DARTS Astro

total 181

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 4U 1820-30 275.9251 -30.4172 275.121541 -30.443999 275.136917 -7.082068 2.74021083 -7.94370371 265.2009 55111.1096643518 2009-10-07 02:37:55 55111.700162037 2009-10-07 16:48:14 404069050 21.7674 20 21.7674 21.7674 0 21.7674 1 1 0 1 1 0 0 15.6743 15.6743 51.0039 0 PROCESSED 57548.7799884259 2016-06-09 18:43:11 55496 2010-10-27 00:00:00 55127.2938194445 2009-10-23 07:03:06 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 042004 Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. GALACTIC POINT SOURCES 4 A MANUEL LINARES EUR 4 AO4 ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404069050/ Quick Look
3 GX 9+9 262.9404 -16.8929 262.215892 -16.856936 263.194726 6.381396 8.57505694 9.06920034 97.5329 55271.6738773148 2010-03-16 16:10:23 55273.9918981482 2010-03-18 23:48:20 404071010 85.1871 75 85.2087 85.2031 0 85.1871 2 1 0 2 1 0 0 61.6942 61.6942 200.2639 0 PROCESSED 57550.9767476852 2016-06-11 23:26:31 55652 2011-04-01 00:00:00 55285.4179513889 2010-03-30 10:01:51 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 042011 We propose two 75 ks Suzaku observations of the bright neutron star low mass X-ray binary (LMXB) GX9+9, spread over six months. We will investigate the presence of X-ray narrow absorption features in the Suzaku spectra, which are a signature of a disk wind. Such features, identified with ions such as Fe XXV and Fe XXVI, have been observed in a number of LMXBs and give us information about the mass outflow rate and the launching mechanism of the wind. We will study the connection of the disk wind to the presence of radio jet emission with simultaneous radio observations. Finally, we will determine if the broad Fe emission line indicated by the XMM-Newton spectrum is relativistically broadened. Variability will be studied as a function of accretion rate in the two proposed observations. GALACTIC POINT SOURCES 4 B MARIA DIAZ TRIGO EUR 4 AO4 A STUDY OF THE DISK WIND-JET CONNECTION IN GX9+9 WITH MULTIWAVELENGTH OBSERVATIONS HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404071010/ Quick Look
4 G54.1+0.3 292.6593 18.8091 292.105949 18.703083 298.434306 40.039537 54.05763723 0.20765467 245.096 54403.6644560185 2007-10-30 15:56:49 54406.3335532407 2007-11-02 08:00:19 502077010 101.6411 100 101.6411 101.6491 0 101.6491 2 2 0 2 1 0 0 92.9235 92.9235 230.5857 3 PROCESSED 57540.4530324074 2016-06-01 10:52:22 54786 2008-11-16 00:00:00 54417.8870833333 2007-11-13 21:17:24 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 022032 A proprietary XMM-Newton observation reveals that the pulsar wind nebula G54.1+0.3 has a very hard spectrum (gamma ~ 1.5) and possibly a break between 5 and 10 keV. We propose a 100 ks SUZAKU observation to confirm unambiguously the presence of the break. If confirmed, the break would pose stringent constraints on models of electron emission and propagation in pulsar wind nebulae. GALACTIC DIFFUSE EMISSION 5 C FABRIZIO BOCCHINO EUR 2 AO2 THE BREAK IN THE HARD X-RAY ENERGY OF THE PULSAR WIND NEBULA G54.1+0.3 HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502077010/ Quick Look
5 HER X-1 254.4632 35.2657 254.012163 35.341297 246.023504 57.418254 58.05457552 37.50615868 268.4858 55461.0002083333 2010-09-22 00:00:18 55461.4494675926 2010-09-22 10:47:14 405058030 19.924 20 19.924 19.924 0 20.2438 2 2 0 1 1 0 0 17.5073 17.5073 38.8119 0 PROCESSED 57553.4994560185 2016-06-14 11:59:13 55836 2011-10-02 00:00:00 55470.1508796296 2010-10-01 03:37:16 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 052001 We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity? GALACTIC POINT SOURCES 4 B R DIGER STAUBERT EUR 5 AO5 VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1 HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405058030/ Quick Look
6 GX 339-4 255.7015 -48.7852 254.753736 -48.714186 259.571673 -25.859287 338.94105133 -4.32146688 83.6944 55603.7634722222 2011-02-11 18:19:24 55604.2349421296 2011-02-12 05:38:19 405063010 22.4594 100 22.4594 22.4594 0 22.4834 2 2 0 2 1 0 0 19.3287 19.3287 40.7279 0 PROCESSED 57600.9244675926 2016-07-31 22:11:14 55983 2012-02-26 00:00:00 55617.4120601852 2011-02-25 09:53:22 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 052015 We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 GALACTIC POINT SOURCES 4 A CLEMENT CABANAC EUR 5 AO5-TOO PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405063010/ Quick Look
7 GX 339-4 255.7013 -48.7848 254.753541 -48.713785 259.571479 -25.858904 338.94128957 -4.32111913 86.3597 55608.9686111111 2011-02-16 23:14:48 55609.6501967593 2011-02-17 15:36:17 405063020 21.0157 20 21.0157 21.0157 0 21.0157 2 2 0 2 1 0 0 17.5958 17.5958 58.8839 0 PROCESSED 57600.9613773148 2016-07-31 23:04:23 55988 2012-03-02 00:00:00 55621.1561342593 2011-03-01 03:44:50 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 052015 We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 GALACTIC POINT SOURCES 4 A CLEMENT CABANAC EUR 5 AO5-TOO PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405063020/ Quick Look
8 GX 339-4 255.7016 -48.7831 254.753859 -48.712086 259.571491 -25.857192 338.94276391 -4.32024293 90.1024 55616.8233680556 2011-02-24 19:45:39 55617.4487268518 2011-02-25 10:46:10 405063030 19.182 20 19.19 19.198 0 19.182 2 2 0 2 1 0 0 15.684 15.684 54.0259 1 PROCESSED 57601.0471180556 2016-08-01 01:07:51 55996 2012-03-10 00:00:00 55628.1679976852 2011-03-08 04:01:55 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 052015 We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 GALACTIC POINT SOURCES 4 A CLEMENT CABANAC EUR 5 AO5-TOO PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405063030/ Quick Look
9 GX 17+2 274.0108 -14.0482 273.300467 -14.065956 273.933278 9.337698 16.42401351 1.2676957 264.7715 55853.116099537 2011-10-19 02:47:11 55855.5287037037 2011-10-21 12:41:20 406070010 6.5069 100 6.7572 6.5069 0 6.7572 3 2 0 2 1 0 0 87.3599 87.3599 208.4297 3 PROCESSED 57603.5270023148 2016-08-03 12:38:53 56241 2012-11-10 00:00:00 55873.2944444445 2011-11-08 07:04:00 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 062003 The behaviour of dense matter in neutron stars remains enigmatic. To probe this requires accurate measurements of neutron star radii and masses. We have recently shown that broad relativistic Fe emission lines in neutron star low-mass X-ray binaries can be used to constrain the neutron star radius. These sources also provide another tool, kHz quasi-periodic oscillations (QPOs). Combining a measurement of the velocity of the gas in the inner disk (from the Fe line) and the frequency of the kHz QPOs provides a method to measure the neutron star mass if kHz QPOs originate at the inner disk. We propose 100 ksec observations of GX 349+2 and GX 17+2 to provide a detailed Fe line profile. Simultaneously, we will also observe with RXTE to detect the kHz QPOs, allowing us to test this technique. GALACTIC POINT SOURCES 4 A EDWARD CACKETT EUR 6 AO6 EXPLORING THE IRON LINE - KHZ QPO CONNECTION XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406070010/ Quick Look
10 4U 0352+30 58.8427 31.0494 58.059686 30.903757 63.208913 10.461571 163.07655547 -17.13553633 77.7002 56166.360150463 2012-08-27 08:38:37 56170.0980208333 2012-08-31 02:21:09 407088010 153.4893 150 153.4893 153.4893 0 153.4893 2 2 0 2 1 0 0 140.9919 140.9919 322.9236 3 PROCESSED 57607.0637268518 2016-08-07 01:31:46 56582 2013-10-17 00:00:00 56212.7609722222 2012-10-12 18:15:48 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 072011 After 40 years of studies, surprisingly little is known about accreting pulsars at low-luminosities, yet these may be the most numerous class of neutron star binaries in the Galaxy. Upcoming large-scale surveys will likely reveal many such objects, but to identify them it is crucial to fully understand their properties. X Per, the archetypal source of this class, at 1 kpc from Earth is ideal target for detailed studies. In spite of that X Per is still puzzling. With the proposed program we aim to study X Per in detail, constrain its X-ray spectrum also as a function of the spin phase. Our study will be key to characterize the properties of low-luminosity X-ray pulsars population and will help to identify it in upcoming surveys. GALACTIC POINT SOURCES 4 B VICTOR DOROSHENKO EUR 7 AO7 CRACKING THE X PER XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407088010/ Quick Look
11 J1522-5734 230.5286 -57.5816 229.552952 -57.402737 244.521376 -37.577548 322.05619938 -0.4156844 274.4971 56154.6486342593 2012-08-15 15:34:02 56155.0078356482 2012-08-16 00:11:17 407094010 30.0295 25 30.0455 30.0295 0 30.0455 1 1 0 1 1 0 0 23.6862 23.6862 31.0239 0 PROCESSED 57606.8538194444 2016-08-06 20:29:30 56638 2013-12-12 00:00:00 56272.6647222222 2012-12-11 15:57:12 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 072019 The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances. GALACTIC POINT SOURCES 4 A MARTINO MARELLI EUR 7 AO7 SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407094010/ Quick Look
12 RBS1066 181.3063 39.3578 180.66961 39.636099 163.015077 36.071469 158.19944471 74.44309108 133.5252 56973.6795486111 2014-11-12 16:18:33 56973.8890277778 2014-11-12 21:20:12 809105010 10.2376 12 10.2376 10.5256 0 10.5256 1 1 0 1 0 0 0 0 0 0 0 PROCESSED 57616.7665509259 2016-08-16 18:23:50 57358 2015-12-02 00:00:00 56992.4200810185 2014-12-01 10:04:55 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 092015 Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500. EXTRAGALACTIC DIFFUSE SOURCES 8 C LORENZO LOVISARI EUR 9 AO9 SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809105010/ Quick Look
13 H 1743+322 266.5667 -32.234 265.750828 -32.215343 267.051923 -8.827937 357.25546218 -1.83442728 271.9807 56924.2942476852 2014-09-24 07:03:43 56927.2779861111 2014-09-27 06:40:18 409059010 119.0885 100 119.0885 119.0965 0 119.5626 3 2 0 1 0 0 0 0 0 0 0 PROCESSED 57616.6267361111 2016-08-16 15:02:30 57310 2015-10-15 00:00:00 56940.6644560185 2014-10-10 15:56:49 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 092020 We propose a triggered Suzaku 100 ks observation of a high-inclination Galactic black hole binary in the hard intermediate state. This will be simultaneous with an already accepted XMM-Newton observation (PI: A. Ingram) to test the Lense-Thirring model for the low frequency quasi-periodic oscillations seen in black hole (and neutron star) binaries. The Suzaku PIN data will enable us to extend the energy range over which the QPO can be studied, allowing us to get much better constraints on the reflection component in the QPO spectrum, and hence to more tightly probe the geometry and emission processes in the regions closest to the black hole. GALACTIC POINT SOURCES 4 A MAGNUS AXELSSON EUR 9 AO9-TOO TESTING THE LENSE-THIRRING ORIGIN OF THE LOW FREQUENCY QPO IN BLACK HOLE BINARIES XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409059010/ Quick Look
14 ABELL2244 255.6885 34.0502 255.230084 34.120069 248.255538 56.413781 56.77689495 36.30222985 232.8204 54392.7992013889 2007-10-19 19:10:51 54394.3959953704 2007-10-21 09:30:14 802078010 71.3811 63 71.3891 71.3971 0 71.3811 2 2 0 2 1 0 0 69.1077 69.1077 137.9498 3 PROCESSED 57540.332337963 2016-06-01 07:58:34 54771 2008-11-01 00:00:00 54403.2516666667 2007-10-30 06:02:24 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 022036 In order to use clusters as cosmological probes, accurate mass determinations are needed. The ICM is an ideal candidate since it provides a map of the DM potential. Measuring the gas properties to the virial radius is imperative for determining the proper cluster mass, since a large part of the cluster mass resides beyond 1/2 r_vir. Current discrepancies in outer cluster kT profiles are due to large uncertainties due to the high background in Chandra and XMM-Newton. With its lower background, Suzaku is able to make this measurement. We propose a 50 ks observation of A2244. A2244 is an ideal candidate to make this measurement; at a redshift of z~0.1, the virial radius can be fit inside Suzaku's field of view, moreover A2244 is an unusual example of a relaxed cluster without a cool core. EXTRAGALACTIC DIFFUSE SOURCES 8 B DANIEL HUDSON EUR 2 AO2 A2244 - MEASURING CLUSTER GAS TEMPERATURE TO THE VIRIAL RADIUS IN A RELAXED ISOTHERMAL CLUSTER XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802078010/ Quick Look
15 4U 1820-30 275.9218 -30.4206 275.118218 -30.447383 275.13391 -7.085348 2.73584989 -7.94270191 269.3964 55116.6321064815 2009-10-12 15:10:14 55117.1759143518 2009-10-13 04:13:19 404069060 24.6687 100 0 24.6687 0 24.6687 0 1 0 2 1 0 0 16.9505 16.9505 46.978 0 PROCESSED 57548.8754861111 2016-06-09 21:00:42 55507 2010-11-07 00:00:00 55131.3693518518 2009-10-27 08:51:52 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 042004 Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. GALACTIC POINT SOURCES 4 A MANUEL LINARES EUR 4 AO4 ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404069060/ Quick Look
16 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
17 J1620-4927 245.1748 -49.4572 244.240353 -49.338216 252.062857 -27.548671 333.89109656 0.40900491 274.3002 56157.8029513889 2012-08-18 19:16:15 56158.5203356482 2012-08-19 12:29:17 407091010 29.2601 25 29.2601 29.2841 0 29.2601 1 1 0 1 1 0 0 29.8402 29.8402 61.9679 0 PROCESSED 57606.8716898148 2016-08-06 20:55:14 56592 2013-10-27 00:00:00 56226.6098148148 2012-10-26 14:38:08 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 072019 The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances. GALACTIC POINT SOURCES 4 A MARTINO MARELLI EUR 7 AO7 SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407091010/ Quick Look
18 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
19 GT MUS 174.8799 -65.348 174.296149 -65.070756 218.231345 -58.061728 295.52044001 -3.51633969 94.8564 54446.4736689815 2007-12-12 11:22:05 54449.187662037 2007-12-15 04:30:14 402095010 93.3087 80 93.3087 93.3087 0 93.3087 2 2 0 2 1 0 0 94.6965 94.6965 234.4699 3 PROCESSED 57540.9318287037 2016-06-01 22:21:50 54828 2008-12-28 00:00:00 54460.7707060185 2007-12-26 18:29:49 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 022020 We propose to perform broad-band X-ray spectroscopy of the RS CVn-like system GT Muscae, with the aim to study the thermal and non-thermal components of its X-ray emitting plasma. Our target is a known hard X-ray source, detected with Uhuru and recently with Integral/IBIS in the 20-40 keV band, but lacking a dedicated observation with modern X-ray spectrometers. The proposed observation will allow us to investigate both the quiescent and flaring states of this complex (possibly interacting) binary system, by means of a variability study and a time-resolved spectral analysis of its X-ray emission. We aim to detect and constrain the non-thermal hard X-ray emission component, and to search for a possible Fe Kalpha line emission, thanks to the superb broad-band spectral capabilities of Suzaku. GALACTIC POINT SOURCES 4 B ANTONIO MAGGIO EUR 2 AO2 BROAD-BAND X-RAY SPECTROSCOPY OF AN EXTREMELY ACTIVE CORONAL SOURCE HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402095010/ Quick Look
20 A3526 191.1432 -39.6142 190.459557 -39.340673 207.301582 -31.717062 301.49310157 23.23836897 110.0059 55944.2688078704 2012-01-18 06:27:05 55944.754375 2012-01-18 18:06:18 806090010 18.3702 16 18.3782 18.3702 0 18.3857 2 2 0 2 1 0 0 14.795 14.795 41.9499 2 PROCESSED 57604.405775463 2016-08-04 09:44:19 56352 2013-03-01 00:00:00 55985.1138310185 2012-02-28 02:43:55 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 062001 Suzaku has enabled a breakthrough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in a cluster to beyond the virial radius. This is important for understanding the properties of clusters and for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The observational breakthrough has been possible due to the combination of the low orbit and thus low background of the Suzaku FI detectors and particularly X-ray bright clusters. We propose here to exploit Suzaku's unique capability to extend this result to an X-ray bright nearby relaxed cluster. EXTRAGALACTIC DIFFUSE SOURCES 8 B ANDREW FABIAN EUR 6 AO6 TO BEYOND THE VIRIAL RADIUS IN THE NEARBY CENTAURUS CLUSTER XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806090010/ Quick Look
21 J2218.8-0258 334.694 -2.9598 334.046783 -3.210826 335.453457 7.033577 59.75779093 -46.24852305 49.9996 56072.7972685185 2012-05-25 19:08:04 56073.7370833333 2012-05-26 17:41:24 807086010 38.3981 35 38.4061 38.3981 0 38.4061 2 2 0 2 1 0 0 36.9739 36.9739 81.1958 1 PROCESSED 57605.5228703704 2016-08-05 12:32:56 56500 2013-07-27 00:00:00 56134.0402199074 2012-07-26 00:57:55 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 072018 We propose to observe the three clusters of galaxies J2218.2-0350, J2218.6-0346 and J2218.8-0258 with exposure times of 15, 25 and 35 ks respectively. These clusters are part of a structure of four linearly aligned clusters, separated from each other by 4 to 10 Mpc. We will accurately determine their masses and orientation. This will allow us to fully map the tidal force field of the structure, which is the prime force behind the formation of filaments in the cosmic web. We will study the effects of cluster mass, separation and mutual orientation on the filamentary structure of the cosmic web and on the evolution of galaxies therein. EXTRAGALACTIC DIFFUSE SOURCES 8 A E.G. PATRICK BOS EUR 7 AO7 CLUSTERS AND THE COSMIC WEB XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807086010/ Quick Look
22 HESS J1731-347 263.0179 -34.7706 262.185573 -34.73474 264.142481 -11.47104 353.53173388 -0.68198005 79.8005 54154.7807060185 2007-02-23 18:44:13 54155.7432291667 2007-02-24 17:50:15 401099010 40.6189 38 40.6269 40.6189 0 40.6269 2 2 0 2 1 0 0 34.6479 34.6479 83.1559 0 PROCESSED 57537.4739351852 2016-05-29 11:22:28 54528 2008-03-03 00:00:00 54160.3931944444 2007-03-01 09:26:12 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 012042 The hard (Gamma=2.0) TeV source HESS J1731-347 discovered in the H.E.S.S. Galactic plane survey has an intriguing possible counterpart seen in ROSAT survey data. The X-ray data show an unidentified, extended nebular structure with a hard spectrum, in close coincidence to the TeV source. It is plausible to assume that the same energetic particle population is responsible for the emission in both bands. Suzaku is optimally suited to establish the likely non-thermal nature of the X-ray spectrum and to search for the high-energy end of the emitting particle spectrum, which is likely visible in the HXD domain. The observations will help to clarify the nature of HESS J1731-347, which may be a new type of Galactic particle accelerator. GALACTIC POINT SOURCES 4 A GERD PUEHLHOFER EUR 1 AO1 THE HIGH ENERGY PARTICLE SPECTRUM OF THE TEV/X-RAY NEBULA HESS J1731-347 XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401099010/ Quick Look
23 SU AUR 73.9934 30.5715 73.195309 30.492884 76.133121 7.898373 172.51103259 -7.93275707 85.9197 54339.1713541667 2007-08-27 04:06:45 54340.7502199074 2007-08-28 18:00:19 402090010 57.3034 55 57.3114 57.3034 0 57.3114 2 2 0 2 1 0 0 54.3848 54.3848 136.4018 1 PROCESSED 57539.9114699074 2016-05-31 21:52:31 54723 2008-09-14 00:00:00 54350.6381597222 2007-09-07 15:18:57 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 022007 We propose to observe the cTTS TW~Hya, SU~Aur and XZ~Tau with the Suzaku XIS in order to search for soft X-ray "excesses", indicating the presence of accretion induced X-rays in cTTS. We plan to utilize the sensitivity and capability of the Suzaku XIS to resolve the OVIII/OVII lines.With grating observations the absence of the forbidden line in the latter was found to provide strong evidence for the presence of accretion in the X-ray spectra of a few cTTS. With the increased sensitivity of Suzaku the presence of soft X-ray excesses can be demonstrated in a far larger sample of stars, and we want to demonstrate the existence of a soft X-ray, probably accretion induced component in cTTS with extremely hot coronae exhibiting the presence of the 6.7 keV iron line complex in their spectra. GALACTIC POINT SOURCES 4 A JURGEN SCHMITT EUR 2 AO2 ACCRETION RELATED SOFT X-RAY EMISSION IN CLASSICAL T TAURI STARS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402090010/ Quick Look
24 XTE J1759-220 269.9393 -22.0118 269.18599 -22.009675 269.934127 1.429042 7.5831003 0.77858469 86.479 54566.5188773148 2008-04-10 12:27:11 54567.6460532407 2008-04-11 15:30:19 403072010 48.961 50 49.361 49.425 0 48.961 2 2 0 2 1 0 0 43.9129 43.9129 97.3639 1 PROCESSED 57542.2983912037 2016-06-03 07:09:41 54953 2009-05-02 00:00:00 54580.4766550926 2008-04-24 11:26:23 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 032012 Dipping low-mass X-ray binaries (LMXBs), a subclass of LMXBs that are viewed close to the disk plane, provide us with a rare opportunity to probe the structure of accretion disks. This was nicely illustrated with the discovery of Fe XXV and Fe XXVI absorption lines in all the dipping LMXBs observed with XMM and Chandra. It revealed the existence of a highly-ionized atmosphere above the disk which is likely present in any LMXB but only detectable in the ones seen close to edge-on. We propose to observe two recently discovered dipping binaries with Suzaku, to constrain the basic astrophysical properties (orbital period, distance, variability, high energy cutoff, etc) of these yet poorly observed sources, and to further investigate the ionized atmosphere in X-ray binaries in general. GALACTIC POINT SOURCES 4 B LAURENCE BOIRIN EUR 3 AO3 NEW DIPPING X-RAY BINARIES TO PROBE ACCRETION DISKS AND THEIR IONIZED ATMOSPHER XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403072010/ Quick Look
25 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
26 4U 1820-30 275.9248 -30.4209 275.121217 -30.447698 275.136502 -7.085754 2.73676025 -7.94514519 265.9319 55088.3645833333 2009-09-14 08:45:00 55088.8141087963 2009-09-14 19:32:19 404069020 21.0373 20 21.0373 21.0373 0 21.0373 1 1 0 1 1 0 0 17.17 17.17 38.8319 0 PROCESSED 57548.569837963 2016-06-09 13:40:34 55469 2010-09-30 00:00:00 55103.4457407407 2009-09-29 10:41:52 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 042004 Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. GALACTIC POINT SOURCES 4 A MANUEL LINARES EUR 4 AO4 ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404069020/ Quick Look
27 10 LAC 339.8111 39.0619 339.249017 38.801118 0.373962 43.220063 96.65409432 -16.97165842 81.7456 55344.5001967593 2010-05-28 12:00:17 55345.0690162037 2010-05-29 01:39:23 405060010 25.0284 25 25.0284 25.0284 0 25.0284 2 2 0 2 1 0 0 21.7431 21.7431 49.1359 2 PROCESSED 57551.6393287037 2016-06-12 15:20:38 55731 2011-06-19 00:00:00 55365.1824305556 2010-06-18 04:22:42 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 052005 We propose to obtain XIS spectra of two O stars with weak winds. They belong to a class of O stars which show significantly weaker mass loss than predicted by the theory of radiation-driven winds. In this respect they resemble the first generation of stars in the early universe, which presumably had only weak winds due to their low metallicity. As explanation for the weak-wind phenomenon it has been suggested that X-rays affect the ionization balance and thus lead to a reduction of the wind-driving force. To check this hypothesis the proposed Suzaku observations are needed. The new data will allow us to discriminate between possible mechanisms for the generation of X-rays, such as magnetic wind confinement or dynamical friction, and serve as input parameters in numerical models. GALACTIC POINT SOURCES 4 A LIDIA OSKINOVA EUR 5 AO5 STRONG EXPLORATION OF WEAK STELLAR WINDS WITH SUZAKU XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405060010/ Quick Look
28 EXO 2030+375 308.0462 37.6555 307.574628 37.484842 325.998165 53.954312 77.15821576 -1.21997822 58.3113 56070.8420717593 2012-05-23 20:12:35 56072.789849537 2012-05-25 18:57:23 407089010 77.9451 75 77.9531 77.9569 0 77.9451 2 1 0 2 1 0 0 72.515 72.515 168.2558 0 PROCESSED 57605.5425347222 2016-08-05 13:01:15 56449 2013-06-06 00:00:00 56083.2088888889 2012-06-05 05:00:48 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 072013 We propose to observe the Be/X-ray binary system EXO 2030+375 in the ascending part of one of its normal periastron flares for 75ks to study the onset of the pulsar activity. Quasi-periodic hour-long flux oscillations were recently observed during INTEGRAL serendipitous observations and by EXOSAT in 1985. They appear to happen at the viscous time-scale of a disk, evidencing some kind of instability in the transition zone between the magnetosphere and the accretion disk. The broad-band coverage and sensitivity of Suzaku will allow us to investigate in detail the opening of the magnetic gate for this high-magnetic field neutron star by studying the high time resolution light curve, the shape of its pulsed signal and the spectral properties. GALACTIC POINT SOURCES 4 A CARLO FERRIGNO EUR 7 AO7 UNVEIL ACCRETION ONSET DURING A NORMAL OUTBURST OF EXO 2030+375 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407089010/ Quick Look
29 CPD-28 2561 118.9748 -28.6234 118.467111 -28.489607 129.605392 -48.156505 245.44211654 -0.09136967 288.1635 56775.1365509259 2014-04-28 03:16:38 56775.9174768518 2014-04-28 22:01:10 409055010 26.9471 25 26.9471 26.9551 0 26.9631 2 2 0 2 1 0 0 23.1261 23.1261 67.4619 0 PROCESSED 57615.0079513889 2016-08-15 00:11:27 57214 2015-07-11 00:00:00 56848.6257638889 2014-07-10 15:01:06 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 092005 We propose SUZAKU observations of the representative members of the class of magnetic massive O-type stars. The targets have measured magnetic fields and belong to similar spectral types. SUZAKU data will allow to compare the X-ray spectra of these objects that have similar stellar and wind parameters yet different magnetospheres. These observations will result in the first firm X-ray detections of our target stars. The analysis of XIS spectra will determine the emission measures and the temperatures of the hot gas. Our careful selection of targets will allow us to study the interplay between magnetic fields and stellar winds in O-type stars. These new observations for a comparative analysis of a homogeneous class of objects will be critical for driving the development of the theory. GALACTIC POINT SOURCES 4 B LIDIA OSKINOVA EUR 9 AO9 COMPARATIVE STUDY OF MAGNETIC O-TYPE STARS WITH SUZAKU XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409055010/ Quick Look
30 HESS J1718-385 259.5512 -38.6075 258.69231 -38.554942 261.534502 -15.472357 348.79652534 -0.53531102 91.2393 54154.3587731482 2007-02-23 08:36:38 54154.7773611111 2007-02-23 18:39:24 501105010 20.744 19 20.744 20.744 0 20.744 1 1 0 1 1 0 0 15.8365 15.8365 36.1519 0 PROCESSED 57537.4491435185 2016-05-29 10:46:46 54527 2008-03-02 00:00:00 54158.2865740741 2007-02-27 06:52:40 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 012044 HESS J1718-385 is a newly discovered TeV gamma-ray source, with an unusually hard energy spectrum, which lies in close proximity to an energetic pulsar. It is likely that this object belongs to the class of offset pulsar wind nebula (PWN), accelerating electrons and positrons up to ~100 TeV. So far no sensitive X-ray observations of this region have taken place. The synchrotron spectrum of the nebula is predicted to peak in the energy range of the Suzaku HXD. The unprecedented high energy sensitivity of this instrument is required to study the highest energy particles accelerated in this object. Spectral measurements by Suzaku would confirm the inverse-Compton origin of the VHE gamma-rays and place tight constraints on the maximum energy of accelerated electrons. GALACTIC DIFFUSE EMISSION 5 A JAMES HINTON EUR 1 AO1 PROBING THE LIMITS OF PARTICLE ACCELERATION IN A NEW HARD SPECTRUM TEV GAMMA-RAY SOURCE XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501105010/ Quick Look
31 AX J1714.1-3912 258.5249 -39.1972 257.66219 -39.139743 260.755226 -16.122974 347.85266774 -0.22742448 85.6964 55608.0538078704 2011-02-16 01:17:29 55608.9654050926 2011-02-16 23:10:11 505076010 32.6017 30 32.6017 32.6017 0 32.6017 2 2 0 2 1 0 0 28.3362 28.3362 78.7579 1 PROCESSED 57600.9625115741 2016-07-31 23:06:01 55988 2012-03-02 00:00:00 55621.1409027778 2011-03-01 03:22:54 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 052012 Molecular clouds are predicted to emit strong non-thermal X-rays when they are close to particle-accelerating SNRs, but this emission has not been confirmed yet. We propose to observe the non-thermal X-ray source AX J1714.1-3912 to investigate its relationship with the SNR RX J1713.7-3946. ASCA observations have shown that the hard spectrum of the source may be associated with bremsstrahlung emission from particles accelerated in the SNR and diffusing in a nearby molecular cloud. This emission has never been observed in other SNRs. However, the association of the source with the remnant is still controversial and the ASCA data do not allow us to constrain the spectral properties. We aim at verifying the association with the remnant and at investigating the physical origin of the emission. GALACTIC DIFFUSE EMISSION 5 A MARCO MICELI EUR 5 AO5 INVESTIGATING THE PHYSICAL ORIGIN OF AX J1714.1-3912 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505076010/ Quick Look
32 G7.6+2.0 268.7973 -21.391 268.047539 -21.383335 268.869887 2.045161 7.58937554 2.00788461 270.4016 56194.0843865741 2012-09-24 02:01:31 56194.4237037037 2012-09-24 10:10:08 507065010 16.521 10 16.529 16.521 0 16.5347 2 2 0 2 1 0 0 12.1603 12.1603 29.3139 2 PROCESSED 57607.1654050926 2016-08-07 03:58:11 56676 2014-01-19 00:00:00 56315.5110069444 2013-01-23 12:15:51 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 072014 We propose to investigate the four brightest and most-promising RASS-detected SNR candidates. With the observations we will be able to determine if the objects are supernova remnants, and if so, measure their spectral characteristics (temperature, abundance), details of their morphology (angular size) and their expansion velocity. This study will complete previous surveys of SNR in other wavelength and provide insight into the structure and composition of the ISM. Follow-up radio continuum and linear polarization observations, and optical studies will be performed. GALACTIC DIFFUSE EMISSION 5 A TOBIAS PRINZ EUR 7 AO7 IDENTIFICATION OF X-RAY SELECTED SUPERNOVA REMNANTS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507065010/ Quick Look
33 3C400.2 SE 294.8215 17.1213 294.25847 17.005668 300.577132 37.964226 53.58084569 -2.4098547 81.5889 56770.9416898148 2014-04-23 22:36:02 56771.4758449074 2014-04-24 11:25:13 509070010 24.9467 20 24.9547 24.9467 0 24.9627 1 1 0 1 1 0 0 22.7494 22.7494 46.1359 0 PROCESSED 57614.9903009259 2016-08-14 23:46:02 57152 2015-05-10 00:00:00 56789.6293865741 2014-05-12 15:06:19 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 092010 Mixed morphology supernova remnants are an important, but peculiar class of supernova remnants. They have a shell-type morphology in the radio, but the X-ray emission is centrally dominated. X-ray spectroscopy of several of these supernova remnants, indicate that their central plasma is often over-ionised and have enhanced abundances. Here we propose to study a typical member of this class, which has so far not received much attention, despite being bright and only mildly absorbed: 3C400.2. The remnant can be covered with four pointings, and is bright enough for imaging spectroscopy on the scale of the Suzaku PSF. This will enable us to study spectroscopic variation, confirm the preliminary detection of an RRC and map its distribution, and study the abundances. GALACTIC DIFFUSE EMISSION 5 A JACCO VINK EUR 9 AO9 THE MIXED-MORPHOLOGY SUPERNOVA REMNANT 3C400.2 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509070010/ Quick Look
34 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
35 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
36 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
37 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
38 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
39 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
40 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
41 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
42 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
43 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
44 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
45 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
46 MCG-03-58-007 342.3795 -19.2152 341.708645 -19.480081 336.393592 -10.851288 42.20057234 -60.96689333 68.5139 55350.7016203704 2010-06-03 16:50:20 55352.8940046296 2010-06-05 21:27:22 705052010 99.0873 100 99.0873 99.0873 0 99.0873 2 2 0 2 1 0 0 81.42 81.42 189.406 1 PROCESSED 57551.8454513889 2016-06-12 20:17:27 55734 2011-06-22 00:00:00 55365.563912037 2010-06-18 13:32:02 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 052011 Despite their relevance, less than two dozens of confirmed Compton-thick (CT) AGN have been found so far. We have recently selected a well defined sample of CT AGN candidates using FX/Fir ratios and X-ray colors. Due to their heavy obscuration, good statistics at 6.4 keV and data above 10 keV are needed to assess the real nature of these sources. We propose deep Suzaku observations (100 and 150 ks) for two sources for which data above 10 keV are not available and the quality of XMM data is poor. This request is a continuation of an approved AO4 proposal. These observations will allow us to possibly unveil two more examples of CT AGN, provide a physical characterization of the relatively bright tail of our sample, and estimate the efficiency of our method in selecting CT AGN. EXTRAGALACTIC COMPACT SOURCES 7 A PAOLA SEVERGNINI EUR 5 AO5 SUZAKU OBSERVATIONS OF TWO COMPTON-THICK CANDIDATES HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705052010/ Quick Look
47 CENTAURUS B 206.7018 -60.4061 205.845186 -60.15638 231.230588 -45.191821 309.72060452 1.73379394 97.6796 55572.6060763889 2011-01-11 14:32:45 55572.7919444444 2011-01-11 19:00:24 705059010 8.7611 10 8.7691 8.7691 0 8.7611 1 1 0 1 1 0 0 6.4526 6.4526 16.0559 0 PROCESSED 57600.577650463 2016-07-31 13:51:49 55962 2012-02-05 00:00:00 55595.2069675926 2011-02-03 04:58:02 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 052018 We propose a 100 ks Suzaku observation of 4U 1344-60, a poorly studied (because at low Galactic latitude) but bright (about 2 millicrabs) AGN which showed, in an XMM-Newton observation, a strong relativistic disk iron line. The main aim of the proposal is to determine in detail the parameters of the disk, which is possible only with a high quality broad band observation which permits to control the continuum beneath the line. Presently, only Suzaku has the right combination of sensitivity, energy resolution and broad band coverage to achieve this objective. EXTRAGALACTIC COMPACT SOURCES 7 C JIRI SVOBODA EUR 5 AO5 4U 1344-60: A BRIGHT AGN WITH A STRONG RELATIVISTIC IRON LINE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705059010/ Quick Look
48 PKS 0548-322 87.6707 -32.2739 87.20583 -32.286363 86.511257 -55.687672 237.56869078 -26.144265 287.028 56023.6105555556 2012-04-06 14:39:12 56026.3891435185 2012-04-09 09:20:22 707040010 102.6567 100 102.6567 102.6567 0 102.6567 2 2 0 2 1 0 0 91.5237 91.5237 240.0558 3 PROCESSED 57605.1844907407 2016-08-05 04:25:40 56415 2013-05-03 00:00:00 56044.314525463 2012-04-27 07:32:55 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 072006 We propose Suzaku observations of the two brightest extreme BL Lac objects, PKS 0548-322 and RGB J0710+591 (100 ksec each), whose synchrotron bump peaks in the medium-hard X-ray band. The requested observations, never performed by Suzaku on this two sources, will permit to measure their continuum in the 0.6-70 keV range, fully exploiting the unique capabilities of the Suzaku satellite. With its wide energy coverage and good response, Suzaku will allow us to determine with unprecedented precision the spectral properties of the sources in the hard, medium and soft X-ray ranges, allowing us to measure the physical properties of the emitting relativistic electrons and, complemented by data at other frequencies, to infer the physical conditions in the emitting region. EXTRAGALACTIC COMPACT SOURCES 7 A FABRIZIO TAVECCHIO EUR 7 AO7 REVEALING THE HIGH-ENERGY SYNCHROTRON PEAK OF EXTREME BL LACS WITH SUZAKU XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707040010/ Quick Look
49 MARKARIAN 1040 37.056 31.3166 36.314628 31.093376 44.885956 15.789444 146.10796909 -27.16282444 69.5695 56515.9165740741 2013-08-11 21:59:52 56519.1681597222 2013-08-15 04:02:09 707046010 137.4353 135 137.4353 137.4353 0 137.4353 2 2 0 2 1 0 0 136.328 136.328 280.9053 1 PROCESSED 57612.3140625 2016-08-12 07:32:15 56955 2014-10-25 00:00:00 56587.9502662037 2013-10-22 22:48:23 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 072025 Mrk 1040 is a nearby type-1 Seyfert galaxy where a recent XMM observation revealed the presence of a deep soft X-ray warm absorber. However the current data are unable to resolve the components of the absorber so very little is known about its properties. We propose to obtain a 200 ks definitive Chandra HETG observation of Mrk 1040 from 0.5-9.0 keV where we will resolve the lines for the first time enabling a detailed analysis of the kinematics and energetics to be made. We will also obtain the first high-resolution spectrum > 2 keV in this source allowing us to resolve the narrow Fe K alpha core. Furthermore, through a 125 ks Suzaku observation we will also study the Fe K complex in unprecedented detail while simultaneously determining the origin of the hard excess. EXTRAGALACTIC COMPACT SOURCES 7 S ANDREW LOBBAN EUR 7 AO7 A HIGH-RESOLUTION VIEW OF THE WARM ABSORBER AND IRON LINE IN MRK 1040 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707046010/ Quick Look
50 FAIRALL 51 281.2231 -62.3584 280.059194 -62.409813 276.677853 -39.177664 333.20555808 -23.08834808 251.8035 56542.816087963 2013-09-07 19:35:10 56543.4286689815 2013-09-08 10:17:17 708046030 23.9301 30 23.9381 23.9439 0 23.9301 1 1 0 1 1 0 0 35.6507 35.6507 52.9199 0 PROCESSED 57612.5525694445 2016-08-12 13:15:42 56990 2014-11-29 00:00:00 56625.6038078704 2013-11-29 14:29:29 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 082016 Fairall 51 is a variable bright active galaxy (about 1 millicrab), classified as a polar-scattered Seyfert~1 galaxy. It was observed twice with high-quality X-ray spectrometers on-board the XMM-Newton satellite. The two observations are separated by half a year and the spectra significantly differ from each other. The difference can be well explained by a variable covering fraction of a cold (very low-ionised) absorber (Ricci et al., 2010). Two additional Swift data, separated by five days, suggest that the variability may occur at time-scales as short as a few days. The ultimate goal of the proposal is to locate this variable absorber by the determination of the typical time-scale of the variability. We therefore propose a series of observations of Fairall 51 with short exposures. EXTRAGALACTIC COMPACT SOURCES 7 A JIRI SVOBODA EUR 8 AO8 STUDY OF THE VARIABLE ABSORBER IN A BRIGHT ACTIVE GALAXY FAIRALL 51 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708046030/ Quick Look
51 MARKARIAN 3 93.8812 71.0496 92.43086 71.064939 91.873944 47.634543 143.28137914 22.71605454 71.2169 56953.1510532407 2014-10-23 03:37:31 56953.6731828704 2014-10-23 16:09:23 709022030 22.7461 20 22.7541 22.7541 0 22.7461 1 1 0 1 0 0 0 0 0 0 0 PROCESSED 57616.6616087963 2016-08-16 15:52:43 57376 2015-12-20 00:00:00 57010.3833217593 2014-12-19 09:11:59 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 092008 We propose to measure size and distance from the black hole of the optically-thick absorbing and reprocessing system(s) in the heavily obscured Seyfert Galaxy Markarian~3 by means of its known X-ray spectral variability. We aim at simultaneously measuring: the variability timescale of the primary emission, seen in transmission through a photoelectric column density of (0.7--1.1)x10^{24} atoms/cm/cm; the variability timescale of its Compton-reflection, dominating the continuum flux in the 3-10 keV energy band; and the variability timescale of the nuclear obscuration. Only the scientific payload on-board Suzaku possesses the required combination of broadband X-ray coverage, sensitivity, and spectroscopic capabilities to perform this experiment. We request 5 observations of 20 ks each. EXTRAGALACTIC COMPACT SOURCES 7 A MATTEO GUAINAZZI EUR 9 AO9 MEASURING THE TORUS SPATIAL SCALE(S) IN SEYFERT GALAXIES: A SUZAKU MONITORING OF MARKARIAN 3 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709022030/ Quick Look
52 A3526 191.7105 -40.5689 191.023079 -40.2959 208.274178 -32.365083 301.98862911 22.29443097 109.9992 55942.9777314815 2012-01-16 23:27:56 55943.2362847222 2012-01-17 05:40:15 806086010 13.6391 12 13.6471 13.6471 0 13.6391 1 1 0 1 1 0 0 11.41 11.41 22.3279 0 PROCESSED 57604.3734606482 2016-08-04 08:57:47 56352 2013-03-01 00:00:00 55985.0806944444 2012-02-28 01:56:12 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 062001 Suzaku has enabled a breakthrough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in a cluster to beyond the virial radius. This is important for understanding the properties of clusters and for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The observational breakthrough has been possible due to the combination of the low orbit and thus low background of the Suzaku FI detectors and particularly X-ray bright clusters. We propose here to exploit Suzaku's unique capability to extend this result to an X-ray bright nearby relaxed cluster. EXTRAGALACTIC DIFFUSE SOURCES 8 B ANDREW FABIAN EUR 6 AO6 TO BEYOND THE VIRIAL RADIUS IN THE NEARBY CENTAURUS CLUSTER XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806086010/ Quick Look
53 A2877-NORTH 17.5135 -45.1865 16.956259 -45.452478 352.566996 -47.330769 292.51418745 -71.56330592 266.5006 56649.9225810185 2013-12-23 22:08:31 56651.7884027778 2013-12-25 18:55:18 808102010 72.629 70 72.637 72.629 0 72.645 2 2 0 2 1 0 0 69.2641 69.2641 161.1857 0 PROCESSED 57613.7012615741 2016-08-13 16:49:49 57033 2015-01-11 00:00:00 56665.7969097222 2014-01-08 19:07:33 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 082014 We propose to observe the galaxy group A2877 for a combine observation time of 150 ks, with two different pointings. The aim of the project is to obtain temperature and surface brightness profiles out to large radii to constrain entropies. We aim to see if the entropy profile flattens at large radii, which could indicate gas clumping and/or other processes. This would possibly be the first unrelaxed galaxy group whose entropy profile would have been studied in the outskirts. EXTRAGALACTIC DIFFUSE SOURCES 8 C BHARADWAJ VIJAYSARATHY EUR 8 AO8 INVESTIGATING THE OUTSKIRTS OF THE UNRELAXED GALAXY GROUP A2877 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808102010/ Quick Look
54 IC1262 263.2444 43.7719 262.868526 43.80553 257.468416 66.917452 69.53148075 32.08557503 39.6325 56784.7266319444 2014-05-07 17:26:21 56784.9377777778 2014-05-07 22:30:24 809103010 8.569 10 8.569 8.569 0 8.569 1 1 0 1 1 0 0 8.943 8.943 18.2319 0 PROCESSED 57615.0791898148 2016-08-15 01:54:02 57166 2015-05-24 00:00:00 56800.6274537037 2014-05-23 15:03:32 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 092015 Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500. EXTRAGALACTIC DIFFUSE SOURCES 8 B LORENZO LOVISARI EUR 9 AO9 SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809103010/ Quick Look
55 NGC 7556 348.9407 -2.3789 348.297581 -2.651844 348.895625 2.187169 76.06549974 -56.282291 247.7522 56983.6865972222 2014-11-22 16:28:42 56984.009837963 2014-11-23 00:14:10 809109010 15.119 15 15.119 15.119 0 15.119 1 1 0 1 0 0 0 0 0 0 0 PROCESSED 57616.8029861111 2016-08-16 19:16:18 57365 2015-12-09 00:00:00 57009.4127777778 2014-12-18 09:54:24 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 092015 Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500. EXTRAGALACTIC DIFFUSE SOURCES 8 C LORENZO LOVISARI EUR 9 AO9 SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809109010/ Quick Look
56 NGC4325 185.7751 10.6242 185.139474 10.901318 181.016229 12.032879 279.57257446 72.19853871 120.2615 56997.2271990741 2014-12-06 05:27:10 56997.680775463 2014-12-06 16:20:19 809110010 17.4681 15 17.4761 17.4681 0 17.4761 1 1 0 1 1 0 0 16.8093 16.8093 39.184 0 PROCESSED 57617.4727083333 2016-08-17 11:20:42 57376 2015-12-20 00:00:00 57010.1165162037 2014-12-19 02:47:47 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 092015 Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500. EXTRAGALACTIC DIFFUSE SOURCES 8 C LORENZO LOVISARI EUR 9 AO9 SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809110010/ Quick Look
57 MARKARIAN 509 311.0428 -10.7274 310.361715 -10.908973 310.545221 7.124071 35.9681072 -29.85888698 254.2043 54054.375150463 2006-11-15 09:00:13 54055.0113541667 2006-11-16 00:16:21 701093030 24.4466 25 24.4466 24.4466 0 24.4466 2 2 0 2 1 0 0 18.327 18.327 54.9679 1 PROCESSED 57536.1015162037 2016-05-28 02:26:11 54456 2007-12-22 00:00:00 54088.6171875 2006-12-19 14:48:45 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 012050 We propose to perform 4 repeated Suzaku observations of 25 ks each of the Seyfert 1 galaxy MKN 509, the brightest Seyfert galaxy of the Piccinotti sample in the 2-100 keV band that is not strongly affected by neutral or ionized absorbing material. The aim of the study is to disentangle the different physical explanations for the origin of the soft excess looking at the long time--scale correlations between the variations of the emission and shape of the soft excess and the emission at high energy (E > 10 keV). EXTRAGALACTIC COMPACT SOURCES 7 A GABRIELE PONTI EUR 1 AO1 SOLVING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701093030/ Quick Look
58 EXO 0748-676 117.1051 -67.7525 117.068716 -67.625708 198.866436 -79.490243 279.97237585 -19.82332654 158.0884 54459.2369560185 2007-12-25 05:41:13 54460.2919444444 2007-12-26 07:00:24 402092010 45.8988 40 45.9126 45.8988 0 45.9046 2 2 0 2 1 0 0 43.5747 43.5747 91.1358 1 PROCESSED 57540.9732175926 2016-06-01 23:21:26 54854 2009-01-23 00:00:00 54483.1839351852 2008-01-18 04:24:52 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 022014 We propose Suzaku observations of the dipping Low Mass X-ray Binaries (LMXBs) EXO 0748-676 and X 1624-490. The changes in both the continuum and the He- and H- like Fe K absorption features during dips have been demonstrated to be consistent with a change in the properties of the photoionized absorbers present in these systems. We will use the XIS to characterise the absorbers and the HXD to uniquely determine the underlying continuum shapes including any contributions due to reflection components. This will allow to reliably determine the absolute values of the ionization parameters for each of the sources, which was not possible with XMM due to the lack of contemporaneous high energy spectra, providing for a detailed comparison of the absorbers with source properties such as luminosity. GALACTIC POINT SOURCES 4 C MARIA DIAZ TRIGO EUR 2 AO2 BROAD-BAND OBSERVATIONS OF HIGHLY-IONIZED ABSORBERS IN DIPPING LMXBS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402092010/ Quick Look
59 ABELL 3341 81.3893 -31.5876 80.918035 -31.630439 77.271182 -54.650323 235.16288585 -31.086571 266.8997 57094.3290393518 2015-03-13 07:53:49 57094.5780092593 2015-03-13 13:52:20 809104010 11.439 10 11.439 11.439 0 11.439 1 1 0 1 0 0 0 0 0 0 0 PROCESSED 57617.7607407407 2016-08-17 18:15:28 57478 2016-03-31 00:00:00 57108.4097685185 2015-03-27 09:50:04 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 092015 Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500. EXTRAGALACTIC DIFFUSE SOURCES 8 B LORENZO LOVISARI EUR 9 AO9 SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809104010/ Quick Look
60 ESO 137-G034 248.7664 -58.1298 247.710529 -58.026542 256.37198 -35.687232 329.07669192 -7.11373135 296.1293 54744.462650463 2008-10-05 11:06:13 54746.6745833333 2008-10-07 16:11:24 403075010 92.0525 90 92.0613 92.0587 0 92.0525 2 2 0 2 1 0 0 83.6615 83.6615 191.0897 1 PROCESSED 57544.095775463 2016-06-05 02:17:55 55148 2009-11-13 00:00:00 54780.6031828704 2008-11-10 14:28:35 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 032025 Suzaku observations of hard X-ray (> 15 keV) selected, bright AGN discovered by INTEGRAL and Swift have revealed several examples of previously unknown Compton Thick (NH > 1e24 cm-2) AGN in the nearby Universe. Their broad band X-ray spectra show a high degree of complexity and a wide range of the relative intensities of the various components (i.e. scattered/reflected fraction; iron line intensity, etc.). We propose a medium/deep Suzaku observation of a bright source detected by INTEGRAL above 15 keV and optically identified with a nearby Seyfert 2 galaxy. Besides the various soft X-ray components, the flat 2-10 keV spectrum and the strong (EW ~ 1 keV) iron line present in an archival XMM-Newton observation strongly suggest that the nucleus is obscured by Compton-Thick gas. GALACTIC POINT SOURCES 4 B ROBERTO GILLI EUR 3 AO3 ANOTHER COMPTON-THICK AGN JUST AROUND THE CORNER HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403075010/ Quick Look
61 4U 1820-30 275.9267 -30.4234 275.123101 -30.450207 275.138047 -7.08832 2.73525617 -7.94773658 265.1815 55083.1120023148 2009-09-09 02:41:17 55083.2015740741 2009-09-09 04:50:16 404069010 3.5175 20 3.5255 3.5175 0 3.5255 1 1 0 1 1 0 0 3.7124 3.7124 7.738 0 PROCESSED 57548.5052546296 2016-06-09 12:07:34 55475 2010-10-06 00:00:00 55109.4203125 2009-10-05 10:05:15 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 042004 Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. GALACTIC POINT SOURCES 4 A MANUEL LINARES EUR 4 AO4 ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404069010/ Quick Look
62 MU COL 86.4962 -32.3107 86.031401 -32.328862 84.748669 -55.688941 237.28985275 -27.10600903 93.5874 55455.752337963 2010-09-16 18:03:22 55456.3113541667 2010-09-17 07:28:21 405059010 25.961 20 25.961 25.961 0 25.961 1 1 0 1 1 0 0 21.8734 21.8734 48.2879 0 PROCESSED 57553.4381018518 2016-06-14 10:30:52 55836 2011-10-02 00:00:00 55469.2452314815 2010-09-30 05:53:08 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 052005 We propose to obtain XIS spectra of two O stars with weak winds. They belong to a class of O stars which show significantly weaker mass loss than predicted by the theory of radiation-driven winds. In this respect they resemble the first generation of stars in the early universe, which presumably had only weak winds due to their low metallicity. As explanation for the weak-wind phenomenon it has been suggested that X-rays affect the ionization balance and thus lead to a reduction of the wind-driving force. To check this hypothesis the proposed Suzaku observations are needed. The new data will allow us to discriminate between possible mechanisms for the generation of X-rays, such as magnetic wind confinement or dynamical friction, and serve as input parameters in numerical models. GALACTIC POINT SOURCES 4 A LIDIA OSKINOVA EUR 5 AO5 STRONG EXPLORATION OF WEAK STELLAR WINDS WITH SUZAKU XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405059010/ Quick Look
63 4U 1909+07 287.7097 7.5883 287.10413 7.505006 290.320155 29.788203 41.89273161 -0.82371888 247.9131 55502.7037847222 2010-11-02 16:53:27 55503.4337731482 2010-11-03 10:24:38 405073010 29.2982 25 29.2982 29.2982 0 29.2982 2 2 0 2 1 0 0 21.3911 21.3911 63.0519 0 PROCESSED 57553.9348958333 2016-06-14 22:26:15 55882 2011-11-17 00:00:00 55515.2869328704 2010-11-15 06:53:11 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 052024 We propose the first observation of the neutron star HMXB 4U 1909+07 with Suzaku. The aim of the proposed 25 ksec observation is to study the broadband spectrum of the source. The data will provide information about the structure and ionization state of the accreted medium, as well as of the geometry of the accretion column and the strength of the magnetic field. No high-resolution CCD spectra of this source have been published so far. The source shows flaring behavior, so the wind is expected to be strongly clumped, which could be probed by studying the evolution of N_H and the iron line with high time resolution. Furthermore we will perform phase resolved spectroscopy to study the spectral variation with pulse phase and perform a detailed search for a CRSF. GALACTIC POINT SOURCES 4 A FELIX FUERST EUR 5 AO5 STUDYING ACCRETION IN THE UNCELEBRATED HMXB 4U 1909+07 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405073010/ Quick Look
64 IGR J16318-4848 247.9691 -48.8061 247.034981 -48.699533 253.953463 -26.583352 335.63186461 -0.44896472 266.5948 53961.4825 2006-08-14 11:34:48 53964.3488310185 2006-08-17 08:22:19 401094010 97.2538 100 97.2698 97.2538 97.2698 97.2698 2 2 2 2 1 0 0 87.1128 87.1128 247.6059 5 PROCESSED 57535.3483564815 2016-05-27 08:21:38 54526 2008-03-01 00:00:00 54020.9181597222 2006-10-12 22:02:09 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 012034 We propose a detailed study of Compton thick X-ray absorption in neutral or weakly ionized material by using 100ksec of Suzaku observations of the strongly absorbed (N_H~2E24cm2) Galactic X-ray binary IGR J16318-4848. Measuring a high signal to noise ratio broad band spectrum will allow us to determine the curvature in the >10keV continuum caused by Compton downscattering in the absorber, to deduce its ionization state from observations of the Fe Kalpha line, and to study the variability of the source and the absorber. These observations will also shed more light onto the nature of the compact object in IGR J16318-4848. GALACTIC POINT SOURCES 4 B JOERN WILMS EUR 1 AO1 OBSERVING IGR J16318-4848: PROBING COMPTON-THICK ABSORPTION XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401094010/ Quick Look
65 4U 1543-624 236.9719 -62.5774 235.885471 -62.423392 250.451121 -41.357182 321.74901084 -6.34183385 299.1939 55826.4056828704 2011-09-22 09:44:11 55827.6217592593 2011-09-23 14:55:20 406072010 49.1851 50 49.1931 49.1851 0 49.2011 2 2 0 2 1 0 0 45.3094 45.3094 105.0599 1 PROCESSED 57603.2564699074 2016-08-03 06:09:19 56222 2012-10-22 00:00:00 55851.4556134259 2011-10-17 10:56:05 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 062010 We propose to observe the ultra-compact X-ray binaries 4U 0614+091 and 4U 1543-624 for 50 ksec each. The aim of these observations is to constrain the inner radius of the accretion disc for both sources using the recently discovered in both sources relativistialy broadened OVIII Ly alpha line at ~0.7 keV. This constrains the radius of the neutron star. The second goal is to constrain the continuum using more physical model than was used in the literature so far. The unique, large energy coverage of Suzaku will enable us to break possible degeneracies between the properties of the broadened lines and the continuum, providing more convidence on the results. GALACTIC POINT SOURCES 4 A OLIWIA MADEJ EUR 6 AO6 INVESTIGATING THE ORIGIN OF THE CONTINUUM AND LINE EMISSION IN THE UCXBS 4U 0614+091 AND 4U 1543-624 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406072010/ Quick Look
66 SGR 1806-20 272.1687 -20.4711 271.424026 -20.47983 272.024767 2.954425 9.94559743 -0.27498509 268.1397 54387.2332060185 2007-10-14 05:35:49 54388.333599537 2007-10-15 08:00:23 402094010 52.2477 50 52.2477 52.2717 0 52.2637 2 2 0 2 1 0 0 50.0895 50.0895 95.0599 1 PROCESSED 57540.2839583333 2016-06-01 06:48:54 54771 2008-11-01 00:00:00 54403.9548611111 2007-10-30 22:55:00 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 022016 Among magnetars, SGR 1806-20 is particularly interesting since it emitted two years ago the most powerful giant flare ever observed. We are performing a long term monitoring in the soft X-rays with XMM-Newton and hard X-rays with INTEGRAL to study how the source evolves back to quiescence. We obtained in AO-1 a Suzaku observation that was carried out simultaneously with XMM-Newton and provided for the first time a broad band spectrum of SGR 1806-20 on a short timescale. A new observation is required to study the spectral variability in the hard X-ray range and possibly the properties of bursts. GALACTIC POINT SOURCES 4 C SANDRO MEREGHETTI EUR 2 AO2 CONTINUED MONITORING OF SGR 1806-20 AFTER THE GIANT FLARE WITH SUZAKU AND XMM-NEWTON HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402094010/ Quick Look
67 RBS 315 36.2519 18.8398 35.555924 18.614311 40.065414 4.223463 151.73247281 -38.74296898 76.7825 53941.8167013889 2006-07-25 19:36:03 53943.0404976852 2006-07-27 00:58:19 701077010 47.8309 50 47.8309 47.8309 47.8309 47.8309 2 2 2 2 1 0 0 43.425 43.425 105.7299 1 PROCESSED 57535.0495023148 2016-05-27 01:11:17 54400 2007-10-27 00:00:00 53955.7322106482 2006-08-08 17:34:23 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 012008 We propose to observe with Suzaku the X-ray bright blazar RBS 315, showing a very hard spectrum (Gamma<1.2) in the 2-10 keV range as determined by XMM. The requested observation will allow us to measure the continuum in the full Suzaku range (0.3-200 keV), fully exploiting the unique capabilities of the satellite. With its wide energy coverage and good response at soft energies, Suzaku will allow to determine with precision the spectral properties of the source in the hard medium and soft X-ray ranges, providing important clues on the physics and the environment of relativistic jets. A good measurement of the continuum will allow us to determine the luminosity emitted via the IC mechanism which usually dominates the radiative output and the total kinetic power carried by the outflow. EXTRAGALACTIC COMPACT SOURCES 7 B FABRIZIO TAVECCHIO EUR 1 AO1 SUZAKU OBSERVATION OF THE HARD BROAD BAND CONTINUUM OF THE POWERFUL BLAZAR RBS 315 HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701077010/ Quick Look
68 4U 1820-30 275.9314 -30.4193 275.127829 -30.44613 275.142299 -7.084391 2.74079847 -7.94949913 261.8762 55102.6696759259 2009-09-28 16:04:20 55103.5002662037 2009-09-29 12:00:23 404069040 28.6994 20 28.6994 28.6994 0 28.6994 3 2 0 3 1 0 0 24.9261 24.9261 71.7519 2 PROCESSED 57548.6752546296 2016-06-09 16:12:22 55499 2010-10-30 00:00:00 55133.2273263889 2009-10-29 05:27:21 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 042004 Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. GALACTIC POINT SOURCES 4 A MANUEL LINARES EUR 4 AO4 ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404069040/ Quick Look
69 HER X-1 254.4619 35.2659 254.010863 35.341503 246.021498 57.41824 58.05460857 37.50723847 268.3041 55461.7937037037 2010-09-22 19:02:56 55462.2467476852 2010-09-23 05:55:19 405058040 21.74 20 21.74 21.796 0 21.8704 1 1 0 1 1 0 0 19.803 19.803 39.1359 0 PROCESSED 57553.5121180556 2016-06-14 12:17:27 55840 2011-10-06 00:00:00 55474.0995486111 2010-10-05 02:23:21 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 052001 We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity? GALACTIC POINT SOURCES 4 B R DIGER STAUBERT EUR 5 AO5 VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1 HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405058040/ Quick Look
70 GX 339-4 255.7013 -48.7851 254.753538 -48.714085 259.571516 -25.859202 338.94105066 -4.32130146 91.6296 55620.1778703704 2011-02-28 04:16:08 55620.8022569445 2011-02-28 19:15:15 405063040 21.799 20 21.799 21.807 0 21.8168 3 3 0 3 1 0 0 18.8502 18.8502 53.9239 0 PROCESSED 57601.0624074074 2016-08-01 01:29:52 56009 2012-03-23 00:00:00 55642.1310300926 2011-03-22 03:08:41 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 052015 We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 GALACTIC POINT SOURCES 4 A CLEMENT CABANAC EUR 5 AO5-TOO PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405063040/ Quick Look
71 4U 1705-44 257.2257 -44.096 256.322601 -44.032282 260.19112 -21.088012 343.32512852 -2.33758895 104.9955 56013.5320486111 2012-03-27 12:46:09 56016.4231134259 2012-03-30 10:09:17 406076010 100.8112 100 100.8112 100.8192 0 100.8209 2 2 0 2 1 0 0 90.0759 90.0759 249.7677 2 PROCESSED 57605.1022453704 2016-08-05 02:27:14 56393 2013-04-11 00:00:00 56027.2013657407 2012-04-10 04:49:58 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 062019 We propose a ToO Suzaku 100-ks observation of the neutron star X-ray binary 4U 1705-44, to perform a detailed study of its broad-band (0.4-200 keV) X-ray spectrum during a hard state. XIS data will provide important information on the iron K-shell features, and the broad-band spectral capabilities of the HXD will allow to study the hard X-ray spectrum and in particular the Compton reflection bump at 20-50 keV. We plan to fit both the iron features and the reflection bump with a self-consistent model, which will allow to prove (or disprove) a disk origin of the iron line. Moreover the proposed observation will allow to study the correlation between the spectral index of the primary spectrum and the reflection amplitude, which gives important constraints on the geometry of the system. GALACTIC POINT SOURCES 4 A TIZIANA DI SALVO EUR 6 AO6-TOO SUZAKU BROAD-BAND OBSERVATION OF 4U 1705-44: PROBING THE DISK ORIGIN OF THE IRON LINE IN THE HARD STATE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406076010/ Quick Look
72 NGC 3147 154.2433 73.3869 153.186306 73.636446 117.480978 56.071635 136.29780832 39.47682975 262.9224 55340.8248611111 2010-05-24 19:47:48 55343.2925231482 2010-05-27 07:01:14 705054010 150.0476 150 150.0476 150.0556 0 150.0556 2 2 0 2 1 0 0 132.9136 132.9136 213.1818 2 PROCESSED 57553.0649074074 2016-06-14 01:33:28 55765 2011-07-23 00:00:00 55393.4710648148 2010-07-16 11:18:20 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 052013 NGC3147 is the best candidate to be a true Seyfert 2, i.e., with no BLR. We propose a 150 ks observation with Suzaku to study the Fe line profile which in the short XMM-Newton observation shows some structure. If the iron line will turn out to be originated from the accretion disc, the lack of the BLR cannot be attributed to the lack of ionizing photons; if originated from the torus, this would put constraints on models assuming a common origin for the torus and the BLR; if the presence of an ionized iron line is confirmed, a BLR might exist but so highly ionized to be invisible at optical/UV wavelengths. An important added value of this observation is to confirm NGC3147 as a true Seyfert 2 by ruling out a Compton-thick nature, which only Suzaku can do thanks to its hard X-ray coverage. EXTRAGALACTIC COMPACT SOURCES 7 B GIORGIO MATT EUR 5 AO5 SUZAKU OBSERVATION OF THE BEST ``TRUE SEYFERT 2'' GALAXY CANDIDATE, NGC 3147 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705054010/ Quick Look
73 FS AURIGAE 86.945 28.5962 86.152995 28.579446 87.308718 5.183997 180.53629966 0.22811281 90.5955 56541.1879050926 2013-09-06 04:30:35 56542.802974537 2013-09-07 19:16:17 408041010 62.1842 62 62.1842 62.1842 0 62.1842 2 2 0 2 1 0 0 61.0287 61.0287 139.5158 0 PROCESSED 57612.5675810185 2016-08-12 13:37:19 56981 2014-11-20 00:00:00 56616.7165046296 2013-11-20 17:11:46 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 082012 FS Aur represents one of the most unusual cataclysmic variable to have ever been observed. It is famous for a variety of uncommon and puzzling periodic photometric and spectroscopic variabilities. Tovmassian, Zharikov & Neustroev (2007) proposed that the precession of a fast-rotating magnetically accreting white dwarf can successfully explain these phenomena. We request 62 ks observations of FS Aur to detect the magnetic WD, determine its spin period, confirm the flux and spectral variability with the precession period, inconclusively detected by Chandra and Swift, and thus to check the proposed model. The theory of compact objects predicts certain relations between the spin and precession periods, and our findings will provide a good test for the theory. GALACTIC POINT SOURCES 4 B VITALY NEUSTROEV EUR 8 AO8 PROBING THE PRECESSION OF WHITE DWARF IN CLOSE BINARY SYSTEMS - FS AURIGAE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408041010/ Quick Look
74 4U 1735-44 264.7398 -44.4536 263.827347 -44.425856 265.968173 -21.085622 346.05003995 -6.99385769 96.4379 57098.6918402778 2015-03-17 16:36:15 57099.2717824074 2015-03-18 06:31:22 408043030 4.3665 20 4.3665 4.9159 0 4.967 2 2 0 2 0 0 0 0 0 0 0 PROCESSED 57617.8209027778 2016-08-17 19:42:06 57479 2016-04-01 00:00:00 57112.402662037 2015-03-31 09:39:50 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 082017 We propose to observe the bursting low-mass X-ray binary 4U 1735-44 with Suzaku for a total exposure time of 60 ks. We plan to investigate the broad-band X-ray spectrum by performing a detailed spectroscopic and timing analysis in the energy range 0.4-100 keV. The main scientific aims of this observation are to detect and study the iron Kalpha line at 6.4-7 keV, simultaneously with the expected iron edge at 7-9 keV, emission lines at lower energy (such as S, Ar and Ca at 2.62 keV, 3.31 keV and 3.90 keV, respectively), and either a Compton reflection hump at 20-40 keV or a hard tail at energy above 25 keV (depending of the state of the source), thanks to the broad-band capabilities of Suzaku. This will allow to infer and probe the origin of these components, which is still debated. GALACTIC POINT SOURCES 4 A ELISE EGRON EUR 8 AO8 BROAD-BAND SPECTRAL ANALYSIS AND STUDY OF THE DISK REFLECTION COMPONENT IN 4U 1735-44 WITH SUZAKU XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408043030/ Quick Look
75 G278.0+12.4 158.151 -43.7043 157.610146 -43.446336 182.388463 -47.807278 278.01040448 12.3478226 304.0284 56102.6152199074 2012-06-24 14:45:55 56102.9842476852 2012-06-24 23:37:19 507067010 18.996 17.5 19.004 18.996 0 19.004 1 1 0 1 1 0 0 16.442 16.442 31.8799 0 PROCESSED 57605.7438078704 2016-08-05 17:51:05 56582 2013-10-17 00:00:00 56219.6572916667 2012-10-19 15:46:30 3.0.22.44 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 072014 We propose to investigate the four brightest and most-promising RASS-detected SNR candidates. With the observations we will be able to determine if the objects are supernova remnants, and if so, measure their spectral characteristics (temperature, abundance), details of their morphology (angular size) and their expansion velocity. This study will complete previous surveys of SNR in other wavelength and provide insight into the structure and composition of the ISM. Follow-up radio continuum and linear polarization observations, and optical studies will be performed. GALACTIC DIFFUSE EMISSION 5 A TOBIAS PRINZ EUR 7 AO7 IDENTIFICATION OF X-RAY SELECTED SUPERNOVA REMNANTS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507067010/ Quick Look
76 MRK 0359 21.8893 19.1757 21.213343 18.916781 27.368924 9.282102 134.6025573 -42.87605962 244.6178 54137.9789699074 2007-02-06 23:29:43 54140.3738078704 2007-02-09 08:58:17 701082010 107.507 100 107.507 107.507 0 107.507 2 2 0 2 1 0 0 102.5761 102.5761 206.8678 2 PROCESSED 57537.3689930556 2016-05-29 08:51:21 54735 2008-09-26 00:00:00 54151.5150925926 2007-02-20 12:21:44 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 012023 Markarian 359 was the first source to be identified as a Narrow Line Seyfert 1 (NLS1) AGN, and its importance as an unusual source has been recognised for a long time. In the optical, it has unusually narrow lines for a NLS1. X-ray observations of the source are rare, but based on an XMM-Newton observation a strong reflection 'hump' is predicted. The source is therefore a critical one in the investigation of relativistically blurred photoionized disc reflection models. A detailed Suzaku observation will provide improved data quality in the XIS waveband, allow investigation of spectral variability in this waveband, and constrain the amount of reflection independently by using the HXD. EXTRAGALACTIC COMPACT SOURCES 7 C JAMIE CRUMMY EUR 1 AO1 NVESTIGATING REFLECTION IN MARKARIAN 359 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701082010/ Quick Look
77 UGC03957 NORTH 114.9138 55.8102 113.899292 55.925218 106.552165 33.791456 161.76581362 28.79157051 294.9973 56006.0767939815 2012-03-20 01:50:35 56007.0710532407 2012-03-21 01:42:19 806091010 41.3662 45 41.3662 41.3662 0 41.3662 2 2 0 2 1 0 0 40.6312 40.6312 85.9019 1 PROCESSED 57604.9833217593 2016-08-04 23:35:59 56389 2013-04-07 00:00:00 56022.2738888889 2012-04-05 06:34:24 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 062024 Upcoming surveys of galaxy clusters require precise calibration of X-ray observables and mass down to low mass regimes to constraint cosmological parameters. However, it's still debated if groups can be treated as simply scaled-down clusters. Precise calibration needs to account for systematics due to the complex baryonic physics. Detailed and extended measurements out to large radii have the potential of accomplish this by exploring most of the system's volume and getting rid of biases derived from extrapolations. Suzaku is a powerful tool to address these studies with massive cluster, but we propose to demonstrate that by selecting the optimal target this can be extended to groups. We also show promising results from our Suzaku analysis of cluster outskirts. EXTRAGALACTIC DIFFUSE SOURCES 8 C BRENDA MIRANDA OCEJO EUR 6 AO6 MEASUREMENTS OF THE INTRACLUSTER EMISSION OF THE GROUP OF GALAXIES UGC03957 OUT TO $R_{200}$ WITH SUZAKU XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806091010/ Quick Look
78 UGC03957 SOUTH 115.5259 55.024 114.524001 55.141747 107.151159 33.092194 162.70412876 29.04503782 294.9967 56007.0719907407 2012-03-21 01:43:40 56008.1328125 2012-03-22 03:11:15 806092010 48.8159 45 48.8159 48.8159 0 48.8159 2 2 0 2 1 0 0 46.4169 46.4169 91.6439 3 PROCESSED 57604.9862731482 2016-08-04 23:40:14 56389 2013-04-07 00:00:00 56022.2514930556 2012-04-05 06:02:09 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 062024 Upcoming surveys of galaxy clusters require precise calibration of X-ray observables and mass down to low mass regimes to constraint cosmological parameters. However, it's still debated if groups can be treated as simply scaled-down clusters. Precise calibration needs to account for systematics due to the complex baryonic physics. Detailed and extended measurements out to large radii have the potential of accomplish this by exploring most of the system's volume and getting rid of biases derived from extrapolations. Suzaku is a powerful tool to address these studies with massive cluster, but we propose to demonstrate that by selecting the optimal target this can be extended to groups. We also show promising results from our Suzaku analysis of cluster outskirts. EXTRAGALACTIC DIFFUSE SOURCES 8 C BRENDA MIRANDA OCEJO EUR 6 AO6 MEASUREMENTS OF THE INTRACLUSTER EMISSION OF THE GROUP OF GALAXIES UGC03957 OUT TO $R_{200}$ WITH SUZAKU XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806092010/ Quick Look
79 MARKARIAN 509 311.0427 -10.7271 310.361616 -10.908673 310.545205 7.124386 35.96837179 -29.85867019 254.3019 54022.3263888889 2006-10-14 07:50:00 54023.0856365741 2006-10-15 02:03:19 701093020 25.9298 25 25.9618 25.9298 25.9538 25.9618 2 2 2 2 1 0 0 23.4497 23.4497 65.5899 1 PROCESSED 57535.8399305556 2016-05-27 20:09:30 54526 2008-03-01 00:00:00 54053.6032638889 2006-11-14 14:28:42 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 012050 We propose to perform 4 repeated Suzaku observations of 25 ks each of the Seyfert 1 galaxy MKN 509, the brightest Seyfert galaxy of the Piccinotti sample in the 2-100 keV band that is not strongly affected by neutral or ionized absorbing material. The aim of the study is to disentangle the different physical explanations for the origin of the soft excess looking at the long time--scale correlations between the variations of the emission and shape of the soft excess and the emission at high energy (E > 10 keV). EXTRAGALACTIC COMPACT SOURCES 7 A GABRIELE PONTI EUR 1 AO1 SOLVING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701093020/ Quick Look
80 MARKARIAN 509 311.0451 -10.7278 310.364015 -10.909382 310.547312 7.12309 35.96880101 -29.86110163 254.2048 54066.1625810185 2006-11-27 03:54:07 54067.12875 2006-11-28 03:05:24 701093040 33.0944 32 33.0944 33.0944 0 33.0944 2 2 0 2 1 0 0 29.4544 29.4544 83.4659 1 PROCESSED 57536.2044212963 2016-05-28 04:54:22 54456 2007-12-22 00:00:00 54088.5895023148 2006-12-19 14:08:53 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 012050 We propose to perform 4 repeated Suzaku observations of 25 ks each of the Seyfert 1 galaxy MKN 509, the brightest Seyfert galaxy of the Piccinotti sample in the 2-100 keV band that is not strongly affected by neutral or ionized absorbing material. The aim of the study is to disentangle the different physical explanations for the origin of the soft excess looking at the long time--scale correlations between the variations of the emission and shape of the soft excess and the emission at high energy (E > 10 keV). EXTRAGALACTIC COMPACT SOURCES 7 A GABRIELE PONTI EUR 1 AO1 SOLVING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701093040/ Quick Look
81 PHOENIX GALAXY 120.9921 5.0644 120.329999 5.206365 122.073674 -14.991802 216.72692126 18.43029643 304.6737 54222.3296296296 2007-05-02 07:54:40 54223.9585069445 2007-05-03 23:00:15 702111010 58.8677 50 58.8677 58.8677 0 58.8677 2 2 0 2 1 0 0 49.6978 49.6978 140.7239 5 PROCESSED 57538.5788078704 2016-05-30 13:53:29 54744 2008-10-05 00:00:00 54230.3771527778 2007-05-10 09:03:06 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 022002 We propose a 50 ks Suzaku observation of the Seyfert galaxy UGC4203 (a.k.a. Mrk 1210), the ``Phoenix Galaxy''. It is one of the sources which have been discovered to change from Compton-thin to reflection-dominated states. The aim of the proposal is to understand the origin of this variation (i.e. as either due to flux or to NH variations) by measuring its column density and compare it to previous observations. Suzaku is unique for this task, because thanks to its broad band it may probe column densities up to several times 10^24 cm^-2 in this source, which has never been observed above 10 keV. EXTRAGALACTIC COMPACT SOURCES 7 B GIORGIO MATT EUR 2 AO2 THE NATURE OF THE VARIATIONS OF STATE IN THE PHOENIX GALAXY HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702111010/ Quick Look
82 IC4329A 207.3329 -30.3099 206.618741 -30.061746 216.345977 -17.776956 317.49868436 30.91898994 293.8517 54318.0289930556 2007-08-06 00:41:45 54318.8786226852 2007-08-06 21:05:13 702113020 30.6233 25 30.6233 30.6233 0 30.6233 2 2 0 2 1 0 0 25.7461 25.7461 73.384 3 PROCESSED 57539.4343287037 2016-05-31 10:25:26 54730 2008-09-21 00:00:00 54347.5971180556 2007-09-04 14:19:51 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 022009 IC 4329A is the brightest known Seyfert 1 galaxy between ~2-30 keV (F(2-10 keV)~1-2e-10 erg/cm2s). With its clear warm absorber and reflection component, it is often taken as the prototypical Sey 1 galaxy. Its X-ray variability is strong enough (and on a sufficiently long time scale, ideal for Suzaku) to make multiple observations critical for probing the origin of the Compton reflection component, and to attempt measuring variations of the high energy cut-off. We thus propose 5x20 ks observations to monitor i) the correlated variability of the reflection continuum plus FeK line to primary continuum variations, and ii) the variations in the high-E cut-off, and their relation with the power-law, and iii) check the evidence for a blueshifted (v~0.1c) FeK absorption line at ~7.7 keV. EXTRAGALACTIC COMPACT SOURCES 7 A MASSIMO CAPPI EUR 2 AO2 SUZAKU MULTIPLE OBSERVATIONS OF IC4329A TO PROBE THE ORIGIN OF THE COMPTON REFLECTION COMPONENT AND HIGH-ENERGY CUT-OFF XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702113020/ Quick Look
83 IRAS18325-5926 279.2243 -59.4565 278.116624 -59.498471 275.782962 -36.20075 335.92469241 -21.3483138 281.9669 54399.3814699074 2007-10-26 09:09:19 54401.4169444444 2007-10-28 10:00:24 702118010 78.4348 80 78.4348 78.4428 0 78.4428 2 2 0 2 1 0 0 74.2917 74.2917 175.8357 0 PROCESSED 57540.4011458333 2016-06-01 09:37:39 54777 2008-11-07 00:00:00 54409.305474537 2007-11-05 07:19:53 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 022025 We propose a 80 ks observation of the Seyfert galaxy IRAS 18325-5926. Previous observations show evidence for reflection from highly ionized matter, absorption features in the 8-10 keV band, and a possible roll-over of the continuum spectrum at around 30 keV. The observation goal is to elucidate the continuum roll-over and to investigate variability of the spectral features, which would have many important implications for the physical condition and the geometry of the accretion disc and the illuminating source. This study will provide crucial keys to understand the geometry of primary X-ray source and immediate surroundings. The broad-band coverage and the high sensitivity at the hard X-ray band provided by Suzaku are ideally suited to study this unique AGN. EXTRAGALACTIC COMPACT SOURCES 7 C KAZUTAMI MISAKI EUR 2 AO2 HARD X-RAY SPECTRUM OF IRAS 18325-5926: REFLECTION FROM AN IONIZED DISC AND CONTINUUM ROLL-OVER HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702118010/ Quick Look
84 G299.5-0.6 184.8049 -63.1515 184.121711 -62.873858 220.875708 -53.463768 299.30360744 -0.50694599 313.6989 56144.5663773148 2012-08-05 13:35:35 56144.9523032407 2012-08-05 22:51:19 507064010 13.8351 10 13.8431 13.8351 0 13.8431 1 1 0 1 1 0 0 13.2722 13.2722 33.3359 0 PROCESSED 57606.7635763889 2016-08-06 18:19:33 56630 2013-12-04 00:00:00 56264.5463541667 2012-12-03 13:06:45 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 072014 We propose to investigate the four brightest and most-promising RASS-detected SNR candidates. With the observations we will be able to determine if the objects are supernova remnants, and if so, measure their spectral characteristics (temperature, abundance), details of their morphology (angular size) and their expansion velocity. This study will complete previous surveys of SNR in other wavelength and provide insight into the structure and composition of the ISM. Follow-up radio continuum and linear polarization observations, and optical studies will be performed. GALACTIC DIFFUSE EMISSION 5 A TOBIAS PRINZ EUR 7 AO7 IDENTIFICATION OF X-RAY SELECTED SUPERNOVA REMNANTS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507064010/ Quick Look
85 PKS1549-79 239.2836 -79.2302 237.405254 -79.084019 259.929288 -56.865354 311.18735019 -19.47008602 310.7048 54752.6495833333 2008-10-13 15:35:24 54754.9009375 2008-10-15 21:37:21 703059010 82.1755 80 82.197 82.1835 0 82.1755 2 2 0 2 1 0 0 79.9736 79.9736 194.4977 2 PROCESSED 57544.1654398148 2016-06-05 03:58:14 55148 2009-11-13 00:00:00 54780.6256597222 2008-11-10 15:00:57 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 032005 Galaxy merger models predict rapid black hole growth and strong outflows late in the merger as the accretion rate increases. PKS1549-79 is a powerful, low redshift, high accretion rate active galaxy which has undergone a recent merger. It is therefore an ideal object to test our understanding of galaxy activity and mergers and for studying feedback between AGN and their host galaxies. We propose an 80 ksec Suzaku observation to: (i) determine the amount and ionisation state of the nuclear obscuring material in PKS1549-79 and hence confirm its status as a local proto-quasar; (ii) search for the massive, probably highly ionised, outflowing wind predicted by galaxy evolution models and hence complete a census of outflow components in this object; and (iii) quantify the high energy spectrum. EXTRAGALACTIC COMPACT SOURCES 7 B PAUL O'BRIEN EUR 3 AO3 UNVEILING PKS 1549-79 WITH SUZAKU XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703059010/ Quick Look
86 NGC4102 181.5322 52.6534 180.899339 52.931664 153.57589 47.373492 138.20676485 63.11040703 305.2196 54981.0678009259 2009-05-30 01:37:38 54983.4203009259 2009-06-01 10:05:14 704057010 105.5579 100 105.5819 105.5579 0 105.5659 2 2 0 2 1 0 0 97.2802 97.2802 203.2139 2 PROCESSED 57547.4983912037 2016-06-08 11:57:41 55363 2010-06-16 00:00:00 54994.4413541667 2009-06-12 10:35:33 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 042014 The nature of Low Ionization Nuclear Emission-line Region (LINER) galaxies has been the subject of a strong controversy. The distinction between LINER nuclei and other families of Active Galactic Nuclei (AGN) can be due to different amounts and/or properties of the obscuring material. A high population of LINERs are Compton-thick candidates. However the Equivalent Width (EW) of the FeKa emission line are lower than those measured for Compton-thick AGN. We propose to use the unprecedented sensitivity of HXD and XIS on board Suzaku to study NGC4102, one of the brightest LINER in the 36-month Swift/BAT survey. NGC4102 is a Compton-thick LINER candidate with EW(FeKa)<500keV, it is therefore an ideal case to investigate the properties of absorption and the FeKa emission line. EXTRAGALACTIC COMPACT SOURCES 7 B OMAIRA GONZALEZ-MARTIN EUR 4 AO4 PROBING COMPTON-THICK OBSCURATION AND LOW EW(FEKA) OF LINERS: THE CASE OF NGC4102 HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704057010/ Quick Look
87 4U 1344-60 206.8966 -60.619 206.036622 -60.369696 231.500761 -45.327278 309.76861534 1.50528265 97.6008 55572.7924189815 2011-01-11 19:01:05 55575.4751273148 2011-01-14 11:24:11 705058010 93.8773 100 93.9013 93.8933 0 93.8773 2 2 0 2 1 0 0 79.5617 79.5617 231.7537 3 PROCESSED 57600.6768865741 2016-07-31 16:14:43 55975 2012-02-18 00:00:00 55607.6933333333 2011-02-15 16:38:24 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 052018 We propose a 100 ks Suzaku observation of 4U 1344-60, a poorly studied (because at low Galactic latitude) but bright (about 2 millicrabs) AGN which showed, in an XMM-Newton observation, a strong relativistic disk iron line. The main aim of the proposal is to determine in detail the parameters of the disk, which is possible only with a high quality broad band observation which permits to control the continuum beneath the line. Presently, only Suzaku has the right combination of sensitivity, energy resolution and broad band coverage to achieve this objective. EXTRAGALACTIC COMPACT SOURCES 7 C JIRI SVOBODA EUR 5 AO5 4U 1344-60: A BRIGHT AGN WITH A STRONG RELATIVISTIC IRON LINE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705058010/ Quick Look
88 MRK 205 185.2459 75.2485 184.69782 75.525765 124.91832 63.698525 125.52269394 41.72619699 309.3435 55338.764849537 2010-05-22 18:21:23 55340.8203125 2010-05-24 19:41:15 705062010 100.9605 126 100.9685 100.9605 0 100.9685 2 2 0 2 1 0 0 91.9525 91.9525 177.5778 0 PROCESSED 57551.6334606482 2016-06-12 15:12:11 55723 2011-06-11 00:00:00 55355.4313773148 2010-06-08 10:21:11 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 052026 Mrk 205 (z=0.071) is a ``bare'' radio-quiet quasar, showing a peculiar continuum and FeK complex. From our analysis of past XMM-Newton observations, it shows a prominent and variable soft excess down to a two-day timescale. In 2000, an unusual FeK profile was found with an unresolved narrow line at 6.4keV and a broadened line centered at 6.7keV; while in 2006 a broad line has been observed near 6.4keV with a visible energy shift to 6.5keV occurring when the source flux increased. Our aims are to: (i) determine the FeK origin from its profile, and its possible variability on sub-orbital time-scales, (ii) to obtain an unprecedented simultaneous measurement of the Compton hump which is critical for modelling the true FeK profile (iii) and hence to infer a global picture of this object. EXTRAGALACTIC COMPACT SOURCES 7 B DELPHINE PORQUET EUR 5 AO5 PROBING THE ORIGIN OF THE FEK COMPLEX IN THE ``BARE'' NUCLEUS OF MRK205. HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705062010/ Quick Look
89 IRAS 09104+4109 138.3378 40.9513 137.53478 41.157946 128.03448 23.67766 180.99146588 43.55010524 90.0004 55883.9878356482 2011-11-18 23:42:29 55885.7675694444 2011-11-20 18:25:18 706038010 81.3276 80 81.3356 81.3276 0 81.3356 2 2 0 2 1 0 0 76.5883 76.5883 153.73 2 PROCESSED 57603.9341203704 2016-08-03 22:25:08 56264 2012-12-03 00:00:00 55895.209849537 2011-11-30 05:02:11 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 062009 We propose to observe IRAS 09104+4109 for 80 ks with Suzaku in order to confirm the ~3 sigma BeppoSAX PDS detection of the source and increase the detection significance with the HXD/PIN to 10 sigma in the 10--80 keV band, allowing the detailed spectral shape to be determined. IRAS 09104+4109 is a hyperluminous Type 2 quasar embedded in a central cluster galaxy at redshift 0.442. It is likely to be the hard-X-ray-brightest such object observed with Suzaku and could well be the prototype Compton-thick Type 2 quasar. The Suzaku observation, especially above 10 keV will most likely reveal one of the most luminous Compton--thick Type 2 QSO to date. EXTRAGALACTIC COMPACT SOURCES 7 C CHIA-YING CHIANG EUR 6 AO6 THE TYPE 2 HYPERLUMINOUS QUASAR IRAS 09104+4109 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706038010/ Quick Look
90 3C400.2 SW 294.5545 17.147 293.991762 17.032549 300.267467 38.043132 53.47817432 -2.17482828 81.5886 56761.5284375 2014-04-14 12:40:57 56762.0730555556 2014-04-15 01:45:12 509069010 24.1528 20 24.1528 24.1528 0 24.1537 2 2 0 2 1 0 0 23.915 23.915 47.0479 3 PROCESSED 57614.2434027778 2016-08-14 05:50:30 57138 2015-04-26 00:00:00 56772.6111226852 2014-04-25 14:40:01 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 092010 Mixed morphology supernova remnants are an important, but peculiar class of supernova remnants. They have a shell-type morphology in the radio, but the X-ray emission is centrally dominated. X-ray spectroscopy of several of these supernova remnants, indicate that their central plasma is often over-ionised and have enhanced abundances. Here we propose to study a typical member of this class, which has so far not received much attention, despite being bright and only mildly absorbed: 3C400.2. The remnant can be covered with four pointings, and is bright enough for imaging spectroscopy on the scale of the Suzaku PSF. This will enable us to study spectroscopic variation, confirm the preliminary detection of an RRC and map its distribution, and study the abundances. GALACTIC DIFFUSE EMISSION 5 A JACCO VINK EUR 9 AO9 THE MIXED-MORPHOLOGY SUPERNOVA REMNANT 3C400.2 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509069010/ Quick Look
91 FAIRALL 51 281.2285 -62.3615 280.064534 -62.412939 276.680669 -39.180999 333.20299178 -23.09155943 253.9697 56548.4894444445 2013-09-13 11:44:48 56549.3146990741 2013-09-14 07:33:10 708046040 30.1926 30 30.2006 30.1926 0 30.1926 2 2 0 2 1 0 0 37.1812 37.1812 71.2679 1 PROCESSED 57612.6129050926 2016-08-12 14:42:35 56990 2014-11-29 00:00:00 56625.6172337963 2013-11-29 14:48:49 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 082016 Fairall 51 is a variable bright active galaxy (about 1 millicrab), classified as a polar-scattered Seyfert~1 galaxy. It was observed twice with high-quality X-ray spectrometers on-board the XMM-Newton satellite. The two observations are separated by half a year and the spectra significantly differ from each other. The difference can be well explained by a variable covering fraction of a cold (very low-ionised) absorber (Ricci et al., 2010). Two additional Swift data, separated by five days, suggest that the variability may occur at time-scales as short as a few days. The ultimate goal of the proposal is to locate this variable absorber by the determination of the typical time-scale of the variability. We therefore propose a series of observations of Fairall 51 with short exposures. EXTRAGALACTIC COMPACT SOURCES 7 A JIRI SVOBODA EUR 8 AO8 STUDY OF THE VARIABLE ABSORBER IN A BRIGHT ACTIVE GALAXY FAIRALL 51 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708046040/ Quick Look
92 MARKARIAN 509 311.0194 -10.6637 310.338544 -10.845188 310.53976 7.19158 36.02321332 -29.81091499 73.1708 53850.7831481482 2006-04-25 18:47:44 53851.5252199074 2006-04-26 12:36:19 701093010 24.5756 25 24.5756 24.5756 24.5916 24.5916 2 2 2 2 1 0 0 15.407 15.407 64.0979 1 PROCESSED 57533.5586342593 2016-05-25 13:24:26 54394 2007-10-21 00:00:00 53907.6894560185 2006-06-21 16:32:49 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 012050 We propose to perform 4 repeated Suzaku observations of 25 ks each of the Seyfert 1 galaxy MKN 509, the brightest Seyfert galaxy of the Piccinotti sample in the 2-100 keV band that is not strongly affected by neutral or ionized absorbing material. The aim of the study is to disentangle the different physical explanations for the origin of the soft excess looking at the long time--scale correlations between the variations of the emission and shape of the soft excess and the emission at high energy (E > 10 keV). EXTRAGALACTIC COMPACT SOURCES 7 A GABRIELE PONTI EUR 1 AO1 SOLVING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701093010/ Quick Look
93 ARK 564 340.6583 29.7351 340.07073 29.472916 355.35057 34.71587 92.13955378 -25.32593551 75.7895 57167.0898842593 2015-05-25 02:09:26 57168.4029282407 2015-05-26 09:40:13 710018010 52.5104 50 52.5104 53.9344 0 53.9344 2 2 0 2 1 0 0 27.9802 27.9802 100.9477 2 PROCESSED 57618.7636921296 2016-08-18 18:19:43 57548 2016-06-09 00:00:00 57178.248587963 2015-06-05 05:57:58 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 102721 A NuSTAR legacy is emerging through long observations of bare Seyfert galaxies that reveal an unprecedented look at relativistic reflection off an ionized accretion disc. We propose now to look at the Seyfert galaxy Ark 564 for 200 ks with NuSTAR and 50 ks with Suzaku in order to understand the reflection in this bright source. Ark 564 has been well-studied in the soft band, revealing a steep spectrum, strong soft excess, broad iron K emission line and dramatic variability on the order of hours. It is very akin to two other well-known bare Seyferts, 1H0707-405 and IRAS 13224-3809, except it is an order of magnitude brighter. With this 200 ks observation, we will probe the geometry of the corona, through a complete spectral and timing analysis. EXTRAGALACTIC COMPACT SOURCES 7 B ERIN KARA EUR 10 AO10 UNDERSTANDING REFLECTION IN THE BARE SEYFERT I ARK 564 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710018010/ Quick Look
94 B2 1023+25 156.5986 25.7113 155.903697 25.966089 148.79406 14.812793 207.05661505 57.60744793 288.3095 56442.6428125 2013-05-30 15:25:39 56444.9133449074 2013-06-01 21:55:13 708044010 100.8874 100 100.8954 100.8874 0 100.8954 2 2 0 2 1 0 0 96.5787 96.5787 196.1298 2 PROCESSED 57611.461099537 2016-08-11 11:03:59 56821 2014-06-13 00:00:00 56455.8205324074 2013-06-12 19:41:34 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 082005 We propose a deep (100 ksec) Suzaku observation of the recently discovered high redshift blazar candidate B2 1023+25 (z=5.3). A very hard (Gamma <2) spectrum would confirm its blazar nature, allowing to study the physical properties of the relativistic jet in this extremely powerful and very high redshift source. The proposed observation will yield an X-ray spectrum of sufficient quality to determine the X-ray shape. The confirmation of a second blazar at this redshift has profound cosmological implications, placing stronger constraints on the number density of high mass BH at high z EXTRAGALACTIC COMPACT SOURCES 7 A VALENTINA BRAITO EUR 8 AO8 THE HIGH-REDSHIFT BLAZAR CANDIDATE B2 1023+25 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708044010/ Quick Look
95 A3526 191.8847 -40.8272 191.196139 -40.554367 208.554246 -32.533282 302.13618529 22.03852437 109.9993 55942.6812037037 2012-01-16 16:20:56 55942.9772569444 2012-01-16 23:27:15 806085010 15.0057 11 15.0097 15.0057 0 15.0116 2 2 0 2 1 0 0 14.9297 14.9297 25.576 0 PROCESSED 57604.3736805556 2016-08-04 08:58:06 56331 2013-02-08 00:00:00 55960.1598726852 2012-02-03 03:50:13 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 062001 Suzaku has enabled a breakthrough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in a cluster to beyond the virial radius. This is important for understanding the properties of clusters and for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The observational breakthrough has been possible due to the combination of the low orbit and thus low background of the Suzaku FI detectors and particularly X-ray bright clusters. We propose here to exploit Suzaku's unique capability to extend this result to an X-ray bright nearby relaxed cluster. EXTRAGALACTIC DIFFUSE SOURCES 8 B ANDREW FABIAN EUR 6 AO6 TO BEYOND THE VIRIAL RADIUS IN THE NEARBY CENTAURUS CLUSTER XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806085010/ Quick Look
96 MARKARIAN 3 93.8907 71.0457 92.440546 71.061085 91.87875 47.630769 143.28642165 22.71781378 80.3638 56937.8059953704 2014-10-07 19:20:38 56938.0751967593 2014-10-08 01:48:17 709022020 17.7277 20 17.7357 17.7357 0 17.7277 1 1 0 1 0 0 0 0 0 0 0 PROCESSED 57616.6163078704 2016-08-16 14:47:29 57358 2015-12-02 00:00:00 56992.4094560185 2014-12-01 09:49:37 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 092008 We propose to measure size and distance from the black hole of the optically-thick absorbing and reprocessing system(s) in the heavily obscured Seyfert Galaxy Markarian~3 by means of its known X-ray spectral variability. We aim at simultaneously measuring: the variability timescale of the primary emission, seen in transmission through a photoelectric column density of (0.7--1.1)x10^{24} atoms/cm/cm; the variability timescale of its Compton-reflection, dominating the continuum flux in the 3-10 keV energy band; and the variability timescale of the nuclear obscuration. Only the scientific payload on-board Suzaku possesses the required combination of broadband X-ray coverage, sensitivity, and spectroscopic capabilities to perform this experiment. We request 5 observations of 20 ks each. EXTRAGALACTIC COMPACT SOURCES 7 A MATTEO GUAINAZZI EUR 9 AO9 MEASURING THE TORUS SPATIAL SCALE(S) IN SEYFERT GALAXIES: A SUZAKU MONITORING OF MARKARIAN 3 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709022020/ Quick Look
97 QSO 1222+216 186.2289 21.3877 185.599556 21.664582 176.758894 22.007996 255.04256268 81.66684682 123.6039 56989.2953356482 2014-11-28 07:05:17 56989.4064583333 2014-11-28 09:45:18 709025020 0.5272 15 0.5352 0.5272 0 0.8088 1 1 0 1 0 0 0 0 0 0 0 PROCESSED 57617.4022222222 2016-08-17 09:39:12 57368 2015-12-12 00:00:00 57002.4417361111 2014-12-11 10:36:06 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 092023 EXTRAGALACTIC COMPACT SOURCES 7 C MARCUS LANGEJAHN EUR 9 AO9 false XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709025020/ Quick Look
98 IGR J19378-0617 294.4023 -6.2869 293.733278 -6.400449 295.156006 15.047751 32.53385066 -13.11752642 260.9167 55485.0705324074 2010-10-16 01:41:34 55487.3016087963 2010-10-18 07:14:19 705055010 77.8014 80 77.8174 77.8014 0 77.8174 2 2 0 2 1 0 0 70.5712 70.5712 192.7439 1 PROCESSED 57553.8036226852 2016-06-14 19:17:13 55867 2011-11-02 00:00:00 55498.2386805556 2010-10-29 05:43:42 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 052014 We propose to observe with Suzaku three Narrow Line Seyfert 1 galaxies detected by INTEGRAL/IBIS and/or Swift/BAT with a flux in excess of 1.5e-11 cgs in the 15-50keV band (corresponding to the HXD/PIN band). The proposed observations will provide rare high quality spectra of NLS1s in the 0.5-50keV band. The good quality data above 10keV will dramatically help us removing the spectral degeneracies inherent to limited bandpass analysis (such as that with XMM-Newton and Chandra) and the ambiguities between the different proposed models invoked to explain the unique spectral and variability properties of these most extreme class of high accretion rate sources. EXTRAGALACTIC COMPACT SOURCES 7 A GIOVANNI MINIUTTI EUR 5 AO5 BROADBAND X-RAY PROPERTIES OF HARD-X-RAY-BRIGHT NLS1 GALAXIES HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705055010/ Quick Look
99 A2163 243.8156 -6.2315 243.147928 -6.107198 243.010913 14.789433 6.59879538 30.51803676 282.2871 54696.6726851852 2008-08-18 16:08:40 54700.4008449074 2008-08-22 09:37:13 803071010 135.7864 130 135.7944 135.7864 0 135.7944 2 2 0 2 1 0 0 122.1262 122.1262 322.0615 5 PROCESSED 57543.4331597222 2016-06-04 10:23:45 55080 2009-09-06 00:00:00 54713.5071875 2008-09-04 12:10:21 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 032023 Measurements of intracluster gas temperatures out to large radii, where much of the cluster mass resides, are of the utmost importance for the use of clusters in precision cosmology and for studies of cluster physics. Previous attempts to measure robust temperatures at cluster virial radii failed. Here, we demonstrate that such measurements are feasible now for the first time with the Suzaku X-ray CCDs, using our observation of the cluster A2204, carefully treating background and PSF. To determine the temperature profile of the cluster population as a whole, more such observations are required. We show that A2163 is the optimal complementary target for such an investigation. We, therefore, propose to observe A2163 to measure the gas temperature to 15% accuracy out to the virial radius. EXTRAGALACTIC DIFFUSE SOURCES 8 A THOMAS REIPRICH EUR 3 AO3 GALAXY CLUSTER GAS TEMPERATURE MEASUREMENT UP TO THE VIRIAL RADIUS OF A2163 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803071010/ Quick Look
100 MRK 478 220.4959 35.3708 219.98335 35.583266 202.392109 47.875746 59.0913373 65.0766343 294.6097 55756.9652777778 2011-07-14 23:10:00 55758.8334837963 2011-07-16 20:00:13 706041010 85.3236 80 85.3316 85.3396 0 85.3236 3 2 0 2 1 0 0 77.6366 77.6366 161.3897 1 PROCESSED 57602.6370601852 2016-08-02 15:17:22 56151 2012-08-12 00:00:00 55783.7198842593 2011-08-10 17:16:38 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 062028 The NLS1 galaxy Mrk 478 has exceptionally unusual properties. It shows up to a factor of five variability while keeping its spectral shape constant. Previous short XMM-Newton observations show that it is probably reflection-dominated, where light-bending effects are at their extreme. This is the only known object that shows such high variability while remaining in a reflection-dominated state. All other known objects show reflection-dominated spectra only when in a faint state, making their study very difficult. This object is reflection-dominated yet bright enough to study with relatively short exposures.Here we propose to observe this object for 80 ks. The goal is to detect the reflection hump using Suzaku capabilities above 10 keV and probe light-bending around this black hole. EXTRAGALACTIC COMPACT SOURCES 7 A ABDERAHMEN ZOGHBI EUR 6 AO6 PROBING EXTREME RELATIVISITC LIGHT-BENDING IN MRK 478 HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706041010/ Quick Look
101 A76 WEST 9.903 6.838 9.256884 6.56348 11.779086 2.367721 117.68922859 -55.91332108 260 55183.8756481482 2009-12-18 21:00:56 55184.3334953704 2009-12-19 08:00:14 804088010 15.1164 15 15.1244 15.1164 0 15.1324 2 2 0 2 1 0 0 14.2066 14.2066 39.5479 0 PROCESSED 57549.8934722222 2016-06-10 21:26:36 55575 2011-01-14 00:00:00 55209.4668055556 2010-01-13 11:12:12 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 042018 In our flux limited survey of galaxy clusters in the ROSAT All-Sky Atlas we find that about 5 - 10 percent of the galaxy clusters have a diffuse, low X-ray surface brightness. These objects could possibly be explained as dynamically very young clusters, which have not yet formed a central core. Three such clusters in our XMM-Newton study of an unbiased sub-sample of 33 galaxy clusters, REXCESS, show suprisingly high entropies in their centers which does not readily support the early formation stage. To shed more light on the nature of these clusters we propose to observe two extremely low surface brightness clusters at low redshift, for which we also have detailed optical data. SUZAKU with its low background is ideally suited for this study. EXTRAGALACTIC DIFFUSE SOURCES 8 B HANS BOEHRINGER EUR 4 AO4 SHEDDING LIGHT ON THE NATURE OF EXTREMELY LOW SURFACE BRIGHTNESS CLUSTERS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804088010/ Quick Look
102 RE J1034+396 158.663 39.6488 157.936699 39.907419 144.538164 28.290615 180.26295059 59.06449262 115.7032 56245.9648726852 2012-11-14 23:09:25 56248.0689583333 2012-11-17 01:39:18 707039010 99.9113 100 99.9193 99.9113 0 99.9193 2 2 0 2 1 0 0 93.446 93.446 181.7639 3 PROCESSED 57608.0485416667 2016-08-08 01:09:54 56640 2013-12-14 00:00:00 56274.6249884259 2012-12-13 14:59:59 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 072005 Understanding the nature of the emission from the extreme active galaxy, RE J1034+396 can help us to unravel the properties of accretion as the Eddington limit is reached. A fleeting glimpse of the unique quasi-periodic oscillation (QPO) in this source has shown a complex timing behaviour with the emission below ~2 keV apparently crucial to its presence. Thus by understanding the origin and properties of the soft emission we can probe the physical mechanism of signals that cannot be resolved in stellar mass X-ray binaries but must be associated with the regions closest to the black hole. A new observation with Suzaku will allow a much deeper analysis of the soft emission and will shed light on how its changing properties can trigger such unique behaviour as the QPO. EXTRAGALACTIC COMPACT SOURCES 7 C MATTHEW MIDDLETON EUR 7 AO7 REVEALING THE NATURE OF RE J1034+396 AND THE EXTREME SOFT EXCESS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707039010/ Quick Look
103 PG 1404+226 211.5907 22.3868 211.009924 22.624644 200.393386 32.82418 21.44706338 72.36251102 287.2346 56486.8565972222 2013-07-13 20:33:30 56489.1889583333 2013-07-16 04:32:06 708045010 102.3327 100 102.3704 102.3327 0 102.3625 2 2 0 2 1 0 0 95.3407 95.3407 201.5059 2 PROCESSED 57612.0131828704 2016-08-12 00:18:59 56872 2014-08-03 00:00:00 56503.7358796296 2013-07-30 17:39:40 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 082010 Suzaku observations reveal evidence of relativistically-broadened emission lines from the inner regions of supermassive black holes, providing a unique tool for studying accreting systems. It is understood that the X-ray source is compact at low-fluxes, and increases in size at higher fluxes. Thus variable sources are essential for probing the physics of the innermost regions. Previous studies of the low-flux 'state' have been limited by low count rates. We propose to observe PG 1404+226, which shares many properties of other AGN showing reverberation, but even at low-fluxes, it is a factor of three brighter than similar objects. This source, never before observed with Suzaku, provides a unique opportunity for probing strong-field accretion because of its high luminosity and variability. EXTRAGALACTIC COMPACT SOURCES 7 B ERIN KARA EUR 8 AO8 MAPPING THE X-RAY EMISSION IN THE VICINITY OF THE BLACK HOLE PG 1404+226 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708045010/ Quick Look
104 FAIRALL 51 281.2261 -62.3592 280.062181 -62.410627 276.679536 -39.178599 333.20510197 -23.08989761 251.799 56540.8073958333 2013-09-05 19:22:39 56541.1744212963 2013-09-06 04:11:10 708046020 30.958 30 30.958 30.958 0 30.9646 1 1 0 1 1 0 0 23.2171 23.2171 31.7039 0 PROCESSED 57612.5333333333 2016-08-12 12:48:00 56956 2014-10-26 00:00:00 56588.7741319444 2013-10-23 18:34:45 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 082016 Fairall 51 is a variable bright active galaxy (about 1 millicrab), classified as a polar-scattered Seyfert~1 galaxy. It was observed twice with high-quality X-ray spectrometers on-board the XMM-Newton satellite. The two observations are separated by half a year and the spectra significantly differ from each other. The difference can be well explained by a variable covering fraction of a cold (very low-ionised) absorber (Ricci et al., 2010). Two additional Swift data, separated by five days, suggest that the variability may occur at time-scales as short as a few days. The ultimate goal of the proposal is to locate this variable absorber by the determination of the typical time-scale of the variability. We therefore propose a series of observations of Fairall 51 with short exposures. EXTRAGALACTIC COMPACT SOURCES 7 A JIRI SVOBODA EUR 8 AO8 STUDY OF THE VARIABLE ABSORBER IN A BRIGHT ACTIVE GALAXY FAIRALL 51 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708046020/ Quick Look
105 UGC03957 WEST 114.5487 55.2415 113.541037 55.354916 106.445391 33.192967 162.38027408 28.51701147 289.9984 56004.175150463 2012-03-18 04:12:13 56005.2466550926 2012-03-19 05:55:11 806093010 48.2169 45 48.2249 48.2169 0 48.2249 1 1 0 1 1 0 0 46.846 46.846 92.5679 0 PROCESSED 57604.9538773148 2016-08-04 22:53:35 56388 2013-04-06 00:00:00 56020.0984837963 2012-04-03 02:21:49 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 062024 Upcoming surveys of galaxy clusters require precise calibration of X-ray observables and mass down to low mass regimes to constraint cosmological parameters. However, it's still debated if groups can be treated as simply scaled-down clusters. Precise calibration needs to account for systematics due to the complex baryonic physics. Detailed and extended measurements out to large radii have the potential of accomplish this by exploring most of the system's volume and getting rid of biases derived from extrapolations. Suzaku is a powerful tool to address these studies with massive cluster, but we propose to demonstrate that by selecting the optimal target this can be extended to groups. We also show promising results from our Suzaku analysis of cluster outskirts. EXTRAGALACTIC DIFFUSE SOURCES 8 C BRENDA MIRANDA OCEJO EUR 6 AO6 MEASUREMENTS OF THE INTRACLUSTER EMISSION OF THE GROUP OF GALAXIES UGC03957 OUT TO $R_{200}$ WITH SUZAKU XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806093010/ Quick Look
106 SERSIC 159-03 348.4959 -42.7314 347.802109 -43.003937 330.666566 -34.355163 348.33340728 -64.81387916 47.3295 53851.5323611111 2006-04-26 12:46:36 53853.2668055556 2006-04-28 06:24:12 801093010 67.7843 70 67.8003 67.8003 67.7843 67.7923 2 2 2 2 1 0 0 41.5833 41.5833 149.8278 2 PROCESSED 57533.6210532407 2016-05-25 14:54:19 54400 2007-10-27 00:00:00 53907.8625231482 2006-06-21 20:42:02 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 012045 We propose to observe the cluster of galaxies Sersic 159-03 using a total exposure time of 70 ks to investigate the soft excess emission previously detected in the observations with ROSAT and XMM-Newton. The superior redistribution function of Suzaku will allow us to determine whether the O VII line emission detected with XMM-Newton is of local (Galactic) origin or is emitted by the warm-hot intergalactic medium (WHIM) in the vicinity of the cluster. The strong soft emission around this cluster together with the much improved response function of the XIS detectors at low energies make Sersic 159-03 the most promising target to unambiguously detect the WHIM for the first time in emission with Suzaku.