DARTS Astro

total 518

No.
target_name
center_ra
center_dec
center_ra_b1950
center_dec_b1950
center_ecliptic_lon
center_ecliptic_lat
center_galactic_lon
center_galactic_lat
roll_angle
observation_start_time_mjd
observation_start_time
observation_end_time_mjd
observation_end_time
observation_id
exposure
proposal_exposure
xis0_exposure
xis1_exposure
xis2_exposure
xis3_exposure
xis0_observation_mode
xis1_observation_mode
xis2_observation_mode
xis3_observation_mode
hxd_observation_mode
hxd_coarse_clock_rate_exposure
hxd_first_clock_rate_exposure
hxd_normal_clock_rate_exposure
hxd_all_clock_rate_exposure
hxd_wam_exposure
hxd_burst_num
processing_status
processing_end_time_mjd
processing_end_time
public_date_mjd
public_date
distribute_start_date_mjd
distribute_start_date
processing_version
processing_quantity
processing_software
proposal_id
proposal_abstract
proposal_category
proposal_category_code
proposal_priority
pi_name
co_pi_name
proposal_affiliated_country
proposal_cycle_count
observation_type
proposal_title
main_detector
xis_injection_flag
data_access_url
ql_access_url
ql_image_url
1 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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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/