6621 | 54946.7002777778 | 2009-04-25 16:48:24 | 54947.7564699074 | 2009-04-26 18:09:19 | 704015010 | 44.8459 | 40 | 44.8539 | 44.8459 | 0 | 44.8459 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.3275 | 42.3275 | 91.232 | 0 | PROCESSED | 57546.4795717593 | 2016-06-07 11:30:35 | 55339 | 2010-05-23 00:00:00 | 54973.9296875 | 2009-05-22 22:18:45 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040060 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe three Compton thick AGN candidates in the 22 months BAT catalog with Suzaku. To resolve the degeneracy of spectral modeling, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 4 | AO4 | DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704015010/ | Quick Look | ![]() |
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359 | 3C 35 | 18.0181 | 49.4424 | 17.27928 | 49.177164 | 38.209927 | 38.103766 | 126.37585323 | -13.29131796 | 245.0044 | 55200.6165509259 | 2010-01-04 14:47:50 | 55202.466875 | 2010-01-06 11:12:18 | 704019010 | 84.7566 | 80 | 85.0286 | 84.7566 | 0 | 85.0206 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 66.3143 | 66.3143 | 147.5778 | 2 | PROCESSED | 57550.0615277778 | 2016-06-11 01:28:36 | 55584 | 2011-01-23 00:00:00 | 55218.1479050926 | 2010-01-22 03:32:59 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040096 | Suzaku observations of two giant radio galaxies, 3C 35 and DA 240, with a total size of about 1 Mpc are proposed, in order to detect diffuse inverse Compton X-ray emission from their radio lobes. The X-ray flux from the lobes, in comparison with the radio one, provides a precise determination of electron and magnetic field energies there. A comparison of them with those in smaller radio galaxies is used to probe into the history of jets and lobes. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | NAOKI ISOBE | JAP | 4 | AO4 | SUZAKU OBSERVATION OF GIANT RADIO GALAXIES AS A PROBE OF JET HISTORY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704019010/ | Quick Look | ![]() |
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360 | IGRJ01528 | 28.2011 | -3.4464 | 27.56858 | -3.692494 | 24.925792 | -14.053354 | 157.35013019 | -62.14500791 | 77.3667 | 55007.0338078704 | 2009-06-25 00:48:41 | 55008.1426388889 | 2009-06-26 03:25:24 | 704043010 | 46.9159 | 40 | 46.9159 | 47.6119 | 0 | 47.6248 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 42.1043 | 42.1043 | 95.7918 | 0 | PROCESSED | 57547.6882407407 | 2016-06-08 16:31:04 | 55386 | 2010-07-09 00:00:00 | 55019.1922337963 | 2009-07-07 04:36:49 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041414 | We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | EZEQUIEL TREISTER | USA | 4 | AO4 | THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704043010/ | Quick Look | ![]() |
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361 | 1150+497 | 178.3624 | 49.5318 | 177.710529 | 49.809967 | 153.770918 | 43.67464 | 145.51949415 | 64.97605225 | 131.4133 | 55512.7136805556 | 2010-11-12 17:07:42 | 55514.1042824074 | 2010-11-14 02:30:10 | 705003010 | 105.6558 | 100 | 105.7118 | 105.6558 | 0 | 105.7198 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 84.6438 | 84.6438 | 120.128 | 1 | PROCESSED | 57554.1053356482 | 2016-06-15 02:31:41 | 55892 | 2011-11-27 00:00:00 | 55524.2197337963 | 2010-11-24 05:16:25 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050007 | A Suzaku observation of the iron line emitting blazar 1150+497 is proposed. The object is reported to exhibit a signature iron line. By measuring the equivalent width and line width, Suzaku will reveal the state of the accretion disc with the jet activity. It is notable that the blazar, aligning the jet with the line of sight, allow us to observe the jet and the accretion disc with a sufficient isochronism even with the violently variable sources. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | HIROMI SETA | JAP | 5 | AO5 | SUZAKU OBSERVATION OF AN FE-LINE BLAZAR 1150+497 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705003010/ | Quick Look | ![]() |
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362 | EMS1535 | 345.6918 | 44.7374 | 345.120256 | 44.468031 | 9.799428 | 45.696922 | 103.4061071 | -13.97501662 | 63.3944 | 55373.2448611111 | 2010-06-26 05:52:36 | 55374.0174768518 | 2010-06-27 00:25:10 | 705016010 | 42.3955 | 40 | 42.4035 | 42.3955 | 0 | 42.4035 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 42.7545 | 42.7545 | 66.7539 | 0 | PROCESSED | 57552.4062268518 | 2016-06-13 09:44:58 | 55772 | 2011-07-30 00:00:00 | 55404.2240625 | 2010-07-27 05:22:39 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050050 | We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 5 | AO5 | SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705016010/ | Quick Look | ![]() |
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363 | 1RXS J032613.6+02252 | 51.5615 | 2.4213 | 50.912043 | 2.246984 | 49.792333 | -15.817317 | 180.7494445 | -42.4285339 | 253.9336 | 55596.8403356482 | 2011-02-04 20:10:05 | 55597.6203125 | 2011-02-05 14:53:15 | 705038010 | 32.1971 | 32 | 32.1971 | 32.1971 | 0 | 32.1971 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.6441 | 22.6441 | 67.3879 | 1 | PROCESSED | 57600.8622106482 | 2016-07-31 20:41:35 | 55983 | 2012-02-26 00:00:00 | 55614.1886342593 | 2011-02-22 04:31:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051402 | High frequency peaked BL Lacs are a peculiar subclass of Blazars characterized by non-thermal emission across the whole electromagnetic spectrum. Their spectral energy distributions (SEDs) include two main components: a low-energy component with power peaking in the range from the UV to the X-ray band, and a substantial high-energy component often dominated by gamma-rays. We propose 3 observations (32 ks each) of a selected sample of HBLs to study the behavior of the first component, widely interpreted as synchrotron radiation. First, we will be able to disentangle between different spectral shapes of the synchrotron SED of HBLs. Second, we will use the proposed observations to investigate the properties of the most representative sample of TeV candidate HBLs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | FRANCESCO MASSARO | USA | 5 | AO5 | X-RAY CURVED SPECTRA IN HIGH FREQUENCY PEAKED BL LACS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705038010/ | Quick Look | ![]() |
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364 | CBS 126 | 153.2712 | 35.8701 | 152.538495 | 36.117901 | 141.901695 | 23.115205 | 188.30426979 | 55.38335717 | 124.145 | 55487.3144907407 | 2010-10-18 07:32:52 | 55489.5529861111 | 2010-10-20 13:16:18 | 705042010 | 101.542 | 100 | 101.566 | 101.542 | 0 | 101.566 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 90.7438 | 90.7438 | 193.3897 | 2 | PROCESSED | 57553.8238541667 | 2016-06-14 19:46:21 | 55867 | 2011-11-02 00:00:00 | 55498.3270949074 | 2010-10-29 07:51:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051432 | We propose to carry out a 100 ks Suzaku observation of Broad Line Seyfert 1 (BLS1) galaxy CBS 126. This source exhibits many properties which are thought to be typical of a Narrow Line Seyfert 1 (NLS1), such as a large soft X-ray excess and strong spectral variability, but unusual for a BLS1. Taking advantage of Suzaku's unique broad band X-ray energy window, our main goal is to clarify the nature of the unusual, variable, optically polarized spectrum of CBS 126. These interesting spectral features cover a wide energy range where Suzaku is ideal. With these proposed studies we will gain better understanding of accretion-powered AGN in general. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | SACHIKO TSURUTA | USA | 5 | AO5 | SPECTRAL AND TEMPORAL STUDIES OF THE SEYFERT 1 GALAXY CBS 126 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705042010/ | Quick Look | ![]() |
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365 | NGC6251_LOBE | 246.4248 | 82.6439 | 247.78516 | 82.752174 | 100.137256 | 73.058322 | 116.00587189 | 31.32598662 | 26.9674 | 55666.2760069444 | 2011-04-15 06:37:27 | 55667.0258564815 | 2011-04-16 00:37:14 | 706003010 | 38.0779 | 40 | 38.0779 | 38.0779 | 0 | 38.0779 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.5276 | 37.5276 | 64.784 | 0 | PROCESSED | 57601.5103356482 | 2016-08-01 12:14:53 | 56058 | 2012-05-11 00:00:00 | 55690.9897685185 | 2011-05-09 23:45:16 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060004 | We propose a Suzaku observation of "Gamma-ray lobe" accociated with a FR-I/II radio galaxy NGC6251. This is the second discovery next to Cen-A lobe with Fermi-LAT above 100 MeV. Compared to huge angular extent of Cen-A (~10 degree), the lobe of NGC 6251 is comfortably fit within an XIS-FOV, but its physical size is almost the same as Cen-A(~Mpc). We can therefore estimate the total power accumulated in lobe with much less uncertainties, and pressure balance between non-thermal electrons and external thermal cluster medium, that may reveal possible contributions of hidden protons in the lobe. We propose a 40 ksec observation of NGC 6251 centered on the NW-lobe, with additional 20 ksec x 2 observations at "OFF-src" positions to improve the background estimate. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 6 | AO6 | SUZAKU OBSERVATION OF "GAMMA-RAY LOBE'' IN A RADIO GALAXY NGC6251 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706003010/ | Quick Look | ![]() |
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366 | NGC6251_LOBE_BGD2 | 245.3877 | 82.3337 | 246.650515 | 82.446813 | 101.124392 | 73.239187 | 115.79036875 | 31.61025625 | 299.99 | 55789.4176967593 | 2011-08-16 10:01:29 | 55789.6225 | 2011-08-16 14:56:24 | 706005020 | 11.178 | 10 | 11.178 | 11.178 | 0 | 11.178 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.788 | 9.788 | 17.6879 | 0 | PROCESSED | 57602.7824421296 | 2016-08-02 18:46:43 | 56173 | 2012-09-03 00:00:00 | 55805.1871527778 | 2011-09-01 04:29:30 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060004 | We propose a Suzaku observation of "Gamma-ray lobe" accociated with a FR-I/II radio galaxy NGC6251. This is the second discovery next to Cen-A lobe with Fermi-LAT above 100 MeV. Compared to huge angular extent of Cen-A (~10 degree), the lobe of NGC 6251 is comfortably fit within an XIS-FOV, but its physical size is almost the same as Cen-A(~Mpc). We can therefore estimate the total power accumulated in lobe with much less uncertainties, and pressure balance between non-thermal electrons and external thermal cluster medium, that may reveal possible contributions of hidden protons in the lobe. We propose a 40 ksec observation of NGC 6251 centered on the NW-lobe, with additional 20 ksec x 2 observations at "OFF-src" positions to improve the background estimate. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 6 | AO6 | SUZAKU OBSERVATION OF "GAMMA-RAY LOBE'' IN A RADIO GALAXY NGC6251 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706005020/ | Quick Look | ![]() |
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367 | SWIFT J0709.4-3559 | 107.3109 | -36.0226 | 106.863563 | -35.940797 | 116.901156 | -57.856606 | 247.327711 | -12.25710974 | 260.0142 | 55653.0945601852 | 2011-04-02 02:16:10 | 55655.0640393518 | 2011-04-04 01:32:13 | 706008010 | 81.1739 | 80 | 81.1739 | 81.1739 | 0 | 81.1739 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61.4621 | 61.4621 | 170.1239 | 2 | PROCESSED | 57601.393287037 | 2016-08-01 09:26:20 | 56037 | 2012-04-20 00:00:00 | 55670.2451967593 | 2011-04-19 05:53:05 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060030 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Previously, such studies have been limited to AGNs with low to intermediate luminosities. Here we propose to observe two of the most luminous AGNs in the latest BAT catalog to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 6 | AO6 | BROAD BAND SPECTRA OF HARD X-RAY SELECTED ULTRALUMINOUS AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706008010/ | Quick Look | ![]() |
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368 | PG 1322+659 | 200.9787 | 65.7065 | 200.558033 | 65.966727 | 149.375947 | 63.481771 | 117.62442893 | 51.08576313 | 141.5827 | 55892.4154050926 | 2011-11-27 09:58:11 | 55894.0862268518 | 2011-11-29 02:04:10 | 706018010 | 81.6869 | 80 | 81.7109 | 81.6869 | 0 | 81.7109 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 78.9168 | 78.9168 | 144.3439 | 2 | PROCESSED | 57603.9954513889 | 2016-08-03 23:53:27 | 56274 | 2012-12-13 00:00:00 | 55907.1929282407 | 2011-12-12 04:37:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060069 | Measurement of iron abundance in active galactic nuclei (AGN) relative to that of alpha-elements possesses potential of elucidating the cosmic chemical evolution, in particular, when the formation of the first stars initiated. However, it has been found that iron abundances estimated from FeII(opt) and FeII(UV) in the broad line region (BLR) do not agree and their ratio is dependent on the BLR cloud column densities. Thus, in order to derive precise AGN iron abundances, independent measurement of the BLR cloud column densities is required. Here we propose to obtain precise X-ray energy spectra of several AGNs, of which FeII(opt)/FeII(UV) values we have already measured. By combining the optical and X-ray spectra, we can estimate iron abundances of these targets more precisely than ever. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | HIROAKI SAMESHIMA | JAP | 6 | AO6 | X-RAY MEASUREMENTS OF COLUMN DENSITIES OF THE BROAD LINE REGION CLOUDS TO CONSTRAIN THE COSMIC CHEMICAL EVOLUTION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706018010/ | Quick Look | ![]() |
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369 | RX J1633+4718 | 248.3661 | 47.3315 | 248.006234 | 47.43491 | 228.796037 | 67.698232 | 73.56753068 | 42.5999019 | 136.9343 | 55939.8747337963 | 2012-01-13 20:59:37 | 55940.8307407407 | 2012-01-14 19:56:16 | 706027030 | 44.1271 | 40 | 44.1271 | 44.1271 | 0 | 44.1271 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38.9578 | 38.9578 | 82.592 | 0 | PROCESSED | 57604.3578703704 | 2016-08-04 08:35:20 | 56331 | 2013-02-08 00:00:00 | 55960.228587963 | 2012-02-03 05:29:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060089 | RX J1633+4718 was detected in the ROSAT all sky survey, later identified as a radio loud narrow line Seyfert 1 (NLS1) galaxy. The soft X-ray spectrum of this source was fitted with a blackbody with temperature of 32eV plus a flat power law component. The blackbody temperature is much lower than 100-200eV, typical soft X-ray excess commonly observed in NLS1. Since radio to UV continuum spectrum of this souce resembles those of blazars, the flat power law X-ray component is likely to be a jet origin. The jet might supress accretion corona, and thus the emission from the accretion disk might visible in its bare form. Suzaku observation of this source will give us X-ray spectrum above 2keV and CCD resolution spectrum below 2keV for the 1st time. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KIYOSHI HAYASHIDA | JAP | 6 | AO6 | X-RAY EMISSION FROM DISK AND JET AROUND A SMBH IN RX J1633+4718 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706027030/ | Quick Look | ![]() |
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370 | MRK 231 | 193.9205 | 56.8603 | 193.380984 | 57.130758 | 158.183244 | 55.13624 | 121.76268106 | 60.25831511 | 352.6128 | 55678.6054282407 | 2011-04-27 14:31:49 | 55682.3543402778 | 2011-05-01 08:30:15 | 706037010 | 197.5113 | 200 | 197.5113 | 197.5113 | 0 | 197.5113 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 191.7434 | 191.7434 | 323.8756 | 2 | PROCESSED | 57602.0326851852 | 2016-08-02 00:47:04 | 56065 | 2012-05-18 00:00:00 | 55697.4231597222 | 2011-05-16 10:09:21 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062008 | We propose the first Suzaku observation of the nearest low-ionization BAL quasar/ULIRG, i.e. MRK 231, for which we have recently reported the most clear-cut evidence for AGN-driven feedback onto the host galaxy cold molecular gas component. Our target exhibits an hard X-ray (> 15 keV) excess in a previous BeppoSAX/PDS spectrum, suggesting the presence of a heavily obscured quasar at the heart of this peculiar system. By exploiting the Suzaku unique broad-band spectral coverage, we aim at deriving the column density of the nuclear absorber and, in turn, the intrinsic luminosity of the quasar with unprecedented accuracy. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ENRICO PICONCELLI | EUR | 6 | AO6 | BROAD-BAND X-RAY SPECTROSCOPY OF THE NEAREST BAL QUASAR/ULIRG MARKARIAN 231 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706037010/ | Quick Look | ![]() |
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371 | LMC X-4 | 83.1886 | -66.3594 | 83.180179 | -66.392471 | 1.047321 | -87.279275 | 276.32297371 | -32.53740633 | 226.9086 | 54500.7929513889 | 2008-02-04 19:01:51 | 54501.0521875 | 2008-02-05 01:15:09 | 702036010 | 0 | 20 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 5.6729 | 5.6729 | 22.3779 | 1 | PROCESSED | 57541.4899537037 | 2016-06-02 11:45:32 | 54883 | 2009-02-21 00:00:00 | 54515.6401851852 | 2008-02-19 15:21:52 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021127 | We propose for a series of three 20ks observations of the binary X-ray pulsar LMC X-4. This source shows 13.5 s pulsations, a 1.4 d orbital period, and a long-period (~30 d) variability due to a warped, precessing accretion disk. The proposed analysis will use pulse-phase spectroscopy with XIS to explore changes in the X-ray pulses and spectra at three different phases in the disk precession. This work will give us a detailed picture of the accretion flow, particularly for the inner regions of the accretion disk that are illuminated by the X-rays from the neutron star. This project takes advantage of the strengths of the XIS, particularly its excellent spectral resolution, sufficient (1s) time resolution in Window mode, and wide PSF that limits pile-up effects. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RYAN HICKOX | USA | 2 | AO2 | SUPERORBITAL VARIATION OF LMC X-4: EXPLORING THE ACCRETION FLOW | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702036010/ | Quick Look | ![]() |
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372 | 4C+74.26 | 310.7114 | 75.111 | 310.85824 | 74.929178 | 50.846162 | 74.615216 | 108.98584774 | 19.50187948 | 247.6342 | 55888.5409027778 | 2011-11-23 12:58:54 | 55890.613275463 | 2011-11-25 14:43:07 | 706028010 | 101.4125 | 100 | 101.4125 | 101.4125 | 0 | 101.4125 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 117.8827 | 117.8827 | 179.0297 | 2 | PROCESSED | 57603.9949074074 | 2016-08-03 23:52:40 | 56269 | 2012-12-08 00:00:00 | 55901.2441203704 | 2011-12-06 05:51:32 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060101 | We propose the 120 ks observation of Broad Line Radio Galaxy 4C+74.26. The purpose is to estimate the angular momentum of the central super massive black hole from the broadness of Fe-K line. We study the spectral changes on spectra in details on the Fe-K lines and reflection hump in HXD-PIN band. We try to study the correlation between the radio intensity and black hole spins. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | HIROFUMI NODA | JAP | 6 | AO6 | STUSY OF BROAD IRON LINE OF 4C+74.26 TO ESTIMATE THE SPIN OF CENTRAL SUPER MASSIVE BLACK HOLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706028010/ | Quick Look | ![]() |
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373 | 1H0419-577 | 66.5116 | -57.211 | 66.267931 | -57.322556 | 29.331877 | -75.671402 | 266.99901337 | -41.98911345 | 55.5914 | 54306.2319328704 | 2007-07-25 05:33:59 | 54309.0835532407 | 2007-07-28 02:00:19 | 702041010 | 205.8628 | 200 | 205.8708 | 205.8708 | 0 | 205.8628 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 152.8317 | 152.8317 | 246.3578 | 2 | PROCESSED | 57539.3963888889 | 2016-05-31 09:30:48 | 54706 | 2008-08-28 00:00:00 | 54339.7211111111 | 2007-08-27 17:18:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021304 | A hotly debated question is whether Seyfert X-ray spectra are dominated by components that are blurred by strong gravitational effects close (< 20rg) to the central black hole. Models featuring either complex absorption or blurred disk spectra provide equally good parameterizations of the mean X-ray spectrum of many objects. To make progress with current instruments we require observations with a temporal baseline and flux that will allow us to look for key parameter correlations, as the two scenarios predict different time-dependent behavior. To that end, we propose a Suzaku observation of 1H0419-577, a target that exhibits a remarkable degree of spectral variability in the X-ray regime promising some definitive results in this important area. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TRACEY TURNER | USA | 2 | AO2 | HOW IMPORTANT IS STRONG RELATIVISTIC BLURRING IN SPECTRA OF SEYFERT GALAXIES? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702041010/ | Quick Look | ![]() |
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374 | NGC5548 | 214.4931 | 25.1252 | 213.926181 | 25.355393 | 201.995661 | 36.403773 | 31.92399813 | 70.49805067 | 305.6592 | 54275.9121643518 | 2007-06-24 21:53:31 | 54276.6918055556 | 2007-06-25 16:36:12 | 702042020 | 35.9152 | 30 | 35.9152 | 35.9152 | 0 | 35.9152 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33.175 | 33.175 | 67.3419 | 3 | PROCESSED | 57539.0421759259 | 2016-05-31 01:00:44 | 54695 | 2008-08-17 00:00:00 | 54322.4919675926 | 2007-08-10 11:48:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021307 | We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARTIN ELVIS | USA | 2 | AO2 | NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702042020/ | Quick Look | ![]() |
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375 | NGC7582 | 349.5634 | -42.322 | 348.875032 | -42.595557 | 331.740868 | -34.366673 | 348.21143031 | -65.69925686 | 64.738 | 54248.9237152778 | 2007-05-28 22:10:09 | 54249.7328587963 | 2007-05-29 17:35:19 | 702052020 | 28.769 | 25 | 28.769 | 28.769 | 0 | 28.769 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24.6824 | 24.6824 | 69.9059 | 0 | PROCESSED | 57538.7538541667 | 2016-05-30 18:05:33 | 54695 | 2008-08-17 00:00:00 | 54255.6928472222 | 2007-06-04 16:37:42 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021332 | We propose to perform 4 Suzaku observations of 25 ks each (for a total of 100 ks) of the bright Seyfert 2 galaxy,NGC 7582.The aim of this proposal is to measure the distance of the gas that absorbs the nuclear radiation, by analyzing the pattern of variability of its column density.NGC7582 is the ideal target for this kind of analysis, because it already showed large variations of the column density of the absorber between X-ray observations taken a few years apart.With the present proposal, we intend to probe a wider range of timescales, from a week to about six months, in order to measure the distance of the absorber from the nucleus. This measure is crucial to understand the nature of the absorber in type 2 objects and the validity of the torus paradigm. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARCO CHIABERGE | USA | 2 | AO2 | MEASURING THE DISTANCE OF THE ABSORBER IN NGC 7582 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702052020/ | Quick Look | ![]() |
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376 | 4C+74.26 | 310.5668 | 75.0616 | 310.712656 | 74.880312 | 50.693329 | 74.661974 | 108.92036641 | 19.50581044 | 289.6922 | 54401.4314467593 | 2007-10-28 10:21:17 | 54403.2606944444 | 2007-10-30 06:15:24 | 702057010 | 91.583 | 100 | 91.583 | 91.583 | 0 | 91.591 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 94.114 | 94.114 | 158.0298 | 1 | PROCESSED | 57540.3825925926 | 2016-06-01 09:10:56 | 54776 | 2008-11-06 00:00:00 | 54409.2446064815 | 2007-11-05 05:52:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021354 | We propose a 100 ks observation of the bright broad-line radio galaxy 4C+74.26. A previous 35 ks XMM-Newton observation of 4C+74.26 yielded the first indication of a relativistically broadened Fe K line in a radio-loud AGN as well as other typical AGN properties (e.g., a warm absorber). The long observation proposed here will allow a detailed investigation of the Fe K line profile and improve significantly on the previous observation by detecting the associated Compton reflection hump with the HXD/PIN instrument. Modeling of these features will allow the first accurate determination of the geometry and structure of the inner accretion disk in a radio-loud AGN, and hence provide invaluable information for modeling the physics of the disk/jet interaction. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | DAVID BALLANTYNE | USA | 2 | AO2 | A CLOSE LOOK AT 4C+74.26 WITH SUZAKU: FOCUSING IN ON THE DISK/JET INTERACTION | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702057010/ | Quick Look | ![]() |
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377 | RBS 1124 | 187.6975 | 70.7093 | 187.160497 | 70.985277 | 134.358757 | 62.072206 | 125.39855918 | 46.31993489 | 339.073 | 54204.9538078704 | 2007-04-14 22:53:29 | 54206.5786921296 | 2007-04-16 13:53:19 | 702114010 | 86.2284 | 88 | 86.2284 | 86.2284 | 0 | 86.2284 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 88.8555 | 88.8555 | 140.384 | 3 | PROCESSED | 57538.4340740741 | 2016-05-30 10:25:04 | 54744 | 2008-10-05 00:00:00 | 54210.6501851852 | 2007-04-20 15:36:16 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022019 | We propose a 70 ks observation of RBS 1124 (z=0.208). This is the X--ray brightest radio--quiet quasar (> 4e45 erg/s in the 2-10 keV band) from the ROSAT bright source catalogue. The expected number of counts (e.g. about 120,000 in just one FI XIS unit and about 11,000 in the HXD/PIN) will provide the best quality X-ray spectrum so far for such a high luminosity AGN. We will investigate the main X-ray spectral components shedding light on this extreme class of objects with unprecedented accuracy making full use of the Suzaku sensitivity across the whole band (XIS and HXD). | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GIOVANNI MINIUTTI | EUR | 2 | AO2 | REVEALING THE X-RAY EMISSION/ACCRETION PROCESSES IN THE VERY LUMINOUS RADIO-QUIET AND X-RAY BRIGHT QUASAR RBS 1124 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702114010/ | Quick Look | ![]() |
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378 | 3C 452 | 341.4131 | 39.7498 | 340.846907 | 39.486403 | 2.315539 | 43.172801 | 98.13461856 | -16.98917572 | 65.3539 | 54267.3964351852 | 2007-06-16 09:30:52 | 54268.8294444444 | 2007-06-17 19:54:24 | 702073010 | 66.68 | 53 | 66.696 | 66.68 | 0 | 66.696 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61.4487 | 61.4487 | 123.8018 | 3 | PROCESSED | 57538.9941550926 | 2016-05-30 23:51:35 | 54695 | 2008-08-17 00:00:00 | 54319.4923032407 | 2007-08-07 11:48:55 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021372 | The nature and even the existence of type II quasars is highly controversial. Due to their highly obscured nature, very hard (> 15 keV) observations are needed to probe their properties. With the 9-month SWIFT BAT all-sky AGN survey, detection of heavily obscured sources is now possible. Indeed, 6 type II quasars have been identified. Their properties, however, are a challenge to standard AGN models e.g., all but one of these sources are strong radio sources and several have optical spectra indicative of an un-absorbed source. We propose Suzaku observations of the 5 without broadband high signal to noise x-ray data to perform a detailed analysis of their x-ray properties and to understand their relationship to the lower luminosity well studied Seyfert IIs. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RICHARD MUSHOTZKY | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF SWIFT BAT TYPE II QUASARS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702073010/ | Quick Look | ![]() |
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379 | MCG+8-11-11 | 88.7233 | 46.5039 | 87.789525 | 46.495439 | 89.047199 | 23.067702 | 165.67352488 | 10.43795472 | 91.6485 | 54360.0736342593 | 2007-09-17 01:46:02 | 54362.2640509259 | 2007-09-19 06:20:14 | 702112010 | 98.7481 | 100 | 98.7481 | 98.7561 | 0 | 98.7641 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89.2138 | 89.2138 | 186.4387 | 1 | PROCESSED | 57540.0368055556 | 2016-06-01 00:53:00 | 54751 | 2008-10-12 00:00:00 | 54371.4963078704 | 2007-09-28 11:54:41 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022004 | We propose to observe with Suzaku for 100 ks one of the X-ray brightest AGN, the Seyfert 1 galaxy MCG+8-11-11, with the aim to measure the fraction of the reflection component and the iron abundance. Suzaku provides a unique opportunity to perform this kind of analysis, thanks to its broadband coverage. Moreover, the proposed observation will provide an extremely good spectrum, which will allow us to measure the iron line width, its Compton Shoulder and the ionization stage of iron. These three measurements will contribute to provide useful information on the nature of the iron line emitting material, its distance from the central Black Hole and the mass of the latter. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | STEFANO BIANCHI | EUR | 2 | AO2 | MCG+8-11-11: A BROADBAND SPECTRUM OF ONE OF THE X-RAY BRIGHTEST AGN | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702112010/ | Quick Look | ![]() |
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380 | IC4329A | 207.3319 | -30.3116 | 206.617739 | -30.063444 | 216.345797 | -17.778855 | 317.49719871 | 30.9175719 | 295.4804 | 54323.458599537 | 2007-08-11 11:00:23 | 54324.2127777778 | 2007-08-12 05:06:24 | 702113030 | 26.8959 | 25 | 26.8959 | 26.8959 | 0 | 26.8959 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23.8723 | 23.8723 | 65.1309 | 0 | PROCESSED | 57539.4615972222 | 2016-05-31 11:04:42 | 54730 | 2008-09-21 00:00:00 | 54347.7226041667 | 2007-09-04 17:20:33 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022009 | IC 4329A is the brightest known Seyfert 1 galaxy between ~2-30 keV (F(2-10 keV)~1-2e-10 erg/cm2s). With its clear warm absorber and reflection component, it is often taken as the prototypical Sey 1 galaxy. Its X-ray variability is strong enough (and on a sufficiently long time scale, ideal for Suzaku) to make multiple observations critical for probing the origin of the Compton reflection component, and to attempt measuring variations of the high energy cut-off. We thus propose 5x20 ks observations to monitor i) the correlated variability of the reflection continuum plus FeK line to primary continuum variations, and ii) the variations in the high-E cut-off, and their relation with the power-law, and iii) check the evidence for a blueshifted (v~0.1c) FeK absorption line at ~7.7 keV. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MASSIMO CAPPI | EUR | 2 | AO2 | SUZAKU MULTIPLE OBSERVATIONS OF IC4329A TO PROBE THE ORIGIN OF THE COMPTON REFLECTION COMPONENT AND HIGH-ENERGY CUT-OFF | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702113030/ | Quick Look | ![]() |
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381 | MRK 1073 | 48.7401 | 42.0969 | 47.912237 | 41.911835 | 57.846592 | 23.153427 | 149.47083071 | -13.26071681 | 81.0781 | 53949.235162037 | 2006-08-02 05:38:38 | 53949.3834722222 | 2006-08-02 09:12:12 | 701007010 | 3.4746 | 40 | 3.4746 | 3.4806 | 3.4786 | 3.4766 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 4.1358 | 4.1358 | 12.806 | 0 | PROCESSED | 57535.0684375 | 2016-05-27 01:38:33 | 54735 | 2008-09-26 00:00:00 | 54132.9684490741 | 2007-02-01 23:14:34 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010037 | We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YUICHI TERASHIMA | JAP | 1 | AO1 | COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701007010/ | Quick Look | ![]() |
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382 | SWIFT J2127.4+5654 | 322.001 | 56.878 | 321.622917 | 56.659223 | 3.253872 | 64.455644 | 97.78160785 | 4.29621592 | 243.6186 | 54443.0645023148 | 2007-12-09 01:32:53 | 54445.0487962963 | 2007-12-11 01:10:16 | 702122010 | 91.7304 | 88 | 0 | 91.7304 | 0 | 91.7304 | 0 | 2 | 0 | 2 | 1 | 0 | 0 | 89.3485 | 89.3485 | 171.3799 | 2 | PROCESSED | 57540.867974537 | 2016-06-01 20:49:53 | 55000 | 2009-06-18 00:00:00 | 54633.7130439815 | 2008-06-16 17:06:47 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022034 | We propose to observe with Suzaku two Narrow Line Seyfert 1 galaxies detected by SWIFT/BAT and INTEGRAL with a flux in excess of $10^{-11}$~erg~s$^{-1}$~cm$^{-2}$ in the HXD/PIN band for 70~ks each. These proposed observations provide rare high quality spectra of NLS1s above 10~keV. This will remove the spectral degeneracies inherent to limited bandpass analysis (such as that with XMM--Newton and Chandra) and the ambiguities between the different proposed models invoked to explain the unique spectral and variability properties of these most extreme class of high accretion rate sources (namely absorption, reflection, nature of the soft excess...). | EXTRAGALACTIC COMPACT SOURCES | 7 | C | GIOVANNI MINIUTTI | EUR | 2 | AO2 | HUNTING HARD-X-RAY-BRIGHT NLS1 GALAXIES FROM THE INTEGRAL CATALOGUE WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702122010/ | Quick Look | ![]() |
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383 | SWIFT J0911.2+4533 | 137.9062 | 45.5305 | 137.073312 | 45.735684 | 126.030873 | 27.898314 | 174.70874001 | 43.11152809 | 111.3983 | 54764.185787037 | 2008-10-25 04:27:32 | 54766.2105787037 | 2008-10-27 05:03:14 | 703008010 | 93.879 | 80 | 93.879 | 93.879 | 0 | 93.895 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80.2256 | 80.2256 | 174.9298 | 4 | PROCESSED | 57544.2883564815 | 2016-06-05 06:55:14 | 55148 | 2009-11-13 00:00:00 | 54782.4040625 | 2008-11-12 09:41:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030034 | The hard X-ray survey with Swift BAT have been finding various types of AGNs. Many buried AGNs with very low scattered X-rays have been discovered, for example. We propose to obtain broad band spectra of Compton-thin buried AGNs in the Swift sample. The data will be used to measure the amount of absoption in the direct and reflected emission and to constrain the structure of the obscuring matter around the AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YUICHI TERASHIMA | JAP | 3 | AO3 | THE STRUCTURE OF BURIED COMPTON-THIN AGNS DISCOVERED BY SWIFT | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703008010/ | Quick Look | ![]() |
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384 | MRK 110 | 141.3383 | 52.3497 | 140.469294 | 52.565715 | 125.649662 | 35.070751 | 164.91808924 | 44.3703784 | 110.1475 | 54406.3443055556 | 2007-11-02 08:15:48 | 54408.31625 | 2007-11-04 07:35:24 | 702124010 | 90.8712 | 100 | 90.8712 | 90.8792 | 0 | 90.8792 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86.5231 | 86.5231 | 170.3558 | 2 | PROCESSED | 57540.442037037 | 2016-06-01 10:36:32 | 54786 | 2008-11-16 00:00:00 | 54417.3880092593 | 2007-11-13 09:18:44 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 023012 | We request a 100 ks SUZAKU observation of Mrk 110 to quantify the accretion disk geometry in this high luminosity narrow line Seyfert 1 galaxy. This is an unique low mass AGN which shows an almost featureless X-ray continuum described by a two component Comptonization model. It has shown, based on an XMM-Newton data, energy dependent delays which are consistent with the idea of a Comptonized plasma confined within 10 Schwartzschild radius of the central black hole. The proposed long observation will provide high signal-to-noise hard X-ray data, thus allowing us to extend the observed delay to higher energies and also to quantify the high energy spectral parameters like cut-off energy and reflection parameters. This will help us to identify the accretion disk geometry in this source. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | ARIKKALA RAO | Gulab Dewangan | EUS | 2 | AO2 | PROBING THE ACCRETION DISK GEOMETRY IN THE TYPE I SEYFERT GALAXY MRK 110 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702124010/ | Quick Look | ![]() |
385 | Q0827+243 | 127.7159 | 24.1868 | 126.975524 | 24.355663 | 124.075193 | 5.096736 | 200.01721235 | 31.87611482 | 114.1438 | 54766.2156828704 | 2008-10-27 05:10:35 | 54767.3363310185 | 2008-10-28 08:04:19 | 703003010 | 48.2277 | 40 | 48.2277 | 48.2277 | 0 | 48.2277 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.3031 | 39.3031 | 96.8001 | 0 | PROCESSED | 57544.2665625 | 2016-06-05 06:23:51 | 54557 | 2008-04-01 00:00:00 | 54788.24125 | 2008-11-18 05:47:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030004 | We propose intensive Suzaku observations of 11 "VIP" blazars with 40ksec each, as a long-category project. We stress that all of the sources will be monitored simultaneously by GLAST (GeV), Swift XRT/UVOT (UV to X-ray), as well as ground-based radio-to-optical telescopes. We will obtain the broadband spectra and light-curves from 10^9 Hz to 10^25 Hz, which reveals for the first time the nature of gamma-loud blazars in their quiescent states. The proposed 40ksec x 11 Suzaku observations will allow us to investigate | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 3 | AO3 | REVEALING THE NATURE OF GAMMA-LOUD BLAZARS VIA SUZAKU/GLAST AND WORLD-WIDE GROUND-BASED OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703003010/ | Quick Look | ![]() |
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386 | 3C454.3 | 343.4943 | 16.1419 | 342.876691 | 15.875412 | 351.363443 | 21.32571 | 86.11034311 | -38.19103065 | 250.8076 | 54792.3878703704 | 2008-11-22 09:18:32 | 54793.6884143518 | 2008-11-23 16:31:19 | 703006010 | 46.9239 | 40 | 46.9239 | 46.9239 | 0 | 46.9239 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.344 | 43.344 | 112.3139 | 2 | PROCESSED | 57544.5029976852 | 2016-06-05 12:04:19 | 54557 | 2008-04-01 00:00:00 | 54811.7229050926 | 2008-12-11 17:20:59 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030004 | We propose intensive Suzaku observations of 11 "VIP" blazars with 40ksec each, as a long-category project. We stress that all of the sources will be monitored simultaneously by GLAST (GeV), Swift XRT/UVOT (UV to X-ray), as well as ground-based radio-to-optical telescopes. We will obtain the broadband spectra and light-curves from 10^9 Hz to 10^25 Hz, which reveals for the first time the nature of gamma-loud blazars in their quiescent states. The proposed 40ksec x 11 Suzaku observations will allow us to investigate | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 3 | AO3 | REVEALING THE NATURE OF GAMMA-LOUD BLAZARS VIA SUZAKU/GLAST AND WORLD-WIDE GROUND-BASED OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703006010/ | Quick Look | ![]() |
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387 | SWIFT J0959.5-2258 | 149.843 | -22.8716 | 149.261565 | -22.631568 | 161.273539 | -32.730158 | 259.02796733 | 24.98206567 | 303.2834 | 54635.9091087963 | 2008-06-18 21:49:07 | 54636.8148611111 | 2008-06-19 19:33:24 | 703013010 | 43.6634 | 40 | 43.6714 | 43.6794 | 0 | 43.6634 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.4061 | 42.4061 | 78.2379 | 0 | PROCESSED | 57542.8554861111 | 2016-06-03 20:31:54 | 55016 | 2009-07-04 00:00:00 | 54650.0591782407 | 2008-07-03 01:25:13 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030045 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe the remaining four Compton thick AGN candidates in the 2nd BAT catalog with Suzaku to make it complete. To resolve the degeneracy of spectral modeling to the XMM spectra of these sources, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 3 | AO3 | DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703013010/ | Quick Look | ![]() |
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388 | SWIFT J0501.9-3239 | 79.8743 | -32.7041 | 79.409754 | -32.754183 | 74.820458 | -55.614502 | 236.069923 | -32.60257079 | 297.9191 | 54567.6584259259 | 2008-04-11 15:48:08 | 54568.8788194444 | 2008-04-12 21:05:30 | 703014010 | 41.2985 | 40 | 41.2985 | 41.2985 | 0 | 41.2985 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36.4342 | 36.4342 | 105.4259 | 0 | PROCESSED | 57542.3107291667 | 2016-06-03 07:27:27 | 54953 | 2009-05-02 00:00:00 | 54580.5155208333 | 2008-04-24 12:22:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030045 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe the remaining four Compton thick AGN candidates in the 2nd BAT catalog with Suzaku to make it complete. To resolve the degeneracy of spectral modeling to the XMM spectra of these sources, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 3 | AO3 | DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703014010/ | Quick Look | ![]() |
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389 | SWIFT J0134.1-3625 | 23.4345 | -36.4661 | 22.87514 | -36.722141 | 4.413021 | -42.266283 | 261.71382804 | -77.05672525 | 34.1001 | 54606.6796180556 | 2008-05-20 16:18:39 | 54607.8390277778 | 2008-05-21 20:08:12 | 703016010 | 48.5116 | 40 | 48.5196 | 48.5116 | 0 | 48.5276 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.2927 | 41.2927 | 100.1498 | 0 | PROCESSED | 57542.6141898148 | 2016-06-03 14:44:26 | 54985 | 2009-06-03 00:00:00 | 54616.4068402778 | 2008-05-30 09:45:51 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030045 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe the remaining four Compton thick AGN candidates in the 2nd BAT catalog with Suzaku to make it complete. To resolve the degeneracy of spectral modeling to the XMM spectra of these sources, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 3 | AO3 | DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703016010/ | Quick Look | ![]() |
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390 | SWIFT J0444.1+2813 | 71.029 | 28.2793 | 70.24739 | 28.187015 | 73.273115 | 5.933796 | 172.68057795 | -11.38105828 | 85.0234 | 54719.7173958333 | 2008-09-10 17:13:03 | 54721.6306944445 | 2008-09-12 15:08:12 | 703021010 | 81.2986 | 80 | 81.2986 | 81.2986 | 0 | 81.2986 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 67.7654 | 67.7654 | 165.3039 | 0 | PROCESSED | 57543.831087963 | 2016-06-04 19:56:46 | 55148 | 2009-11-13 00:00:00 | 54780.4776736111 | 2008-11-10 11:27:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030124 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright, absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe two of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 3 | AO3 | BROAD BAND SPECTRA OF SWIFT/BAT SELECTED AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703021010/ | Quick Look | ![]() |
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391 | NGC3227 | 155.8766 | 19.8689 | 155.194036 | 20.122276 | 150.387342 | 9.143225 | 216.98457422 | 55.44588075 | 115.8562 | 54767.3422685185 | 2008-10-28 08:12:52 | 54768.8487731482 | 2008-10-29 20:22:14 | 703022010 | 58.9172 | 50 | 58.9172 | 58.9172 | 0 | 58.9172 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52.0337 | 52.0337 | 130.1478 | 1 | PROCESSED | 57544.2886689815 | 2016-06-05 06:55:41 | 54557 | 2008-04-01 00:00:00 | 54788.4566203704 | 2008-11-18 10:57:32 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031013 | We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARTIN ELVIS | USA | 3 | AO3 | NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703022010/ | Quick Look | ![]() |
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392 | NGC3227 | 155.8768 | 19.8689 | 155.194236 | 20.122276 | 150.38752 | 9.143295 | 216.98468368 | 55.44605831 | 113.2489 | 54782.1173032407 | 2008-11-12 02:48:55 | 54783.7293865741 | 2008-11-13 17:30:19 | 703022030 | 56.5715 | 50 | 56.5772 | 56.5852 | 0 | 56.5715 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50.2231 | 50.2231 | 139.2698 | 1 | PROCESSED | 57544.401724537 | 2016-06-05 09:38:29 | 54557 | 2008-04-01 00:00:00 | 54797.3603356482 | 2008-11-27 08:38:53 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031013 | We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARTIN ELVIS | USA | 3 | AO3 | NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703022030/ | Quick Look | ![]() |
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393 | NGC 4051 | 180.7984 | 44.5394 | 180.160059 | 44.817725 | 159.257872 | 40.347523 | 148.85547697 | 70.08163582 | 138.344 | 54776.3187847222 | 2008-11-06 07:39:03 | 54782.1112731482 | 2008-11-12 02:40:14 | 703023010 | 274.5305 | 340 | 274.5305 | 274.5305 | 0 | 274.5305 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 220.1993 | 220.1993 | 441.4488 | 3 | PROCESSED | 57544.5089930556 | 2016-06-05 12:12:57 | 54557 | 2008-04-01 00:00:00 | 54795.7746527778 | 2008-11-25 18:35:30 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031014 | The powerful combination of Principal Components Analysis with time-resolved X-ray spectroscopy of Seyfert AGN has shown strong evidence that changes in a complex absorber are the origin of much of observed AGN spectral and flux variability. Large column, high ionization layers of gas may arise in a disk wind, representing a significant new, and possibly dominant, component, responsible for shaping the X-ray spectrum of AGN. The broad bandpass of Suzaku gives us a unique opportunity to model primary and reflected continua and the effects of variable absorbing zones, and test wind and other models. We propose a long 340 ks exposure on the NLSy1 NGC 4051 whose large amplitude of variability and well-studied complex absorption will test those models to the limit | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TRACEY TURNER | USA | 3 | AO3 | DECONSTRUCTING SEYFERT SPECTRA - TIME FOR A PARADIGM SHIFT? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703023010/ | Quick Look | ![]() |
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394 | PDS 456 | 262.0806 | -14.2617 | 261.369911 | -14.221632 | 262.221213 | 8.965556 | 10.39448289 | 11.16711992 | 96.2509 | 56359.500150463 | 2013-03-08 12:00:13 | 56362.375162037 | 2013-03-11 09:00:14 | 707035030 | 108.3397 | 450 | 108.3477 | 108.3477 | 0 | 108.3397 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 94.226 | 94.226 | 248.3918 | 3 | PROCESSED | 57610.7991435185 | 2016-08-10 19:10:46 | 56018 | 2012-04-01 00:00:00 | 56373.5603125 | 2013-03-22 13:26:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071431 | PDS 456 is the most luminous nearby (z=0.184) AGN, more typical of quasars at high redshift. A 2007 Suzaku observation resolved iron K absorption at 9 keV in the QSO frame, moving at near relativistic velocities (0.25c). A follow-up 2011 observation was highly absorbed and showed a direct response of the iron K absorber to a decrease in the ionizing flux, while the harder photons lag behind the soft, by 10^4 secs. We propose to monitor the remarkable spectral variability and outflow from PDS 456, through a deep 450ks Suzaku observation. We wish to:- (i) quantify the time lags and determine the location of the reprocessor, (ii) determine the origin and timescale of the absorber variability and (iii) measure the hard X-ray variability from a Compton thick absorber in PDS 456. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | JAMES REEVES | USA | 7 | AO7 | VARIABILITY AND REVERBERATION OF THE QUASAR WIND IN PDS 456 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707035030/ | Quick Look | ![]() |
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395 | SN 2005KD | 60.8552 | 71.7156 | 59.486745 | 71.577171 | 76.353108 | 49.655537 | 136.84988934 | 14.24754739 | 218.8053 | 54568.8904976852 | 2008-04-12 21:22:19 | 54570.0348842593 | 2008-04-14 00:50:14 | 703025010 | 51.6289 | 50 | 51.6289 | 51.6369 | 0 | 51.6449 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 63.5726 | 63.5726 | 98.8639 | 1 | PROCESSED | 57542.2950694444 | 2016-06-03 07:04:54 | 54947 | 2009-04-26 00:00:00 | 54581.1998842593 | 2008-04-25 04:47:50 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031241 | Supernovae (SNe) 2005kd and 2006jd are some of the brightest SNe ever detected in X-rays. The high X-ray luminosities (>E41 erg/s) are the results of the SN shock interacting with dense material in the environment of the SNe. We propose one Suzaku observation of each SN to obtain high-quality spectra that will be used to measure the temperature of the forward and reverse shock and to establish the rate of decline in comparison with existing Swift, Chandra and XMM-Newton data. The data will further be used to measure the circumstellar matter density and mass-loss rate of the progenitors to probe the nature of the SN progenitors. Our science objectives rely on Suzaku's uniqueness, i.e. the large collecting area, good spectral resolution, and the high sensitivity in the hard X-ray band. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | STEFAN IMMLER | USA | 3 | AO3 | SUZAKU OBSERVATIONS OF X-RAY BRIGHT SUPERNOVAE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703025010/ | Quick Look | ![]() |
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396 | MRK421 | 166.0521 | 38.1644 | 165.357194 | 38.434126 | 151.189395 | 29.439264 | 179.96763761 | 64.99940635 | 318.3733 | 53853.2821412037 | 2006-04-28 06:46:17 | 53854.2711226852 | 2006-04-29 06:30:25 | 701024010 | 41.4709 | 40 | 41.4789 | 41.4709 | 41.4789 | 41.4789 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 34.7033 | 34.7033 | 85.4301 | 1 | PROCESSED | 57533.6140162037 | 2016-05-25 14:44:11 | 54394 | 2007-10-21 00:00:00 | 53908.0343055556 | 2006-06-22 00:49:24 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010157 | We propose to conduct a series of simultaneous X-ray/VHE (very high energy) gamma-ray observations of northern TeV Blazars (Mkn 421, Mkn 501, 1ES1218+304, and 1ES1426+428) with Suzaku XIS and HXD in conjunction with the HESS (High Energy Stereoscopic System) and MAGIC ground based gamma-ray observatories. The goal of these observations is to study the spectral energy distribution of these highly variable objects for the first time simultaneously in the soft to hard X-ray (0.3 keV-100 keV) | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | SIMULTANEOUS X-RAY/VHE GAMMA-RAY OBSERVATIONS OF NORTHERN BLAZARS WITH SUZAKU AND HESS/MAGIC | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701024010/ | Quick Look | ![]() |
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397 | MRK 348 | 12.1911 | 31.9636 | 11.514938 | 31.691174 | 24.328489 | 24.485278 | 122.27104531 | -30.90471809 | 71.8836 | 54645.9325694444 | 2008-06-28 22:22:54 | 54648.0591203704 | 2008-07-01 01:25:08 | 703029010 | 87.4614 | 80 | 88.5334 | 87.4614 | 0 | 88.5334 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 78.5504 | 78.5504 | 183.7239 | 0 | PROCESSED | 57542.9708333333 | 2016-06-03 23:18:00 | 55031 | 2009-07-19 00:00:00 | 54664.7845601852 | 2008-07-17 18:49:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031322 | X-ray observations of Seyfert 2 have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by the AGN Unification Scheme. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (80 ksec each) of three bright Compton-thin Seyfert 2 galaxies, selected from the Swift/BAT survey, with a hard X-ray flux exceeding 9e-11cgs, to form a flux-limited sample. The unprecedented bandpass of Suzaku offers a unique tool to investigate the X-ray emission of these sources, allowing us to put strong constraints on the reprocessing matter in Seyfert 2s. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | VALENTINA BRAITO | USA | 3 | AO3 | THE NATURE OF THE X-RAY ABSORBER IN SEYFERT 2 GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703029010/ | Quick Look | ![]() |
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398 | PKS 0326-288 | 52.1551 | -28.6965 | 51.63485 | -28.868348 | 39.555316 | -45.73648 | 224.90475513 | -55.39691379 | 250.3682 | 55226.8889699074 | 2010-01-30 21:20:07 | 55228.3266087963 | 2010-02-01 07:50:19 | 704039010 | 58.0237 | 60 | 58.0238 | 58.0237 | 0 | 58.0237 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 49.6247 | 49.6247 | 124.1859 | 3 | PROCESSED | 57550.4794560185 | 2016-06-11 11:30:25 | 55616 | 2011-02-24 00:00:00 | 55249.7586805556 | 2010-02-22 18:12:30 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041413 | We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195~keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log($L_x$) $> 45.5$~ergs~sec$^{-1}$) absorbed tyoe II QSOs in the local universe and the most ripe for study with suzaku. 3C~332 is believed to be Compton-thick as suggested by chandra observations, and the newly discovered source SWIFT~J2344.6-4233 at a redshift of $z=0.6$ is the most luminous object in the BAT sample with log($L_x$) $=46.5$~ergs~sec$^{-1}$. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | WAYNE BAUMGARTNER | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704039010/ | Quick Look | ![]() |
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399 | 3C 332 | 244.4239 | 32.3632 | 243.942335 | 32.484407 | 233.11322 | 52.57597 | 52.6372471 | 45.34839384 | 292.5008 | 55051.0341782407 | 2009-08-08 00:49:13 | 55052.4655092593 | 2009-08-09 11:10:20 | 704038010 | 59.8339 | 60 | 59.8339 | 59.8339 | 0 | 59.8339 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.0491 | 46.0491 | 123.652 | 0 | PROCESSED | 57548.1132407407 | 2016-06-09 02:43:04 | 55437 | 2010-08-29 00:00:00 | 55067.2557986111 | 2009-08-24 06:08:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041413 | We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195~keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log($L_x$) $> 45.5$~ergs~sec$^{-1}$) absorbed tyoe II QSOs in the local universe and the most ripe for study with suzaku. 3C~332 is believed to be Compton-thick as suggested by chandra observations, and the newly discovered source SWIFT~J2344.6-4233 at a redshift of $z=0.6$ is the most luminous object in the BAT sample with log($L_x$) $=46.5$~ergs~sec$^{-1}$. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | WAYNE BAUMGARTNER | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704038010/ | Quick Look | ![]() |
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400 | Q0940-1050 | 145.7249 | -11.0726 | 145.114895 | -10.843374 | 152.028873 | -23.330401 | 246.39011763 | 30.43738638 | 275.7617 | 54616.2125578704 | 2008-05-30 05:06:05 | 54617.1321064815 | 2008-05-31 03:10:14 | 703040010 | 32.3623 | 28 | 32.3623 | 32.3623 | 0 | 32.3623 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.7776 | 26.7776 | 79.4378 | 1 | PROCESSED | 57542.689212963 | 2016-06-03 16:32:28 | 54999 | 2009-06-17 00:00:00 | 54633.6981828704 | 2008-06-16 16:45:23 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031334 | Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GEORGE CHARTAS | USA | 3 | AO3 | A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703040010/ | Quick Look | ![]() |
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401 | PKS 0528+134 | 82.7307 | 13.5905 | 82.023508 | 13.553568 | 82.834667 | -9.669991 | 191.31463869 | -10.98486414 | 89.0231 | 54736.1098611111 | 2008-09-27 02:38:12 | 54741.6752777778 | 2008-10-02 16:12:24 | 703048010 | 203.4574 | 200 | 203.4654 | 203.4654 | 0 | 203.4574 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 135.3629 | 135.3629 | 443.8619 | 4 | PROCESSED | 57544.2063888889 | 2016-06-05 04:57:12 | 55148 | 2009-11-13 00:00:00 | 54780.7843287037 | 2008-11-10 18:49:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031345 | We propose a Suzaku observation of bright gamma-ray blazar PKS 0528+134, to be conducted jointly with GLAST, radio, and optical telescopes. This observation was accepted in the previous AO, but was not conducted due to GLAST launch delays. The goal is to obtain time-resolved broadband spectra. The X-ray and gamma-ray fluxes are known to be rapidly variable, but the information regarding the correlation between the X-ray and gamma-ray flux is limited. Such detailed spectral and variability studies are crucial to discriminate between different radiation scenarios responsible for production of X-rays and gamma-rays, and to constrain the matter content and by extension, the formation process of the jet, dissipation of the jet energy, and energization of the radiating particles. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GRZEGORZ MADEJSKI | USA | 3 | AO3 | SUZAKU AND GLAST OBSERVATIONS OF PKS 0528+134 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703048010/ | Quick Look | ![]() |
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402 | 3C120 | 68.298 | 5.3556 | 67.633455 | 5.25115 | 67.433074 | -16.401934 | 190.3728125 | -27.39468757 | 237.4583 | 53782.5602199074 | 2006-02-16 13:26:43 | 53783.5876967593 | 2006-02-17 14:06:17 | 700001020 | 41.5545 | 160 | 41.5545 | 41.5545 | 41.5545 | 41.5545 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 36.8461 | 36.8461 | 88.772 | 2 | PROCESSED | 57533.0172685185 | 2016-05-25 00:24:52 | 54247 | 2007-05-27 00:00:00 | 54041.2956365741 | 2006-11-02 07:05:43 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001003 | Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 0 | SWG | BROAD-BAND MONITORING OF 3C120 IN VARIOUS ACCRETING STATES | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700001020/ | Quick Look | ![]() |
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403 | 3C120 | 68.2979 | 5.3541 | 67.633361 | 5.249649 | 67.432732 | -16.403401 | 190.37414386 | -27.39561637 | 262.5053 | 53796.9456828704 | 2006-03-02 22:41:47 | 53797.8606365741 | 2006-03-03 20:39:19 | 700001040 | 40.9051 | 160 | 40.9131 | 40.9211 | 40.9211 | 40.9051 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 40.3118 | 40.3118 | 79.0459 | 0 | PROCESSED | 57533.1408912037 | 2016-05-25 03:22:53 | 54247 | 2007-05-27 00:00:00 | 54041.627025463 | 2006-11-02 15:02:55 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001003 | Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 0 | SWG | BROAD-BAND MONITORING OF 3C120 IN VARIOUS ACCRETING STATES | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700001040/ | Quick Look | ![]() |
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404 | NGC 5506 | 213.312 | -3.2124 | 212.663098 | -2.97888 | 212.190832 | 9.596053 | 339.14600253 | 53.80603682 | 287.3743 | 53955.6875578704 | 2006-08-08 16:30:05 | 53957.003900463 | 2006-08-10 00:05:37 | 701030010 | 47.7531 | 150 | 47.7531 | 47.7531 | 47.7531 | 47.7531 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 41.0973 | 41.0973 | 113.7259 | 2 | PROCESSED | 57535.2578587963 | 2016-05-27 06:11:19 | 54695 | 2008-08-17 00:00:00 | 54116.2715740741 | 2007-01-16 06:31:04 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011312 | NGC 5506 is one of the brightest Seyferts in the X-ray sky, the second brightest in the PIN bandpass. Obscuring gas has kept the true nature of this AGN secret until recent optical and infrared studies have unmasked the narrow-line-seyfert 1 nucleus. With this knowledge, NGC 5506 is the perfect candidate for confirming the generality of a new result based on a recent XMM observation of Mkn 766, ie that the ionized component of Fe K emission originates from the inner accretion disk and closely tracks the hard X-ray continuum flux. This immediately gives us the ionization-state and size-scale of the inner disk. We request a 150 ks Suzaku observation to see whether a similar result holds for NGC 5506 and, by extension, may be a property of NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TRACEY TURNER | USA | 1 | AO1 | SUZAKU STUDY OF THE BRIGHTEST NARROW LINE SEYFERT 1: NGC 5506 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701030010/ | Quick Look | ![]() |
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405 | PKS1258-321 | 195.0396 | -32.3625 | 194.354396 | -32.09316 | 206.904154 | -23.820406 | 305.06853624 | 30.47306853 | 293.0551 | 55027.0059259259 | 2009-07-15 00:08:32 | 55027.6050231482 | 2009-07-15 14:31:14 | 704007010 | 28.4607 | 20 | 28.4607 | 28.7327 | 0 | 28.7274 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 24.0275 | 24.0275 | 51.7559 | 0 | PROCESSED | 57547.8136921296 | 2016-06-08 19:31:43 | 55406 | 2010-07-29 00:00:00 | 55040.1188657407 | 2009-07-28 02:51:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040049 | We propose the first X-ray follow-up observations of 4 gamma-ray bright Seyferts and starburst galaxy, recently discovered by Fermi gamma-ray space telescope. The detection of GeV emission provides new evidence for relativistic jets in radio-quiet AGNs, but steep gamma-ray spectrum as well as an exotic spectral energy distribution (where GeV flux is 2-4 orders of magnitude brighter than radio) indicates that non-thermal emission is relatively weak, and less enhanced compared to radio-loud AGNs. Throughout multiwavelength observations including Suzaku and Fermi satellites, we will investigate the jet power, accretion rate and line intensity of these new comers (i.e., gamma-loud Seyferts) towards the unification scheme of radio-loud and radio-quiet AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF GAMMA-LOUD SEYFERTS AND STARBURST GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704007010/ | Quick Look | ![]() |
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406 | CENTAURUS_A | 201.3281 | -43.0649 | 200.594745 | -42.804861 | 217.131954 | -31.381221 | 309.48077241 | 19.37569293 | 303.3465 | 55057.3798148148 | 2009-08-14 09:06:56 | 55059.1051388889 | 2009-08-16 02:31:24 | 704018030 | 55.9442 | 50 | 55.9522 | 55.9442 | 0 | 55.9442 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.4915 | 46.4915 | 149.0478 | 3 | PROCESSED | 57548.1889699074 | 2016-06-09 04:32:07 | 55434 | 2010-08-26 00:00:00 | 55068.1674768518 | 2009-08-25 04:01:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040085 | We propose to observe a nearby radio galaxy Centaurus A (Cen A) in order to search for non-thermal X-ray emission associated with a mis-alighned jet. Recently TeV gamma-ray was detected from M87 and nonthermal X-ray emission was detected from 3C120 with Suzaku, where they are not a blazar and harbor a mis-alighned jet. COMPTEL and EGRET reported a hint of gamma-ray emission from Cen A, but it has not been established. So far, only Seyfert-like thermal-Compoton powerlaw has been detected from Cen A. By taking advantage of Suzaku capability, we study a temporal spectral variation to extract nonthermal emission by considering a different variability time scale of accretion disk component and jet one, as demonstrated for 3C120 with Suzaku. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YASUSHI FUKAZAWA | JAP | 4 | AO4 | SEARCH FOR NON-THERMAL X-RAY EMISSION FROM A NEARBY RADIO GALAXY CENTAURUS A | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704018030/ | Quick Look | ![]() |
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407 | EMS0992 | 230.2572 | -3.8213 | 229.602576 | -3.642087 | 228.859181 | 14.124861 | 358.15856297 | 42.46037658 | 113.2867 | 55593.7858564815 | 2011-02-01 18:51:38 | 55594.1841898148 | 2011-02-02 04:25:14 | 705026010 | 18.979 | 20 | 18.979 | 18.979 | 0 | 18.979 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 14.832 | 14.832 | 34.3939 | 0 | PROCESSED | 57600.8001388889 | 2016-07-31 19:12:12 | 55973 | 2012-02-16 00:00:00 | 55607.0454976852 | 2011-02-15 01:05:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050126 | Fermi Gamma-ray Space Telescope has detected a lot of unidentified GeV sources in high latitude. Among these, we focus on five Fermi unIDs whose error circles contain ROSAT faint X-ray sources and propose an X-ray follow-up observation with Suzaku. From an X-ray spectral and variability information, we identify these objects, as well as find new class of GeV emitters. We also aim to study emission and particle acceleration mechanism of these objects. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YASUYUKI TANAKA | JAP | 5 | AO5 | SEARCH FOR X-RAY COUNTERPARTS OF FERMI HIGH-LATITUDE UNIDENTIFIED GEV SOURCES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705026010/ | Quick Look | ![]() |
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408 | IRAS08572+3915 | 135.0664 | 39.0091 | 134.264876 | 39.204772 | 126.11779 | 21.048672 | 183.47368885 | 40.96543811 | 300.022 | 53839.0903240741 | 2006-04-14 02:10:04 | 53840.7752199074 | 2006-04-15 18:36:19 | 701053010 | 77.1974 | 75 | 77.2214 | 77.1974 | 77.2134 | 77.2214 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 62.3339 | 62.3339 | 145.4999 | 9 | PROCESSED | 57533.486875 | 2016-05-25 11:41:06 | 54401 | 2007-10-28 00:00:00 | 53906.2114699074 | 2006-06-20 05:04:31 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011344 | Ultraluminous infrared galaxies (ULIRGs) produce the energy outputs of quasars with nearly all the power emerging in the far-IR via reprocessing of optical, UV, and X-ray radiation by dust. The ultimate nuclear power source, be it AGN or compact starburst, of ULIRGs has been the focus of much debate since their discovery with the IRAS mission. While observations with Spitzer are unlocking the secrets of many nearby ULIRGs, some have nuclei that are apparently so obscured as to be optically thick even in the mid-IR. We have chosen three local ULIRGs, IRAS 08572+3915, IRAS15250+3609, and IRAS20551-4250 that are IR-bright, yet highly obscured for deep Suzaku observations to search for the tell-tale signs of a buried AGN: hard X-ray emission behind significant column densities of HI gas. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | SARAH GALLAGHER | USA | 1 | AO1 | ULTRAHARD X-RAY CASE STUDIES OF ULIRGS WITH DEEP SILICATE ABSORPTION | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701053010/ | Quick Look | ![]() |
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409 | MKN 841 | 225.9811 | 10.3761 | 225.377197 | 10.570593 | 220.178092 | 26.525473 | 11.09749436 | 54.61837916 | 292.433 | 54304.6970949074 | 2007-07-23 16:43:49 | 54306.218912037 | 2007-07-25 05:15:14 | 701084020 | 50.9253 | 50 | 50.9253 | 50.9333 | 0 | 50.9333 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.6556 | 47.6556 | 131.4738 | 2 | PROCESSED | 57539.3432060185 | 2016-05-31 08:14:13 | 54800 | 2008-11-30 00:00:00 | 54339.5240277778 | 2007-08-27 12:34:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012028 | We propose to perform two 50 ks Suzaku observations of Mkn 841, at an interval of a few months, in order to elucidate the origin of its different X-ray components. Strong soft excess and complex iron line profile are known to be present in this source and recent XMM observations reveal their extreme and puzzling spectral and temporal behaviors. Nevertheless, while the XMM observations help to better constrain their natures, their physical interpretation strongly suffer from the lack of data above 10 keV. Two dedicated Suzaku observations will provide crucial information for our understanding of these components, allowing 1) to obtain high S/N and striclty simultaneous broad band X-ray spectra from the soft X-ray up to the reflection bump and 2) to study their spectral variability behaviors | EXTRAGALACTIC COMPACT SOURCES | 7 | B | PIERRE-OLIVIER PETRUCCI | EUR | 1 | AO1 | PROBING THE ORIGIN OF THE STRONG SOFT EXCESS AND PUZZLING REFLECTION COMPONENTS IN MKN 841 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701084020/ | Quick Look | ![]() |
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410 | MRK 352 | 14.9991 | 31.7575 | 14.31506 | 31.488197 | 26.597079 | 23.289939 | 125.05610732 | -31.07894727 | 255.5628 | 55202.4718402778 | 2010-01-06 11:19:27 | 55203.6009143518 | 2010-01-07 14:25:19 | 704025010 | 45.6717 | 40 | 45.6877 | 45.6717 | 0 | 45.6872 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.3693 | 22.3693 | 97.5358 | 1 | PROCESSED | 57550.0955439815 | 2016-06-11 02:17:35 | 55602 | 2011-02-10 00:00:00 | 55235.27125 | 2010-02-08 06:30:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041402 | The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | LISA WINTER | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704025010/ | Quick Look | ![]() |
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411 | QSO 1828+487 | 277.4042 | 48.7379 | 277.077989 | 48.702797 | 285.744941 | 71.774201 | 77.22058509 | 23.48843965 | 218.1356 | 56983.2742592593 | 2014-11-22 06:34:56 | 56983.6771875 | 2014-11-22 16:15:09 | 709026010 | 14.1766 | 15 | 14.1766 | 14.1766 | 0 | 14.1766 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8008912037 | 2016-08-16 19:13:17 | 57442 | 2016-02-24 00:00:00 | 57076.4104861111 | 2015-02-23 09:51:06 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092023 | EXTRAGALACTIC COMPACT SOURCES | 7 | C | MARCUS LANGEJAHN | EUR | 9 | AO9 | false | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709026010/ | Quick Look | ![]() |
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412 | EMS1341 | 301.2467 | 70.0571 | 301.259152 | 69.912683 | 31.029252 | 78.090273 | 102.85714193 | 19.4440121 | 233.7732 | 55527.303275463 | 2010-11-27 07:16:43 | 55527.7619675926 | 2010-11-27 18:17:14 | 705027010 | 23.0668 | 20 | 23.0668 | 23.0668 | 0 | 23.0668 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 21.5055 | 21.5055 | 39.6239 | 0 | PROCESSED | 57554.2240856482 | 2016-06-15 05:22:41 | 55903 | 2011-12-08 00:00:00 | 55537.0214814815 | 2010-12-07 00:30:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050126 | Fermi Gamma-ray Space Telescope has detected a lot of unidentified GeV sources in high latitude. Among these, we focus on five Fermi unIDs whose error circles contain ROSAT faint X-ray sources and propose an X-ray follow-up observation with Suzaku. From an X-ray spectral and variability information, we identify these objects, as well as find new class of GeV emitters. We also aim to study emission and particle acceleration mechanism of these objects. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YASUYUKI TANAKA | JAP | 5 | AO5 | SEARCH FOR X-RAY COUNTERPARTS OF FERMI HIGH-LATITUDE UNIDENTIFIED GEV SOURCES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705027010/ | Quick Look | ![]() |
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413 | SWIFT J0904.3+5538 | 136.117 | 55.5749 | 135.191467 | 55.77395 | 120.650833 | 36.933195 | 161.50516347 | 40.6960792 | 282.0039 | 54949.092025463 | 2009-04-28 02:12:31 | 54949.700162037 | 2009-04-28 16:48:14 | 704027010 | 41.9438 | 40 | 41.9438 | 41.9438 | 0 | 41.9438 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 35.8838 | 35.8838 | 52.5359 | 1 | PROCESSED | 57546.4424537037 | 2016-06-07 10:37:08 | 55343 | 2010-05-27 00:00:00 | 54973.440474537 | 2009-05-22 10:34:17 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041402 | The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | LISA WINTER | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704027010/ | Quick Look | ![]() |
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414 | UGC 6728 | 176.2197 | 79.6106 | 175.467594 | 79.888182 | 114.113262 | 63.856037 | 126.64092866 | 37.03371002 | 285.5693 | 54988.5646759259 | 2009-06-06 13:33:08 | 54989.5125925926 | 2009-06-07 12:18:08 | 704029010 | 49.0039 | 40 | 49.0039 | 49.0039 | 0 | 49.0039 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.5347 | 41.5347 | 81.8839 | 0 | PROCESSED | 57547.4998726852 | 2016-06-08 11:59:49 | 55364 | 2010-06-17 00:00:00 | 54998.3390740741 | 2009-06-16 08:08:16 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041402 | The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | LISA WINTER | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704029010/ | Quick Look | ![]() |
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415 | MCG-2-58-22 | 346.1839 | -8.6878 | 345.532632 | -8.95779 | 343.915361 | -2.560866 | 64.09176202 | -58.7610593 | 247.1128 | 55167.9420486111 | 2009-12-02 22:36:33 | 55170.9356365741 | 2009-12-05 22:27:19 | 704032010 | 138.9688 | 130 | 139.0088 | 138.9688 | 0 | 139.0088 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 105.4957 | 105.4957 | 258.6277 | 2 | PROCESSED | 57549.8017361111 | 2016-06-10 19:14:30 | 55553 | 2010-12-23 00:00:00 | 55187.5510763889 | 2009-12-22 13:13:33 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041404 | We propose a 130 ks Suzaku long-look to study the Fe K emission complex of the Seyfert 1.5 AGN MCG--2-58-22, which has the unique combination of being X-ray bright, ``bare'' (i.e., lacking a strong ionized absorber), and possibly hosting both a truncated accretion disk and ionized circumnuclear material. We aim to accurately constrain the geometry and ionization state of the accreting circumnuclear material of this likely low-Compton reflection source by resolving the Fe K alpha line and constraining its origin, which may likely be a truncated thin disk, and verifying a previous claim of emission from H-like Fe. We will also determine the origin of this object's soft excess. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | ALEX MARKOWITZ | USA | 4 | AO4 | A SUZAKU OBSERVATION OF MCG--2-58-22: A TRUNCATED OR IONIZED ACCRETION DISK? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704032010/ | Quick Look | ![]() |
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416 | MRK1018 | 31.5471 | -0.2351 | 30.907355 | -0.473179 | 29.3057 | -12.234469 | 159.73232745 | -57.66458833 | 73.6945 | 55015.0121759259 | 2009-07-03 00:17:32 | 55016.0939699074 | 2009-07-04 02:15:19 | 704044010 | 43.9014 | 40 | 43.9094 | 43.9014 | 0 | 43.9094 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.6884 | 37.6884 | 93.4578 | 5 | PROCESSED | 57547.7689467593 | 2016-06-08 18:27:17 | 55395 | 2010-07-18 00:00:00 | 55027.1070023148 | 2009-07-15 02:34:05 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041414 | We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | EZEQUIEL TREISTER | USA | 4 | AO4 | THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704044010/ | Quick Look | ![]() |
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417 | NGC 3718 | 173.2341 | 53.1118 | 172.54734 | 53.387989 | 147.276263 | 44.880657 | 146.87581124 | 60.21394242 | 142.7392 | 55128.8497800926 | 2009-10-24 20:23:41 | 55130.255775463 | 2009-10-26 06:08:19 | 704048010 | 59.8882 | 60 | 59.9202 | 59.8882 | 0 | 59.9202 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52.4392 | 52.4392 | 121.4599 | 0 | PROCESSED | 57548.9845138889 | 2016-06-09 23:37:42 | 55507 | 2010-11-07 00:00:00 | 55141.3212384259 | 2009-11-06 07:42:35 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041415 | The SWIFT BAT hard (14-195 KeV) survey is performing the first unbiased hard X-ray survey of the entire sky with follow-up observations with the Swift XRT to fully identify the sample. In this survey we have found two very low luminosity nearby hard X-ray sources which show little, if any, evidence for nuclear activity in the optical or UV band, and have very low apparent Eddington ratios. We propose Suzaku observations of these objects to determine whether there is an X-ray spectral signature of a low Eddington ratio, as predicted if these objects are indeed in a radiatively inefficient accretion flow. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RICHARD MUSHOTZKY | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF NGC4138 AND NGC3718 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704048010/ | Quick Look | ![]() |
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418 | NGC 3997 | 179.448 | 25.2646 | 178.805338 | 25.542926 | 168.8766 | 22.834867 | 218.72362191 | 77.82883353 | 305.585 | 56439.4793981482 | 2013-05-27 11:30:20 | 56441.452974537 | 2013-05-29 10:52:17 | 708002010 | 87.1383 | 80 | 87.1383 | 87.1383 | 0 | 87.1383 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 83.0504 | 83.0504 | 170.508 | 2 | PROCESSED | 57611.4399305556 | 2016-08-11 10:33:30 | 56816 | 2014-06-08 00:00:00 | 56450.866724537 | 2013-06-07 20:48:05 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080015 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Here we propose to observe two of the lowest luminosity BAT AGNs to measure the amount of the reflection component with unpreceded accuracy, a key parameter to determine the contribution of Compton thick AGNs to the X-ray background. We will also study how the torus structure of low luminosity AGNs differs from that of more luminous AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 8 | AO8 | BROAD BAND SPECTRA OF HARD X-RAY SELECTED VERY LOW LUMINOSITY AGNS AND THEIR TORUS STRUCTURE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708002010/ | Quick Look | ![]() |
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419 | NGC 1365 | 53.3909 | -36.1409 | 52.913513 | -36.307906 | 36.789839 | -53.036651 | 237.95774893 | -54.60665436 | 30.5416 | 55374.0284143518 | 2010-06-27 00:40:55 | 55377.9834606482 | 2010-06-30 23:36:11 | 705031010 | 151.6134 | 450 | 151.6294 | 151.6134 | 0 | 151.6214 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 123.2422 | 123.2422 | 341.6577 | 2 | PROCESSED | 57552.5171064815 | 2016-06-13 12:24:38 | 55287 | 2010-04-01 00:00:00 | 55434.2469444445 | 2010-08-26 05:55:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051112 | We propose 3 observations (~4 days each) of the Seyfert galaxy NGC 1365, at 2-week intervals. We aim to use eclipses to unambiguously identify the broad Fe K line, examine variability of the HXD/PIN excess, and to search for changes in the physical properties of the ionized absorber in this bright, nearby AGN. Shorter observations of this galaxy with XMM-Newton, Chandra and Suzaku showcase several remarkable physical traits: (1) FeXXV and FeXXVI K-shell absorption lines (the highest s/n detection so far among AGN), (2) rapidly varying cold absorption, (3) a highly significant relativistic Fe K emission line, and (4) a factor ~4 excess flux at high energies. The proposed observations will provide legacy spectra for what is arguably the single most physically-revealing obscured AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | LAURA BRENNEMAN | USA | 5 | AO5 | A LONG LOOK AT NGC 1365: DISC TOMOGRAPHY, IONIZED ABSORPTION AND HIGH ENERGY EXCESS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705031010/ | Quick Look | ![]() |
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420 | NGC 6251 | 248.2903 | 82.5391 | 249.646931 | 82.638978 | 99.623854 | 73.274498 | 115.75265542 | 31.17774629 | 182.5432 | 55532.2390625 | 2010-12-02 05:44:15 | 55534.0341898148 | 2010-12-04 00:49:14 | 705039010 | 87.0706 | 85 | 87.0706 | 87.0706 | 0 | 87.0706 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 75.8074 | 75.8074 | 155.0879 | 1 | PROCESSED | 57554.3327546296 | 2016-06-15 07:59:10 | 55931 | 2012-01-05 00:00:00 | 55565.375162037 | 2011-01-04 09:00:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051411 | We propose an 85-ks Suzaku observation of NGC 6251, the brightest example of a low-excitation radio galaxy (LERG). We have previously suggested that LERGs violate conventional AGN unification schemes: they may lack an obscuring torus and are likely to accrete in a radiatively inefficient manner, with almost all of the energy released by the accretion process being channeled into powerful jets. However, Suzaku observations at low and high energies are needed to test this model directly. We will use the XIS and HXD to search for the signatures of accretion-related X-ray emission: (1) the 6.4 keV Fe Ka line, (2) heavily absorbed X-ray emission, and (3) the >10 keV Compton reflection bump. These results will have important implications for models of accretion and feedback in radio-loud AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | DANIEL EVANS | USA | 5 | AO5 | A DIRECT TEST OF THE NUCLEAR X-RAY DICHOTOMY IN RADIO-LOUD AGN | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705039010/ | Quick Look | ![]() |
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421 | PDS 456 | 262.0809 | -14.2537 | 261.370252 | -14.213634 | 262.221057 | 8.97356 | 10.4015562 | 11.17111116 | 96.1694 | 55636.625462963 | 2011-03-16 15:00:40 | 55639.3564930556 | 2011-03-19 08:33:21 | 705041010 | 125.5272 | 130 | 125.5352 | 125.5272 | 0 | 125.5327 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 100.875 | 100.875 | 235.9276 | 2 | PROCESSED | 57601.2862615741 | 2016-08-01 06:52:13 | 56050 | 2012-05-03 00:00:00 | 55677.3183564815 | 2011-04-26 07:38:26 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051421 | PDS 456 is the most luminous nearby AGN and a recent Suzaku observation revealed a powerful ionized outflow moving at 0.25c with kinetic output matching the quasar bolometric luminosity. Above 10 keV the HXD appears to show a factor 3 rise in flux over the XIS, implying that a high column density absorber (>10^24 cm^-2) is located close to the X-ray source in order to partially covers its emission. We propose to study the remarkable X-ray absorption towards PDS 456 through two further 130 ks Suzaku observations. This will:-i) confirm the nature of the hard excess, ii) determine whether spectral variability can be explained by variable partial covering and iii) enable us to measure the imprint of the ionized outflow at Fe K with unprecedented accuracy. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TRACEY TURNER | USA | 5 | AO5 | THE COMPTON-THICK OUTFLOW IN THE TYPE I QSO PDS 456 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705041010/ | Quick Look | ![]() |
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422 | SPT-CLJ2344-4243 | 356.1816 | -42.7169 | 355.522212 | -42.994645 | 336.755816 | -37.082735 | 339.63806237 | -69.34299043 | 226.1467 | 56605.0105902778 | 2013-11-09 00:15:15 | 56607.4106597222 | 2013-11-11 09:51:21 | 708012010 | 86.2043 | 80 | 86.2043 | 86.2043 | 0 | 86.2043 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80.0289 | 80.0289 | 207.3477 | 3 | PROCESSED | 57613.3115625 | 2016-08-13 07:28:39 | 56383 | 2013-04-01 00:00:00 | 56653.7570949074 | 2013-12-27 18:10:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080071 | SPT-CLJ2344-4243 is a distant (z=0.596) extremely luminous (Lx=8x10^45erg/s) cluster with a strong cooling flow rate of 3820 Msun/year. The central galaxy of the cluster shows huge star formation activity and has a luminous (Lx=3x10^45 erg/s) AGN. According to the paper by McDonald et al. (2012) and Fe I detection by our analysis of the archived data of Suzaku, this AGN is likely to be a type 2 QSO, for which we don ft know any other example situated at the center of a cluster. We are observing a special phase of co-evolution of a cluster, its central galaxy, and SMBH at its center. We propose to perform 80ks x 4 times observations with Suzaku to estimate SMBH mass in this system through X-ray variability and to get Fe I line detection with higher confidence. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | SHUTARO UEDA | JAP | 8 | AO8 | CO-EVOLUTION IN SMBH, GALAXY AND CLUSTERS; SUZAKU OBSERVATION OF A TYPE 2 QSO AT THE CENTER OF SPT-CLJ2344-4243 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708012010/ | Quick Look | ![]() |
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423 | MKN 590 | 33.6446 | -0.7698 | 33.006332 | -1.002435 | 31.137585 | -13.457637 | 163.50990373 | -56.94179664 | 250.4206 | 55584.0937615741 | 2011-01-23 02:15:01 | 55585.6252083333 | 2011-01-24 15:00:18 | 705043010 | 61.5547 | 150 | 61.5867 | 61.5547 | 0 | 61.5707 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 55.1599 | 55.1599 | 132.2758 | 0 | PROCESSED | 57600.7325 | 2016-07-31 17:34:48 | 55965 | 2012-02-08 00:00:00 | 55599.1867824074 | 2011-02-07 04:28:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051433 | We propose a 150 ks Suzaku long-look to study the Compton reflection component, soft excess, ionized emission and possible ionized reflection of the Seyfert 1.2 AGN Mkn 590, which has an unobscured line of sight or "bare nucleus" and as of yet unquantified reflection. We aim to accurately constrain the geometry of the circumnuclear material and determine the ionization states of both the Compton-thin and Compton-thick material surrounding the black hole by studying the origin of the soft excess, determining the likelihood of ionized reflection and accurately measuring the intensity of neutral, H-like and He-like Fe emission lines. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | ELIZABETH RIVERS | USA | 5 | AO5 | QUANTIFYING THE COMPTON REFLECTION AND IONIZED EMISSION IN MKN 590 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705043010/ | Quick Look | ![]() |
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424 | NGC 2992 | 146.4352 | -14.2714 | 145.83373 | -14.040218 | 154.019094 | -26.058459 | 249.66741784 | 28.82528499 | 102.6298 | 53680.5956481482 | 2005-11-06 14:17:44 | 53681.5850925926 | 2005-11-07 14:02:32 | 700005010 | 37.5029 | 120 | 37.5029 | 38.7568 | 37.518 | 37.715 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 32.073 | 32.073 | 85.4859 | 1 | PROCESSED | 57527.9475231482 | 2016-05-19 22:44:26 | 54247 | 2007-05-27 00:00:00 | 54037.5593518518 | 2006-10-29 13:25:28 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001013 | NGC 2992 is a nearby Seyfert 1.9 galaxy showing long-term (20 yrs) large amplitude (factor of 20) variability. This object showed switching between Compton-thick and -thin. Recent RXTE monitoring has shown that this object is highly variable on shorter time scales (2 weeks). We propose three Suzaku observations to monitor the variability of absorption column, broad band continuum shape, and Fe line intensity to understand the cause of the remarkable variability. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YUICHI TERASHIMA | JAP | 0 | SWG | THE SPECTRAL VARIABILITY IN NGC 2992: FE-LINE, REFLECTION, AND COMPTON-THIN/THICK SWITCHING | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700005010/ | Quick Look | ![]() |
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425 | NGC 4945 | 196.3459 | -49.5284 | 195.615808 | -49.260687 | 217.044106 | -38.699389 | 305.256234 | 13.28040137 | 283.285 | 55381.636087963 | 2010-07-04 15:15:58 | 55382.6765856482 | 2010-07-05 16:14:17 | 705047010 | 39.0737 | 40 | 39.0817 | 39.0817 | 0 | 39.0737 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 34.0751 | 34.0751 | 89.8719 | 1 | PROCESSED | 57552.4706481482 | 2016-06-13 11:17:44 | 55770 | 2011-07-28 00:00:00 | 55404.2681134259 | 2010-07-27 06:26:05 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051442 | We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GUIDO RISALITI | USA | 5 | AO5 | HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705047010/ | Quick Look | ![]() |
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426 | NGC 4945 | 196.3265 | -49.5207 | 195.596537 | -49.252961 | 217.025208 | -38.698833 | 305.24375345 | 13.28878787 | 296.6587 | 55403.0670717593 | 2010-07-26 01:36:35 | 55404.1745717593 | 2010-07-27 04:11:23 | 705047030 | 40.3266 | 40 | 40.3426 | 40.3266 | 0 | 40.3426 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.6182 | 34.6182 | 95.6358 | 0 | PROCESSED | 57552.7156134259 | 2016-06-13 17:10:29 | 55780 | 2011-08-07 00:00:00 | 55414.0832407407 | 2010-08-06 01:59:52 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051442 | We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GUIDO RISALITI | USA | 5 | AO5 | HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705047030/ | Quick Look | ![]() |
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427 | 3C78 | 47.1071 | 4.1138 | 46.452233 | 3.923143 | 45.835066 | -12.996467 | 174.85308943 | -44.51284685 | 84.4195 | 55793.5846990741 | 2011-08-20 14:01:58 | 55795.7502430556 | 2011-08-22 18:00:21 | 706013010 | 97.0122 | 100 | 97.0122 | 97.0122 | 0 | 97.0122 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 85.9075 | 85.9075 | 187.0878 | 0 | PROCESSED | 57602.928275463 | 2016-08-02 22:16:43 | 56176 | 2012-09-06 00:00:00 | 55806.3891435185 | 2011-09-02 09:20:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060046 | We propose to observe two radio galaxies 3C78 and PKS0625-354 which were detected by the Fermi gamma-ray satellte survey during the 1st year, in order to investigate the X-ray emission more precisely than ever. In the case of jet emission, we can constrain the jet parameter well from the multi-wavelength spectrum and obtain the jet kinetic energy. In the case of disk emission, we can obtain the jet to disk energy ratio. This observation will enable us to obtain the jet parameters of these galaxies and compare them with others. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YASUSHI FUKAZAWA | JAP | 6 | AO6 | ORIGIN OF THE X-RAY EMISSION OF GAMAM-RAY RADIO GALAXIES 3C78 AND PKS0625-354 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706013010/ | Quick Look | ![]() |
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428 | NGC6251_LOBE_BGD1 | 247.6537 | 82.9256 | 249.113456 | 83.028127 | 99.179697 | 72.901441 | 116.18672095 | 31.0445068 | 26.9624 | 55667.0269328704 | 2011-04-16 00:38:47 | 55667.4328125 | 2011-04-16 10:23:15 | 706004010 | 18.822 | 20 | 18.8357 | 18.822 | 0 | 18.8356 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 18.9572 | 18.9572 | 35.0659 | 1 | PROCESSED | 57601.5125694445 | 2016-08-01 12:18:06 | 56058 | 2012-05-11 00:00:00 | 55691.0888194444 | 2011-05-10 02:07:54 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060004 | We propose a Suzaku observation of "Gamma-ray lobe" accociated with a FR-I/II radio galaxy NGC6251. This is the second discovery next to Cen-A lobe with Fermi-LAT above 100 MeV. Compared to huge angular extent of Cen-A (~10 degree), the lobe of NGC 6251 is comfortably fit within an XIS-FOV, but its physical size is almost the same as Cen-A(~Mpc). We can therefore estimate the total power accumulated in lobe with much less uncertainties, and pressure balance between non-thermal electrons and external thermal cluster medium, that may reveal possible contributions of hidden protons in the lobe. We propose a 40 ksec observation of NGC 6251 centered on the NW-lobe, with additional 20 ksec x 2 observations at "OFF-src" positions to improve the background estimate. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 6 | AO6 | SUZAKU OBSERVATION OF "GAMMA-RAY LOBE'' IN A RADIO GALAXY NGC6251 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706004010/ | Quick Look | ![]() |
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429 | HESS J1943+213 | 295.9916 | 21.301 | 295.448325 | 21.18018 | 303.194 | 41.793482 | 57.76229591 | -1.30331963 | 246.7107 | 55875.6293055556 | 2011-11-10 15:06:12 | 55876.6015393518 | 2011-11-11 14:26:13 | 706007010 | 38.8815 | 40 | 38.8815 | 38.8895 | 0 | 38.8895 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.313 | 35.313 | 83.972 | 1 | PROCESSED | 57603.7570601852 | 2016-08-03 18:10:10 | 56256 | 2012-11-25 00:00:00 | 55890.6970833333 | 2011-11-25 16:43:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060028 | A new point-like source HESS J1943+213 has been detected at TeV energies at the position coinciding with the unidentified hard X-ray objects IGR J19443+2117. All the available observational constraints favor an identification of HESS J1943+213 as a BL Lac at redshift z>0.14. If correct, this would be the first time an AGN is discovered serendipitously from TeV observations in the Galactic Plane. It would be also the most extreme BL Lac known, with the persistent synchrotron continuum extending up to the observed energies >100 keV. A good quality broad X-ray spectrum is needed to confirm the blazar association and the extreme character of the peculiar object HESS J1943+213. Here we argue that a relatively moderate Suzaku exposure of 40 ksec will enable us to obtain such a spectrum. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | LUKASZ STAWARZ | JAP | 6 | AO6 | PECULIAR UNIDENTIFIED TEV SOURCE HESS J1943+213 IN THE GALACTIC PLANE: EXTREME BLAZAR OR SOMETHING ELSE? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706007010/ | Quick Look | ![]() |
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430 | SWIFT J1310.9-5553 | 197.6868 | -55.8722 | 196.924529 | -55.606324 | 222.251055 | -43.758692 | 305.6577855 | 6.89731776 | 290.4478 | 55761.4489467593 | 2011-07-19 10:46:29 | 55762.6432523148 | 2011-07-20 15:26:17 | 706009010 | 82.785 | 80 | 82.793 | 82.785 | 0 | 82.785 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 67.5081 | 67.5081 | 103.1779 | 1 | PROCESSED | 57602.6323263889 | 2016-08-02 15:10:33 | 56213 | 2012-10-13 00:00:00 | 55845.247662037 | 2011-10-11 05:56:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060030 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Previously, such studies have been limited to AGNs with low to intermediate luminosities. Here we propose to observe two of the most luminous AGNs in the latest BAT catalog to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 6 | AO6 | BROAD BAND SPECTRA OF HARD X-RAY SELECTED ULTRALUMINOUS AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706009010/ | Quick Look | ![]() |
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431 | 3C 98 | 59.723 | 10.4395 | 59.038566 | 10.297703 | 59.781896 | -9.882185 | 179.82925767 | -31.05249617 | 81.003 | 55812.5811342593 | 2011-09-08 13:56:50 | 55815.280787037 | 2011-09-11 06:44:20 | 706015010 | 101.144 | 100 | 101.144 | 101.144 | 0 | 101.144 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89.8389 | 89.8389 | 233.214 | 3 | PROCESSED | 57603.1723611111 | 2016-08-03 04:08:12 | 56218 | 2012-10-18 00:00:00 | 55851.4528356482 | 2011-10-17 10:52:05 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060055 | Whether radio-loud and radio-quiet AGN may be unified under one model is still open to debate. The most important limitation in such work is that jet beaming swamps nuclear emission, so we must study powerful radio sources which are not affected by this bias. These are the Narrow Line Radio Galaxies (NLRGs). Heavy obscuration means that their primary emission is visible only above 10 keV. 3C 98 is an important member of the NLRG class because its hard band power dominates the full radio to X-ray core luminosity. We propose a 100 ks observation of this source with Suzaku to detect the core continuum emission and reflection above 10 keV. 3C~98 is one of few NLRGs for which we can expect to model (rather than just detect) the hard X-ray flux, and hence use it for testing unification schemes. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | POSHAK GANDHI | JAP | 6 | AO6 | HARD X-RAY EMISSION AND REFLECTION IN RADIO GALAXIES: 3C 98 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706015010/ | Quick Look | ![]() |
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432 | 1FGL J0103.1+4840 | 15.7305 | 48.657 | 15.006375 | 48.388615 | 36.058904 | 38.14189 | 124.88749892 | -14.17113818 | 69.2705 | 55753.0127430556 | 2011-07-11 00:18:21 | 55755.0002199074 | 2011-07-13 00:00:19 | 706025010 | 84.3622 | 80 | 84.3622 | 84.3622 | 0 | 84.3622 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79.727 | 79.727 | 171.6957 | 2 | PROCESSED | 57602.5903935185 | 2016-08-02 14:10:10 | 56148 | 2012-08-09 00:00:00 | 55778.4339814815 | 2011-08-05 10:24:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060084 | In this proposal, we'd like to make a suggestion of 2 "steady" unassociated Fermi-LAT gamma-ray sources with Suzaku. 2-year Fermi-LAT observation detected 2412 sources, but 1194 sources are still unassociated. Proposed objects are located at high Galactic latitude, and selected not likely to be associated with blazar(AGN) and pulsar. These lightcurves do not show the significant temporal variability. To confirm their stability, we checked Test Statistic Value of 1FGL and 2-year Fermi observation. Deep Observation with Suzaku (1FGLJ0103: 80ks, 1FGL1946:40ks) is expected to reveal the nature of these unassociated objects, or at least impose strict limits at 2-10keV. Of course, it is necessary that multi-wavelength observation. We'll plan to arrange tie-ups with other wavelength researcher. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | KOTO MAEDA | JAP | 6 | AO6 | SUZAKU OBSERVATION OF "STEADY" UNASSOCIATED FERMI-LAT GAMMA-RAY SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706025010/ | Quick Look | ![]() |
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433 | RX J1633+4718 | 248.3647 | 47.3332 | 248.004849 | 47.436616 | 228.791999 | 67.699433 | 73.56993988 | 42.60070523 | 133.9355 | 55962.6778240741 | 2012-02-05 16:16:04 | 55963.7502430556 | 2012-02-06 18:00:21 | 706027040 | 45.4834 | 40 | 45.4834 | 45.4834 | 0 | 45.4834 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.3113 | 40.3113 | 92.6459 | 0 | PROCESSED | 57604.5712152778 | 2016-08-04 13:42:33 | 56345 | 2013-02-22 00:00:00 | 55978.5479282407 | 2012-02-21 13:09:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060089 | RX J1633+4718 was detected in the ROSAT all sky survey, later identified as a radio loud narrow line Seyfert 1 (NLS1) galaxy. The soft X-ray spectrum of this source was fitted with a blackbody with temperature of 32eV plus a flat power law component. The blackbody temperature is much lower than 100-200eV, typical soft X-ray excess commonly observed in NLS1. Since radio to UV continuum spectrum of this souce resembles those of blazars, the flat power law X-ray component is likely to be a jet origin. The jet might supress accretion corona, and thus the emission from the accretion disk might visible in its bare form. Suzaku observation of this source will give us X-ray spectrum above 2keV and CCD resolution spectrum below 2keV for the 1st time. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KIYOSHI HAYASHIDA | JAP | 6 | AO6 | X-RAY EMISSION FROM DISK AND JET AROUND A SMBH IN RX J1633+4718 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706027040/ | Quick Look | ![]() |
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434 | SMC X-1 | 19.2772 | -73.44 | 18.945719 | -73.703155 | 312.351206 | -66.472298 | 300.41207357 | -43.56242986 | 167.9636 | 55825.1720949074 | 2011-09-21 04:07:49 | 55825.6536805556 | 2011-09-21 15:41:18 | 706030070 | 18.1239 | 18 | 18.2772 | 18.2852 | 0 | 18.1239 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 18.3687 | 18.3687 | 41.5959 | 0 | PROCESSED | 57603.2202662037 | 2016-08-03 05:17:11 | 56218 | 2012-10-18 00:00:00 | 55851.4509027778 | 2011-10-17 10:49:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JOSEPH NEILSEN | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030070/ | Quick Look | ![]() |
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435 | SMC X-1 | 19.2766 | -73.4376 | 18.945062 | -73.700756 | 312.356716 | -66.471322 | 300.41185267 | -43.56483062 | 244.987 | 55907.8985069444 | 2011-12-12 21:33:51 | 55908.2709722222 | 2011-12-13 06:30:12 | 706030090 | 17.3055 | 18 | 17.4079 | 17.4079 | 0 | 17.3055 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.413 | 18.413 | 32.1719 | 0 | PROCESSED | 57604.1197685185 | 2016-08-04 02:52:28 | 56289 | 2012-12-28 00:00:00 | 55920.9743981482 | 2011-12-25 23:23:08 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JOSEPH NEILSEN | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030090/ | Quick Look | ![]() |
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436 | H1821+643 | 275.4676 | 64.3592 | 275.403785 | 64.332814 | 318.33431 | 86.843842 | 94.01912066 | 27.4276768 | 65.0012 | 56398.4117013889 | 2013-04-16 09:52:51 | 56402.5419328704 | 2013-04-20 13:00:23 | 708037010 | 246.5839 | 400 | 246.5839 | 246.5919 | 0 | 246.5999 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 251.0273 | 251.0273 | 356.8299 | 0 | PROCESSED | 57611.1526273148 | 2016-08-11 03:39:47 | 56383 | 2013-04-01 00:00:00 | 56425.7059606482 | 2013-05-13 16:56:35 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081436 | H1821+643 (z=0.297) is not "just another quasar". This luminous active galactic nucleus (AGN) is an extremely rare example of a powerful quasar at the center of a rich, cooling-core cluster of galaxies. As such, it may represent a key evolutionary stage in the complex interplay between AGN and the core regions of the intracluster medium (ICM). Our analysis of archival XMM-Newton data has found evidence for a relativistically broad iron line. Here, we build on this request deep (400ks) Suzaku spectroscopy of H1821+643 to (1) measure the spin of this supermassive black hole and (2) search for powerful highly ionized outflows. In addition to measuring spin in the most luminous and distant object yet, this will enable us to test key predictions of recent models for AGN feedback. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | CHRISTOPHER REYNOLDS | USA | 8 | AO8 | THE BLACK HOLE SPIN AND IONIZED OUTFLOWS IN THE COOLING-FLOW QUASAR H1821+643 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708037010/ | Quick Look | ![]() |
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437 | NGC 4593 | 189.9132 | -5.341 | 189.26831 | -5.066485 | 191.201043 | -0.986248 | 297.48043001 | 57.40595243 | 111.8998 | 57021.7640856482 | 2014-12-30 18:20:17 | 57025.333287037 | 2015-01-03 07:59:56 | 709014050 | 145.2819 | 30 | 145.2819 | 145.3032 | 0 | 145.2899 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5760069445 | 2016-08-17 13:49:27 | 57415 | 2016-01-28 00:00:00 | 57049.4542939815 | 2015-01-27 10:54:11 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090097 | In the AO-8 cycle, we proposed six X-ray and optical simultaneous observations of type I Seyfert galaxy NGC 3516, and now obtaining a good correlation between those wavelengths. In the observations, we confirmed that a hard X-ray primary component (HXPC) found in Noda et al. (2013) was dominant, and its variation is well correlated with an optical one. To verify the probability that a variation of HXPC in other Seyfert also correlates with that in its optical, we propose six X-ray and optical simultaneous observations of NGC 4593, which has an X-ray spectrum dominated by HXPC as well as NGC 3516 in 2013. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 9 | AO9 | X-RAY AND OPTICAL SIMULTANEOUS OBSERVATIONS OF TYPICAL TYPE I SEYFERT NGC 4593 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709014050/ | Quick Look | ![]() |
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438 | NGC 1566 | 65.0038 | -54.9403 | 64.723209 | -55.058612 | 32.065014 | -73.361775 | 264.31301386 | -43.39149342 | 351.3031 | 56066.0671759259 | 2012-05-19 01:36:44 | 56067.2738310185 | 2012-05-20 06:34:19 | 707002010 | 72.791 | 80 | 72.791 | 72.791 | 0 | 72.791 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71.9581 | 71.9581 | 104.2239 | 2 | PROCESSED | 57605.4671875 | 2016-08-05 11:12:45 | 56442 | 2013-05-30 00:00:00 | 56076.0434606482 | 2012-05-29 01:02:35 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070003 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Previously, such studies have been limited to AGNs with intermediate to high luminosities. Here we propose to observe two of the lowest luminosity AGNs in the latest BAT catalog to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 7 | AO7 | BROAD BAND SPECTRA OF HARD X-RAY SELECTED LOW LUMINOSITY AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707002010/ | Quick Look | ![]() |
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439 | ARK 120 | 79.0439 | -0.2064 | 78.404432 | -0.260846 | 78.068932 | -23.195412 | 201.74563913 | -21.16237248 | 274.9546 | 54191.755162037 | 2007-04-01 18:07:26 | 54193.905150463 | 2007-04-03 21:43:25 | 702014010 | 100.8635 | 100 | 100.8635 | 100.8635 | 0 | 100.8635 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95.3121 | 95.3121 | 185.7439 | 1 | PROCESSED | 57538.0955324074 | 2016-05-30 02:17:34 | 54744 | 2008-10-05 00:00:00 | 54200.5657060185 | 2007-04-10 13:34:37 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020035 | We propose to obtain the broad-band spectra of the bright Seyfert 1 Ark 120 with Suzaku. Since Ark 120 shows no strong absorption features in its X-ray spectrum, we can cleanly measure the shape of the continuum and Fe K line without introducing any ambiguity caused by absorption along the line of sight. The spectrum will be used to test the diskline hypothesis in Seyferts and to study the fundamental processes producing broad band spectra of AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YUICHI TERASHIMA | JAP | 2 | AO2 | THE ORIGIN OF THE BROAD FE LINE IN THE SEYFERT 1 ARK 120 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702014010/ | Quick Look | ![]() |
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440 | ESO 511-G030 | 214.8452 | -26.6475 | 214.125784 | -26.417987 | 221.40413 | -12.023995 | 326.22882256 | 32.21510552 | 286.6511 | 56128.5082523148 | 2012-07-20 12:11:53 | 56128.7501388889 | 2012-07-20 18:00:12 | 707023010 | 5.7461 | 270 | 5.7461 | 5.7541 | 0 | 5.7621 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3.9886 | 3.9886 | 20.8879 | 0 | PROCESSED | 57606.6388194444 | 2016-08-06 15:19:54 | 56646 | 2013-12-20 00:00:00 | 56214.9581944445 | 2012-10-14 22:59:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071413 | The study of "bare" Seyfert 1 AGN is essential to measure the true properties of the inner regions of the accretion disk. The nearby Seyfert ESO 511-G30 is a prime candidate for fulfilling this role due to its broad Fe K component and lack of any intrinsic warm absorption. It is also one of the X-ray brightest bare Seyferts featured in the Swift 58 month BAT catalogue as yet unobserved with Suzaku. We propose a 270 ks Suzaku observation of ESO 511-G30 to unambiguously constrain the properties of the accretion disk and subsequently the black hole spin. In addition, the HXD data will allow us to measure the Compton reflection hump, while the excellent soft X-ray spectral resolution of XIS will allow the origin of the soft excess to be determined. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JAMES REEVES | USA | 7 | AO7 | MEASURING THE ACCRETION DISK AND BLACK HOLE PROPERTIES OF ESO 511-G30 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707023010/ | Quick Look | ![]() |
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441 | PG 1404+226 | 211.5943 | 22.4043 | 211.013582 | 22.642135 | 200.388612 | 32.841534 | 21.50519934 | 72.36517417 | 124.2434 | 56284.2179398148 | 2012-12-23 05:13:50 | 56286.1272453704 | 2012-12-25 03:03:14 | 707026010 | 80.2969 | 80 | 80.3129 | 80.2969 | 0 | 80.3049 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.5848 | 70.5848 | 164.9457 | 1 | PROCESSED | 57608.3815972222 | 2016-08-08 09:09:30 | 56687 | 2014-01-30 00:00:00 | 56320.7751157407 | 2013-01-28 18:36:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071419 | We propose a 80 ks observation of a NLS galaxy, PG1404+226, with Suzaku/XIS to investigate the physical conditions of extreme absorbers known as the ultra-fast-outflows (UFOs; v/c~0.1-0.2) of variable resonant absorption features from many ions (e.g. Ne IX, Ne X, Mg XII and S XVI) in the soft X-ray band (~0.5-3.5 keV), and we propose the first Suzaku observation of this object to (i) independently confirm/refute the previous claims of the presence of these UFOs including a potential detection of Fe K-shell absorbers, (ii) examine their variabilities and compare the outflow properties at low and high XIS-flux states, (iii) compare its outflow rate and kinetic power with those in other AGN UFOs, and (iv) utilize a high-quality Suzaku data to improve our MHD disk-wind model. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | KEIGO FUKUMURA | USA | 7 | AO7 | PROBING THE ULTRA-FAST-OUTFLOWS OF PG1404+226 WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707026010/ | Quick Look | ![]() |
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442 | NGC 3516 | 166.6912 | 72.5534 | 165.838584 | 72.823761 | 123.385975 | 57.972253 | 133.24889589 | 42.41461595 | 284.0065 | 56441.4603009259 | 2013-05-29 11:02:50 | 56442.6355787037 | 2013-05-30 15:15:14 | 708006040 | 54.218 | 50 | 54.218 | 54.218 | 0 | 54.218 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53.1207 | 53.1207 | 101.54 | 1 | PROCESSED | 57615.5831134259 | 2016-08-15 13:59:41 | 56383 | 2013-04-01 00:00:00 | 56503.6575347222 | 2013-07-30 15:46:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080066 | We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 8 | AO8 | THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006040/ | Quick Look | ![]() |
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443 | SBS 1301+540 | 196.0153 | 53.8063 | 195.478385 | 54.074176 | 163.182611 | 53.62856 | 118.79430047 | 63.22042238 | 133.9261 | 56991.9979976852 | 2014-11-30 23:57:07 | 56994.5141435185 | 2014-12-03 12:20:22 | 709018010 | 94.3176 | 100 | 94.3176 | 95.1576 | 0 | 95.1736 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 105.4641 | 105.4641 | 217.3498 | 5 | PROCESSED | 57617.4634143518 | 2016-08-17 11:07:19 | 57451 | 2016-03-04 00:00:00 | 57084.1361574074 | 2015-03-03 03:16:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091411 | We propose to carry out Suzaku observations, 100 ks each, of two Seyfert I nuclei, IGR J16558-5203 and SBS 1301+540, hard X-ray selected by Swift. Our goal is to distinguish between various competing models proposed for the X-ray spectra of Seyfert I nuclei. Specifically we will explore the effects of strong gravity, by testing the ionized relativistic reflection (hereafter IRR) and by measuring the spin of the black hole. We will take advantage of Suzaku s excellent capability in the broad bands from the soft through medium to hard X-ray bands. With our proposed studies we will gain deeper understanding of accretion-powered AGN in general. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | SACHIKO TSURUTA | USA | 9 | AO9 | SPECTRAL STUDIES OF SOME HARD X RAY SELECTED SEYFERT NUCLEI | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709018010/ | Quick Look | ![]() |
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444 | IRAS 05078+1626 | 77.6911 | 16.4922 | 76.970259 | 16.431142 | 78.130409 | -6.443089 | 186.12002752 | -13.50176431 | 259.3263 | 56351.6301736111 | 2013-02-28 15:07:27 | 56352.6112847222 | 2013-03-01 14:40:15 | 707029010 | 46.0167 | 45 | 46.0167 | 46.0167 | 0 | 46.0167 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.1101 | 44.1101 | 84.7558 | 1 | PROCESSED | 57610.7197916667 | 2016-08-10 17:16:30 | 56749 | 2014-04-02 00:00:00 | 56372.578287037 | 2013-03-21 13:52:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071424 | A hard X-ray-selected (BAT) AGN sample shows a remarkable 70% of the local population of type 1 AGN to have extreme hard excesses above 20 keV, likely caused by Compton-thick gas in the line-of-sight, covering at least 50% of the source. We request six snapshot observations to complete a Suzaku survey of a BAT-flux-limited sample and make a complete and unbiased measurement of the incidence. Analysis of the new sources will be performed in conjunction with existing exposures, providing exciting new insight into the previously unknown structures in hard X-ray selected AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TRACEY TURNER | USA | 7 | AO7 | INVESTIGATING COMPTON-THICK ABSORBERS IN TYPE 1 AGN: OVERHAULING THE AGN PARADIGM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707029010/ | Quick Look | ![]() |
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445 | MCG-5-23-16 | 146.9228 | -30.9448 | 146.373555 | -30.712217 | 162.622685 | -41.142645 | 262.74496877 | 17.23993252 | 295.4404 | 56448.2467476852 | 2013-06-05 05:55:19 | 56450.9584606482 | 2013-06-07 23:00:11 | 708021020 | 138.8466 | 300 | 138.8466 | 138.8466 | 0 | 138.8466 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 140.4914 | 140.4914 | 234.282 | 2 | PROCESSED | 57611.5159490741 | 2016-08-11 12:22:58 | 56383 | 2013-04-01 00:00:00 | 56461.7776736111 | 2013-06-18 18:39:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081416 | Significant recent developments in probing environments around AGN black holes has been achieved using X-ray reverberation. They were initially detected in the soft excess of several NLS1s, then recently, the first Fe K reverberation was also seen. In addition to measuring x-rays reverberating a few r_g from the event horizon, short/long delays from different radii have been separated for the first time in NGC4151. Here we propose to observe MCG-5-23-1 for 300 ks in order to study its iron K reverberation. It is optimally one of the brightest and most variable AGN in X-rays. Archival data already show very exciting signatures of Fe K reverberation. With new observations we aim to constrain the emitting region size and study the emission originating at different distances from of the hole. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ABDERAHMEN ZOGHBI | USA | 8 | AO8 | IRON K REVERBERATION IN MCG 5-23-16 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708021020/ | Quick Look | ![]() |
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446 | MKN 915 | 339.1982 | -12.5468 | 338.534901 | -12.806507 | 336.087416 | -3.520949 | 51.05925373 | -55.2984956 | 243.0396 | 56622.9636458333 | 2013-11-26 23:07:39 | 56624.1320601852 | 2013-11-28 03:10:10 | 708029010 | 41.22 | 40 | 41.22 | 41.22 | 0 | 41.22 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.3893 | 37.3893 | 100.9399 | 0 | PROCESSED | 57613.4605787037 | 2016-08-13 11:03:14 | 56383 | 2013-04-01 00:00:00 | 56637.6375347222 | 2013-12-11 15:18:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081419 | The BAT AGN sample constitutes an unprecedented all-sky hard X-ray survey of the local AGN population. However, to properly model the X-ray absorption & reflection, coverage below 10 keV is needed with CCD spectral resolution and adequate signal-to-noise. We propose to observe 11 AGN with Suzaku, which will increase the completeness of a flux-limited sample with such coverage from 85 to 158 sources. The 11 AGN only have severely underexposed Swift XRT coverage below 10 keV whereas the remaining sources have either Suzaku or XMM coverage. The Suzaku data have the additional advantage of sensitivity above 10 keV that helps to mitigate the long time-baseline of the BAT spectra. The new observations will create a significantly enhanced legacy data set that will provide value for years to come. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TAHIR YAQOOB | USA | 8 | AO8 | ROBUST CHARACTERIZATION OF ABSORPTION AND REFLECTION IN A LOCAL FLUX-LIMITED AGN POPULATION FROM THE SWIFT BAT SURVEY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708029010/ | Quick Look | ![]() |
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447 | MKN 1148 | 12.9805 | 17.4231 | 12.320857 | 17.151473 | 18.75445 | 10.92233 | 123.09650608 | -45.44849404 | 266.997 | 56656.2855555556 | 2013-12-30 06:51:12 | 56657.0627662037 | 2013-12-31 01:30:23 | 708033010 | 28.3189 | 30 | 28.3189 | 28.3269 | 0 | 28.3269 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23.1005 | 23.1005 | 67.1379 | 2 | PROCESSED | 57613.7155324074 | 2016-08-13 17:10:22 | 56383 | 2013-04-01 00:00:00 | 56702.7526273148 | 2014-02-14 18:03:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081419 | The BAT AGN sample constitutes an unprecedented all-sky hard X-ray survey of the local AGN population. However, to properly model the X-ray absorption & reflection, coverage below 10 keV is needed with CCD spectral resolution and adequate signal-to-noise. We propose to observe 11 AGN with Suzaku, which will increase the completeness of a flux-limited sample with such coverage from 85 to 158 sources. The 11 AGN only have severely underexposed Swift XRT coverage below 10 keV whereas the remaining sources have either Suzaku or XMM coverage. The Suzaku data have the additional advantage of sensitivity above 10 keV that helps to mitigate the long time-baseline of the BAT spectra. The new observations will create a significantly enhanced legacy data set that will provide value for years to come. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TAHIR YAQOOB | USA | 8 | AO8 | ROBUST CHARACTERIZATION OF ABSORPTION AND REFLECTION IN A LOCAL FLUX-LIMITED AGN POPULATION FROM THE SWIFT BAT SURVEY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708033010/ | Quick Look | ![]() |
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448 | NGC 4593 | 189.9148 | -5.3464 | 189.269905 | -5.071886 | 191.204626 | -0.990591 | 297.48422734 | 57.40070716 | 292.7769 | 56830.338275463 | 2014-06-22 08:07:07 | 56831.0988657407 | 2014-06-23 02:22:22 | 709014020 | 30.961 | 30 | 30.977 | 30.961 | 0 | 30.985 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 30.408 | 30.408 | 65.688 | 0 | PROCESSED | 57615.3154976852 | 2016-08-15 07:34:19 | 57212 | 2015-07-09 00:00:00 | 56846.5106365741 | 2014-07-08 12:15:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090097 | In the AO-8 cycle, we proposed six X-ray and optical simultaneous observations of type I Seyfert galaxy NGC 3516, and now obtaining a good correlation between those wavelengths. In the observations, we confirmed that a hard X-ray primary component (HXPC) found in Noda et al. (2013) was dominant, and its variation is well correlated with an optical one. To verify the probability that a variation of HXPC in other Seyfert also correlates with that in its optical, we propose six X-ray and optical simultaneous observations of NGC 4593, which has an X-ray spectrum dominated by HXPC as well as NGC 3516 in 2013. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 9 | AO9 | X-RAY AND OPTICAL SIMULTANEOUS OBSERVATIONS OF TYPICAL TYPE I SEYFERT NGC 4593 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709014020/ | Quick Look | ![]() |
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449 | PMN J1603-4904 | 240.9652 | -49.0681 | 240.045662 | -48.930987 | 248.937832 | -27.726173 | 332.15292306 | 2.57171396 | 292.7209 | 56547.6621643518 | 2013-09-12 15:53:31 | 56548.4842013889 | 2013-09-13 11:37:15 | 708035010 | 50.9129 | 50 | 50.9252 | 50.9129 | 0 | 50.9172 | 3 | 2 | 0 | 3 | 1 | 0 | 0 | 49.2803 | 49.2803 | 70.99 | 0 | PROCESSED | 57612.626875 | 2016-08-12 15:02:42 | 56956 | 2014-10-26 00:00:00 | 56588.7813657407 | 2013-10-23 18:45:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081432 | We propose a 50ksec Suzaku observation of the gamma-ray emitting compact symmetric radio source PMN J1603-4904 as a crucial part of the first simultaneous radio to gamma-ray campaign on this object. Constraining the X-ray spectrum of the compact radio source is needed to properly model the broadband spectral energy distribution (SED), which is essential for understanding the physical nature of this unusual object. The Swift detection allows no spectral modeling of its very faint X-ray counterpart, hence, precise spectral investigations with Suzaku are strongly required. PMN J1603-4904 is one of the few young radio galaxy candidates associated with a bright Fermi gamma-ray source, thus it plays a key role in investigating the underlying emission mechanism of newly born active galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ROOPESH OJHA | USA | 8 | AO8 | CONSTRAINING THE NATURE OF PMN J1603-4904: IS IT A GAMMA-LOUD YOUNG RADIO GALAXY? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708035010/ | Quick Look | ![]() |
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450 | SWIFT J0250.7+4142 | 42.6629 | 41.6747 | 41.856234 | 41.468698 | 53.00104 | 24.122797 | 145.63636615 | -15.88173015 | 76.5152 | 56872.0541898148 | 2014-08-03 01:18:02 | 56873.8814930556 | 2014-08-04 21:09:21 | 709006010 | 82.1549 | 80 | 82.1629 | 82.1629 | 0 | 82.1549 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.4596527778 | 2016-08-16 11:01:54 | 57267 | 2015-09-02 00:00:00 | 56902.7258564815 | 2014-09-02 17:25:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090019 | Swift/BAT extragalactic survey above E >15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe two Compton thick AGN candidates in the 70 month BAT catalog with Suzaku. To resolve the degeneracy of spectral modeling, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | DETERMINATION OF NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709006010/ | Quick Look | ![]() |
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451 | NGC 4593 | 189.9131 | -5.3423 | 189.268209 | -5.067785 | 191.201461 | -0.987483 | 297.48045078 | 57.40464867 | 113.7512 | 57006.6309375 | 2014-12-15 15:08:33 | 57007.3023263889 | 2014-12-16 07:15:21 | 709014030 | 30.5312 | 30 | 30.5312 | 30.5392 | 0 | 30.5392 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5109722222 | 2016-08-17 12:15:48 | 57383 | 2015-12-27 00:00:00 | 57017.413900463 | 2014-12-26 09:56:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090097 | In the AO-8 cycle, we proposed six X-ray and optical simultaneous observations of type I Seyfert galaxy NGC 3516, and now obtaining a good correlation between those wavelengths. In the observations, we confirmed that a hard X-ray primary component (HXPC) found in Noda et al. (2013) was dominant, and its variation is well correlated with an optical one. To verify the probability that a variation of HXPC in other Seyfert also correlates with that in its optical, we propose six X-ray and optical simultaneous observations of NGC 4593, which has an X-ray spectrum dominated by HXPC as well as NGC 3516 in 2013. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 9 | AO9 | X-RAY AND OPTICAL SIMULTANEOUS OBSERVATIONS OF TYPICAL TYPE I SEYFERT NGC 4593 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709014030/ | Quick Look | ![]() |
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452 | SDSSJ084234.9+362503 | 130.6534 | 36.3531 | 129.855939 | 36.532969 | 123.380084 | 17.503637 | 186.36195466 | 37.19411123 | 266.2333 | 53868.6856018518 | 2006-05-13 16:27:16 | 53871.41625 | 2006-05-16 09:59:24 | 701004010 | 109.9556 | 120 | 109.9716 | 109.9636 | 109.9556 | 109.9636 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 127.2306 | 127.2306 | 235.8948 | 1 | PROCESSED | 57534.3648032407 | 2016-05-26 08:45:19 | 54400 | 2007-10-27 00:00:00 | 53920.287650463 | 2006-07-04 06:54:13 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010036 | Type 2 QSOs are one of the key class to understand the structure and evolution of AGN, origin of the Cosmic X-ray background, and the history of black hole growth. We propose to measure a hard X-ray spectrum of the most luminous and brightest type 2 QSO candidate in the Sloan Digital Sky Survey. The selection by optical narrow line spectra is not biased toward Compton-thin AGNs and enables us to investigate the true nature of type 2 QSOs. The data will be used to measure the absorption column density, intrinsic luminosity, and to constrain the structure of the absorber. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YUICHI TERASHIMA | JAP | 1 | AO1 | THE MOST LUMINOUS TYPE 2 QSO IN SDSS | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701004010/ | Quick Look | ![]() |
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453 | PKS1510-089 | 228.2094 | -9.0956 | 227.535962 | -8.908847 | 228.284042 | 8.500549 | 351.2919833 | 40.14272744 | 102.2005 | 54858.1887615741 | 2009-01-27 04:31:49 | 54859.2258564815 | 2009-01-28 05:25:14 | 703005010 | 44.3054 | 40 | 44.3054 | 44.3054 | 0 | 44.3054 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.6537 | 16.6537 | 89.5979 | 0 | PROCESSED | 57545.3861342593 | 2016-06-06 09:16:02 | 54557 | 2008-04-01 00:00:00 | 54880.5404282407 | 2009-02-18 12:58:13 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030004 | We propose intensive Suzaku observations of 11 "VIP" blazars with 40ksec each, as a long-category project. We stress that all of the sources will be monitored simultaneously by GLAST (GeV), Swift XRT/UVOT (UV to X-ray), as well as ground-based radio-to-optical telescopes. We will obtain the broadband spectra and light-curves from 10^9 Hz to 10^25 Hz, which reveals for the first time the nature of gamma-loud blazars in their quiescent states. The proposed 40ksec x 11 Suzaku observations will allow us to investigate | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 3 | AO3 | REVEALING THE NATURE OF GAMMA-LOUD BLAZARS VIA SUZAKU/GLAST AND WORLD-WIDE GROUND-BASED OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703005010/ | Quick Look | ![]() |
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454 | M81 | 148.8559 | 68.9951 | 147.832512 | 69.232018 | 119.540473 | 51.512284 | 142.17660014 | 40.93097712 | 281.1688 | 53863.0052083333 | 2006-05-08 00:07:30 | 53864.5209953704 | 2006-05-09 12:30:14 | 701022010 | 103.5186 | 100 | 103.5266 | 103.5266 | 103.5266 | 103.5186 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 70.7369 | 70.7369 | 130.9421 | 0 | PROCESSED | 57534.2973726852 | 2016-05-26 07:08:13 | 54397 | 2007-10-24 00:00:00 | 53913.9816550926 | 2006-06-27 23:33:35 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010151 | We propose observations of the nearby Low Luminosity AGN, M81 and M106, for 100 ks for each target. We aim to detect both targets up to ~200 keV for the first time. We will determine the photon indices of the hard X-ray power-law continuum, with searching for other possible characteristics such as Compton hump around 10-20 keV and cutoff around 100-200 keV which would lead major discoveries. We will study the shape of Fe-K line(s) around 6-7 keV and their time variances. Our goal is to compare their hard X-ray spectra with those of SWG seyfert galaxies, with unprecedented accuracy, to study the accresion mechanism of LLAGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TAKESHI ITOH | JAP | 1 | AO1 | OBSERVATIONS OF HARD X-RAYS FROM LOW LUMINOSITY ACTIVE GALACTIC NUCLEI | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701022010/ | Quick Look | ![]() |
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455 | SWIFT J0350.1-5019 | 57.5315 | -50.3337 | 57.174394 | -50.483946 | 28.735241 | -67.001155 | 259.74491819 | -49.02538792 | 320.5309 | 53838.5046875 | 2006-04-13 12:06:45 | 53838.6752199074 | 2006-04-13 16:12:19 | 701017010 | 2.6998 | 20 | 2.7158 | 2.7158 | 2.6998 | 2.7078 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 1.1771 | 1.1771 | 9.165 | 0 | PROCESSED | 57533.4464930556 | 2016-05-25 10:42:57 | 54750 | 2008-10-11 00:00:00 | 53905.4679398148 | 2006-06-19 11:13:50 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010133 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 1 | AO1 | DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701017010/ | Quick Look | ![]() |
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456 | HOLMBERG IX X-1 | 149.4599 | 69.05 | 148.442008 | 69.288451 | 119.782652 | 51.677007 | 141.95121201 | 41.07533054 | 294.5528 | 56780.1586111111 | 2014-05-03 03:48:24 | 56780.8752546296 | 2014-05-03 21:00:22 | 709015010 | 31.886 | 30 | 31.886 | 31.886 | 0 | 31.886 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.8618 | 30.8618 | 61.9159 | 0 | PROCESSED | 57615.0271990741 | 2016-08-15 00:39:10 | 57218 | 2015-07-15 00:00:00 | 56852.5963194444 | 2014-07-14 14:18:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091251 | Broadband X-ray spectroscopy of ultraluminous X-ray sources (ULXs) with NuSTAR and Suzaku has begun to provide important information regarding the nature of these enigmatic sources. Recent NuSTAR observations of the extreme ULX Holmberg IX X-1 revealed unusual spectral variability, and different competing evolutionary scenarios can explain the available data. Resolving this degeneracy is critical to determining the nature of the accretion onto this source, and requires multi-epoch broadband spectroscopy probing a more diverse range of fluxes. We propose to undertake 4x30 ks coordinated Suzaku+NuSTAR observations of Holmberg IX X-1 to provide the additional spectra needed to robustly determine the nature of the observed evolution, providing a vital step in our understanding of extreme ULXs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | DOMINIC WALTON | USA | 9 | AO9 | MULTI-EPOCH BROADBAND X-RAY SPECTROSCOPY OF HOLMBERG IX X-1 WITH SUZAKU AND NUSTAR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709015010/ | Quick Look | ![]() |
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457 | Q0142-100 | 26.3171 | -9.7556 | 25.697719 | -10.005838 | 20.677718 | -19.226515 | 161.63610788 | -68.48152364 | 68.9469 | 56854.9601041667 | 2014-07-16 23:02:33 | 56856.4794328704 | 2014-07-18 11:30:23 | 709019010 | 60.9751 | 55 | 60.9831 | 60.9831 | 0 | 60.9751 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.53 | 10.53 | 22.736 | 0 | PROCESSED | 57615.4077083333 | 2016-08-15 09:47:06 | 57261 | 2015-08-27 00:00:00 | 56895.341412037 | 2014-08-26 08:11:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091431 | The origin of AGN iron K alpha emission has been debated for two decades. We propose to constrain iron line emission sizes using quasar X-ray microlensing. Our Chandra Cycle 11 observations have shown that the iron line equivalent widths (EWs) in six lensed systems are significantly higher than those measured in local AGNs. This implies that the iron line emission is microlensed more strongly than the X-ray continuum and originates from very compact regions. We propose to confirm the high iron line EWs in lensed quasars by monitoring two more lenses, Q0142-100 and HE0512+3329 using Suzaku, with a total exposure time 115 kilo-seconds. This will provide independent constraints for settling the debate on the origin of the iron line emission. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | BIN CHEN | USA | 9 | AO9 | CONSTRAINING QUASAR IRON LINE EMISSION USING MICROLENSING | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709019010/ | Quick Look | ![]() |
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458 | HE0512-3329 | 78.54 | -33.4465 | 78.079714 | -33.502938 | 72.667363 | -56.201883 | 236.6358247 | -33.85842065 | 104.8837 | 56933.2970833333 | 2014-10-03 07:07:48 | 56934.0071180556 | 2014-10-04 00:10:15 | 709020020 | 27.5086 | 60 | 27.5086 | 27.5166 | 0 | 27.5166 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6104976852 | 2016-08-16 14:39:07 | 57345 | 2015-11-19 00:00:00 | 56979.4110300926 | 2014-11-18 09:51:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091431 | The origin of AGN iron K alpha emission has been debated for two decades. We propose to constrain iron line emission sizes using quasar X-ray microlensing. Our Chandra Cycle 11 observations have shown that the iron line equivalent widths (EWs) in six lensed systems are significantly higher than those measured in local AGNs. This implies that the iron line emission is microlensed more strongly than the X-ray continuum and originates from very compact regions. We propose to confirm the high iron line EWs in lensed quasars by monitoring two more lenses, Q0142-100 and HE0512+3329 using Suzaku, with a total exposure time 115 kilo-seconds. This will provide independent constraints for settling the debate on the origin of the iron line emission. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | BIN CHEN | USA | 9 | AO9 | CONSTRAINING QUASAR IRON LINE EMISSION USING MICROLENSING | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709020020/ | Quick Look | ![]() |
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459 | MARKARIAN 3 | 93.8921 | 71.0501 | 92.441744 | 71.065491 | 91.879164 | 47.635184 | 143.28202475 | 22.71957945 | 87.4437 | 56931.9222337963 | 2014-10-01 22:08:01 | 56932.4181597222 | 2014-10-02 10:02:09 | 709022010 | 23.831 | 20 | 23.831 | 23.831 | 0 | 23.8376 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5994328704 | 2016-08-16 14:23:11 | 57345 | 2015-11-19 00:00:00 | 56979.4072569444 | 2014-11-18 09:46:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092008 | We propose to measure size and distance from the black hole of the optically-thick absorbing and reprocessing system(s) in the heavily obscured Seyfert Galaxy Markarian~3 by means of its known X-ray spectral variability. We aim at simultaneously measuring: the variability timescale of the primary emission, seen in transmission through a photoelectric column density of (0.7--1.1)x10^{24} atoms/cm/cm; the variability timescale of its Compton-reflection, dominating the continuum flux in the 3-10 keV energy band; and the variability timescale of the nuclear obscuration. Only the scientific payload on-board Suzaku possesses the required combination of broadband X-ray coverage, sensitivity, and spectroscopic capabilities to perform this experiment. We request 5 observations of 20 ks each. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MATTEO GUAINAZZI | EUR | 9 | AO9 | MEASURING THE TORUS SPATIAL SCALE(S) IN SEYFERT GALAXIES: A SUZAKU MONITORING OF MARKARIAN 3 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709022010/ | Quick Look | ![]() |
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460 | NGC5548 | 214.4931 | 25.1284 | 213.926191 | 25.358593 | 201.994041 | 36.406695 | 31.93341942 | 70.49864062 | 309.3821 | 54269.9362847222 | 2007-06-18 22:28:15 | 54270.6389814815 | 2007-06-19 15:20:08 | 702042010 | 31.1188 | 30 | 31.1188 | 31.1188 | 0 | 31.1188 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.1759 | 27.1759 | 60.7059 | 0 | PROCESSED | 57538.9803703704 | 2016-05-30 23:31:44 | 54695 | 2008-08-17 00:00:00 | 54319.4659953704 | 2007-08-07 11:11:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021307 | We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARTIN ELVIS | USA | 2 | AO2 | NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702042010/ | Quick Look | ![]() |
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461 | IGR J16185-5928 | 244.6464 | -59.4001 | 243.583076 | -59.27851 | 254.074844 | -37.350679 | 326.66672881 | -6.44446627 | 90.0003 | 54505.6700115741 | 2008-02-09 16:04:49 | 54507.0211111111 | 2008-02-11 00:30:24 | 702123010 | 76.6076 | 88 | 76.631 | 76.6236 | 0 | 76.6076 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 75.2553 | 75.2553 | 116.7259 | 0 | PROCESSED | 57541.5586226852 | 2016-06-02 13:24:25 | 54888 | 2009-02-26 00:00:00 | 54515.6564699074 | 2008-02-19 15:45:19 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022034 | We propose to observe with Suzaku two Narrow Line Seyfert 1 galaxies detected by SWIFT/BAT and INTEGRAL with a flux in excess of $10^{-11}$~erg~s$^{-1}$~cm$^{-2}$ in the HXD/PIN band for 70~ks each. These proposed observations provide rare high quality spectra of NLS1s above 10~keV. This will remove the spectral degeneracies inherent to limited bandpass analysis (such as that with XMM--Newton and Chandra) and the ambiguities between the different proposed models invoked to explain the unique spectral and variability properties of these most extreme class of high accretion rate sources (namely absorption, reflection, nature of the soft excess...). | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GIOVANNI MINIUTTI | EUR | 2 | AO2 | HUNTING HARD-X-RAY-BRIGHT NLS1 GALAXIES FROM THE INTEGRAL CATALOGUE WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702123010/ | Quick Look | ![]() |
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462 | SWIFT J1322.2-1641 | 200.5819 | -16.7858 | 199.912392 | -16.524578 | 205.294799 | -7.530887 | 313.4989766 | 45.45121448 | 290.037 | 55013.9738310185 | 2009-07-01 23:22:19 | 55014.9981365741 | 2009-07-02 23:57:19 | 704022010 | 41.3487 | 40 | 41.3487 | 41.6207 | 0 | 41.6127 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36.2368 | 36.2368 | 88.4858 | 7 | PROCESSED | 57547.7444097222 | 2016-06-08 17:51:57 | 55393 | 2010-07-16 00:00:00 | 55027.0523148148 | 2009-07-15 01:15:20 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 043059 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright, absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe three of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. With these observations we can make the spectral survey of bright absorbed Swift/BAT AGNs complete. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | MAURO DADINA | JEU | 4 | AO4 | SPECTRAL SURVEY OF A COMPLETE SAMPLE OF SWIFT/BAT SELECTED AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704022010/ | Quick Look | ![]() |
463 | PKS0625-354 | 96.7724 | -35.4904 | 96.328951 | -35.45865 | 100.652009 | -58.681247 | 243.45420005 | -19.97253333 | 121.4596 | 55868.6502199074 | 2011-11-03 15:36:19 | 55871.6231597222 | 2011-11-06 14:57:21 | 706014010 | 100.7198 | 100 | 100.7278 | 100.7278 | 0 | 100.7198 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86.4342 | 86.4342 | 256.8138 | 4 | PROCESSED | 57603.7550231482 | 2016-08-03 18:07:14 | 56250 | 2012-11-19 00:00:00 | 55881.2887731482 | 2011-11-16 06:55:50 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060046 | We propose to observe two radio galaxies 3C78 and PKS0625-354 which were detected by the Fermi gamma-ray satellte survey during the 1st year, in order to investigate the X-ray emission more precisely than ever. In the case of jet emission, we can constrain the jet parameter well from the multi-wavelength spectrum and obtain the jet kinetic energy. In the case of disk emission, we can obtain the jet to disk energy ratio. This observation will enable us to obtain the jet parameters of these galaxies and compare them with others. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YASUSHI FUKAZAWA | JAP | 6 | AO6 | ORIGIN OF THE X-RAY EMISSION OF GAMAM-RAY RADIO GALAXIES 3C78 AND PKS0625-354 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706014010/ | Quick Look | ![]() |
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464 | IC 342 X2 | 56.548 | 68.1243 | 55.335293 | 67.96844 | 72.578132 | 46.699378 | 138.10903546 | 10.56584534 | 237.0509 | 55640.3693981482 | 2011-03-20 08:51:56 | 55641.8058101852 | 2011-03-21 19:20:22 | 705009020 | 75.4467 | 80 | 75.4707 | 75.4467 | 0 | 75.4787 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74.2577 | 74.2577 | 124.0898 | 1 | PROCESSED | 57601.2497800926 | 2016-08-01 05:59:41 | 56019 | 2012-04-02 00:00:00 | 55652.0183680556 | 2011-04-01 00:26:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050041 | The nature of ultraluminous X-ray sources (ULXs) is one of the important unresolved issues in the modern astrophysics. A Suzaku HXD spectrum above 10 keV and its variation, in combination with those with XIS, provide us with an unique opportunity to determine unambiguously the physical state of ULXs, which is a key information to solve their nature. Here, two 80 ks Suzaku exposures are proposed on a bright ULX IC 342 X2, one of the most promising candidates for hard X-ray detection. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NAOKI ISOBE | JAP | 5 | AO5 | HARD X-RAY STUDY OF ULTRALUMINOUS X-RAY SOURCES WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705009020/ | Quick Look | ![]() |
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465 | EMS1274 | 285.5178 | -51.1684 | 284.542504 | -51.240609 | 280.974965 | -28.317711 | 345.57919311 | -22.40122796 | 103.8598 | 55299.2761921296 | 2010-04-13 06:37:43 | 55300.0056944445 | 2010-04-14 00:08:12 | 705014010 | 43.9253 | 40 | 43.9253 | 43.9333 | 0 | 43.9333 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.9581 | 34.9581 | 63.0159 | 0 | PROCESSED | 57551.1958333333 | 2016-06-12 04:42:00 | 55675 | 2011-04-24 00:00:00 | 55309.2111458333 | 2010-04-23 05:04:03 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050050 | We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 5 | AO5 | SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705014010/ | Quick Look | ![]() |
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466 | 3C111 | 64.5838 | 38.0364 | 63.747621 | 37.915108 | 69.36876 | 16.399466 | 161.66578558 | -8.81556542 | 79.7358 | 55441.1593055556 | 2010-09-02 03:49:24 | 55442.8995138889 | 2010-09-03 21:35:18 | 705040010 | 80.683 | 80 | 80.691 | 80.683 | 0 | 80.691 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 73.3707 | 73.3707 | 150.3079 | 1 | PROCESSED | 57553.2986458333 | 2016-06-14 07:10:03 | 55822 | 2011-09-18 00:00:00 | 55456.2202430556 | 2010-09-17 05:17:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051412 | Using our Suzaku observations we discovered ultra-fast outflows (UFOs) in radio-loud Broad-Line Radio Galaxies, with velocities v/c~0.04--0.15 and carrying a mass of the same order as the accretion mass. The bright BLRG 3C~111 was selected for an in-depth study of its UFO through its predicted variability on timescales of approximately one week. We propose 3 Suzaku pointings of 80~ks each separated by one week to determine the gas geometrical, physical, and dynamical characteristics and start addressing its role for the jet-disk connection in radio-loud AGN. Additionally, we will obtain a simultaneous radio-to-GeV Spectral Energy Distribution and model the relative contributions of the accretion and non-thermal components. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RITA SAMBRUNA | USA | 5 | AO5 | PROBING THE ULTRA-FAST OUTFLOW IN 3C 111 WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705040010/ | Quick Look | ![]() |
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467 | 3C111 | 64.5838 | 38.0341 | 63.747638 | 37.912808 | 69.368333 | 16.397202 | 161.66743119 | -8.81719194 | 77.8463 | 55448.0268865741 | 2010-09-09 00:38:43 | 55449.7585416667 | 2010-09-10 18:12:18 | 705040020 | 79.4198 | 80 | 79.4198 | 79.4198 | 0 | 79.4198 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71.809 | 71.809 | 149.6058 | 0 | PROCESSED | 57553.3942592593 | 2016-06-14 09:27:44 | 55827 | 2011-09-23 00:00:00 | 55461.3122106482 | 2010-09-22 07:29:35 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051412 | Using our Suzaku observations we discovered ultra-fast outflows (UFOs) in radio-loud Broad-Line Radio Galaxies, with velocities v/c~0.04--0.15 and carrying a mass of the same order as the accretion mass. The bright BLRG 3C~111 was selected for an in-depth study of its UFO through its predicted variability on timescales of approximately one week. We propose 3 Suzaku pointings of 80~ks each separated by one week to determine the gas geometrical, physical, and dynamical characteristics and start addressing its role for the jet-disk connection in radio-loud AGN. Additionally, we will obtain a simultaneous radio-to-GeV Spectral Energy Distribution and model the relative contributions of the accretion and non-thermal components. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RITA SAMBRUNA | USA | 5 | AO5 | PROBING THE ULTRA-FAST OUTFLOW IN 3C 111 WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705040020/ | Quick Look | ![]() |
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468 | MRK 841 | 226.0057 | 10.444 | 225.402057 | 10.638407 | 220.18036 | 26.59752 | 11.21871304 | 54.63485497 | 108.0015 | 55944.7625347222 | 2012-01-18 18:18:03 | 55947.3599305556 | 2012-01-21 08:38:18 | 706029020 | 110.289 | 350 | 110.2915 | 110.289 | 0 | 110.2915 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92.2182 | 92.2182 | 224.404 | 1 | PROCESSED | 57604.469224537 | 2016-08-04 11:15:41 | 55652 | 2011-04-01 00:00:00 | 55985.3097337963 | 2012-02-28 07:26:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061119 | 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-LP | A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706029020/ | Quick Look | ![]() |
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469 | SWIFT J0544.4-4328 | 86.0099 | -43.419 | 85.632201 | -43.439311 | 82.65148 | -66.759602 | 249.50201979 | -30.05213281 | 308.9989 | 57140.9252083333 | 2015-04-28 22:12:18 | 57143.359212963 | 2015-05-01 08:37:16 | 709005010 | 84.362 | 100 | 84.362 | 92.7251 | 0 | 92.7171 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.0749537037 | 2016-08-18 01:47:56 | 57527 | 2016-05-19 00:00:00 | 57160.6331597222 | 2015-05-18 15:11:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090018 | We propose to observe two hard X-ray bright Seyfert galaxies with a highly accreting small BH. This class of objects is of importance in studying accretion processes under a large mass accretion rate and therefore mass growth of black holes. Our aims are (1) to measure a continuum shape such as spectral slope and high energy cutoff, (2) to compare them with other classes of AGNs, and (3) to search for highly ionized outflows with a large column density. All of these will be fundamental pieces of information to better understand accretion physics and ``feedback'' processes in galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YUICHI TERASHIMA | JAP | 9 | AO9 | ACCRETION AND OUTFLOW IN THE HARD X-RAY SELECTED LOW-MASS SEYFERTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709005010/ | Quick Look | ![]() |
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470 | OT+081 | 267.8906 | 9.6366 | 267.297097 | 9.648276 | 267.507831 | 33.058606 | 34.9082961 | 17.63584745 | 268.2827 | 55830.0996759259 | 2011-09-26 02:23:32 | 55830.3911921296 | 2011-09-26 09:23:19 | 706047010 | 10.774 | 10 | 10.774 | 10.774 | 0 | 10.774 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.036 | 11.036 | 25.1519 | 1 | PROCESSED | 57603.2492708333 | 2016-08-03 05:58:57 | 56225 | 2012-10-25 00:00:00 | 55875.6247569444 | 2011-11-10 14:59:39 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061601 | We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | SVETLANA JORSTAD | USA | 6 | AO6 | EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706047010/ | Quick Look | ![]() |
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471 | RXJ0134-4258 | 23.5686 | -42.9671 | 23.03099 | -43.222871 | 359.764354 | -47.882347 | 276.92816891 | -71.93227434 | 245.0998 | 56290.2726851852 | 2012-12-29 06:32:40 | 56292.2506481482 | 2012-12-31 06:00:56 | 707014010 | 81.429 | 50 | 81.4485 | 81.445 | 0 | 81.429 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.1219 | 16.1219 | 37.6859 | 0 | PROCESSED | 57608.396087963 | 2016-08-08 09:30:22 | 56702 | 2014-02-14 00:00:00 | 56336.5473263889 | 2013-02-13 13:08:09 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070081 | RXJ0134.2-4258 was detected in the ROSAT all sky observation (RASS), later identified as a radio loud (RL) narrow line Seyfert 1 galaxy. During the RASS, the soft X-ray spectrum of this source was steep. Following observations with ROSAT, ASCA, Swift, and XMM-Newton (XMM) showed flatter spectra. The XMM spectra are fitted with a power law with an cut-off (EC) at 4 keV, where a blackbody (BB) component was not evident. Either type of spectrum is not common for Seyferts. We consider this peculiarity is related to the RL nature of this object, originated in the jet. We will observe this source with Suzaku, which has higher energy resolution than XMM, to reveal the long term variability of this source. Particular interests go to the EC energy, bb component, and the iron K emission line. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | HIROAKI TAKAHASHI | JAP | 7 | AO7 | X-RAY EMISSION FROM THE BRIGHTEST RADIO LOUD NARROW LINE SEYFERT 1 RXJ0134.2-4258 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707014010/ | Quick Look | ![]() |
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472 | 0827+243 | 127.7155 | 24.1863 | 126.975126 | 24.355162 | 124.074961 | 5.096162 | 200.01763935 | 31.87561316 | 105.3936 | 56213.3893287037 | 2012-10-13 09:20:38 | 56213.5959837963 | 2012-10-13 14:18:13 | 707041010 | 8.0392 | 10 | 8.0472 | 8.0392 | 0 | 8.0472 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.737 | 7.737 | 17.8479 | 0 | PROCESSED | 57607.7474652778 | 2016-08-07 17:56:21 | 56598 | 2013-11-02 00:00:00 | 56232.4327199074 | 2012-11-01 10:23:07 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071601 | We propose to perform two 2-week multi-frequency campaigns of observations of a sample of gamma-ray blazars during Fermi Cycle 5. The campaigns will involve: (1) gamma-ray monitoring with the Fermi LAT, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B, V, R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku and Swift; (6) mid-IR measurements with IRTF; and (7) near-IR photometric J, H, and K observations. The research aims i) to search for correlated variability on short timescales; ii) to compile SEDs at different states of gamma-ray and radio jet activitiy; and iii) to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | SVETLANA JORSTAD | USA | 7 | AO7 | MULTI-FREQUENCY CAMPAIGNS TO STUDY RAPID VARIABILITY IN GAMMA_RAY BLAZARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707041010/ | Quick Look | ![]() |
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473 | MKN 6 | 103.0685 | 74.413 | 101.450971 | 74.472117 | 95.572656 | 51.225087 | 140.3435691 | 26.1094153 | 254.4482 | 57133.5883333333 | 2015-04-21 14:07:12 | 57134.7015046296 | 2015-04-22 16:50:10 | 710001010 | 50.6541 | 50 | 50.6541 | 51.3396 | 0 | 51.3396 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.0317476852 | 2016-08-18 00:45:43 | 57548 | 2016-06-09 00:00:00 | 57154.4415162037 | 2015-05-12 10:35:47 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 101730 | We request two quasi-simultaneous NuSTAR + Suzaku-XIS pointings of the radio-loud Sy 1.5 Mkn 6 to understand the complexity of its accreting circumnuclear gas structures. A series of high-quality, broadband X-ray spectra, including coverage above 10 keV, are needed to properly quantify the variable and complex line of sight absorbers. These new observations, in conjunction with radio and previous X-ray observations, will be a unique opportunity to understand accretion modes in the innermost regions of a radio-loud AGN that has recently undergone a merger. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ALEX MARKOWITZ | USA | 10 | AO10 | COMPLEX CIRCUMNUCLEAR ABSORPTION IN RADIO-LOUD AGN: VARIABLE ABSORPTION IN MKN 6 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710001010/ | Quick Look | ![]() |
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474 | MARKARIAN 3 | 93.9093 | 71.025 | 92.46011 | 71.040478 | 91.888941 | 47.610328 | 143.30979342 | 22.71730777 | 267.1766 | 57116.4730902778 | 2015-04-04 11:21:15 | 57116.9877199074 | 2015-04-04 23:42:19 | 709022050 | 21.4556 | 20 | 21.4556 | 21.4556 | 0 | 21.4556 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.9089814815 | 2016-08-17 21:48:56 | 57550 | 2016-06-11 00:00:00 | 57183.6622916667 | 2015-06-10 15:53:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092008 | We propose to measure size and distance from the black hole of the optically-thick absorbing and reprocessing system(s) in the heavily obscured Seyfert Galaxy Markarian~3 by means of its known X-ray spectral variability. We aim at simultaneously measuring: the variability timescale of the primary emission, seen in transmission through a photoelectric column density of (0.7--1.1)x10^{24} atoms/cm/cm; the variability timescale of its Compton-reflection, dominating the continuum flux in the 3-10 keV energy band; and the variability timescale of the nuclear obscuration. Only the scientific payload on-board Suzaku possesses the required combination of broadband X-ray coverage, sensitivity, and spectroscopic capabilities to perform this experiment. We request 5 observations of 20 ks each. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MATTEO GUAINAZZI | EUR | 9 | AO9 | MEASURING THE TORUS SPATIAL SCALE(S) IN SEYFERT GALAXIES: A SUZAKU MONITORING OF MARKARIAN 3 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709022050/ | Quick Look | ![]() |
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475 | NGC 3516 | 166.6817 | 72.5579 | 165.82888 | 72.82825 | 123.376111 | 57.97325 | 133.24892211 | 42.40929053 | 306.0068 | 57154.3345023148 | 2015-05-12 08:01:41 | 57157.0348611111 | 2015-05-15 00:50:12 | 710009010 | 117.7012 | 120 | 117.7012 | 123.0032 | 0 | 124.7632 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.6915277778 | 2016-08-18 16:35:48 | 57593 | 2016-07-24 00:00:00 | 57224.4439467593 | 2015-07-21 10:39:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 100040 | In the AO-8 cycle, we have proposed several X-ray and optical simultaneous observations of a type I Seyfert galaxy NGC 3516, and obtained a good correlation between those wavelengths in its faint phase. The result suggests that a hard primary X-ray continua found in NGC 3516 by Noda et al. (2013) is generated in a corona formed closely to an accretion disk, which is possibly a radiatively inefficient accretion flow. As a next step, we examine whether or not an X-ray variation is also correlated with that in optical, when NGC 3516 is in the bright phase, and the other primary X-ray continuum, also reported by Noda et al. (2013), is dominant. For it, we propose an X-ray and optical simultaneous observation of NGC 3516 with an exposure of 120 ksec, which is triggered by a Swift monitoring. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 10 | AO10-TOO | X-RAY AND OPTICAL SIMULTANEOUS OBSERVATIONS OF NGC 3516 IN ITS BRIGHT PHASE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710009010/ | Quick Look | ![]() |
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476 | OJ 287 | 133.7046 | 20.1043 | 132.989527 | 20.295378 | 130.505611 | 2.596765 | 206.8173824 | 35.82032681 | 285.8742 | 57145.5508449074 | 2015-05-03 13:13:13 | 57148.4467592593 | 2015-05-06 10:43:20 | 710011010 | 111.6388 | 323 | 111.6388 | 111.6388 | 0 | 111.6388 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.1122800926 | 2016-08-18 02:41:41 | 57113 | 2015-04-01 00:00:00 | 57164.5257523148 | 2015-05-22 12:37:05 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 101431 | Kepler will observe OJ 287 with 1 min sampling and >90% duty cycle for ~75 days in 2015, providing an unprecedented opportunity to quantitatively compare optical and X-ray variations in one of the brightest and most active blazars in the sky. We request continuous Suzaku coverage for 128 orbits (323 ks) in a simultaneous campaign including XMM, Swift, radio and multi-color optical monitoring. Suzaku samples key intermediate timescales of hours-days, allowing measurement of CCFs and PSDs spanning a wide range of temporal frequencies. These will be used to test models and determine source parameters e.g. if the X-rays are due to synchrotron-self Compton the optical should lead the X-rays by ~1 day, but if they are "synchrotron flashes" the bands should vary nearly simultaneously. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RICK EDELSON | USA | 10 | AO10 | SIMULTANEOUS SUZAKU/KEPLER/MULTIWAVELENGTH MONITORING OF OJ 287 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710011010/ | Quick Look | ![]() |
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477 | NGC 2992 | 146.4592 | -14.2821 | 145.857736 | -14.050853 | 154.047551 | -26.059819 | 249.69438343 | 28.83515423 | 128.4959 | 53717.4275462963 | 2005-12-13 10:15:40 | 53718.506412037 | 2005-12-14 12:09:14 | 700005030 | 46.8361 | 120 | 46.8441 | 46.8681 | 46.8361 | 46.8601 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 44.2983 | 44.2983 | 93.2079 | 1 | PROCESSED | 57532.4690046296 | 2016-05-24 11:15:22 | 54247 | 2007-05-27 00:00:00 | 54039.2254861111 | 2006-10-31 05:24:42 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001013 | NGC 2992 is a nearby Seyfert 1.9 galaxy showing long-term (20 yrs) large amplitude (factor of 20) variability. This object showed switching between Compton-thick and -thin. Recent RXTE monitoring has shown that this object is highly variable on shorter time scales (2 weeks). We propose three Suzaku observations to monitor the variability of absorption column, broad band continuum shape, and Fe line intensity to understand the cause of the remarkable variability. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YUICHI TERASHIMA | JAP | 0 | SWG | THE SPECTRAL VARIABILITY IN NGC 2992: FE-LINE, REFLECTION, AND COMPTON-THIN/THICK SWITCHING | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700005030/ | Quick Look | ![]() |
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478 | NGC 5506 | 213.3095 | -3.2029 | 212.660624 | -2.969373 | 212.1852 | 9.604154 | 339.1508826 | 53.81542712 | 91.2728 | 54131.0918055556 | 2007-01-31 02:12:12 | 54132.6279513889 | 2007-02-01 15:04:15 | 701030030 | 57.4063 | 150 | 57.4143 | 57.4063 | 0 | 57.4143 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.7027 | 47.7027 | 132.6858 | 0 | PROCESSED | 57536.9491666667 | 2016-05-28 22:46:48 | 54695 | 2008-08-17 00:00:00 | 54139.3642361111 | 2007-02-08 08:44:30 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011312 | NGC 5506 is one of the brightest Seyferts in the X-ray sky, the second brightest in the PIN bandpass. Obscuring gas has kept the true nature of this AGN secret until recent optical and infrared studies have unmasked the narrow-line-seyfert 1 nucleus. With this knowledge, NGC 5506 is the perfect candidate for confirming the generality of a new result based on a recent XMM observation of Mkn 766, ie that the ionized component of Fe K emission originates from the inner accretion disk and closely tracks the hard X-ray continuum flux. This immediately gives us the ionization-state and size-scale of the inner disk. We request a 150 ks Suzaku observation to see whether a similar result holds for NGC 5506 and, by extension, may be a property of NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TRACEY TURNER | USA | 1 | AO1 | SUZAKU STUDY OF THE BRIGHTEST NARROW LINE SEYFERT 1: NGC 5506 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701030030/ | Quick Look | ![]() |
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479 | CIRCINUS GALAXY | 213.2971 | -65.3336 | 212.329588 | -65.099539 | 238.600438 | -47.951762 | 311.32997737 | -3.80345965 | 276.4798 | 53937.5207986111 | 2006-07-21 12:29:57 | 53939.0475 | 2006-07-23 01:08:24 | 701036010 | 108.0217 | 100 | 108.0457 | 108.0217 | 108.0457 | 108.0297 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 94.272 | 94.272 | 131.8879 | 1 | PROCESSED | 57535.0550578704 | 2016-05-27 01:19:17 | 54401 | 2007-10-28 00:00:00 | 53943.5986574074 | 2006-07-27 14:22:04 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011331 | The light of AGN dominates the hard cosmic X-ray background. However, the contribution of Compton thick objects is poorly constrained because they emit chiefly above the energy range where Chandra and XMM are sensitive. Here we propose to observe the Circinus galaxy, one of the two brightest AGN reflection sources below 10 keV and with a known high column density. Our observations below 10 keV will provide CCD spectra of the rich emission line and continuum spectra, allowing limited photoionization modelling and searches for variability, possibly seen in Circinus. In the range 10 - 60 keV, we shall obtain a spectrum of the directly viewed continuum with unprecedented S/N in the key band for the HCXB. Above 60 keV, we will detect Circinus and check whether the spectrum has a rollover. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | ANDREW WILSON | USA | 1 | AO1 | THE HARD X-RAY BACKGROUND, COMPTON-THICK AGN AND WATER VAPOR MEGAMASERS | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701036010/ | Quick Look | ![]() |
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480 | APM 08279+5255 | 127.9195 | 52.7471 | 126.987464 | 52.916366 | 116.240703 | 32.704357 | 165.76446097 | 36.2381521 | 299.485 | 54183.9301041667 | 2007-03-24 22:19:21 | 54186.4654513889 | 2007-03-27 11:10:15 | 701057030 | 117.1433 | 125 | 117.1433 | 117.1513 | 0 | 117.1433 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 110.9324 | 110.9324 | 219.0418 | 3 | PROCESSED | 57538.0464467593 | 2016-05-30 01:06:53 | 54702 | 2008-08-24 00:00:00 | 54209.5933680556 | 2007-04-19 14:14:27 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011353 | Motivated by the detection of a relativistic outflow of highly ionized gas in previous XMM-Newton and Chandra observations of the lensed quasar APM08279+5255 we propose to monitor this object with three 100ks observations with the aim of improving our understanding of the significance of such outflows in regulating black hole growth and in influencing structure formation. The main scientific goals are : (a) verify the present interpretations of Fe line features in this quasar, (b) monitor the time variability of the Fe absorption features and thus constrain the acceleration mechanism, (c) constrain the kinematic, ionization and absorbing properties of the outflow, and (d) show whether the low-energy ionized absorber is part of the relativistic outflow. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GEORGE CHARTAS | USA | 1 | AO1 | VIEWS OF RELATIVISTIC WINDS THROUGH NATURAL LENSES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701057030/ | Quick Look | ![]() |
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481 | 1ES 1553+113 | 238.8999 | 11.1305 | 238.306227 | 11.275519 | 233.852477 | 30.750337 | 21.81691499 | 43.96274027 | 296.7536 | 53940.6127777778 | 2006-07-24 14:42:24 | 53941.8036342593 | 2006-07-25 19:17:14 | 701070010 | 55.6355 | 55 | 55.6435 | 55.6515 | 55.6515 | 55.6355 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 53.2015 | 53.2015 | 102.8819 | 0 | PROCESSED | 57535.0418171296 | 2016-05-27 01:00:13 | 54401 | 2007-10-28 00:00:00 | 53955.6133680556 | 2006-08-08 14:43:15 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011376 | Detecting absorption effects in TeV blazar spectra from TeV photon collisions on the extragalactic IR background (EBL) is a powerful tool to probe the EBL. It requires a thorough understanding of the intrinsic blazar spectra. We propose XIS and HXD observations, with emphasis on the hard X-rays, for the 3 most distant HESS blazars, coordinated with HESS observations. Thanks to Suzaku's sensitivity in a broad energy range, we expect to set tight limits on the models' parameter space, and constrain emission and acceleration scenarios by studying the shape and evolution of the particle distribution, most sensitively conducted in the important hard X-ray energy range. In coordination with TeV observations, it allows us to disentangle EBL absorption effects from the blazar intrinsic spectra. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ANITA REIMER | USA | 1 | AO1 | CHALLENGING JET MODELS OF THE MOST DISTANT TEV-BLAZARS | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701070010/ | Quick Look | ![]() |
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482 | 1ES 1959+650 | 299.9645 | 65.1588 | 299.84329 | 65.020024 | 7.34886 | 77.791428 | 98.00607393 | 17.68746705 | 45.1602 | 53878.0509606482 | 2006-05-23 01:13:23 | 53880.1718055556 | 2006-05-25 04:07:24 | 701075010 | 98.8622 | 100 | 98.8782 | 98.8622 | 98.8702 | 98.8782 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 96.106 | 96.106 | 183.2028 | 2 | PROCESSED | 57534.4674305556 | 2016-05-26 11:13:06 | 54408 | 2007-11-04 00:00:00 | 53928.2478472222 | 2006-07-12 05:56:54 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012002 | We request to observe 1ES1959+650 and 1ES2344+514 for 100 ks each with SUZAKU simultaneously with the Whipple Cherenkov telescope. Whipple will extensively monitor these sources for months in 2006-2007. There are three well defined scientific cases that we would like to address. We want to study 1) the correlation between the soft and hard X-ray and TeV fluxes and spectra, extremely variable in these sources, sometimes showing extreme conditions; 2) the mystery of the ''orphan'' flares; i.e. events observed only in the TeV gamma rays without a counterpart in the X-rays: this is currently not understood in the framework of SSC models; 3) the origin of the lag observed between soft and hard X-ray variability in some blazars and the implications for the TeV emission. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GIANPIERO TAGLIAFERRI | EUR | 1 | AO1 | JETS ON TEST: SIMULTANEOUS X-RAY AND TEV OBSERVATIONS OF 1ES1959+650 AND 1ES2344+514 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701075010/ | Quick Look | ![]() |
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483 | 3C 390.3 | 280.629 | 79.7686 | 281.497615 | 79.715169 | 81.957835 | 76.491681 | 111.4356997 | 27.05756334 | 197.286 | 54083.1426851852 | 2006-12-14 03:25:28 | 54085.1384722222 | 2006-12-16 03:19:24 | 701060010 | 0.024 | 100 | 99.3678 | 99.3678 | 0.024 | 99.3678 | 2 | 2 | 1 | 2 | 1 | 0 | 0 | 97.8813 | 97.8813 | 172.4199 | 3 | PROCESSED | 57536.3784722222 | 2016-05-28 09:05:00 | 54702 | 2008-08-24 00:00:00 | 54132.9968055556 | 2007-02-01 23:55:24 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011363 | We propose Suzaku observations of the X-ray bright Broad-Line Radio Galaxies 3C382 and 3C390.3 to study their complex broad-band X-ray spectra. The HXD will constrain the continuum above 10 keV, discriminating between competing physically-different models, while at the same time the XIS will determine the parameters of the FeKalpha line and the shape of the soft X-rays. The proposed observations will allow us to shed light on the origin of reflection features in radio-loud AGN, ultimately determining the structure and ionization state of the accretion flow in these objects. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | RITA SAMBRUNA | USA | 1 | AO1 | THE BROAD-BAND X-RAY SPECTRUM OF BROAD-LINE RADIO GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701060010/ | Quick Look | ![]() |
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484 | Q1158-1843 | 180.1895 | -18.9957 | 179.549068 | -18.717273 | 187.964658 | -17.299195 | 286.65628264 | 42.26876142 | 291.8577 | 54636.8208912037 | 2008-06-19 19:42:05 | 54637.4202314815 | 2008-06-20 10:05:08 | 703039010 | 24.085 | 22 | 24.101 | 24.085 | 0 | 24.101 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.4309 | 22.4309 | 51.7819 | 1 | PROCESSED | 57542.8567361111 | 2016-06-03 20:33:42 | 55014 | 2009-07-02 00:00:00 | 54648.3349305556 | 2008-07-01 08:02:18 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031334 | Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GEORGE CHARTAS | USA | 3 | AO3 | A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703039010/ | Quick Look | ![]() |
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485 | MCG-6-30-15 | 203.9706 | -34.2946 | 203.254215 | -34.039458 | 215.17105 | -22.544253 | 313.28931603 | 27.68170589 | 107.0204 | 53744.9738310185 | 2006-01-09 23:22:19 | 53749.1390277778 | 2006-01-14 03:20:12 | 700007010 | 143.1965 | 300 | 143.1965 | 143.3162 | 143.2685 | 143.2445 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 126.2903 | 126.2903 | 359.8399 | 4 | PROCESSED | 57532.7604398148 | 2016-05-24 18:15:02 | 54247 | 2007-05-27 00:00:00 | 54040.4060416667 | 2006-11-01 09:44:42 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001035 | The broad iron line in the Seyfert 1 galaxy MCG-6-30-15 shows that most of the power is released at 2--4 gravitational radii enabling the strong gravity, accretion flow and energy release in that exciting regime to be studied. The spectral variability of the source decomposes into a highly variable power law and a reflection-dominated component, containing the iron line and Compton hump, which varies significantly but with much less amplitude. This can be explained by the extreme gravitational light bending occuring in this region. We propose to observe MCG--6-30-15 for 4 x 50~ks in order to determine for the first time the variability of the reflection over a wide range of energies from below 1 keV to above 40 keV and timescales . | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ANDREW FABIAN | JAP | 0 | SWG | REFLECTION, ABSORPTION AND STRONG GRAVITY AROUND THE SPINNING BLACK HOLE IN MCG--6-30-15 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700007010/ | Quick Look | ![]() |
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486 | NGC 7213 | 332.316 | -47.1629 | 331.53332 | -47.408605 | 315.985734 | -33.170959 | 349.59497628 | -52.58020545 | 231.3714 | 54030.2323611111 | 2006-10-22 05:34:36 | 54032.2759722222 | 2006-10-24 06:37:24 | 701029010 | 90.736 | 100 | 90.76 | 90.744 | 90.736 | 90.752 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 90.3418 | 90.3418 | 176.5358 | 0 | PROCESSED | 57535.9564814815 | 2016-05-27 22:57:20 | 54695 | 2008-08-17 00:00:00 | 54056.3665162037 | 2006-11-17 08:47:47 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011305 | We propose a 100ks Suzaku observation of the low luminosity AGN, NGC 7213. Previous observations show a complex iron line and weak or no Compton reflection. However the iron line and reflection hump are poorly constrained, so the line emitting matter could arise from a truncated disk, BLR or a Compton-thin torus. A high quality Suzaku observation will constrain the iron line profile, resolve the ionized emission and unambiguously determine its origin. Using the unique broad bandpass of Suzaku above 10 keV we will place tight constraints on any reflection hump, enabling us to determine if the iron line originates from a truncated disk. This could provide a direct test of the paradigm that the X-ray emission in low accretion rate AGN occurs in a truncated disk system such as an ADAF. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | JAMES REEVES | USA | 1 | AO1 | DOES THE LOW LUMINOSITY AGN NGC7213 CONTAIN A TRUNCATED ACCRETION DISK? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701029010/ | Quick Look | ![]() |
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487 | IRAS 19254-7245 | 292.8508 | -72.6492 | 291.381636 | -72.754038 | 280.373528 | -50.031737 | 322.5078751 | -28.76929596 | 279.8892 | 54041.9830208333 | 2006-11-02 23:35:33 | 54044.5967476852 | 2006-11-05 14:19:19 | 701052010 | 113.5123 | 120 | 113.5203 | 113.5203 | 113.5123 | 113.5203 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 151.9778 | 151.9778 | 225.8099 | 1 | PROCESSED | 57536.068125 | 2016-05-28 01:38:06 | 54455 | 2007-12-21 00:00:00 | 54088.8285185185 | 2006-12-19 19:53:04 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011342 | We propose a 120 ksec Suzaku exposure of the ULIRG IRAS19254-7245. A previous XMM-Newton observation revealed the presence of a strong iron emission line and a flat continuum, both suggesting that this source hosts a Compton-thick AGN. In this scenario, the 2-10 keV luminosity of IRAS19254-7245 could be greater than 10e44 erg/s. However since no direct continuum is visible in the XMM bandpass, a direct measure of the absorbing column density was not feasible, thus the intrinsic X-ray luminosity of this source was derived only through indirect arguments. The unique bandpass and sensititvity of Suzaku above 10 keV will allow us to confirm the Compton-thick nature of this source and to measure for the first time the intrinsic X-ray luminosity of the AGN hosted in IRAS 19254-7245. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | VALENTINA BRAITO | USA | 1 | AO1 | ASSESSING THE ENERGETIC BUDGET IN THE SUPERANTENNAE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701052010/ | Quick Look | ![]() |
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488 | NGC3227 | 155.8772 | 19.8688 | 155.194637 | 20.122177 | 150.387911 | 9.14334 | 216.98506904 | 55.4463804 | 114.6051 | 54774.1503587963 | 2008-11-04 03:36:31 | 54775.6780555556 | 2008-11-05 16:16:24 | 703022020 | 53.6995 | 50 | 53.6995 | 53.6995 | 0 | 53.6995 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50.2891 | 50.2891 | 131.9718 | 3 | PROCESSED | 57544.3625810185 | 2016-06-05 08:42:07 | 54557 | 2008-04-01 00:00:00 | 54788.4371643518 | 2008-11-18 10:29:31 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031013 | We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARTIN ELVIS | USA | 3 | AO3 | NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703022020/ | Quick Look | ![]() |
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489 | MCG-02-14-009 | 79.0657 | -10.5106 | 78.475918 | -10.56483 | 77.084553 | -33.463679 | 211.75204832 | -25.86275025 | 68.0451 | 54706.9410069444 | 2008-08-28 22:35:03 | 54710.0308333333 | 2008-09-01 00:44:24 | 703060010 | 142.1522 | 125 | 142.1522 | 142.1522 | 0 | 142.1522 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 129.5879 | 129.5879 | 266.9199 | 1 | PROCESSED | 57543.5182986111 | 2016-06-04 12:26:21 | 55100 | 2009-09-26 00:00:00 | 54731.4652430556 | 2008-09-22 11:09:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032009 | MCG--02-14-009 appears to have the strongest relativistic iron line of all the Seyfert 1s: a short 5 ks XMM-Newton observation found the line to have an EW 530-770 eV, two times larger than for MCG-6-30-15. We propose a 125 ks Suzaku observation of this AGN, which provides a unique opportunity to probe the innermost accretion disk in the region of strong gravity. The main goals are: (a) utilise the unique broad bandpass of Suzaku to detect the expected strong reflection hump and determine the form of the X-ray continuum; (b) accurately measure the relativistic iron K line profile and thereby the geometry of the X-ray emitting region and (c) determine whether the iron line responds to the continuum down to the orbital timescales of the inner disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JAMES REEVES | EUR | 3 | AO3 | MCG-02-14-009: PROBING THE PHYSICAL PROPERTIES OF THE STRONGEST IRON K LINE | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703060010/ | Quick Look | ![]() |
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490 | 2MASX J02485937+2630 | 42.225 | 26.5707 | 41.491892 | 26.363374 | 47.759882 | 9.863115 | 153.13364356 | -29.32417791 | 74.088 | 55030.159224537 | 2009-07-18 03:49:17 | 55031.3766782407 | 2009-07-19 09:02:25 | 704013010 | 42.9501 | 40 | 42.9501 | 43.2153 | 0 | 43.2247 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29.5403 | 29.5403 | 105.1719 | 0 | PROCESSED | 57547.8817013889 | 2016-06-08 21:09:39 | 55415 | 2010-08-07 00:00:00 | 55048.2541435185 | 2009-08-05 06:05:58 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040060 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe three Compton thick AGN candidates in the 22 months BAT catalog with Suzaku. To resolve the degeneracy of spectral modeling, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 4 | AO4 | DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704013010/ | Quick Look | ![]() |
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491 | 2FGL J0923.5+1508 | 140.9887 | 15.0811 | 140.300178 | 15.296347 | 138.613889 | -0.175811 | 215.96780071 | 40.48329137 | 287.9737 | 56046.2642939815 | 2012-04-29 06:20:35 | 56048.4933449074 | 2012-05-01 11:50:25 | 707007010 | 95.2554 | 90 | 95.2794 | 95.2554 | 0 | 95.2794 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89.5878 | 89.5878 | 192.568 | 1 | PROCESSED | 57605.3423611111 | 2016-08-05 08:13:00 | 56434 | 2013-05-22 00:00:00 | 56068.6261921296 | 2012-05-21 15:01:43 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070024 | We propose X-ray follow up observations of two high redshift blazar candidates in the Fermi/LAT unidentified sources. The aim of this proposal is to detect X-ray emissions from high redshift blazars (z >> 3) buried in unidentified Fermi/LAT sources and to find the most distant LAT detected blazar. Gamma-ray photons above 10 GeV are attenuated by interactions with UV photons which result in creating electron-positron pairs. Therefore, attenuation signatures are predicted to be observed in gamma-ray spectra and such attenuation of high redshift blazars with redshift up to z ~ 6 provide information about UV background out to the epoch of cosmological reionization. By utilizing the attenuation, we can investigate the UV radiation state of the early universe. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YOSUKE TAKAHASHI | JAP | 7 | AO7 | SUZAKU OBSERVATIONS OF HIGH REDSHIFT BLAZAR CANDIDATES IN THE FERMI UNIDENTIFIED SOURCE SAMPLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707007010/ | Quick Look | ![]() |
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492 | IC4329A | 207.3321 | -30.3098 | 206.617944 | -30.061645 | 216.345264 | -17.777119 | 317.49793706 | 30.91926559 | 298.5047 | 54332.9765740741 | 2007-08-20 23:26:16 | 54333.5558333333 | 2007-08-21 13:20:24 | 702113050 | 24.0262 | 25 | 24.0262 | 24.0262 | 0 | 24.0262 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.8256 | 18.8256 | 50.0439 | 1 | PROCESSED | 57539.6252083333 | 2016-05-31 15:00:18 | 54730 | 2008-09-21 00:00:00 | 54350.649375 | 2007-09-07 15:35:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022009 | IC 4329A is the brightest known Seyfert 1 galaxy between ~2-30 keV (F(2-10 keV)~1-2e-10 erg/cm2s). With its clear warm absorber and reflection component, it is often taken as the prototypical Sey 1 galaxy. Its X-ray variability is strong enough (and on a sufficiently long time scale, ideal for Suzaku) to make multiple observations critical for probing the origin of the Compton reflection component, and to attempt measuring variations of the high energy cut-off. We thus propose 5x20 ks observations to monitor i) the correlated variability of the reflection continuum plus FeK line to primary continuum variations, and ii) the variations in the high-E cut-off, and their relation with the power-law, and iii) check the evidence for a blueshifted (v~0.1c) FeK absorption line at ~7.7 keV. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MASSIMO CAPPI | EUR | 2 | AO2 | SUZAKU MULTIPLE OBSERVATIONS OF IC4329A TO PROBE THE ORIGIN OF THE COMPTON REFLECTION COMPONENT AND HIGH-ENERGY CUT-OFF | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702113050/ | Quick Look | ![]() |
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493 | IC 4329A | 207.3331 | -30.3096 | 206.618942 | -30.061447 | 216.346028 | -17.776613 | 317.49896941 | 30.91923491 | 296.2 | 56152.0924652778 | 2012-08-13 02:13:09 | 56154.6425578704 | 2012-08-15 15:25:17 | 707025010 | 117.5938 | 120 | 117.5938 | 117.5938 | 0 | 117.5938 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 112.9986 | 112.9986 | 220.2637 | 2 | PROCESSED | 57606.8955208333 | 2016-08-06 21:29:33 | 56540 | 2013-09-05 00:00:00 | 56170.1592824074 | 2012-08-31 03:49:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071417 | We propose simultaneous NuSTAR/Suzaku observations of NGC 4151 and IC 4329A. These pointings will achieve three goals: (1) They will provide the best-ever broad-band X-ray spectra of two of the brightest Seyfert galaxies in the 0.5-80 keV band; (2) They will enable broad-band, time-resolved X-ray spectroscopy of these fascinating and variable sources; (3) They will serve as invaluable calibration targets for the two observatories. The spectral coverage and sensitivity will enable the continuum, absorption and reflection components of each spectrum to be conclusively disentangled, allowing us to determine whether inner disk reflection signatures are present. We will also be able to break the degeneracy between the coronal temperature and optical depth in both AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | LAURA BRENNEMAN | USA | 7 | AO7 | SHEDDING NEW LIGHT ON THE BROAD-BAND X-RAY SPECTRA OF NGC 4151 AND IC 4329A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707025010/ | Quick Look | ![]() |
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494 | NGC 1448 | 56.1426 | -44.6942 | 55.730836 | -44.850191 | 33.469346 | -61.660504 | 251.59735556 | -51.37690943 | 264.6522 | 54879.3481828704 | 2009-02-17 08:21:23 | 54880.4501041667 | 2009-02-18 10:48:09 | 703062010 | 52.9653 | 50 | 52.9653 | 52.9653 | 0 | 52.9653 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 55.0869 | 55.0869 | 95.202 | 1 | PROCESSED | 57545.5960763889 | 2016-06-06 14:18:21 | 55330 | 2010-05-14 00:00:00 | 54893.4451041667 | 2009-03-03 10:40:57 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032018 | We propose for a 50 ks Suzaku observation of NGC 1448, a nearby (15 Mpc) gas-rich and dust-obscured Scd galaxy that is optically classified as an HII galaxy. From our Spitzer-IRS mid-IR spectroscopy, we have found the first evidence for an obscured AGN in NGC 1448. On the basis of this data, NGC 1448 appears to be harboring a rapidly growing small obscured black hole (M_BH ~ 6x10^5 M_Sun; Eddington ratio of >0.1), and therefore appears to be an analog of the nearby Compton-thick AGN NGC 4945. To date, no sensitive hard X-ray constraints exist for NGC 1448, which are required to provide a direct measurement of the absorption and mass accretion rate, and thus to test if NGC 1448 is also a Compton-thick AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | DAVID ALEXANDER | EUR | 3 | AO3 | NGC 1448: A MISSING COMPTON-THICK AGN IN OUR BACKYARD? | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703062010/ | Quick Look | ![]() |
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495 | NGC 4138 | 182.4434 | 43.7345 | 181.812692 | 44.012643 | 161.129219 | 40.276316 | 147.09151655 | 71.38668226 | 137.6226 | 55137.5331365741 | 2009-11-02 12:47:43 | 55138.8849305556 | 2009-11-03 21:14:18 | 704047010 | 60.7716 | 60 | 60.8436 | 60.7716 | 0 | 60.8436 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.8724 | 35.8724 | 116.7818 | 2 | PROCESSED | 57549.0852893518 | 2016-06-10 02:02:49 | 55517 | 2010-11-17 00:00:00 | 55151.1923263889 | 2009-11-16 04:36:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041415 | The SWIFT BAT hard (14-195 KeV) survey is performing the first unbiased hard X-ray survey of the entire sky with follow-up observations with the Swift XRT to fully identify the sample. In this survey we have found two very low luminosity nearby hard X-ray sources which show little, if any, evidence for nuclear activity in the optical or UV band, and have very low apparent Eddington ratios. We propose Suzaku observations of these objects to determine whether there is an X-ray spectral signature of a low Eddington ratio, as predicted if these objects are indeed in a radiatively inefficient accretion flow. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RICHARD MUSHOTZKY | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF NGC4138 AND NGC3718 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704047010/ | Quick Look | ![]() |
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496 | EMS1160 | 264.608 | 87.3047 | 269.889788 | 87.318057 | 90.726547 | 69.241949 | 120.03425165 | 27.94259409 | 59.9344 | 55312.9874537037 | 2010-04-26 23:41:56 | 55313.4279513889 | 2010-04-27 10:16:15 | 705012010 | 20.2796 | 20 | 20.2796 | 20.2796 | 0 | 20.2796 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.8004 | 19.8004 | 38.0539 | 1 | PROCESSED | 57551.2894097222 | 2016-06-12 06:56:45 | 55693 | 2011-05-12 00:00:00 | 55327.1544791667 | 2010-05-11 03:42:27 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050050 | We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 5 | AO5 | SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705012010/ | Quick Look | ![]() |
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497 | EMS1388 | 309.878 | -56.3562 | 308.912808 | -56.532938 | 296.209629 | -36.489343 | 341.17879119 | -37.12820094 | 256.6037 | 55497.456400463 | 2010-10-28 10:57:13 | 55498.1383912037 | 2010-10-29 03:19:17 | 705028010 | 21.5336 | 20 | 21.5416 | 21.5416 | 0 | 21.5336 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.3735 | 18.3735 | 58.9099 | 0 | PROCESSED | 57553.876724537 | 2016-06-14 21:02:29 | 55875 | 2011-11-10 00:00:00 | 55508.9886342593 | 2010-11-08 23:43:38 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050126 | Fermi Gamma-ray Space Telescope has detected a lot of unidentified GeV sources in high latitude. Among these, we focus on five Fermi unIDs whose error circles contain ROSAT faint X-ray sources and propose an X-ray follow-up observation with Suzaku. From an X-ray spectral and variability information, we identify these objects, as well as find new class of GeV emitters. We also aim to study emission and particle acceleration mechanism of these objects. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YASUYUKI TANAKA | JAP | 5 | AO5 | SEARCH FOR X-RAY COUNTERPARTS OF FERMI HIGH-LATITUDE UNIDENTIFIED GEV SOURCES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705028010/ | Quick Look | ![]() |
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498 | B3 0309+411 | 48.2809 | 41.3324 | 47.459303 | 41.145685 | 57.252935 | 22.518841 | 149.59257755 | -14.09014879 | 253.0016 | 55976.5100462963 | 2012-02-19 12:14:28 | 55979.0410532407 | 2012-02-22 00:59:07 | 706036010 | 104.6245 | 100 | 104.6245 | 104.6296 | 0 | 104.6245 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95.453 | 95.453 | 218.6719 | 2 | PROCESSED | 57604.7018981482 | 2016-08-04 16:50:44 | 56360 | 2013-03-09 00:00:00 | 55992.2317824074 | 2012-03-06 05:33:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062007 | We propose to observe B3 0309+411, an X--ray bright FRII BLRG detected by INTEGRAL for 100 ks. BRLGs have been poorly studied in X-rays and usually show weak reprocessing spectral features with respect to their radio-quiet counterparts. B3 0309+411 has been already followed-up with XMM-Newton and, the XMM-Newton and INTEGRAL data suggests that the source could 1) be strongly reflection-dominated; 2) exhibit extreme flux/spectral variability; 3) be severely affected by absorption. The Suzaku observation will unveil the puzzling spectral shape of this peculiar BLRG, allowing to determine with accuracy the reflection properties which would have a large impact on our understanding of the disk/jet contribution in BLRG. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | FRANCESCA PANESSA | EUR | 6 | AO6 | B3 0309+411: A REFLECTION--DOMINATED BROAD LINE RADIO GALAXY? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706036010/ | Quick Look | ![]() |
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499 | FAIRALL 51 | 281.2238 | -62.3567 | 280.059933 | -62.408117 | 276.678489 | -39.176005 | 333.20743511 | -23.0882296 | 252.0031 | 56539.073587963 | 2013-09-04 01:45:58 | 56539.5245486111 | 2013-09-04 12:35:21 | 708046010 | 31.5576 | 30 | 31.5576 | 31.5676 | 0 | 31.5656 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.6549 | 25.6549 | 38.9559 | 0 | PROCESSED | 57612.4964236111 | 2016-08-12 11:54:51 | 56956 | 2014-10-26 00:00:00 | 56587.5110763889 | 2013-10-22 12:15:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082016 | Fairall 51 is a variable bright active galaxy (about 1 millicrab), classified as a polar-scattered Seyfert~1 galaxy. It was observed twice with high-quality X-ray spectrometers on-board the XMM-Newton satellite. The two observations are separated by half a year and the spectra significantly differ from each other. The difference can be well explained by a variable covering fraction of a cold (very low-ionised) absorber (Ricci et al., 2010). Two additional Swift data, separated by five days, suggest that the variability may occur at time-scales as short as a few days. The ultimate goal of the proposal is to locate this variable absorber by the determination of the typical time-scale of the variability. We therefore propose a series of observations of Fairall 51 with short exposures. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JIRI SVOBODA | EUR | 8 | AO8 | STUDY OF THE VARIABLE ABSORBER IN A BRIGHT ACTIVE GALAXY FAIRALL 51 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708046010/ | Quick Look | ![]() |
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500 | NGC2273 | 102.5972 | 60.7838 | 101.469265 | 60.841838 | 97.733599 | 37.680709 | 155.04232679 | 23.32753471 | 246.2514 | 54211.2737384259 | 2007-04-21 06:34:11 | 54212.5071643518 | 2007-04-22 12:10:19 | 702003010 | 90.0126 | 50 | 90.0286 | 90.0206 | 0 | 90.0126 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69.5887 | 69.5887 | 106.5579 | 1 | PROCESSED | 57538.4439583333 | 2016-05-30 10:39:18 | 54744 | 2008-10-05 00:00:00 | 54216.1628703704 | 2007-04-26 03:54:32 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020005 | Compton thick Seyfert 2 galaxies may constitute a large fraction of the Seyfert 2 galaxy's population. However, the nature of the Compton-thick objects is still unclear due to the heavy obscuration of the nuclear emission. The wide-band spectroscopy with Suzaku is crucial to expose their nature hidden by thick matter. In order to reveal their nature in the local Universe, we propose Suzaku observations of Risaliti's Compton-thick objects. These observations will also bring us important results to study the structure and evolution of active galactic nuclei. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HISAMITSU AWAKI | JAP | 2 | AO2 | REVEAL THE NATURE OF COMPTON THICK SEYFERT 2 GALAXIES WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702003010/ | Quick Look | ![]() |
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501 | NGC 4941 | 196.0528 | -5.5595 | 195.404956 | -5.291518 | 196.919842 | 1.18027 | 308.80102111 | 57.16661738 | 292.811 | 56100.4695833333 | 2012-06-22 11:16:12 | 56102.2446643518 | 2012-06-24 05:52:19 | 707001010 | 80.8593 | 80 | 80.8593 | 80.8593 | 0 | 80.8593 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 76.7486 | 76.7486 | 153.32 | 1 | PROCESSED | 57605.7725115741 | 2016-08-05 18:32:25 | 56480 | 2013-07-07 00:00:00 | 56113.2872800926 | 2012-07-05 06:53:41 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070003 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Previously, such studies have been limited to AGNs with intermediate to high luminosities. Here we propose to observe two of the lowest luminosity AGNs in the latest BAT catalog to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 7 | AO7 | BROAD BAND SPECTRA OF HARD X-RAY SELECTED LOW LUMINOSITY AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707001010/ | Quick Look | ![]() |
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502 | 2FGL J0022.2-1853 | 5.5431 | -18.8956 | 4.911171 | -19.172887 | 357.260083 | -19.481593 | 82.15155077 | -79.37005347 | 62.0041 | 56077.5533564815 | 2012-05-30 13:16:50 | 56078.2856944445 | 2012-05-31 06:51:24 | 707009010 | 34.8678 | 30 | 34.8678 | 34.8678 | 0 | 34.8678 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.1964 | 35.1964 | 63.2639 | 1 | PROCESSED | 57605.5769444444 | 2016-08-05 13:50:48 | 56456 | 2013-06-13 00:00:00 | 56090.1516435185 | 2012-06-12 03:38:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070034 | We propose Suzaku observations of "unusual" Fermi-LAT sources 2FGL J0022.2, J0037.8 and J0157.2, which are yet unidentified in gamma-ray, but their counterparts have already been detected with snapshot (typically 5ksec) Swift XRT observations. Their positions are determined with an excellent accuracy of several arcseconds. Since all three sources are detected both in radio and X-rays, they could be most likely AGN jet sources but their spectral energy distributions are far from what expected from typical blazars, suggesting "new-type" AGN sources. We propose 30 ksec observations of each to investigate temporal variability, as well as to determine wideband XIS/HXD spectra between 0.5-30 keV (J01572.2 is detectable with HXD/PIN). | EXTRAGALACTIC COMPACT SOURCES | 7 | B | JUN KATAOKA | JAP | 7 | AO7 | FURTHER CHALLENGES TO UNUSUAL FERMI-UNIDS WITH SUZAKU X-RAY OBSERVATORY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707009010/ | Quick Look | ![]() |
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503 | NGC1365 | 53.4048 | -36.1458 | 52.927471 | -36.312752 | 36.803781 | -53.045581 | 237.96516908 | -54.5951856 | 59.0002 | 56116.8446064815 | 2012-07-08 20:16:14 | 56117.6910763889 | 2012-07-09 16:35:09 | 707017020 | 33.5858 | 30 | 33.5938 | 33.6018 | 0 | 33.5858 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.579 | 32.579 | 73.1059 | 2 | PROCESSED | 57606.5919791667 | 2016-08-06 14:12:27 | 56508 | 2013-08-04 00:00:00 | 56142.1709606482 | 2012-08-03 04:06:11 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070095 | NGC1365 is one of AGNs which shows the most highly variable spectral change, and furthermore exhibits strong Fe-K absorption lines blue-shifted by 1000--5000 km/s with EW of about 100eV. These absorption lines indicate a massive outflow and are important to consider the AGN feedback to parent galaxies. Currently, there is no other object by which we can measure the Fe-K absorption lines accurately than NGC 1365. Therefore, we propose to monitor a velocity, depth, and ratio of blue-shifted Fe-K absorption lines, hard X-ray flux above 10 keV of NGC1365 every 10 days, in order to probe the massive outflow dynamically and compare the results with the numerical simulation. } | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YASUSHI FUKAZAWA | JAP | 7 | AO7 | MONITOR OF VELOCITY AND STRENGTH OF BLUE-SHIFTED STRONG FE-K ABSORPTION LINES OF NGC 1365 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707017020/ | Quick Look | ![]() |
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504 | HE0512-3329 | 78.5402 | -33.4449 | 78.079903 | -33.501337 | 72.668068 | -56.200323 | 236.63398617 | -33.8579138 | 105.1284 | 56932.4291435185 | 2014-10-02 10:17:58 | 56932.6252083333 | 2014-10-02 15:00:18 | 709020010 | 6.8649 | 60 | 6.873 | 6.8729 | 0 | 6.8649 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.600474537 | 2016-08-16 14:24:41 | 57345 | 2015-11-19 00:00:00 | 56979.403125 | 2014-11-18 09:40:30 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091431 | The origin of AGN iron K alpha emission has been debated for two decades. We propose to constrain iron line emission sizes using quasar X-ray microlensing. Our Chandra Cycle 11 observations have shown that the iron line equivalent widths (EWs) in six lensed systems are significantly higher than those measured in local AGNs. This implies that the iron line emission is microlensed more strongly than the X-ray continuum and originates from very compact regions. We propose to confirm the high iron line EWs in lensed quasars by monitoring two more lenses, Q0142-100 and HE0512+3329 using Suzaku, with a total exposure time 115 kilo-seconds. This will provide independent constraints for settling the debate on the origin of the iron line emission. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | BIN CHEN | USA | 9 | AO9 | CONSTRAINING QUASAR IRON LINE EMISSION USING MICROLENSING | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709020010/ | Quick Look | ![]() |
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505 | NGC 3516 | 166.74 | 72.5773 | 165.887815 | 72.847717 | 123.371896 | 57.999258 | 133.21492543 | 42.40213112 | 153.6201 | 56572.1874537037 | 2013-10-07 04:29:56 | 56573.9780092593 | 2013-10-08 23:28:20 | 708006050 | 0 | 50 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 37.2053 | 37.2053 | 154.6998 | 0 | PROCESSED | 57612.8632291667 | 2016-08-12 20:43:03 | 56383 | 2013-04-01 00:00:00 | 56631.766712963 | 2013-12-05 18:24:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080066 | We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 8 | AO8 | THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006050/ | Quick Look | ![]() |
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506 | HOLMBERG II X-1 | 124.8826 | 70.7169 | 123.581394 | 70.873481 | 106.843254 | 49.308296 | 144.27185866 | 32.72527495 | 119.959 | 56562.4955555556 | 2013-09-27 11:53:36 | 56563.5730324074 | 2013-09-28 13:45:10 | 708015020 | 49.283 | 50 | 49.283 | 49.283 | 0 | 49.283 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.206 | 48.206 | 93.0879 | 0 | PROCESSED | 57612.7832986111 | 2016-08-12 18:47:57 | 56954 | 2014-10-24 00:00:00 | 56588.5225462963 | 2013-10-23 12:32:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081251 | Recent X-ray observations have produced evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in an unusual super-Eddington state. Current data are unable to deliver a clear answer, as attempts to model the 0.5-10keV spectra have been plagued by degeneracies resulting from the limited bandpass, owing to the previous lack of focusing hard X-ray telescopes. Combined, Suzaku and NuSTAR will obtain high-quality spectra covering 0.5-30keV, providing powerful probes for understanding the accretion modes and nature of the central BHs. A definitive statement on the existence of either 100-1000Msun black holes or extreme accretion states will be an important legacy of both missions. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | DOMINIC WALTON | USA | 8 | AO8 | COORDINATED SUZAKU AND NUSTAR OBSERVATIONS OF HOLMBERG II X-1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708015020/ | Quick Look | ![]() |
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507 | ARP220 | 233.7664 | 23.5658 | 233.223657 | 23.731386 | 223.777121 | 41.366844 | 36.73879852 | 53.01919685 | 114.8377 | 53742.3490856482 | 2006-01-07 08:22:41 | 53744.9654398148 | 2006-01-09 23:10:14 | 700006010 | 98.5506 | 100 | 98.5586 | 98.5506 | 98.5586 | 98.5586 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 93.3623 | 93.3623 | 226.0419 | 2 | PROCESSED | 57532.6850925926 | 2016-05-24 16:26:32 | 54247 | 2007-05-27 00:00:00 | 54040.0356597222 | 2006-11-01 00:51:21 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001033 | We propose a 100 ks observation of the nearest ultraluminous infrared galaxy (ULIG) Arp220. The major objective is to search for evidence of heavily obscured nuclei. First detection of a Compton-thick source may be possible with the HXD's sensitivity, if a powerful nucleus is present, leading to a major discovery. The good quality XIS spectrum can be decisive for the origin of the strong Fe K line, barely detected with the previous XMM-Newton observation. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KAZUSHI IWASAWA | JAP | 0 | SWG | HARD X-RAY EMISSION FROM THE NEAREST ULTRALUMINOUS INFRARED GALAXY ARP220 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700006010/ | Quick Look | ![]() |
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508 | M81 | 148.8829 | 69.0533 | 147.858629 | 69.290285 | 119.502258 | 51.56628 | 142.10623941 | 40.90540672 | 287.1391 | 57160.4721180556 | 2015-05-18 11:19:51 | 57162.9807523148 | 2015-05-20 23:32:17 | 710017010 | 97.7022 | 100 | 97.7022 | 99.738 | 0 | 99.7444 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0.3 | 0 | PROCESSED | 57618.7210532407 | 2016-08-18 17:18:19 | 57543 | 2016-06-04 00:00:00 | 57177.3710300926 | 2015-06-04 08:54:17 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 102700 | We propose to observe the Low-Luminosity Active Galactic Nucleus of M81 for 200 ksec with NuSTAR and for 100 ksec with Suzaku. In low accretion rate AGN, where does the optically thick part of the accretion disk stop? Does it go in to within a few gravitational radii of the black hole, as in higher accretion rate Seyfert galaxies, or does it stop hundreds of gravitational radii from the black hole? Using NuSTAR and Suzaku spectra we will measure the strengths of the Compton reflection hump, Fe K alpha, Fe XXV and Fe XXVI lines. This will determine whether the Fe K alpha line is produced by reflection off the optically thick outer disk, or is produced in the optically thin inner flow. We will measure the reflection fraction and constrain the source geometry and disk transition radius. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ANDREW YOUNG | EUR | 10 | AO10 | M81: ACCRETION GEOMETRY AT LOW EDDINGTON RATES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710017010/ | Quick Look | ![]() |
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509 | WKK 4438 | 223.8214 | -51.5512 | 222.94068 | -51.348796 | 237.577105 | -33.176773 | 321.7239088 | 6.74451921 | 87.8973 | 55948.1066319445 | 2012-01-22 02:33:33 | 55950.0610069444 | 2012-01-24 01:27:51 | 706011010 | 70.3088 | 100 | 70.3168 | 70.3088 | 0 | 70.3248 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61.486 | 61.486 | 168.8259 | 3 | PROCESSED | 57604.5330324074 | 2016-08-04 12:47:34 | 56469 | 2013-06-26 00:00:00 | 56103.2331597222 | 2012-06-25 05:35:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060032 | We propose to observe two hard X-ray bright narrow-line Seyfert 1 galaxies, which are an important class of objects in studying accretion processes under a large mass accretion rate and therefore mass growth of black holes. Our aims are (1) to measure a continuum shape such as spectral slope and high energy cutoff, (2) to compare them with other classes of AGNs, and (3) to search for highly ionized outflows with a large column density. All of these will be a fundamental piece of information to better understand accretion physics and ``feedback'' processes in galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YUICHI TERASHIMA | JAP | 6 | AO6 | ACCRETION AND OUTFLOW IN THE HARD X-RAY SELECTED NARROW-LINE SEYFERT 1S | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706011010/ | Quick Look | ![]() |
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510 | UGC5101 | 143.841 | 61.3185 | 142.895417 | 61.541858 | 122.479903 | 43.806931 | 152.55229096 | 42.85621781 | 331.581 | 53825.1798148148 | 2006-03-31 04:18:56 | 53826.3509722222 | 2006-04-01 08:25:24 | 701002010 | 48.9902 | 70 | 48.9902 | 48.9902 | 48.9902 | 48.9902 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 43.9748 | 43.9748 | 101.1779 | 0 | PROCESSED | 57533.3610763889 | 2016-05-25 08:39:57 | 54735 | 2008-09-26 00:00:00 | 53905.890625 | 2006-06-19 21:22:30 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010001 | We propose Suzaku observations at E > 10 keV of nearby ultraluminous infrared galaxies (ULIRGs), for which our infrared spectroscopy has strongly suggested the presence of luminous AGNs deeply buried in gas and dust. However, extreme starbursts are still a possibility. Through the proposed X-ray observations using Suzaku, we aim to distinguish clearly between buried AGNs (strong X-ray emitters) and extreme starbursts (weak X-ray emitters), and to obtain convincing evidence for luminous buried AGNs. Since buried AGNs in these ULIRGs' cores are likely to suffer from Compton-thick X-ray absorption, the high sensitivity at E > 10 keV achieved by Suzaku HXD PIN is crucial for the success of this experiment. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MASATOSHI IMANISHI | JAP | 1 | AO1 | COMPTON THICK BURIED AGNS IN NEARBY ULTRALUMINOUS INFRARED GALAXIES | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701002010/ | Quick Look | ![]() |
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511 | IRAS13224-3809 | 201.327 | -38.416 | 200.607672 | -38.155977 | 214.865009 | -27.173801 | 310.18598264 | 23.97820794 | 118.5234 | 54126.2420601852 | 2007-01-26 05:48:34 | 54131.0849421296 | 2007-01-31 02:02:19 | 701003010 | 197.9376 | 200 | 197.9536 | 197.9376 | 0 | 197.9516 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 169.6526 | 169.6526 | 418.3978 | 4 | PROCESSED | 57537.0458912037 | 2016-05-29 01:06:05 | 54777 | 2008-11-07 00:00:00 | 54139.7293287037 | 2007-02-08 17:30:14 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010028 | We propose a 200 ks continuous observation of the narrow-line Seyfert 1 galaxy IRAS13224-3809 in order to understand its remarkable and puzzling spectral and variability properties. Suzaku data will enable us to disentangle the two interpretations adopted so far, namely partial covering and relativistically blurred reflection. If the latter then the appearance of the source is controlled by general relativistic effects. In addition, the ability for Suzaku to conduct long continuous observations will allow us to monitor IRAS13224-3809 for giant amplitude flaring (as seen with ROSAT); therefore enabling us to enhance our understanding of AGN variability. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YASUO TANAKA | JAP | 1 | AO1 | THE REMARKABLE NARROW LINE SEYFERT 1 GALAXY IRAS13224-3809 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701003010/ | Quick Look | ![]() |
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512 | SWIFT J0918.5+0425 | 139.5114 | 4.476 | 138.856225 | 4.686688 | 140.50448 | -10.713106 | 227.10001498 | 34.41934616 | 102.3204 | 54408.8894097222 | 2007-11-04 21:20:45 | 54410.2293981482 | 2007-11-06 05:30:20 | 702076010 | 61.0185 | 53 | 61.0185 | 61.0401 | 0 | 61.0185 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 56.1565 | 56.1565 | 115.7659 | 2 | PROCESSED | 57540.4472916667 | 2016-06-01 10:44:06 | 54787 | 2008-11-17 00:00:00 | 54419.0312847222 | 2007-11-15 00:45:03 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021372 | The nature and even the existence of type II quasars is highly controversial. Due to their highly obscured nature, very hard (> 15 keV) observations are needed to probe their properties. With the 9-month SWIFT BAT all-sky AGN survey, detection of heavily obscured sources is now possible. Indeed, 6 type II quasars have been identified. Their properties, however, are a challenge to standard AGN models e.g., all but one of these sources are strong radio sources and several have optical spectra indicative of an un-absorbed source. We propose Suzaku observations of the 5 without broadband high signal to noise x-ray data to perform a detailed analysis of their x-ray properties and to understand their relationship to the lower luminosity well studied Seyfert IIs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | RICHARD MUSHOTZKY | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF SWIFT BAT TYPE II QUASARS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702076010/ | Quick Look | ![]() |
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513 | 1H 0419-577 | 66.5658 | -57.2343 | 66.322649 | -57.345613 | 29.362681 | -75.708089 | 267.01881665 | -41.95465908 | 226.9739 | 55212.4834259259 | 2010-01-16 11:36:08 | 55214.8224421296 | 2010-01-18 19:44:19 | 704064010 | 122.8354 | 140 | 123.1154 | 122.8354 | 0 | 123.1154 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 113.4392 | 113.4392 | 202.0668 | 4 | PROCESSED | 57550.2328472222 | 2016-06-11 05:35:18 | 55594 | 2011-02-02 00:00:00 | 55228.2152893518 | 2010-02-01 05:10:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041417 | A 'hard excess' has been detected in 2007 Suzaku PIN data for the nearby quasar 1H 0419-577 relative to models fitting below 10 keV. The excess can be accounted for with Compton-thick partial-covering gas probably part of a clumpy disk wind originating inside of the BLR. The observed Fe Ka line luminosity is consistent with an origin in an equatorial wind. Blurred reflection models cannot satisfactorily fit the source and so 1H0419-577 provides a rare distinction between two observationally-similar classes of model. We propose two 140 ks follow-up Suzaku observations separated by months to probe the properties of the Compton-thick gas via variability measurements: this is an important new science area that can only be studied using the broad bandpass available from Suzaku. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TRACEY TURNER | USA | 4 | AO4 | STUDYING THE COMPTON-THICK PARTIAL-COVERING ABSORPTION IN 1H 0419-577 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704064010/ | Quick Look | ![]() |
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514 | 3C 105 | 61.8399 | 3.6518 | 61.183972 | 3.519003 | 60.504157 | -16.952891 | 187.66746701 | -33.63397375 | 251.3728 | 54501.5363078704 | 2008-02-05 12:52:17 | 54503.0833912037 | 2008-02-07 02:00:05 | 702074010 | 38.319 | 53 | 38.319 | 38.319 | 0 | 38.319 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.8811 | 48.8811 | 133.6558 | 2 | PROCESSED | 57541.5364351852 | 2016-06-02 12:52:28 | 54883 | 2009-02-21 00:00:00 | 54515.7678819444 | 2008-02-19 18:25:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021372 | The nature and even the existence of type II quasars is highly controversial. Due to their highly obscured nature, very hard (> 15 keV) observations are needed to probe their properties. With the 9-month SWIFT BAT all-sky AGN survey, detection of heavily obscured sources is now possible. Indeed, 6 type II quasars have been identified. Their properties, however, are a challenge to standard AGN models e.g., all but one of these sources are strong radio sources and several have optical spectra indicative of an un-absorbed source. We propose Suzaku observations of the 5 without broadband high signal to noise x-ray data to perform a detailed analysis of their x-ray properties and to understand their relationship to the lower luminosity well studied Seyfert IIs. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RICHARD MUSHOTZKY | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF SWIFT BAT TYPE II QUASARS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702074010/ | Quick Look | ![]() |
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515 | ESO 263-G013 | 152.4256 | -42.8603 | 151.905124 | -42.614062 | 176.412344 | -49.376708 | 273.99206854 | 10.74227458 | 292.0779 | 54252.4568287037 | 2007-06-01 10:57:50 | 54253.5946064815 | 2007-06-02 14:16:14 | 702120010 | 45.2947 | 40 | 45.3027 | 45.3027 | 0 | 45.2947 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.1035 | 40.1035 | 98.2999 | 2 | PROCESSED | 57538.8009143518 | 2016-05-30 19:13:19 | 54745 | 2008-10-06 00:00:00 | 54258.5006134259 | 2007-06-07 12:00:53 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022033 | The high-energy detectors onboard Swift and INTEGRAL are mapping the hard (>10 keV) X-ray sky. Although limited to bright X-ray fluxes (~1e-11 erg/cm2/s), the large area surveyed so far has allowed to build up sizable samples of hard X-ray selected AGN almost unbiased against X-ray absorption. On the basis of a careful analysis of the available X-ray observations below 10 keV, we identified a sample of relatively bright AGN which are likely to be obscured by Compton-thick (logN_H >24) cold gas. Two of them were observed in EAO-1 and the results confirmed our predictions. We propose further Suzaku observations of 3 bright objects (F(20-40 keV) ~ 0.7-1.4 x 1e-11 erg/cm2/s) which will allow us to unveil previously unknown nearby heavily obscured AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | ANDREA COMASTRI | EUR | 2 | AO2 | BRIGHT COMPTON-THICK GALAXIES IN THE BACKYARD - PART II | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702120010/ | Quick Look | ![]() |
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516 | NGC 7469 | 345.7842 | 8.9301 | 345.154297 | 8.660604 | 350.460681 | 13.82437 | 83.10914575 | -45.403242 | 63.4793 | 54641.7015856482 | 2008-06-24 16:50:17 | 54644.683599537 | 2008-06-27 16:24:23 | 703028010 | 112.1128 | 100 | 112.1251 | 112.1331 | 0 | 112.1128 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91.5571 | 91.5571 | 257.6126 | 2 | PROCESSED | 57542.968125 | 2016-06-03 23:14:06 | 55027 | 2009-07-15 00:00:00 | 54658.7891319444 | 2008-07-11 18:56:21 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031311 | We propose a 100 ksec observation of the X-ray bright Seyfert 1 AGN NGC 7469, a strong candidate for having ionized reflection from the accretion disk. Only the broad bandpass provided by Suzaku, including >12 keV coverage via the HXD, will allow us to deconvolve the broadband emitting components, including the strong Compton reflection hump, broad Fe K line, and soft excess. With the XIS, we will study in detail the Fe K emission complex, including the narrow 6.4 keV Fe K core and in particular the prominent ``blue wing'' near 6.9 keV. Our proposed observation will thus be an example of how broad bandpass X-ray observations can critically test blurred, ionized disk reflection model in Seyfert 1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | ALEX MARKOWITZ | USA | 3 | AO3 | IONIZED DISK REFLECTION IN THE SEYFERT AGN NGC 7469 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703028010/ | Quick Look | ![]() |
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517 | IRAS 12072-0444 | 182.4393 | -5.0116 | 181.797769 | -4.733385 | 184.228917 | -3.627834 | 283.97337665 | 56.31820605 | 111.9489 | 55534.0444328704 | 2010-12-04 01:03:59 | 55535.5169328704 | 2010-12-05 12:24:23 | 705045010 | 61.9339 | 60 | 61.9419 | 61.9419 | 0 | 61.9339 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.1596 | 28.1596 | 127.206 | 0 | PROCESSED | 57554.3475810185 | 2016-06-15 08:20:31 | 55910 | 2011-12-15 00:00:00 | 55544.3011226852 | 2010-12-14 07:13:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051441 | We propose two Suzaku-HXD observations of two ULIRGs hosting a deeply buried AGN. These two objects are expected to host a powerful AGN in the luminosity range of quasars, based on solid evidence from mid-IR Spitzer spectroscopy. However, these sources are completely buried behind a screen of dust with column density in excess of 10^24 cm^-2, so not only the primary emission below 10 keV is obscured, but the reflected emission, usually ascribed to a circumnuclear "torus", is also absent. This suggests a complete spherical coverage of the X-ray source along all directions. The unique capabilities of Suzaku at high energies will allow to confirm the existence of these objects, representing the most extreme examples of buried AGNs, both in terms of obscuration and of intrinsic luminosity. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | GUIDO RISALITI | USA | 5 | AO5 | BURIED QUASAR 2S INSIDE ULIRGS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705045010/ | Quick Look | ![]() |
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518 | NGC 6814 | 295.6733 | -10.3371 | 294.986368 | -10.456223 | 295.709061 | 10.841132 | 29.34034439 | -16.02176478 | 260.0004 | 55867.6992013889 | 2011-11-02 16:46:51 | 55868.637662037 | 2011-11-03 15:18:14 | 706032010 | 42.12 | 40 | 42.1435 | 42.136 | 0 | 42.12 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.0918 | 40.0918 | 81.0698 | 1 | PROCESSED | 57603.6893518518 | 2016-08-03 16:32:40 | 56248 | 2012-11-17 00:00:00 | 55881.0746527778 | 2011-11-16 01:47:30 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061411 | Fermi-LAT has revealed gamma-ray emission from Seyfert galaxies in its 1st catalog. Optical and X-ray spectra of Seyferts generally provide important clues to the nature of the accretion process, and thus those objects are promising targets to investigate the connection of the jet to the central source. Here, we propose Suzaku observations of three Seyfert-type AGNs from our gamma-ray candidate list: those objects are also present in the Swift-BAT catalog. Those are III Zw 2, NGC 6814 and ESO 323-G077 and we request pointings of 80 ks, 40 ks and 40 ks respectively. All three candidates appear to be associated with AGN, but show different radio or IR properties. Suzaku data will give us crucial information to investigate the origin of high-energy emission from those Seyfert objects. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MASAAKI HAYASHIDA | USA | 6 | AO6 | SUZAKU OBSERVATIONS OF SEYFERT GALAXIES AS GAMMA-RAY SOURCE CANDIDATES SELECTED FROM THE SWIFT-BAT CATALOG | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706032010/ | Quick Look | ![]() |
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