DARTS/Astro Query System - SQL Search -
All the tables available for SQL Search and information on each table are listed in the Available Data page. Please see the User Guide for the usage of "SQL Search".
total 181
No. |
object_name
|
center_ra
|
center_dec
|
center_ra_b1950
|
center_dec_b1950
|
center_ecliptic_lon
|
center_ecliptic_lat
|
center_galactic_lon
|
center_galactic_lat
|
roll_angle
|
observation_start_time_mjd
|
observation_start_time
|
observation_end_time_mjd
|
observation_end_time
|
observation_id
|
exposure
|
awarded_exposure
|
xis0_exposure
|
xis1_exposure
|
xis2_exposure
|
xis3_exposure
|
xis0_observation_mode
|
xis1_observation_mode
|
xis2_observation_mode
|
xis3_observation_mode
|
hxd_observation_mode
|
hxd_coarse_clock_rate_exposure
|
hxd_first_clock_rate_exposure
|
hxd_normal_clock_rate_exposure
|
hxd_all_clock_rate_exposure
|
hxd_wam_exposure
|
quantity_of_hxd_burst
|
processing_status
|
processing_date_mjd
|
processing_date
|
public_date_mjd
|
public_date
|
distribution_date_mjd
|
distribution_date
|
processing_version
|
processing_count
|
processing_software
|
proposal_id
|
proposal_abstract
|
proposal_category
|
proposal_category_code
|
proposal_priority
|
pi_name
|
co_pi_name
|
proposal_affiliated_country
|
proposal_cycle
|
observation_type
|
proposal_title
|
main_instrument
|
has_xis_injection
|
data_access_url
|
ql_access_url
|
ql_image_url
|
---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
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. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | JELLE KAASTRA | EUR | 1 | AO1 | O VII LINE EMISSION IN SERSIC 159-03 - WHIM OR GALACTIC ORIGIN? | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801093010/ | Quick Look | ![]() |
|
107 | HYDRA A SW | 139.253 | -12.251 | 138.651756 | -12.041032 | 145.924531 | -26.640711 | 242.88145003 | 24.78864489 | 106.4205 | 56241.8334490741 | 2012-11-10 20:00:10 | 56242.8342708333 | 2012-11-11 20:01:21 | 807090010 | 39.8399 | 40 | 39.8479 | 39.8559 | 0 | 39.8399 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 33.7085 | 33.7085 | 86.4639 | 0 | PROCESSED | 57607.9882407407 | 2016-08-07 23:43:04 | 56631 | 2013-12-05 00:00:00 | 56265.6332986111 | 2012-12-04 15:11:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072020 | Galaxy cluster outskirts are the regions where structure formation occurs through the accretion of smaller structures along large-scale filaments. Thanks to its low background, Suzaku has allowed for the first time to measure the thermodynamical properties of the ICM out to the virial radius. Recently, we used archival ROSAT observations to detect cluster emission out to large radii and quantify the deviations from spherical symmetry. Based on this work, we propose to map the outskirts of Hydra A, which was found to have the highest azimuthal scatter. This will allow us to measure the temperature profiles out to the virial radius and infer the bias on the mean thermodynamical properties and the mass reconstruction when clusters are observed along preferential directions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | DOMINIQUE ECKERT | EUR | 7 | AO7 | MAPPING THE OUTSKIRTS OF HYDRA A WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807090010/ | Quick Look | ![]() |
|
108 | NGC 6338 | 258.8129 | 57.4208 | 258.599761 | 57.475287 | 235.015954 | 79.490546 | 85.8195722 | 35.41601483 | 46.4308 | 56771.4831712963 | 2014-04-24 11:35:46 | 56771.8058333333 | 2014-04-24 19:20:24 | 809099010 | 15.4756 | 10 | 15.4756 | 15.4756 | 0 | 15.4756 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 14.5259 | 14.5259 | 26.0449 | 0 | PROCESSED | 57614.9892708333 | 2016-08-14 23:44:33 | 57155 | 2015-05-13 00:00:00 | 56789.6384722222 | 2014-05-12 15:19:24 | 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 | 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/ver3.0/809099010/ | Quick Look | ![]() |
|
109 | AWM4 | 241.2331 | 23.9108 | 240.70062 | 24.045882 | 232.521444 | 43.67819 | 39.92527821 | 46.49145981 | 302.6954 | 56859.2473263889 | 2014-07-21 05:56:09 | 56859.4627314815 | 2014-07-21 11:06:20 | 809102010 | 9.31 | 11 | 9.31 | 9.438 | 0 | 9.438 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.4155092593 | 2016-08-15 09:58:20 | 57239 | 2015-08-05 00:00:00 | 56873.5548958333 | 2014-08-04 13:19:03 | 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/ver3.0/809102010/ | Quick Look | ![]() |
|
110 | ABELL 3733 | 315.4567 | -28.0341 | 314.710836 | -28.231283 | 309.79285 | -10.656463 | 17.77333082 | -39.60697798 | 260.2652 | 56981.8706481482 | 2014-11-20 20:53:44 | 56982.1530439815 | 2014-11-21 03:40:23 | 809108010 | 14.5884 | 15 | 14.5964 | 14.6044 | 0 | 14.5884 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7988541667 | 2016-08-16 19:10:21 | 57362 | 2015-12-06 00:00:00 | 56996.4060300926 | 2014-12-05 09:44:41 | 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/ver3.0/809108010/ | Quick Look | ![]() |
|
111 | A3404 | 101.1266 | -54.2028 | 100.864696 | -54.149703 | 118.987538 | -76.520827 | 263.61200949 | -22.68018452 | 319.1401 | 54971.6181944444 | 2009-05-20 14:50:12 | 54974.625162037 | 2009-05-23 15:00:14 | 804089010 | 122.0929 | 121 | 122.1009 | 122.1009 | 0 | 122.0929 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 106.1261 | 106.1261 | 259.7879 | 4 | PROCESSED | 57546.7060532407 | 2016-06-07 16:56:43 | 55358 | 2010-06-11 00:00:00 | 54992.6862615741 | 2009-06-10 16:28:13 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042025 | Robust and precise mass measurements for a large number of galaxy clusters represent the single most important step to prepare for dark energy cluster surveys to be performed, e.g., with eROSITA. Robustness and precision can best be achieved by a comparative and combined analysis of independent techniques. Here, we propose to use measurements from Suzaku, APEX-SZ, and wide-field optical telescopes to determine cluster masses up to the virial radius. X-ray, SZ, and gravitational lensing reduction and analyses will all be performed by experts at a single location. We demonstrate that we have selected the optimal targets for this study. Further, we show promising results from our Suzaku analysis of cluster outskirts, from our lensing pipeline, as well as from our combined SZ/X-ray method. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | THOMAS REIPRICH | EUR | 4 | AO4 | COMBINED SUZAKU/APEX-SZ/LENSING MASS MEASUREMENTS OF THE GALAXY CLUSTERS A3404 AND A2537 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804089010/ | Quick Look | ![]() |
|
112 | A2877-SOUTH | 17.378 | -46.6527 | 16.824483 | -46.918871 | 351.212416 | -48.486015 | 293.76700694 | -70.15260223 | 237.9995 | 56647.8346643518 | 2013-12-21 20:01:55 | 56649.916875 | 2013-12-23 22:00:18 | 808103010 | 83.5172 | 80 | 83.5172 | 83.5252 | 0 | 83.5332 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81.2993 | 81.2993 | 179.8979 | 4 | PROCESSED | 57613.6802199074 | 2016-08-13 16:19:31 | 57033 | 2015-01-11 00:00:00 | 56665.8173263889 | 2014-01-08 19:36:57 | 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/ver3.0/808103010/ | Quick Look | ![]() |
|
113 | A3528-S OFFSET 1 | 193.8801 | -29.4768 | 193.202783 | -29.206094 | 204.617979 | -21.613954 | 303.99602967 | 33.38651365 | 289.4829 | 56500.4359953704 | 2013-07-27 10:27:50 | 56501.528587963 | 2013-07-28 12:41:10 | 808104010 | 40.3411 | 50 | 40.3491 | 40.3491 | 0 | 40.3411 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.8623 | 40.8623 | 94.384 | 2 | PROCESSED | 57612.0687037037 | 2016-08-12 01:38:56 | 56955 | 2014-10-25 00:00:00 | 56587.7834490741 | 2013-10-22 18:48:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082018 | We propose to observe, for a total of 180 ks, the region between the galaxy cluster A3528 and the complex A3530-A3532, in which we expect to find the filament connecting the clusters. With the requested time we aim to detect the Warm Hot Intergalactic Medium (WHIM) by its thermal soft-Xray emission, to resolve one of the major problems of modern astrophysics - the missing baryons , which are now thought to reside in the filaments connecting clusters. In addition to a full understanding of the typical baryon fraction, the proposed observations will allow us to study the gas clumping in the cluster outskirts. Furthermore, a combined analysis of X-ray and optical data will enable us to shed light on the influence of the environments on galaxy evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | LORENZO LOVISARI | EUR | 8 | AO8 | TRACING A FILAMENT IN THE OUTSKIRTS OF THE SHAPLEY SUPERCLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808104010/ | Quick Look | ![]() |
|
114 | A3526 | 191.2847 | -39.8559 | 190.600127 | -39.582502 | 207.545871 | -31.88181 | 301.61867579 | 22.99978629 | 109.9984 | 55943.9465393518 | 2012-01-17 22:43:01 | 55944.2683333333 | 2012-01-18 06:26:24 | 806089010 | 15.9106 | 15 | 15.9186 | 15.9106 | 0 | 15.9186 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.985 | 12.985 | 27.7919 | 0 | PROCESSED | 57604.3987268518 | 2016-08-04 09:34:10 | 56332 | 2013-02-09 00:00:00 | 55964.1580439815 | 2012-02-07 03:47:35 | 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/ver3.0/806089010/ | Quick Look | ![]() |
|
115 | J2218.6-0346 | 334.6629 | -3.7693 | 334.013965 | -4.02026 | 335.129241 | 6.290164 | 58.79146355 | -46.71055995 | 71.7798 | 56063.8991550926 | 2012-05-16 21:34:47 | 56064.7196875 | 2012-05-17 17:16:21 | 807085010 | 28.629 | 25 | 28.629 | 28.629 | 0 | 28.629 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.8327 | 26.8327 | 70.8839 | 1 | PROCESSED | 57605.4341550926 | 2016-08-05 10:25:11 | 56442 | 2013-05-30 00:00:00 | 56076.0273726852 | 2012-05-29 00:39:25 | 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/ver3.0/807085010/ | Quick Look | ![]() |
|
116 | A3528-S OFFSET 3 | 194.0873 | -29.8404 | 193.408879 | -29.569931 | 204.956936 | -21.869821 | 304.20210274 | 33.01923597 | 288.9994 | 56502.3985300926 | 2013-07-29 09:33:53 | 56503.6522453704 | 2013-07-30 15:39:14 | 808106010 | 61.2339 | 60 | 61.2579 | 61.2499 | 0 | 61.2339 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61.6474 | 61.6474 | 108.3097 | 2 | PROCESSED | 57612.1235763889 | 2016-08-12 02:57:57 | 56955 | 2014-10-25 00:00:00 | 56587.4691782407 | 2013-10-22 11:15:37 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082018 | We propose to observe, for a total of 180 ks, the region between the galaxy cluster A3528 and the complex A3530-A3532, in which we expect to find the filament connecting the clusters. With the requested time we aim to detect the Warm Hot Intergalactic Medium (WHIM) by its thermal soft-Xray emission, to resolve one of the major problems of modern astrophysics - the missing baryons , which are now thought to reside in the filaments connecting clusters. In addition to a full understanding of the typical baryon fraction, the proposed observations will allow us to study the gas clumping in the cluster outskirts. Furthermore, a combined analysis of X-ray and optical data will enable us to shed light on the influence of the environments on galaxy evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | LORENZO LOVISARI | EUR | 8 | AO8 | TRACING A FILAMENT IN THE OUTSKIRTS OF THE SHAPLEY SUPERCLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808106010/ | Quick Look | ![]() |
|
117 | NGC 5728 | 220.5794 | -17.3095 | 219.88301 | -17.096936 | 223.49481 | -1.485509 | 337.26599487 | 38.0606459 | 290.4081 | 53935.7359143518 | 2006-07-19 17:39:43 | 53936.6264930556 | 2006-07-20 15:02:09 | 701079010 | 41.3077 | 40 | 41.3077 | 41.3077 | 41.3077 | 41.3077 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39.569 | 39.569 | 76.9419 | 0 | PROCESSED | 57535.0121064815 | 2016-05-27 00:17:26 | 54400 | 2007-10-27 00:00:00 | 53943.5061111111 | 2006-07-27 12:08:48 | 3.0.22.43 | 6 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012016 | The high-energy detectors onboard Swift and INTEGRAL have started to survey the hard X-ray sky above 10 keV. Although limited to bright X-ray fluxes (~10^-11 cgs), the large area surveyed so far has allowed to build up sizable sa mples of hard X-ray selected AGN almost unbiased against X-ray absorption. The AGN content of these surveys is dominated by obscured AGN. We have identified 3 objects which are most likely obscured by Compton-thick matter and very bright above 10 keV. We propose to observe them with Suzaku for 40 ks each to study their broad-band X-ray spectra and unveil previously unknown nearby heavily obscured AGN, with important consequences for the study of the AGN evolution and the synthesis of the X-ray background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ANDREA COMASTRI | EUR | 1 | AO1 | BRIGHT COMPTON THICK GALAXIES IN THE BACKYARD | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701079010/ | Quick Look | ![]() |
|
118 | XTE J1710-281 | 257.5483 | -28.1282 | 256.762614 | -28.066297 | 258.983914 | -5.161686 | 356.35839186 | 6.92613447 | 86.2275 | 55278.9207638889 | 2010-03-23 22:05:54 | 55281.1460300926 | 2010-03-26 03:30:17 | 404068010 | 76.1385 | 75 | 76.1385 | 76.1465 | 0 | 76.1465 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 23.6565 | 23.6565 | 192.2397 | 3 | PROCESSED | 57551.0466435185 | 2016-06-12 01:07:10 | 55668 | 2011-04-17 00:00:00 | 55301.5227662037 | 2010-04-15 12:32:47 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042003 | We propose to observe XTE J1710-281, a low-mass X-ray binary showing bursts, eclipses and dips. We want to determine the nature of the X-ray emission in this yet poorly-studied system and exploit the fact it is viewed close to edge-on to probe the structure of the disk and of the ionized plasma located above it. The broad-band coverage of Suzaku XIS and HXD will allow us to determine the overall shape of the ionizing continuum, which is a key parameter to infer the properties of the warm absorber whose narrow spectral signatures will be simultaneously detected thanks to the good spectral resolution of XIS near 6 keV. | GALACTIC POINT SOURCES | 4 | C | LAURENCE BOIRIN | EUR | 4 | AO4 | SUZAKU TO INVESTIGATE A LOW-MASS X-RAY BINARY SHOWING BURSTS, ECLIPSES, AND DIPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404068010/ | Quick Look | ![]() |
|
119 | HESS J1718-385 | 259.5578 | -38.4584 | 258.700067 | -38.405877 | 261.528277 | -15.323293 | 348.92137939 | -0.45364037 | 266.9006 | 54706.233599537 | 2008-08-28 05:36:23 | 54706.9286342593 | 2008-08-28 22:17:14 | 503108010 | 23.5097 | 20 | 23.5097 | 23.5097 | 0 | 23.5097 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.4402 | 19.4402 | 60.0479 | 1 | PROCESSED | 57543.4301851852 | 2016-06-04 10:19:28 | 55093 | 2009-09-19 00:00:00 | 54720.4386689815 | 2008-09-11 10:31:41 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032026 | HESS J1718-385 is a newly discovered Very High Energy (VHE) source with an unusually hard energy spectrum, close to an energetic pulsar. The classification as a VHE Pulsar Wind Nebula (PWN) was confirmed by observations of the region with XMM-Newton and Suzaku. XMM showed a compact X-ray PWN around the pulsar, whereas Suzaku revealed low surface brightness emission close to the VHE source. To morphologically connect this low surface brightness emission to the X-ray PWN, we propose another short, 20 ksec Suzaku pointing, aiming between the VHE source center and the pulsar location. The data will allow to identify the new Suzaku source with the compact X-ray PWN. The spectra will be used to investigate the unusual particle energy distribution that is derived from the hard VHE spectrum. | GALACTIC DIFFUSE EMISSION | 5 | A | GERD PUEHLHOFER | EUR | 3 | AO3 | SUZAKU OBSERVATIONS OF THE LOW SURFACE BRIGHTNESS X-RAY PULSAR WIND NEBULA CANDIDATE ASSOCIATED WITH HESS J1718-385 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503108010/ | Quick Look | ![]() |
|
120 | J1803-2149 | 270.7914 | -21.8184 | 270.03917 | -21.820419 | 270.725404 | 1.620434 | 8.14241987 | 0.18738401 | 269.7005 | 56191.3371643518 | 2012-09-21 08:05:31 | 56192.1730671296 | 2012-09-22 04:09:13 | 407092010 | 31.9986 | 25 | 32.0218 | 32.0146 | 0 | 31.9986 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.8812 | 28.8812 | 72.2179 | 1 | PROCESSED | 57607.1276736111 | 2016-08-07 03:03:51 | 56584 | 2013-10-19 00:00:00 | 56218.5534259259 | 2012-10-18 13:16:56 | 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/ver3.0/407092010/ | Quick Look | ![]() |
|
121 | GX 339-4 | 255.7041 | -48.783 | 254.756356 | -48.711998 | 259.573299 | -25.856913 | 338.94384752 | -4.32149031 | 92.8952 | 55627.5468518518 | 2011-03-07 13:07:28 | 55628.0320138889 | 2011-03-08 00:46:06 | 405063050 | 16.9925 | 20 | 16.9925 | 20.2693 | 0 | 20.2693 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.9851 | 15.9851 | 41.8741 | 2 | PROCESSED | 57601.1142476852 | 2016-08-01 02:44:31 | 56015 | 2012-03-29 00:00:00 | 55645.2088078704 | 2011-03-25 05:00:41 | 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/ver3.0/405063050/ | Quick Look | ![]() |
|
122 | AX J1818.8-1559 | 274.7184 | -16.0002 | 273.997976 | -16.021361 | 274.56335 | 7.365738 | 15.02984997 | -0.2600064 | 265.8517 | 55849.5538888889 | 2011-10-15 13:17:36 | 55852.1474537037 | 2011-10-18 03:32:20 | 406074010 | 95.1912 | 100 | 99.3859 | 99.3859 | 0 | 95.1912 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 83.8746 | 83.8746 | 224.0699 | 1 | PROCESSED | 57603.4900347222 | 2016-08-03 11:45:39 | 56241 | 2012-11-10 00:00:00 | 55873.993599537 | 2011-11-08 23:50:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062016 | The Galactic X-ray source AX J1818.8-1559 is a possible new member of the small class of magnetar candidates since a short and soft burst was detected in the 15--100 keV range from this source in 2007 with INTEGRAL. We request a Suzaku pointing of 100 ks in order to carry out a sensitive search for pulsations. This, together with the good quality spectrum, possibly extending in the hard X-ray range, that can be obtained with the Suzaku instruments, will allow us to reveal the nature of AX J1818.8-1559, most likely adding a new member to the small but rapidly increasing family of magnetar candidates | GALACTIC POINT SOURCES | 4 | B | SANDRO MEREGHETTI | EUR | 6 | AO6 | A NEW GALACTIC MAGNETAR CANDIDATE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406074010/ | Quick Look | ![]() |
|
123 | J1746-3239 | 266.7261 | -32.6662 | 265.90725 | -32.648308 | 267.198391 | -9.25684 | 356.95543166 | -2.17351712 | 72.0153 | 56365.6469675926 | 2013-03-14 15:31:38 | 56366.4022453704 | 2013-03-15 09:39:14 | 407093010 | 27.3469 | 25 | 27.3469 | 27.3469 | 0 | 27.3469 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.005 | 27.005 | 65.2519 | 2 | PROCESSED | 57610.8216087963 | 2016-08-10 19:43:07 | 56745 | 2014-03-29 00:00:00 | 56379.530775463 | 2013-03-28 12:44:19 | 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/ver3.0/407093010/ | Quick Look | ![]() |
|
124 | MRK 231 | 193.9205 | 56.8603 | 193.380984 | 57.130758 | 158.183244 | 55.13624 | 121.76268106 | 60.25831511 | 352.6128 | 55678.6054282407 | 2011-04-27 14:31:49 | 55682.3543402778 | 2011-05-01 08:30:15 | 706037010 | 197.5113 | 200 | 197.5113 | 197.5113 | 0 | 197.5113 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 191.7434 | 191.7434 | 323.8756 | 2 | PROCESSED | 57602.0326851852 | 2016-08-02 00:47:04 | 56065 | 2012-05-18 00:00:00 | 55697.4231597222 | 2011-05-16 10:09:21 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062008 | We propose the first Suzaku observation of the nearest low-ionization BAL quasar/ULIRG, i.e. MRK 231, for which we have recently reported the most clear-cut evidence for AGN-driven feedback onto the host galaxy cold molecular gas component. Our target exhibits an hard X-ray (> 15 keV) excess in a previous BeppoSAX/PDS spectrum, suggesting the presence of a heavily obscured quasar at the heart of this peculiar system. By exploiting the Suzaku unique broad-band spectral coverage, we aim at deriving the column density of the nuclear absorber and, in turn, the intrinsic luminosity of the quasar with unprecedented accuracy. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ENRICO PICONCELLI | EUR | 6 | AO6 | BROAD-BAND X-RAY SPECTROSCOPY OF THE NEAREST BAL QUASAR/ULIRG MARKARIAN 231 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706037010/ | Quick Look | ![]() |
|
125 | RBS 1124 | 187.6975 | 70.7093 | 187.160497 | 70.985277 | 134.358757 | 62.072206 | 125.39855918 | 46.31993489 | 339.073 | 54204.9538078704 | 2007-04-14 22:53:29 | 54206.5786921296 | 2007-04-16 13:53:19 | 702114010 | 86.2284 | 88 | 86.2284 | 86.2284 | 0 | 86.2284 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 88.8555 | 88.8555 | 140.384 | 3 | PROCESSED | 57538.4340740741 | 2016-05-30 10:25:04 | 54744 | 2008-10-05 00:00:00 | 54210.6501851852 | 2007-04-20 15:36:16 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022019 | We propose a 70 ks observation of RBS 1124 (z=0.208). This is the X--ray brightest radio--quiet quasar (> 4e45 erg/s in the 2-10 keV band) from the ROSAT bright source catalogue. The expected number of counts (e.g. about 120,000 in just one FI XIS unit and about 11,000 in the HXD/PIN) will provide the best quality X-ray spectrum so far for such a high luminosity AGN. We will investigate the main X-ray spectral components shedding light on this extreme class of objects with unprecedented accuracy making full use of the Suzaku sensitivity across the whole band (XIS and HXD). | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GIOVANNI MINIUTTI | EUR | 2 | AO2 | REVEALING THE X-RAY EMISSION/ACCRETION PROCESSES IN THE VERY LUMINOUS RADIO-QUIET AND X-RAY BRIGHT QUASAR RBS 1124 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702114010/ | Quick Look | ![]() |
|
126 | MCG+8-11-11 | 88.7233 | 46.5039 | 87.789525 | 46.495439 | 89.047199 | 23.067702 | 165.67352488 | 10.43795472 | 91.6485 | 54360.0736342593 | 2007-09-17 01:46:02 | 54362.2640509259 | 2007-09-19 06:20:14 | 702112010 | 98.7481 | 100 | 98.7481 | 98.7561 | 0 | 98.7641 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89.2138 | 89.2138 | 186.4387 | 1 | PROCESSED | 57540.0368055556 | 2016-06-01 00:53:00 | 54751 | 2008-10-12 00:00:00 | 54371.4963078704 | 2007-09-28 11:54:41 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022004 | We propose to observe with Suzaku for 100 ks one of the X-ray brightest AGN, the Seyfert 1 galaxy MCG+8-11-11, with the aim to measure the fraction of the reflection component and the iron abundance. Suzaku provides a unique opportunity to perform this kind of analysis, thanks to its broadband coverage. Moreover, the proposed observation will provide an extremely good spectrum, which will allow us to measure the iron line width, its Compton Shoulder and the ionization stage of iron. These three measurements will contribute to provide useful information on the nature of the iron line emitting material, its distance from the central Black Hole and the mass of the latter. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | STEFANO BIANCHI | EUR | 2 | AO2 | MCG+8-11-11: A BROADBAND SPECTRUM OF ONE OF THE X-RAY BRIGHTEST AGN | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702112010/ | Quick Look | ![]() |
|
127 | IC4329A | 207.3319 | -30.3116 | 206.617739 | -30.063444 | 216.345797 | -17.778855 | 317.49719871 | 30.9175719 | 295.4804 | 54323.458599537 | 2007-08-11 11:00:23 | 54324.2127777778 | 2007-08-12 05:06:24 | 702113030 | 26.8959 | 25 | 26.8959 | 26.8959 | 0 | 26.8959 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23.8723 | 23.8723 | 65.1309 | 0 | PROCESSED | 57539.4615972222 | 2016-05-31 11:04:42 | 54730 | 2008-09-21 00:00:00 | 54347.7226041667 | 2007-09-04 17:20:33 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022009 | IC 4329A is the brightest known Seyfert 1 galaxy between ~2-30 keV (F(2-10 keV)~1-2e-10 erg/cm2s). With its clear warm absorber and reflection component, it is often taken as the prototypical Sey 1 galaxy. Its X-ray variability is strong enough (and on a sufficiently long time scale, ideal for Suzaku) to make multiple observations critical for probing the origin of the Compton reflection component, and to attempt measuring variations of the high energy cut-off. We thus propose 5x20 ks observations to monitor i) the correlated variability of the reflection continuum plus FeK line to primary continuum variations, and ii) the variations in the high-E cut-off, and their relation with the power-law, and iii) check the evidence for a blueshifted (v~0.1c) FeK absorption line at ~7.7 keV. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MASSIMO CAPPI | EUR | 2 | AO2 | SUZAKU MULTIPLE OBSERVATIONS OF IC4329A TO PROBE THE ORIGIN OF THE COMPTON REFLECTION COMPONENT AND HIGH-ENERGY CUT-OFF | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702113030/ | Quick Look | ![]() |
|
128 | M87N BRIGHT | 187.7 | 12.7001 | 187.067492 | 12.976168 | 181.920384 | 14.695127 | 283.404729 | 74.78396174 | 297.7704 | 54625.0923263889 | 2008-06-08 02:12:57 | 54625.6259722222 | 2008-06-08 15:01:24 | 803070010 | 24.2485 | 20 | 24.2565 | 24.2485 | 0 | 24.2565 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20.2709 | 20.2709 | 46.1039 | 1 | PROCESSED | 57542.7423263889 | 2016-06-03 17:48:57 | 55009 | 2009-06-27 00:00:00 | 54642.2018865741 | 2008-06-25 04:50:43 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032011 | We propose to take advantage of Suzaku's low background and good collecting area to observe a strong surface brightness discontinuity, most likely a cold front, in the outskirts of M87. We will make accurate temperature and pressure profiles across this cold front, determine the energy associated with it, and compare this to the energy of known AGN-ICM interaction features in M87. With Suzaku's superior spectral redistribution function we will for the first time measure Mg and O in the M87 outskirts and improve constraints on relative contributions by SNIa and SNII. We will study abundance and abundance-ratio variations across the cold front and determine the role of gas sloshing in transporting metals produced by the central galaxy into the ICM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | EUR | 3 | AO3 | THE ENERGETICS AND METAL ABUNDANCE PATTERNS IN THE OUTSKIRTS OF M87 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803070010/ | Quick Look | ![]() |
|
129 | SWIFT J2127.4+5654 | 322.001 | 56.878 | 321.622917 | 56.659223 | 3.253872 | 64.455644 | 97.78160785 | 4.29621592 | 243.6186 | 54443.0645023148 | 2007-12-09 01:32:53 | 54445.0487962963 | 2007-12-11 01:10:16 | 702122010 | 91.7304 | 88 | 0 | 91.7304 | 0 | 91.7304 | 0 | 2 | 0 | 2 | 1 | 0 | 0 | 89.3485 | 89.3485 | 171.3799 | 2 | PROCESSED | 57540.867974537 | 2016-06-01 20:49:53 | 55000 | 2009-06-18 00:00:00 | 54633.7130439815 | 2008-06-16 17:06:47 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022034 | We propose to observe with Suzaku two Narrow Line Seyfert 1 galaxies detected by SWIFT/BAT and INTEGRAL with a flux in excess of $10^{-11}$~erg~s$^{-1}$~cm$^{-2}$ in the HXD/PIN band for 70~ks each. These proposed observations provide rare high quality spectra of NLS1s above 10~keV. This will remove the spectral degeneracies inherent to limited bandpass analysis (such as that with XMM--Newton and Chandra) and the ambiguities between the different proposed models invoked to explain the unique spectral and variability properties of these most extreme class of high accretion rate sources (namely absorption, reflection, nature of the soft excess...). | EXTRAGALACTIC COMPACT SOURCES | 7 | C | GIOVANNI MINIUTTI | EUR | 2 | AO2 | HUNTING HARD-X-RAY-BRIGHT NLS1 GALAXIES FROM THE INTEGRAL CATALOGUE WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702122010/ | Quick Look | ![]() |
|
130 | MKN 841 | 225.9811 | 10.3761 | 225.377197 | 10.570593 | 220.178092 | 26.525473 | 11.09749436 | 54.61837916 | 292.433 | 54304.6970949074 | 2007-07-23 16:43:49 | 54306.218912037 | 2007-07-25 05:15:14 | 701084020 | 50.9253 | 50 | 50.9253 | 50.9333 | 0 | 50.9333 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.6556 | 47.6556 | 131.4738 | 2 | PROCESSED | 57539.3432060185 | 2016-05-31 08:14:13 | 54800 | 2008-11-30 00:00:00 | 54339.5240277778 | 2007-08-27 12:34:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012028 | We propose to perform two 50 ks Suzaku observations of Mkn 841, at an interval of a few months, in order to elucidate the origin of its different X-ray components. Strong soft excess and complex iron line profile are known to be present in this source and recent XMM observations reveal their extreme and puzzling spectral and temporal behaviors. Nevertheless, while the XMM observations help to better constrain their natures, their physical interpretation strongly suffer from the lack of data above 10 keV. Two dedicated Suzaku observations will provide crucial information for our understanding of these components, allowing 1) to obtain high S/N and striclty simultaneous broad band X-ray spectra from the soft X-ray up to the reflection bump and 2) to study their spectral variability behaviors | EXTRAGALACTIC COMPACT SOURCES | 7 | B | PIERRE-OLIVIER PETRUCCI | EUR | 1 | AO1 | PROBING THE ORIGIN OF THE STRONG SOFT EXCESS AND PUZZLING REFLECTION COMPONENTS IN MKN 841 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701084020/ | Quick Look | ![]() |
|
131 | QSO 1828+487 | 277.4042 | 48.7379 | 277.077989 | 48.702797 | 285.744941 | 71.774201 | 77.22058509 | 23.48843965 | 218.1356 | 56983.2742592593 | 2014-11-22 06:34:56 | 56983.6771875 | 2014-11-22 16:15:09 | 709026010 | 14.1766 | 15 | 14.1766 | 14.1766 | 0 | 14.1766 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8008912037 | 2016-08-16 19:13:17 | 57442 | 2016-02-24 00:00:00 | 57076.4104861111 | 2015-02-23 09:51:06 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092023 | EXTRAGALACTIC COMPACT SOURCES | 7 | C | MARCUS LANGEJAHN | EUR | 9 | AO9 | false | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709026010/ | Quick Look | ![]() |
||
132 | ABELL 2204 | 248.0963 | 5.6404 | 247.481247 | 5.74563 | 245.314616 | 27.222606 | 21.10023438 | 33.35451369 | 261.3606 | 53995.3098958333 | 2006-09-17 07:26:15 | 53996.5098958333 | 2006-09-18 12:14:15 | 801091010 | 49.1113 | 55 | 49.1113 | 49.1113 | 49.1113 | 49.1113 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 51.9372 | 51.9372 | 103.6439 | 1 | PROCESSED | 57535.6038194444 | 2016-05-27 14:29:30 | 54526 | 2008-03-01 00:00:00 | 54020.8840277778 | 2006-10-12 21:13:00 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012018 | Measurements of the intracluster gas temperatures out to large radii, where most 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 temperatures at the cluster virial radius have failed. Here we show that such measurements appear feasible now for the first time with the Suzaku X-ray CCDs. Furthermore, we show that A2204 and A2163 are optimal targets for such an investigation. We, therefore, propose to observe A2204 for 55 ks and A2163 for 100 ks to measure the gas temperature to 10% and 15% accuracy (1-sigma), respectively, out to the cluster virial radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | THOMAS REIPRICH | EUR | 1 | AO1 | A2204 AND A2163: GALAXY CLUSTER GAS TEMPERATURE MEASUREMENT UP TO THE VIRIAL RADIUS | SPE | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801091010/ | Quick Look | ![]() |
|
133 | ABELL 2537 | 347.0895 | -2.1864 | 346.446208 | -2.457426 | 347.265087 | 3.085071 | 73.83613509 | -54.91382092 | 56.4647 | 55368.5295486111 | 2010-06-21 12:42:33 | 55371.9946875 | 2010-06-24 23:52:21 | 805090010 | 124.8232 | 129 | 124.8472 | 124.8232 | 0 | 124.8472 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 108.3908 | 108.3908 | 281.2176 | 1 | PROCESSED | 57552.4996412037 | 2016-06-13 11:59:29 | 55772 | 2011-07-30 00:00:00 | 55403.4592361111 | 2010-07-26 11:01:18 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052007 | Robust and precise mass measurements for a large number of galaxy clusters represent the single most important step to prepare for dark energy cluster surveys to be performed, e.g., with eROSITA. Robustness and precision can best be achieved by a comparative and combined analysis of independent techniques. Here, we propose to use measurements from Suzaku, APEX-SZ, and wide-field optical telescopes to determine cluster masses up to the virial radius. X-ray, SZ, and gravitational lensing reductions and analyses will all be performed by experts at a single location. We demonstrate that we have selected the optimal targets for this study. Further, we show promising results from our Suzaku analysis of cluster outskirts, from our lensing pipeline, as well as from our combined SZ/X-ray method. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | THOMAS REIPRICH | EUR | 5 | AO5 | COMBINED SUZAKU/APEX-SZ/LENSING MASS MEASUREMENTS OF THE GALAXY CLUSTER A2537 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805090010/ | Quick Look | ![]() |
|
134 | TW HYA | 165.4619 | -34.7081 | 164.870404 | -34.438931 | 182.672236 | -37.188941 | 278.67685486 | 22.95004903 | 99.3673 | 54429.0615625 | 2007-11-25 01:28:39 | 54429.6946064815 | 2007-11-25 16:40:14 | 402089020 | 20.0096 | 11 | 20.0096 | 20.0176 | 0 | 20.0256 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17.55 | 17.55 | 54.6879 | 2 | PROCESSED | 57540.5900115741 | 2016-06-01 14:09:37 | 54804 | 2008-12-04 00:00:00 | 54434.1387268518 | 2007-11-30 03:19:46 | 3.0.22.43 | 2 | 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 | B | 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/ver3.0/402089020/ | Quick Look | ![]() |
|
135 | 4U 1820-30 | 275.9316 | -30.4206 | 275.12802 | -30.447431 | 275.142418 | -7.085697 | 2.73970623 | -7.95024046 | 261.8755 | 55096.0447453704 | 2009-09-22 01:04:26 | 55096.8335416667 | 2009-09-22 20:00:18 | 404069030 | 29.2254 | 20 | 29.2254 | 29.2254 | 0 | 29.2254 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 25.9405 | 25.9405 | 68.148 | 1 | PROCESSED | 57548.6598726852 | 2016-06-09 15:50:13 | 55477 | 2010-10-08 00:00:00 | 55110.3989699074 | 2009-10-06 09:34:31 | 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/ver3.0/404069030/ | Quick Look | ![]() |
|
136 | 4U 1735-44 | 264.7467 | -44.4484 | 263.834293 | -44.420689 | 265.97323 | -21.080234 | 346.05710105 | -6.99533469 | 268.9985 | 56917.7849884259 | 2014-09-17 18:50:23 | 56918.9988194444 | 2014-09-18 23:58:18 | 408043020 | 10.1772 | 60 | 10.1772 | 10.2016 | 0 | 10.3047 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5500925926 | 2016-08-16 13:12:08 | 57626 | 2016-08-26 00:00:00 | 56940.6296064815 | 2014-10-10 15:06:38 | 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/ver3.0/408043020/ | Quick Look | ![]() |
|
137 | GRO J1008-57 | 152.4313 | -58.2999 | 151.999865 | -58.053533 | 193.901629 | -61.317749 | 282.99773034 | -1.83149103 | 115.5012 | 56660.6548148148 | 2014-01-03 15:42:56 | 56661.5897569444 | 2014-01-04 14:09:15 | 408044010 | 15.3374 | 20 | 15.3374 | 15.3479 | 0 | 15.3374 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 22.1794 | 22.1794 | 55.0379 | 1 | PROCESSED | 57613.7393981482 | 2016-08-13 17:44:44 | 57040 | 2015-01-18 00:00:00 | 56679.7652662037 | 2014-01-22 18:21:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082019 | We propose to observe the transient XRB GRO J1008−57 for 20 ks during an outburst in 2014 January after the currently ongoing giant outburst. The source exhibits regular outbursts once per orbit. Several of these outbursts have been observed in the past showing that the spectral shape remains constant between outbursts. Since we were able to improve the orbital ephemeris it is possible to predict future outbursts of the source. The source is currently (MJD 56245) exhibiting a giant type II outburst showing that the companion has ejected large amounts of material. We therefore propose to observe the system after this outburst to check for spectral and temporal changes and to study the iron line complex to derive the amount and ionization state of the material. | GALACTIC POINT SOURCES | 4 | A | INGO KREYKENBOHM | EUR | 8 | AO8 | MEASURING THE RESIDUAL MATERIAL IN GRO J1008−57 AFTER THE GIANT OUTBURST | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408044010/ | Quick Look | ![]() |
|
138 | MARKARIAN 3 | 93.8921 | 71.0501 | 92.441744 | 71.065491 | 91.879164 | 47.635184 | 143.28202475 | 22.71957945 | 87.4437 | 56931.9222337963 | 2014-10-01 22:08:01 | 56932.4181597222 | 2014-10-02 10:02:09 | 709022010 | 23.831 | 20 | 23.831 | 23.831 | 0 | 23.8376 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5994328704 | 2016-08-16 14:23:11 | 57345 | 2015-11-19 00:00:00 | 56979.4072569444 | 2014-11-18 09:46:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092008 | We propose to measure size and distance from the black hole of the optically-thick absorbing and reprocessing system(s) in the heavily obscured Seyfert Galaxy Markarian~3 by means of its known X-ray spectral variability. We aim at simultaneously measuring: the variability timescale of the primary emission, seen in transmission through a photoelectric column density of (0.7--1.1)x10^{24} atoms/cm/cm; the variability timescale of its Compton-reflection, dominating the continuum flux in the 3-10 keV energy band; and the variability timescale of the nuclear obscuration. Only the scientific payload on-board Suzaku possesses the required combination of broadband X-ray coverage, sensitivity, and spectroscopic capabilities to perform this experiment. We request 5 observations of 20 ks each. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MATTEO GUAINAZZI | EUR | 9 | AO9 | MEASURING THE TORUS SPATIAL SCALE(S) IN SEYFERT GALAXIES: A SUZAKU MONITORING OF MARKARIAN 3 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709022010/ | Quick Look | ![]() |
|
139 | A3526 | 191.5735 | -40.3305 | 190.887021 | -40.05737 | 208.034799 | -32.201568 | 301.8706053 | 22.53064841 | 109.9984 | 55943.2367592593 | 2012-01-17 05:40:56 | 55943.6161574074 | 2012-01-17 14:47:16 | 806087010 | 14.4943 | 13 | 14.4943 | 14.4943 | 0 | 14.4943 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.3865 | 10.3865 | 32.7799 | 1 | PROCESSED | 57604.3860416667 | 2016-08-04 09:15:54 | 56332 | 2013-02-09 00:00:00 | 55964.1523148148 | 2012-02-07 03:39:20 | 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/ver3.0/806087010/ | Quick Look | ![]() |
|
140 | A3526 | 191.429 | -40.092 | 190.743483 | -39.818735 | 207.789532 | -32.040636 | 301.74515791 | 22.76656347 | 109.9976 | 55943.6166319444 | 2012-01-17 14:47:57 | 55943.9461111111 | 2012-01-17 22:42:24 | 806088010 | 15.0662 | 14 | 15.0702 | 15.0662 | 0 | 15.0662 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.8434 | 14.8434 | 28.458 | 1 | PROCESSED | 57604.3884490741 | 2016-08-04 09:19:22 | 56332 | 2013-02-09 00:00:00 | 55964.2169675926 | 2012-02-07 05:12:26 | 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/ver3.0/806088010/ | Quick Look | ![]() |
|
141 | IGR J16185-5928 | 244.6464 | -59.4001 | 243.583076 | -59.27851 | 254.074844 | -37.350679 | 326.66672881 | -6.44446627 | 90.0003 | 54505.6700115741 | 2008-02-09 16:04:49 | 54507.0211111111 | 2008-02-11 00:30:24 | 702123010 | 76.6076 | 88 | 76.631 | 76.6236 | 0 | 76.6076 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 75.2553 | 75.2553 | 116.7259 | 0 | PROCESSED | 57541.5586226852 | 2016-06-02 13:24:25 | 54888 | 2009-02-26 00:00:00 | 54515.6564699074 | 2008-02-19 15:45:19 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022034 | We propose to observe with Suzaku two Narrow Line Seyfert 1 galaxies detected by SWIFT/BAT and INTEGRAL with a flux in excess of $10^{-11}$~erg~s$^{-1}$~cm$^{-2}$ in the HXD/PIN band for 70~ks each. These proposed observations provide rare high quality spectra of NLS1s above 10~keV. This will remove the spectral degeneracies inherent to limited bandpass analysis (such as that with XMM--Newton and Chandra) and the ambiguities between the different proposed models invoked to explain the unique spectral and variability properties of these most extreme class of high accretion rate sources (namely absorption, reflection, nature of the soft excess...). | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GIOVANNI MINIUTTI | EUR | 2 | AO2 | HUNTING HARD-X-RAY-BRIGHT NLS1 GALAXIES FROM THE INTEGRAL CATALOGUE WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702123010/ | Quick Look | ![]() |
|
142 | HYDRA A FAR SE | 139.7 | -12.375 | 139.09881 | -12.163612 | 146.431142 | -26.609663 | 243.28582967 | 25.05625041 | 300 | 56082.6736342593 | 2012-06-04 16:10:02 | 56083.9368981482 | 2012-06-05 22:29:08 | 807088010 | 40.939 | 40 | 40.947 | 40.939 | 0 | 40.947 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.9143 | 37.9143 | 109.1358 | 0 | PROCESSED | 57605.5894444444 | 2016-08-05 14:08:48 | 56464 | 2013-06-21 00:00:00 | 56096.2405208333 | 2012-06-18 05:46:21 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072020 | Galaxy cluster outskirts are the regions where structure formation occurs through the accretion of smaller structures along large-scale filaments. Thanks to its low background, Suzaku has allowed for the first time to measure the thermodynamical properties of the ICM out to the virial radius. Recently, we used archival ROSAT observations to detect cluster emission out to large radii and quantify the deviations from spherical symmetry. Based on this work, we propose to map the outskirts of Hydra A, which was found to have the highest azimuthal scatter. This will allow us to measure the temperature profiles out to the virial radius and infer the bias on the mean thermodynamical properties and the mass reconstruction when clusters are observed along preferential directions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | DOMINIQUE ECKERT | EUR | 7 | AO7 | MAPPING THE OUTSKIRTS OF HYDRA A WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807088010/ | Quick Look | ![]() |
|
143 | G115.7+17.5 | 336.6801 | 78.3035 | 336.566813 | 78.048018 | 59.497327 | 68.492125 | 115.72297849 | 17.51053762 | 214.3075 | 56311.7506712963 | 2013-01-19 18:00:58 | 56313.7419328704 | 2013-01-21 17:48:23 | 807093010 | 97.8732 | 100 | 97.8892 | 97.8732 | 0 | 97.8892 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 94.3977 | 94.3977 | 172.0079 | 1 | PROCESSED | 57608.5818634259 | 2016-08-08 13:57:53 | 56708 | 2014-02-20 00:00:00 | 56342.5694097222 | 2013-02-19 13:39:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072021 | We propose to observe 4 galaxy clusters from the first all-sky blind Sunyaev Zeldovich (SZ) effect cluster catalogue produced by the Planck satellite. This catalogue has revealed a new population of clusters previously undetected by X-ray surveys. The Planck SZ selected cluster sample consists of hot, massive, morphologically disturbed clusters that are under-luminous in the soft X-ray band. This exciting population has implications not only for understanding the thermodynamic state of the intracluster medium, but also for cluster cosmology where it represents an important area of phase space in the cluster mass function; it is a pointer to the dynamics of how clusters form through mergers, and to the true spatial density of cluster-mass structures not represented in X-ray surveys. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | ANNA SCAIFE | EUR | 7 | AO7 | CONSTRAINING THE THERMODYNAMIC STATE OF NEW PLANCK GALAXY CLUSTERS WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807093010/ | Quick Look | ![]() |
|
144 | PLCK G214.6-37.0 | 137.1752 | 14.6923 | 136.484307 | 14.895327 | 135.215425 | -1.654352 | 214.5759479 | 36.9399481 | 287 | 56413.2455439815 | 2013-05-01 05:53:35 | 56416.322349537 | 2013-05-04 07:44:11 | 808101010 | 119.2637 | 120 | 119.2637 | 119.2637 | 0 | 119.2637 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 106.3127 | 106.3127 | 265.8039 | 5 | PROCESSED | 57611.2793981482 | 2016-08-11 06:42:20 | 56795 | 2014-05-18 00:00:00 | 56429.7933217593 | 2013-05-17 19:02:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082007 | We propose a detailed investigation of the nature of PLCK G214.6-37.0, discovered in the Planck survey. We aim at constraining the presence and properties of filamentary structures connecting and surrounding the clusters. We will unveil the overall dynamics of this complex structure and establish its detailed pressure distribution that can be used for a better estimation of YX to be compared with YSZ. Thus, we will perform a direct search for structures in between identified supercluster components from a careful comparison with the Planck results. Furthermore, the distribution of the PLCK G214.6-37.0 components suggest that it is evolving accreting sub-clusters along the filaments. That makes this supercluster one of the to search for the WHIM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | LORENZO LOVISARI | EUR | 8 | AO8 | TRACKING DOWN THE PLANCK SUPERCLUSTER PLCK G214.6-37.0 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808101010/ | Quick Look | ![]() |
|
145 | UGC03957 EAST | 115.9739 | 55.4967 | 114.966906 | 55.616404 | 107.333122 | 33.607468 | 162.19834712 | 29.35111138 | 294.9944 | 56008.1335648148 | 2012-03-22 03:12:20 | 56009.1717476852 | 2012-03-23 04:07:19 | 806094010 | 46.6221 | 45 | 46.6221 | 46.6221 | 0 | 46.6221 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.2608 | 45.2608 | 89.6879 | 1 | PROCESSED | 57604.9930324074 | 2016-08-04 23:49:58 | 56434 | 2013-05-22 00:00:00 | 56068.628900463 | 2012-05-21 15:05:37 | 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/ver3.0/806094010/ | Quick Look | ![]() |
|
146 | A3528-S OFFSET 2 | 193.9782 | -29.6501 | 193.300361 | -29.379506 | 204.778966 | -21.736125 | 304.09397791 | 33.21155179 | 289.0026 | 56501.5292476852 | 2013-07-28 12:42:07 | 56502.3981481482 | 2013-07-29 09:33:20 | 808105010 | 42.3 | 40 | 42.3 | 42.3078 | 0 | 42.316 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.5258 | 42.5258 | 75.0659 | 2 | PROCESSED | 57612.0639583333 | 2016-08-12 01:32:06 | 56955 | 2014-10-25 00:00:00 | 56587.7982523148 | 2013-10-22 19:09:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082018 | We propose to observe, for a total of 180 ks, the region between the galaxy cluster A3528 and the complex A3530-A3532, in which we expect to find the filament connecting the clusters. With the requested time we aim to detect the Warm Hot Intergalactic Medium (WHIM) by its thermal soft-Xray emission, to resolve one of the major problems of modern astrophysics - the missing baryons , which are now thought to reside in the filaments connecting clusters. In addition to a full understanding of the typical baryon fraction, the proposed observations will allow us to study the gas clumping in the cluster outskirts. Furthermore, a combined analysis of X-ray and optical data will enable us to shed light on the influence of the environments on galaxy evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | LORENZO LOVISARI | EUR | 8 | AO8 | TRACING A FILAMENT IN THE OUTSKIRTS OF THE SHAPLEY SUPERCLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808105010/ | Quick Look | ![]() |
|
147 | M87N FAINT | 187.6988 | 12.9392 | 187.066448 | 13.215269 | 181.818448 | 14.91295 | 283.11850774 | 75.01113844 | 297.6812 | 54625.626400463 | 2008-06-08 15:02:01 | 54627.068275463 | 2008-06-10 01:38:19 | 803069010 | 65.2474 | 60 | 65.2474 | 65.2714 | 0 | 65.2554 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57.9068 | 57.9068 | 124.5638 | 0 | PROCESSED | 57542.7828587963 | 2016-06-03 18:47:19 | 55009 | 2009-06-27 00:00:00 | 54642.2950694444 | 2008-06-25 07:04:54 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032011 | We propose to take advantage of Suzaku's low background and good collecting area to observe a strong surface brightness discontinuity, most likely a cold front, in the outskirts of M87. We will make accurate temperature and pressure profiles across this cold front, determine the energy associated with it, and compare this to the energy of known AGN-ICM interaction features in M87. With Suzaku's superior spectral redistribution function we will for the first time measure Mg and O in the M87 outskirts and improve constraints on relative contributions by SNIa and SNII. We will study abundance and abundance-ratio variations across the cold front and determine the role of gas sloshing in transporting metals produced by the central galaxy into the ICM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | EUR | 3 | AO3 | THE ENERGETICS AND METAL ABUNDANCE PATTERNS IN THE OUTSKIRTS OF M87 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803069010/ | Quick Look | ![]() |
|
148 | ABELL 2877 | 17.5065 | -45.9303 | 16.951425 | -46.196287 | 351.939456 | -47.942764 | 293.04607396 | -70.83949903 | 47.4208 | 56809.9110532407 | 2014-06-01 21:51:55 | 56810.1181712963 | 2014-06-02 02:50:10 | 809100010 | 11.908 | 10 | 11.916 | 11.908 | 0 | 11.9306 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.1778240741 | 2016-08-15 04:16:04 | 57197 | 2015-06-24 00:00:00 | 56828.5915856482 | 2014-06-20 14:11:53 | 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/ver3.0/809100010/ | Quick Look | ![]() |
|
149 | HYDRA A OUT | 139.8502 | -12.6235 | 139.249709 | -12.411636 | 146.680072 | -26.793484 | 243.60142222 | 25.01758475 | 300.0034 | 56085.1461574074 | 2012-06-07 03:30:28 | 56085.6667824074 | 2012-06-07 16:00:10 | 807091010 | 20.3276 | 20 | 20.3516 | 20.3436 | 0 | 20.3276 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.5403 | 16.5403 | 44.9779 | 0 | PROCESSED | 57605.607349537 | 2016-08-05 14:34:35 | 56491 | 2013-07-18 00:00:00 | 56120.2321296296 | 2012-07-12 05:34:16 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072020 | Galaxy cluster outskirts are the regions where structure formation occurs through the accretion of smaller structures along large-scale filaments. Thanks to its low background, Suzaku has allowed for the first time to measure the thermodynamical properties of the ICM out to the virial radius. Recently, we used archival ROSAT observations to detect cluster emission out to large radii and quantify the deviations from spherical symmetry. Based on this work, we propose to map the outskirts of Hydra A, which was found to have the highest azimuthal scatter. This will allow us to measure the temperature profiles out to the virial radius and infer the bias on the mean thermodynamical properties and the mass reconstruction when clusters are observed along preferential directions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | DOMINIQUE ECKERT | EUR | 7 | AO7 | MAPPING THE OUTSKIRTS OF HYDRA A WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807091010/ | Quick Look | ![]() |
|
150 | G171.9-40.7 | 48.2433 | 8.3685 | 47.57264 | 8.181881 | 48.126521 | -9.211403 | 171.97024112 | -40.65556769 | 252.8031 | 56320.012025463 | 2013-01-28 00:17:19 | 56322.7126967593 | 2013-01-30 17:06:17 | 807092010 | 100.9825 | 100 | 100.9905 | 100.9825 | 0 | 100.9848 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93.1617 | 93.1617 | 233.2957 | 0 | PROCESSED | 57608.6871527778 | 2016-08-08 16:29:30 | 56749 | 2014-04-02 00:00:00 | 56365.6023263889 | 2013-03-14 14:27:21 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072021 | We propose to observe 4 galaxy clusters from the first all-sky blind Sunyaev Zeldovich (SZ) effect cluster catalogue produced by the Planck satellite. This catalogue has revealed a new population of clusters previously undetected by X-ray surveys. The Planck SZ selected cluster sample consists of hot, massive, morphologically disturbed clusters that are under-luminous in the soft X-ray band. This exciting population has implications not only for understanding the thermodynamic state of the intracluster medium, but also for cluster cosmology where it represents an important area of phase space in the cluster mass function; it is a pointer to the dynamics of how clusters form through mergers, and to the true spatial density of cluster-mass structures not represented in X-ray surveys. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | ANNA SCAIFE | EUR | 7 | AO7 | CONSTRAINING THE THERMODYNAMIC STATE OF NEW PLANCK GALAXY CLUSTERS WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807092010/ | Quick Look | ![]() |
|
151 | A3528-S OFFSET 4 | 194.1847 | -30.0435 | 193.505704 | -29.773143 | 205.130736 | -22.019409 | 304.29690153 | 32.8141993 | 288.9992 | 56503.6527199074 | 2013-07-30 15:39:55 | 56504.4071064815 | 2013-07-31 09:46:14 | 808107010 | 32.7752 | 30 | 32.7832 | 32.7752 | 0 | 32.7912 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 31.2585 | 31.2585 | 65.1599 | 0 | PROCESSED | 57612.0918634259 | 2016-08-12 02:12:17 | 56955 | 2014-10-25 00:00:00 | 56587.7238310185 | 2013-10-22 17:22:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082018 | We propose to observe, for a total of 180 ks, the region between the galaxy cluster A3528 and the complex A3530-A3532, in which we expect to find the filament connecting the clusters. With the requested time we aim to detect the Warm Hot Intergalactic Medium (WHIM) by its thermal soft-Xray emission, to resolve one of the major problems of modern astrophysics - the missing baryons , which are now thought to reside in the filaments connecting clusters. In addition to a full understanding of the typical baryon fraction, the proposed observations will allow us to study the gas clumping in the cluster outskirts. Furthermore, a combined analysis of X-ray and optical data will enable us to shed light on the influence of the environments on galaxy evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | LORENZO LOVISARI | EUR | 8 | AO8 | TRACING A FILAMENT IN THE OUTSKIRTS OF THE SHAPLEY SUPERCLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808107010/ | Quick Look | ![]() |
|
152 | ABELL 2151A | 241.1446 | 17.7141 | 240.581846 | 17.849628 | 234.487601 | 37.662842 | 31.46236827 | 44.65865226 | 285.8808 | 56883.5616898148 | 2014-08-14 13:28:50 | 56883.843900463 | 2014-08-14 20:15:13 | 809098010 | 11.0268 | 10 | 11.0348 | 11.0348 | 0 | 11.0268 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.4947569444 | 2016-08-16 11:52:27 | 57270 | 2015-09-05 00:00:00 | 56910.6327893518 | 2014-09-10 15:11:13 | 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/ver3.0/809098010/ | Quick Look | ![]() |
|
153 | MARKARIAN 3 | 93.9093 | 71.025 | 92.46011 | 71.040478 | 91.888941 | 47.610328 | 143.30979342 | 22.71730777 | 267.1766 | 57116.4730902778 | 2015-04-04 11:21:15 | 57116.9877199074 | 2015-04-04 23:42:19 | 709022050 | 21.4556 | 20 | 21.4556 | 21.4556 | 0 | 21.4556 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.9089814815 | 2016-08-17 21:48:56 | 57550 | 2016-06-11 00:00:00 | 57183.6622916667 | 2015-06-10 15:53:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092008 | We propose to measure size and distance from the black hole of the optically-thick absorbing and reprocessing system(s) in the heavily obscured Seyfert Galaxy Markarian~3 by means of its known X-ray spectral variability. We aim at simultaneously measuring: the variability timescale of the primary emission, seen in transmission through a photoelectric column density of (0.7--1.1)x10^{24} atoms/cm/cm; the variability timescale of its Compton-reflection, dominating the continuum flux in the 3-10 keV energy band; and the variability timescale of the nuclear obscuration. Only the scientific payload on-board Suzaku possesses the required combination of broadband X-ray coverage, sensitivity, and spectroscopic capabilities to perform this experiment. We request 5 observations of 20 ks each. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MATTEO GUAINAZZI | EUR | 9 | AO9 | MEASURING THE TORUS SPATIAL SCALE(S) IN SEYFERT GALAXIES: A SUZAKU MONITORING OF MARKARIAN 3 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709022050/ | Quick Look | ![]() |
|
154 | ALGOL | 47.0831 | 40.8965 | 46.267674 | 40.705521 | 56.181748 | 22.363141 | 149.0355551 | -14.93487401 | 244.4771 | 54167.6197222222 | 2007-03-08 14:52:24 | 54169.6132986111 | 2007-03-10 14:43:09 | 401093010 | 102.1642 | 105 | 102.1642 | 102.1642 | 0 | 102.1642 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102.4729 | 102.4729 | 172.1928 | 1 | PROCESSED | 57537.6825810185 | 2016-05-29 16:22:55 | 54736 | 2008-09-27 00:00:00 | 54186.3983564815 | 2007-03-27 09:33:38 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012024 | Stellar and solar coronae reveal high-energy phenomena including the presence of accelerated electrons, explosive dissipation of magnetic energy, and heating to extreme temperatures. Many of these processes are likely to be physically related. We propose to use Suzaku's suite of instruments to observe the interplay between thermal and non-thermal high-energy processes in the active, eclipsing binary Algol. Our prime objective is the observation of hard X-rays above 10 keV, but also the appearance of an Fe fluorescence line that could be induced either by irradiation from flaring plasma or by electron beams. These models can be distinguished by correlating the emission with nonthermal hard X-rays as possibly detected by the HXD. | GALACTIC POINT SOURCES | 4 | C | MANUEL GUEDEL | EUR | 1 | AO1 | A SYNOPTIC VIEW OF HIGH-ENERGY PHENOMENA IN THE CORONA OF ALGOL | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401093010/ | Quick Look | ![]() |
|
155 | HER X-1 | 254.4925 | 35.2707 | 254.041525 | 35.346159 | 246.065216 | 57.427888 | 58.06565994 | 37.48335671 | 250.2455 | 55468.7003356482 | 2010-09-29 16:48:29 | 55469.2258912037 | 2010-09-30 05:25:17 | 405058020 | 24.303 | 20 | 24.303 | 24.3223 | 0 | 24.4677 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 22.4837 | 22.4837 | 45.4059 | 0 | PROCESSED | 57553.5917476852 | 2016-06-14 14:12:07 | 55848 | 2011-10-14 00:00:00 | 55482.4726967593 | 2010-10-13 11:20:41 | 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/ver3.0/405058020/ | Quick Look | ![]() |
|
156 | SGR 1806-20 | 272.166 | -20.4729 | 271.421316 | -20.481616 | 272.022208 | 2.952663 | 9.94279657 | -0.27364584 | 269.9473 | 53987.9261921296 | 2006-09-09 22:13:43 | 53989.1668287037 | 2006-09-11 04:00:14 | 401092010 | 48.9155 | 50 | 48.9155 | 48.9235 | 48.9315 | 48.9315 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 55.4085 | 55.4085 | 107.1759 | 1 | PROCESSED | 57535.5272453704 | 2016-05-27 12:39:14 | 54526 | 2008-03-01 00:00:00 | 54021.1112615741 | 2006-10-13 02:40:13 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012017 | The soft gamma-ray repeater SGR 1806-20 has recently emitted the most powerful giant flare ever observed from these sources. This probably involved a large scale restructuring of the magnetosphere, leading to observable variations in the properties of its persistent emission, from IR to hard X-rays. We propose to observe SGR 1806-20 with Suzaku considering the unique opportunity offered by this satellite to study the spectrum of this source simultaneously both in the soft and hard X-ray bands. We also suggest to coordinate this observation with a simultaneous XMM-Newton one, in order to obtain a significantly better determination of the broad band spectral parameters. | GALACTIC POINT SOURCES | 4 | B | SANDRO MEREGHETTI | EUR | 1 | AO1 | COORDINATED SUZAKU AND XMM-NEWTON OBSERVATIONS OF SGR 1806-20 AFTER THE GIANT FLARE | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401092010/ | Quick Look | ![]() |
|
157 | IGR J08408-4503 | 130.2449 | -45.0216 | 129.817019 | -44.842502 | 154.934869 | -59.72126 | 264.03123634 | -1.90203871 | 133.4432 | 55176.7452199074 | 2009-12-11 17:53:07 | 55179.5002199074 | 2009-12-14 12:00:19 | 404070010 | 92.566 | 100 | 92.646 | 92.566 | 0 | 92.63 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69.4344 | 69.4344 | 237.9898 | 2 | PROCESSED | 57549.8697222222 | 2016-06-10 20:52:24 | 55567 | 2011-01-06 00:00:00 | 55200.3941550926 | 2010-01-04 09:27:35 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042007 | We propose a 100 ks Suzaku observation of a Supergiant Fast X-ray Transient (SFXT) displaying periodic outbursts, IGRJ08408-4503, with the main aim of searching for cyclotron lines in its spectrum.This would be the first direct measurement of the neutron star magnetic field in this recently discovered class of HMXBs, and would be crucial in discriminating between different models for the outburst mechanisms, involving highly magnetized neutron stars (1E14 G) versus more typical magnetic fields of 1E12 G.The source is a SFXT displaying recurrent outbursts on short timescales (flaring every about 11 and 24 days).Because in most SFXTs the outbursts are not predictable, fast and difficult to observe,the SFXT we are proposing is a key system to understand the physical properties of this class. | GALACTIC POINT SOURCES | 4 | C | LARA SIDOLI | EUR | 4 | AO4 | SEARCH FOR CYCLOTRON LINES IN THE X-RAY SPECTRUM OF THE SUPERGIANT FAST X-RAY TRANSIENT IGRJ08408-4503 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404070010/ | Quick Look | ![]() |
|
158 | SN 1987A | 83.9013 | -69.2655 | 83.9928 | -69.294887 | 307.391677 | -86.458548 | 279.69660922 | -31.92548266 | 330.0004 | 53894.6930555556 | 2006-06-08 16:38:00 | 53895.6683449074 | 2006-06-09 16:02:25 | 801090010 | 39.6464 | 40 | 39.6464 | 39.6464 | 39.6464 | 39.6464 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39.2519 | 39.2519 | 84.2399 | 0 | PROCESSED | 57534.6267592593 | 2016-05-26 15:02:32 | 54400 | 2007-10-27 00:00:00 | 53928.1346527778 | 2006-07-12 03:13:54 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012006 | In an early Suzaku observation during the SWG time in November 2005 we have already obtained an excellent XIS spectrum. The flux of SN 1987A continues to rise exponentially with an e-folding time of ~800 days. The abundances in the ejecta could be measured with unprecedented accuracy. We confirm that Oxygen and Iron are significantly underabundant with respect to other elements, indicating the formation of dust, maybe even black rust grains (Fe3O4). We propose to monitor the chemical evolution of SN 1987A with Suzaku for 40 ksec in AO-1, where we expect about twice the previous flux. The exponential brightening and the chemical abundance is expected to change, when the full inner ring is engulfed. Simultaneously we can search for a periodic hard signal from the putative pulsar. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | G NTHER HASINGER | EUR | 1 | AO1 | SN 1987A - A RUSTY REMNANT? | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801090010/ | Quick Look | ![]() |
|
159 | VELAFRAGG TAIL | 125.0448 | -47.7009 | 124.65466 | -47.541789 | 151.337516 | -63.864294 | 264.09848727 | -6.37839252 | 263.1844 | 55658.0366898148 | 2011-04-07 00:52:50 | 55658.8565162037 | 2011-04-07 20:33:23 | 506057010 | 49.3543 | 50 | 49.3703 | 49.3543 | 0 | 49.3703 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 43.9581 | 43.9581 | 70.8259 | 1 | PROCESSED | 57601.4287268518 | 2016-08-01 10:17:22 | 56043 | 2012-04-26 00:00:00 | 55673.1976736111 | 2011-04-22 04:44:39 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062021 | The Vela supernova remnant (SNR) displays remarkable features which appear to be ejecta ``shrapnel'' visible beyond the main shell. One of these shrapnel (A) is distinct from the others in that its X-ray spectrum exhibits a high Si abundance, while the other shrapnel exhibit enhanced O, Ne, and Mg abundances. One unexplored ejecta shrapnel (G) is located on the opposite side of the remnant from shrapnel A, suggesting that the SN explosion may have resulted in a jet-counterjet Si-rich structure, reminiscent of Cas A. We propose to observe this shrapnel for the first time to determine if it is also Si-rich like shrapnel A. If this is the case, the Vela SNR may be the first direct evidence of a jet-induced SN explosion. | GALACTIC DIFFUSE EMISSION | 5 | A | FABRIZIO BOCCHINO | EUR | 6 | AO6 | ASYMMETRIC SN EXPLOSION IN VELA SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506057010/ | Quick Look | ![]() |
|
160 | 3C400.2 NW | 294.5044 | 17.3912 | 293.942879 | 17.276968 | 300.273195 | 38.29194 | 53.66788209 | -2.01364052 | 81.5888 | 56770.4644907407 | 2014-04-23 11:08:52 | 56770.9410763889 | 2014-04-23 22:35:09 | 509068010 | 21.47 | 20 | 21.4853 | 21.486 | 0 | 21.47 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.9678 | 20.9678 | 41.1719 | 0 | PROCESSED | 57614.9785416667 | 2016-08-14 23:29:06 | 57152 | 2015-05-10 00:00:00 | 56789.6036805556 | 2014-05-12 14:29:18 | 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/ver3.0/509068010/ | Quick Look | ![]() |
|
161 | 1ES 1959+650 | 299.9645 | 65.1588 | 299.84329 | 65.020024 | 7.34886 | 77.791428 | 98.00607393 | 17.68746705 | 45.1602 | 53878.0509606482 | 2006-05-23 01:13:23 | 53880.1718055556 | 2006-05-25 04:07:24 | 701075010 | 98.8622 | 100 | 98.8782 | 98.8622 | 98.8702 | 98.8782 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 96.106 | 96.106 | 183.2028 | 2 | PROCESSED | 57534.4674305556 | 2016-05-26 11:13:06 | 54408 | 2007-11-04 00:00:00 | 53928.2478472222 | 2006-07-12 05:56:54 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012002 | We request to observe 1ES1959+650 and 1ES2344+514 for 100 ks each with SUZAKU simultaneously with the Whipple Cherenkov telescope. Whipple will extensively monitor these sources for months in 2006-2007. There are three well defined scientific cases that we would like to address. We want to study 1) the correlation between the soft and hard X-ray and TeV fluxes and spectra, extremely variable in these sources, sometimes showing extreme conditions; 2) the mystery of the ''orphan'' flares; i.e. events observed only in the TeV gamma rays without a counterpart in the X-rays: this is currently not understood in the framework of SSC models; 3) the origin of the lag observed between soft and hard X-ray variability in some blazars and the implications for the TeV emission. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GIANPIERO TAGLIAFERRI | EUR | 1 | AO1 | JETS ON TEST: SIMULTANEOUS X-RAY AND TEV OBSERVATIONS OF 1ES1959+650 AND 1ES2344+514 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701075010/ | Quick Look | ![]() |
|
162 | LMC X-3 | 84.7483 | -64.0713 | 84.678356 | -64.09698 | 46.246737 | -86.69028 | 273.56080053 | -32.07680965 | 285.8008 | 56379.6769444445 | 2013-03-28 16:14:48 | 56382.4793634259 | 2013-03-31 11:30:17 | 407086010 | 101.809 | 100 | 101.817 | 101.825 | 0 | 101.809 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92.7246 | 92.7246 | 242.1019 | 1 | PROCESSED | 57611.0169560185 | 2016-08-11 00:24:25 | 56757 | 2014-04-10 00:00:00 | 56391.8067592593 | 2013-04-09 19:21:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072002 | We propose a 100 ksec triggered Suzaku observation of the low/hard state of the black hole LMC X-3. This will constrain the disc emission and Fe line profile in this state, both of which are currently very controversial. LMC X-3 has very low interstellar absorption, so gives the best view of the low temperature/low luminosity disc component in this state. Its moderate flux means it can be observed in standard imaging modes without pileup (further enhancing visibility of the disc as these modes are well calibrated down to 0.4 keV) and making the Fe line profile analysis straightforward. Historically LMC X-3 enters a low/hard state on average once a year. Suzaku will be triggered based on an alert from our Swift monitoring program that the source has entered the low/hard state. | GALACTIC POINT SOURCES | 4 | A | MARI KOLEHMAINEN | EUR | 7 | AO7-TOO | A TOO OF LMC X-3: IS THE DISC TRUNCATED IN THE LOW/HARD STATE OF BLACK HOLE BINARIES? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407086010/ | Quick Look | ![]() |
|
163 | A76 EAST | 10.1332 | 6.8374 | 9.486956 | 6.563068 | 11.989309 | 2.27755 | 118.09579875 | -55.93191571 | 260.0024 | 55183.3444212963 | 2009-12-18 08:15:58 | 55183.8752199074 | 2009-12-18 21:00:19 | 804087010 | 23.621 | 15 | 23.637 | 23.621 | 0 | 23.629 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.6401 | 18.6401 | 45.8559 | 0 | PROCESSED | 57549.8965393518 | 2016-06-10 21:31:01 | 55575 | 2011-01-14 00:00:00 | 55209.4624652778 | 2010-01-13 11:05:57 | 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/ver3.0/804087010/ | Quick Look | ![]() |
|
164 | A3526 | 192.0509 | -41.0558 | 191.361267 | -40.783129 | 208.811762 | -32.67802 | 302.27518183 | 21.81182444 | 109.9986 | 55942.2296990741 | 2012-01-16 05:30:46 | 55942.6807291667 | 2012-01-16 16:20:15 | 806084010 | 16.9645 | 10 | 16.9645 | 16.9645 | 0 | 16.9645 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.6605 | 12.6605 | 38.9639 | 0 | PROCESSED | 57604.361875 | 2016-08-04 08:41:06 | 56331 | 2013-02-08 00:00:00 | 55960.1781712963 | 2012-02-03 04:16:34 | 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/ver3.0/806084010/ | Quick Look | ![]() |
|
165 | HYDRA A FAR N | 139.5397 | -11.7599 | 138.936601 | -11.549023 | 146.034406 | -26.083857 | 242.64361193 | 25.31151573 | 300.0007 | 56083.9377430556 | 2012-06-05 22:30:21 | 56085.1452662037 | 2012-06-07 03:29:11 | 807089010 | 41.276 | 40 | 41.284 | 41.284 | 0 | 41.276 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38.1727 | 38.1727 | 104.3117 | 1 | PROCESSED | 57605.6201851852 | 2016-08-05 14:53:04 | 56465 | 2013-06-22 00:00:00 | 56098.4661689815 | 2012-06-20 11:11:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072020 | Galaxy cluster outskirts are the regions where structure formation occurs through the accretion of smaller structures along large-scale filaments. Thanks to its low background, Suzaku has allowed for the first time to measure the thermodynamical properties of the ICM out to the virial radius. Recently, we used archival ROSAT observations to detect cluster emission out to large radii and quantify the deviations from spherical symmetry. Based on this work, we propose to map the outskirts of Hydra A, which was found to have the highest azimuthal scatter. This will allow us to measure the temperature profiles out to the virial radius and infer the bias on the mean thermodynamical properties and the mass reconstruction when clusters are observed along preferential directions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | DOMINIQUE ECKERT | EUR | 7 | AO7 | MAPPING THE OUTSKIRTS OF HYDRA A WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807089010/ | Quick Look | ![]() |
|
166 | MKW8 | 220.1793 | 3.4582 | 219.549704 | 3.671881 | 216.616533 | 18.149831 | 355.49716412 | 54.76401984 | 291.2239 | 56859.4682986111 | 2014-07-21 11:14:21 | 56859.7009259259 | 2014-07-21 16:49:20 | 809101010 | 10.412 | 10 | 10.412 | 10.488 | 0 | 10.4956 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.4174305556 | 2016-08-15 10:01:06 | 57239 | 2015-08-05 00:00:00 | 56873.5532523148 | 2014-08-04 13:16:41 | 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/ver3.0/809101010/ | Quick Look | ![]() |
|
167 | 3C400.2 NE | 294.7841 | 17.3445 | 294.222174 | 17.229031 | 300.592872 | 38.189932 | 53.75798011 | -2.26924911 | 81.5891 | 56770.0289351852 | 2014-04-23 00:41:40 | 56770.4640162037 | 2014-04-23 11:08:11 | 509071010 | 20.231 | 20 | 20.239 | 20.239 | 0 | 20.231 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.505 | 18.505 | 37.5838 | 0 | PROCESSED | 57614.9798148148 | 2016-08-14 23:30:56 | 57152 | 2015-05-10 00:00:00 | 56789.6056712963 | 2014-05-12 14:32:10 | 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/ver3.0/509071010/ | Quick Look | ![]() |
|
168 | MCG-02-14-009 | 79.0657 | -10.5106 | 78.475918 | -10.56483 | 77.084553 | -33.463679 | 211.75204832 | -25.86275025 | 68.0451 | 54706.9410069444 | 2008-08-28 22:35:03 | 54710.0308333333 | 2008-09-01 00:44:24 | 703060010 | 142.1522 | 125 | 142.1522 | 142.1522 | 0 | 142.1522 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 129.5879 | 129.5879 | 266.9199 | 1 | PROCESSED | 57543.5182986111 | 2016-06-04 12:26:21 | 55100 | 2009-09-26 00:00:00 | 54731.4652430556 | 2008-09-22 11:09:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032009 | MCG--02-14-009 appears to have the strongest relativistic iron line of all the Seyfert 1s: a short 5 ks XMM-Newton observation found the line to have an EW 530-770 eV, two times larger than for MCG-6-30-15. We propose a 125 ks Suzaku observation of this AGN, which provides a unique opportunity to probe the innermost accretion disk in the region of strong gravity. The main goals are: (a) utilise the unique broad bandpass of Suzaku to detect the expected strong reflection hump and determine the form of the X-ray continuum; (b) accurately measure the relativistic iron K line profile and thereby the geometry of the X-ray emitting region and (c) determine whether the iron line responds to the continuum down to the orbital timescales of the inner disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JAMES REEVES | EUR | 3 | AO3 | MCG-02-14-009: PROBING THE PHYSICAL PROPERTIES OF THE STRONGEST IRON K LINE | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703060010/ | Quick Look | ![]() |
|
169 | IC4329A | 207.3321 | -30.3098 | 206.617944 | -30.061645 | 216.345264 | -17.777119 | 317.49793706 | 30.91926559 | 298.5047 | 54332.9765740741 | 2007-08-20 23:26:16 | 54333.5558333333 | 2007-08-21 13:20:24 | 702113050 | 24.0262 | 25 | 24.0262 | 24.0262 | 0 | 24.0262 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.8256 | 18.8256 | 50.0439 | 1 | PROCESSED | 57539.6252083333 | 2016-05-31 15:00:18 | 54730 | 2008-09-21 00:00:00 | 54350.649375 | 2007-09-07 15:35:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022009 | IC 4329A is the brightest known Seyfert 1 galaxy between ~2-30 keV (F(2-10 keV)~1-2e-10 erg/cm2s). With its clear warm absorber and reflection component, it is often taken as the prototypical Sey 1 galaxy. Its X-ray variability is strong enough (and on a sufficiently long time scale, ideal for Suzaku) to make multiple observations critical for probing the origin of the Compton reflection component, and to attempt measuring variations of the high energy cut-off. We thus propose 5x20 ks observations to monitor i) the correlated variability of the reflection continuum plus FeK line to primary continuum variations, and ii) the variations in the high-E cut-off, and their relation with the power-law, and iii) check the evidence for a blueshifted (v~0.1c) FeK absorption line at ~7.7 keV. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MASSIMO CAPPI | EUR | 2 | AO2 | SUZAKU MULTIPLE OBSERVATIONS OF IC4329A TO PROBE THE ORIGIN OF THE COMPTON REFLECTION COMPONENT AND HIGH-ENERGY CUT-OFF | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702113050/ | Quick Look | ![]() |
|
170 | NGC 1448 | 56.1426 | -44.6942 | 55.730836 | -44.850191 | 33.469346 | -61.660504 | 251.59735556 | -51.37690943 | 264.6522 | 54879.3481828704 | 2009-02-17 08:21:23 | 54880.4501041667 | 2009-02-18 10:48:09 | 703062010 | 52.9653 | 50 | 52.9653 | 52.9653 | 0 | 52.9653 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 55.0869 | 55.0869 | 95.202 | 1 | PROCESSED | 57545.5960763889 | 2016-06-06 14:18:21 | 55330 | 2010-05-14 00:00:00 | 54893.4451041667 | 2009-03-03 10:40:57 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032018 | We propose for a 50 ks Suzaku observation of NGC 1448, a nearby (15 Mpc) gas-rich and dust-obscured Scd galaxy that is optically classified as an HII galaxy. From our Spitzer-IRS mid-IR spectroscopy, we have found the first evidence for an obscured AGN in NGC 1448. On the basis of this data, NGC 1448 appears to be harboring a rapidly growing small obscured black hole (M_BH ~ 6x10^5 M_Sun; Eddington ratio of >0.1), and therefore appears to be an analog of the nearby Compton-thick AGN NGC 4945. To date, no sensitive hard X-ray constraints exist for NGC 1448, which are required to provide a direct measurement of the absorption and mass accretion rate, and thus to test if NGC 1448 is also a Compton-thick AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | DAVID ALEXANDER | EUR | 3 | AO3 | NGC 1448: A MISSING COMPTON-THICK AGN IN OUR BACKYARD? | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703062010/ | Quick Look | ![]() |
|
171 | B3 0309+411 | 48.2809 | 41.3324 | 47.459303 | 41.145685 | 57.252935 | 22.518841 | 149.59257755 | -14.09014879 | 253.0016 | 55976.5100462963 | 2012-02-19 12:14:28 | 55979.0410532407 | 2012-02-22 00:59:07 | 706036010 | 104.6245 | 100 | 104.6245 | 104.6296 | 0 | 104.6245 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95.453 | 95.453 | 218.6719 | 2 | PROCESSED | 57604.7018981482 | 2016-08-04 16:50:44 | 56360 | 2013-03-09 00:00:00 | 55992.2317824074 | 2012-03-06 05:33:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062007 | We propose to observe B3 0309+411, an X--ray bright FRII BLRG detected by INTEGRAL for 100 ks. BRLGs have been poorly studied in X-rays and usually show weak reprocessing spectral features with respect to their radio-quiet counterparts. B3 0309+411 has been already followed-up with XMM-Newton and, the XMM-Newton and INTEGRAL data suggests that the source could 1) be strongly reflection-dominated; 2) exhibit extreme flux/spectral variability; 3) be severely affected by absorption. The Suzaku observation will unveil the puzzling spectral shape of this peculiar BLRG, allowing to determine with accuracy the reflection properties which would have a large impact on our understanding of the disk/jet contribution in BLRG. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | FRANCESCA PANESSA | EUR | 6 | AO6 | B3 0309+411: A REFLECTION--DOMINATED BROAD LINE RADIO GALAXY? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706036010/ | Quick Look | ![]() |
|
172 | FAIRALL 51 | 281.2238 | -62.3567 | 280.059933 | -62.408117 | 276.678489 | -39.176005 | 333.20743511 | -23.0882296 | 252.0031 | 56539.073587963 | 2013-09-04 01:45:58 | 56539.5245486111 | 2013-09-04 12:35:21 | 708046010 | 31.5576 | 30 | 31.5576 | 31.5676 | 0 | 31.5656 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.6549 | 25.6549 | 38.9559 | 0 | PROCESSED | 57612.4964236111 | 2016-08-12 11:54:51 | 56956 | 2014-10-26 00:00:00 | 56587.5110763889 | 2013-10-22 12:15:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082016 | Fairall 51 is a variable bright active galaxy (about 1 millicrab), classified as a polar-scattered Seyfert~1 galaxy. It was observed twice with high-quality X-ray spectrometers on-board the XMM-Newton satellite. The two observations are separated by half a year and the spectra significantly differ from each other. The difference can be well explained by a variable covering fraction of a cold (very low-ionised) absorber (Ricci et al., 2010). Two additional Swift data, separated by five days, suggest that the variability may occur at time-scales as short as a few days. The ultimate goal of the proposal is to locate this variable absorber by the determination of the typical time-scale of the variability. We therefore propose a series of observations of Fairall 51 with short exposures. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JIRI SVOBODA | EUR | 8 | AO8 | STUDY OF THE VARIABLE ABSORBER IN A BRIGHT ACTIVE GALAXY FAIRALL 51 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708046010/ | Quick Look | ![]() |
|
173 | M81 | 148.8829 | 69.0533 | 147.858629 | 69.290285 | 119.502258 | 51.56628 | 142.10623941 | 40.90540672 | 287.1391 | 57160.4721180556 | 2015-05-18 11:19:51 | 57162.9807523148 | 2015-05-20 23:32:17 | 710017010 | 97.7022 | 100 | 97.7022 | 99.738 | 0 | 99.7444 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0.3 | 0 | PROCESSED | 57618.7210532407 | 2016-08-18 17:18:19 | 57543 | 2016-06-04 00:00:00 | 57177.3710300926 | 2015-06-04 08:54:17 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 102700 | We propose to observe the Low-Luminosity Active Galactic Nucleus of M81 for 200 ksec with NuSTAR and for 100 ksec with Suzaku. In low accretion rate AGN, where does the optically thick part of the accretion disk stop? Does it go in to within a few gravitational radii of the black hole, as in higher accretion rate Seyfert galaxies, or does it stop hundreds of gravitational radii from the black hole? Using NuSTAR and Suzaku spectra we will measure the strengths of the Compton reflection hump, Fe K alpha, Fe XXV and Fe XXVI lines. This will determine whether the Fe K alpha line is produced by reflection off the optically thick outer disk, or is produced in the optically thin inner flow. We will measure the reflection fraction and constrain the source geometry and disk transition radius. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ANDREW YOUNG | EUR | 10 | AO10 | M81: ACCRETION GEOMETRY AT LOW EDDINGTON RATES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710017010/ | Quick Look | ![]() |
|
174 | J2218.2-0350 | 334.573 | -3.8385 | 333.923892 | -4.08927 | 335.019924 | 6.258076 | 58.63251599 | -46.67973864 | 268.0005 | 56260.6621527778 | 2012-11-29 15:53:30 | 56261.0523148148 | 2012-11-30 01:15:20 | 807084010 | 15.7671 | 15 | 15.7751 | 15.7671 | 0 | 15.7831 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.9145 | 11.9145 | 33.7079 | 0 | PROCESSED | 57608.1412384259 | 2016-08-08 03:23:23 | 56644 | 2013-12-18 00:00:00 | 56275.6610300926 | 2012-12-14 15:51:53 | 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/ver3.0/807084010/ | Quick Look | ![]() |
|
175 | G276.2-7.7 | 135.4479 | -58.0976 | 135.120843 | -57.899721 | 179.6274 | -67.871169 | 276.2324482 | -7.68832918 | 319.4197 | 56102.2534722222 | 2012-06-24 06:05:00 | 56102.610625 | 2012-06-24 14:39:18 | 507066010 | 10.2994 | 10 | 10.2994 | 10.2994 | 0 | 10.2994 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.6275 | 11.6275 | 30.8559 | 0 | PROCESSED | 57605.7340972222 | 2016-08-05 17:37:06 | 56582 | 2013-10-17 00:00:00 | 56219.6536458333 | 2012-10-19 15:41:15 | 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/ver3.0/507066010/ | Quick Look | ![]() |
|
176 | ESO 263-G013 | 152.4256 | -42.8603 | 151.905124 | -42.614062 | 176.412344 | -49.376708 | 273.99206854 | 10.74227458 | 292.0779 | 54252.4568287037 | 2007-06-01 10:57:50 | 54253.5946064815 | 2007-06-02 14:16:14 | 702120010 | 45.2947 | 40 | 45.3027 | 45.3027 | 0 | 45.2947 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.1035 | 40.1035 | 98.2999 | 2 | PROCESSED | 57538.8009143518 | 2016-05-30 19:13:19 | 54745 | 2008-10-06 00:00:00 | 54258.5006134259 | 2007-06-07 12:00:53 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022033 | The high-energy detectors onboard Swift and INTEGRAL are mapping the hard (>10 keV) X-ray sky. Although limited to bright X-ray fluxes (~1e-11 erg/cm2/s), the large area surveyed so far has allowed to build up sizable samples of hard X-ray selected AGN almost unbiased against X-ray absorption. On the basis of a careful analysis of the available X-ray observations below 10 keV, we identified a sample of relatively bright AGN which are likely to be obscured by Compton-thick (logN_H >24) cold gas. Two of them were observed in EAO-1 and the results confirmed our predictions. We propose further Suzaku observations of 3 bright objects (F(20-40 keV) ~ 0.7-1.4 x 1e-11 erg/cm2/s) which will allow us to unveil previously unknown nearby heavily obscured AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | ANDREA COMASTRI | EUR | 2 | AO2 | BRIGHT COMPTON-THICK GALAXIES IN THE BACKYARD - PART II | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702120010/ | Quick Look | ![]() |
|
177 | XB 1916-053 | 289.7027 | -5.2415 | 289.037629 | -5.333849 | 290.520863 | 16.806325 | 31.35614078 | -8.46800846 | 250.2538 | 54047.242974537 | 2006-11-08 05:49:53 | 54048.1119791667 | 2006-11-09 02:41:15 | 401095010 | 38.4647 | 40 | 39.0967 | 39.0887 | 38.4647 | 39.0967 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 37.4857 | 37.4857 | 75.082 | 2 | PROCESSED | 57536.0684259259 | 2016-05-28 01:38:32 | 54735 | 2008-09-26 00:00:00 | 54088.866087963 | 2006-12-19 20:47:10 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012038 | We propose Suzaku observations of the dipping low mass X-ray binaries XB1916-053, XB1323-619, EXO0748-676 and X 1624-490. The changes in both the continuum and the He- and H- like Fe K absorption features during dips have been recently 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 photoionised absorbers and reliably determine the values of the ionization parameter for each source, and the simultaneous spectra of HXD to uniquely determine the underlying continuum shapes including any contributions due to reflection components and to extend the photoionized absorber fits to higher energies. This will test the validity of the ionized absorber model also >10 keV. | GALACTIC POINT SOURCES | 4 | A | MARIA DIAZ TRIGO | EUR | 1 | AO1 | BROAD-BAND OBSERVATIONS OF HIGHLY-IONIZED ABSORBERS IN DIPPING LMXBS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401095010/ | Quick Look | ![]() |
|
178 | 4U 1820-30 | 275.9205 | -30.4212 | 275.116914 | -30.447977 | 275.132756 | -7.085901 | 2.7347979 | -7.94197311 | 270.4164 | 55124.2356134259 | 2009-10-20 05:39:17 | 55124.7925810185 | 2009-10-20 19:01:19 | 404069070 | 24.0566 | 100 | 24.0567 | 24.0726 | 0 | 24.0566 | 3 | 1 | 0 | 2 | 1 | 0 | 0 | 18.9035 | 18.9035 | 48.1079 | 0 | PROCESSED | 57548.9193981482 | 2016-06-09 22:03:56 | 55503 | 2010-11-03 00:00:00 | 55134.2427314815 | 2009-10-30 05:49:32 | 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/ver3.0/404069070/ | Quick Look | ![]() |
|
179 | HER X-1 | 254.4936 | 35.2712 | 254.042629 | 35.346654 | 246.066668 | 57.428555 | 58.06646448 | 37.48255114 | 250.0637 | 55467.7830208333 | 2010-09-28 18:47:33 | 55468.2362962963 | 2010-09-29 05:40:16 | 405058010 | 21.3567 | 20 | 21.3567 | 21.3567 | 0 | 21.5034 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 18.9323 | 18.9323 | 39.1599 | 0 | PROCESSED | 57553.5804050926 | 2016-06-14 13:55:47 | 55843 | 2011-10-09 00:00:00 | 55477.2237152778 | 2010-10-08 05:22:09 | 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/ver3.0/405058010/ | Quick Look | ![]() |
|
180 | V2129 OPH | 246.9149 | -24.3651 | 246.158782 | -24.254235 | 249.041959 | -2.587504 | 353.29078542 | 16.72506486 | 88.3342 | 54866.0202430556 | 2009-02-04 00:29:09 | 54866.5821296296 | 2009-02-04 13:58:16 | 403074010 | 21.0335 | 20 | 21.0335 | 21.0335 | 0 | 21.0335 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.5331 | 16.5331 | 48.5339 | 0 | PROCESSED | 57545.4470833333 | 2016-06-06 10:43:48 | 55329 | 2010-05-13 00:00:00 | 54880.5317708333 | 2009-02-18 12:45:45 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032022 | We propose to observe the classical T Tauri stars CS Cha, MN Lup, V2129 Oph and XZ Tau with the Suzaku XIS to investigate accretion induced X-ray emission in CTTS as evidenced by the presence of excess emission in the soft X-ray regime. Specifically we intend to utilize Suzaku's sensitivity, low background and the capability of the XIS to resolve the OVIII Ly-alpha line from the OVII triplet. XMM-Newton and Chandra grating spectra provide strong evidence for the presence of accretion induced X-ray emission in CTTS, however, due to low SNR and the presence of absorption an accretion scenario often cannot be probed within reasonable exposure times. With the proposed observations we want to investigate a sample of these CTTS showing additional exceptional properties. | GALACTIC POINT SOURCES | 4 | B | JAN ROBRADE | EUR | 3 | AO3 | ACCRETION RELATED SOFT X-RAY EMISSION IN CLASSICAL T TAURI STARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403074010/ | Quick Look | ![]() |
|
181 | HYDRA A SE | 139.5641 | -12.2366 | 138.96256 | -12.025643 | 146.239045 | -26.524458 | 243.07517911 | 25.03717361 | 300.0006 | 56085.6674421296 | 2012-06-07 16:01:07 | 56086.2926388889 | 2012-06-08 07:01:24 | 807087010 | 21.4898 | 20 | 21.4898 | 21.4898 | 0 | 21.4898 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.3651 | 20.3651 | 54.012 | 0 | PROCESSED | 57605.6279976852 | 2016-08-05 15:04:19 | 56465 | 2013-06-22 00:00:00 | 56099.0036921296 | 2012-06-21 00:05:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072020 | Galaxy cluster outskirts are the regions where structure formation occurs through the accretion of smaller structures along large-scale filaments. Thanks to its low background, Suzaku has allowed for the first time to measure the thermodynamical properties of the ICM out to the virial radius. Recently, we used archival ROSAT observations to detect cluster emission out to large radii and quantify the deviations from spherical symmetry. Based on this work, we propose to map the outskirts of Hydra A, which was found to have the highest azimuthal scatter. This will allow us to measure the temperature profiles out to the virial radius and infer the bias on the mean thermodynamical properties and the mass reconstruction when clusters are observed along preferential directions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | DOMINIQUE ECKERT | EUR | 7 | AO7 | MAPPING THE OUTSKIRTS OF HYDRA A WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807087010/ | Quick Look | ![]() |
Used SQL
SELECT * FROM suzaku_master_data WHERE SUBSTRING(proposal_id,3,1) = '2'
Your request has been accepted.
The download will start soon automatically.