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 998
No. |
object_name
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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
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xis2_observation_mode
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xis3_observation_mode
|
hxd_observation_mode
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hxd_coarse_clock_rate_exposure
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hxd_first_clock_rate_exposure
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hxd_normal_clock_rate_exposure
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hxd_all_clock_rate_exposure
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hxd_wam_exposure
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quantity_of_hxd_burst
|
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
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proposal_abstract
|
proposal_category
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proposal_category_code
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proposal_priority
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pi_name
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co_pi_name
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proposal_affiliated_country
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proposal_cycle
|
observation_type
|
proposal_title
|
main_instrument
|
has_xis_injection
|
data_access_url
|
ql_access_url
|
ql_image_url
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1 | E0102-72 | 15.9926 | -72.0236 | 15.587314 | -72.291594 | 314.630688 | -65.030221 | 301.56327722 | -45.07133229 | 226.8326 | 53720.0716203704 | 2005-12-16 01:43:08 | 53723.4377199074 | 2005-12-19 10:30:19 | 100044010 | 59.731 | 20 | 59.735 | 125.9195 | 59.731 | 59.737 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 115.3302 | 115.3302 | 290.8037 | 1 | PROCESSED | 57532.5803935185 | 2016-05-24 13:55:46 | 54247 | 2007-05-27 00:00:00 | 54119.7612615741 | 2007-01-19 18:16:13 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001097 | We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip | CALIBRATION | 1 | A | HIRONORI MATSUMOTO | JAP | 0 | SWG | XIS FLIGHT CAIBRATION PLAN | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100044010/ | Quick Look | ![]() |
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2 | ABELL 773 | 139.3092 | 51.8461 | 138.434684 | 52.055757 | 124.471508 | 34.139728 | 165.95348434 | 43.2527698 | 276.9988 | 55684.9096412037 | 2011-05-03 21:49:53 | 55685.7363541667 | 2011-05-04 17:40:21 | 806027040 | 49.8691 | 50 | 49.8805 | 49.8771 | 0 | 49.8691 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.1285 | 44.1285 | 71.422 | 1 | PROCESSED | 57601.942962963 | 2016-08-01 22:37:52 | 55652 | 2011-04-01 00:00:00 | 55697.3061458333 | 2011-05-16 07:20:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061116 | We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 6 | AO6-LP | THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806027040/ | Quick Look | ![]() |
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3 | GX 349+2 | 256.427 | -36.366 | 255.587548 | -36.298664 | 258.786235 | -13.451096 | 349.14511841 | 2.78820606 | 85.6584 | 53808.5453240741 | 2006-03-14 13:05:16 | 53809.2216782407 | 2006-03-15 05:19:13 | 400003010 | 25.2308 | 50 | 25.2308 | 25.2332 | 25.2308 | 25.2308 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 20.0507 | 20.0507 | 58.434 | 2 | PROCESSED | 57533.2006365741 | 2016-05-25 04:48:55 | 54247 | 2007-05-27 00:00:00 | 54041.9132060185 | 2006-11-02 21:55:01 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001026 | We propose Suzaku observations of two luminous low-mass X-ray binaries (Z sources), GX 349+2 and Cyg X-2, to investigate the origin of the hard tails of Z sources, of which the spectral photon indices are reported to become occasionally less than unity. With the high sensitivity of the HXD, we detect the spectral shape up to several 100 keV and reveal existence of particle acceleration caused by high radiation pressure. | GALACTIC POINT SOURCES | 4 | A | HIROMITSU TAKAHASHI | JAP | 0 | SWG | SUZAKU OBSERVATIONS OF THE HARD TAILS OF LUMINOUS LOW-MASS X-RAY BINARIES (Z SOURCES) | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400003010/ | Quick Look | ![]() |
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4 | SS CYG | 325.6789 | 43.5736 | 325.187819 | 43.344381 | 350.451149 | 52.649921 | 90.55119171 | -7.12024619 | 276.5788 | 53676.0503703704 | 2005-11-02 01:12:32 | 53676.9856944444 | 2005-11-02 23:39:24 | 400006010 | 39.4512 | 40 | 39.4512 | 39.4512 | 39.4512 | 39.4512 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 32.0472 | 32.0472 | 80.81 | 1 | PROCESSED | 57527.7175925926 | 2016-05-19 17:13:20 | 54247 | 2007-05-27 00:00:00 | 54036.9898148148 | 2006-10-28 23:45:20 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001043 | Although the boundary layer that is formed between the rapidly rotating inner accretion disk and the white dwarf surface has been known as a hard-X-ray emitter, its geometry and structure has not been well understood yet. We aim to investigate the boundary layer structure with SS Cyg, the brightest dwarf nova, by means of a soft X-ray component with the BI CCD, a fluorescent Fe K-alpha line with the FI CCDs, and a continuum reflection by the white dwarf surface with the HXD PIN. It is of great use to observe states of a different mass accretion rate, and hence we propose to observe both in quiescence and in outburst. | GALACTIC POINT SOURCES | 4 | A | MANABU ISHIDA | JAP | 0 | SWG | SS CYG OBSERVATION IN QUIESCENCE | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400006010/ | Quick Look | ![]() |
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5 | X1630-472 | 248.4706 | -47.343 | 247.550146 | -47.238721 | 254.054156 | -25.085181 | 336.93140696 | 0.30212129 | 69.0657 | 53781.9791087963 | 2006-02-15 23:29:55 | 53782.5474305556 | 2006-02-16 13:08:18 | 400010020 | 21.429 | 200 | 21.429 | 21.485 | 21.429 | 21.429 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17.0223 | 17.0223 | 49.1019 | 0 | PROCESSED | 57533.0117592593 | 2016-05-25 00:16:56 | 54247 | 2007-05-27 00:00:00 | 54041.4892013889 | 2006-11-02 11:44:27 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001058 | We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active. | GALACTIC POINT SOURCES | 4 | A | JEAN COTTAM | JAP | 0 | SWG-TOO | FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400010020/ | Quick Look | ![]() |
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6 | JUPITER | 226.5694 | -16.1887 | 225.870685 | -15.99606 | 228.664382 | 1.239883 | 343.96536778 | 35.7224308 | 118.4901 | 53790.7643402778 | 2006-02-24 18:20:39 | 53791.7940277778 | 2006-02-25 19:03:24 | 401001010 | 37.7594 | 36 | 37.7674 | 37.7594 | 37.7674 | 37.7674 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 32.8361 | 32.8361 | 88.9361 | 1 | PROCESSED | 57533.0781597222 | 2016-05-25 01:52:33 | 54401 | 2007-10-28 00:00:00 | 53905.533900463 | 2006-06-19 12:48:49 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011003 | We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure. | GALACTIC POINT SOURCES | 4 | C | RONALD ELSNER | USA | 1 | AO1 | JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401001010/ | Quick Look | ![]() |
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7 | COMET_8P_TUTTLE-P2_08 | 40.0642 | -36.6693 | 39.55682 | -36.883219 | 21.03457 | -48.879704 | 242.2833952 | -65.12116443 | 253.2206 | 54490.9649421296 | 2008-01-25 23:09:31 | 54491.0959953704 | 2008-01-26 02:18:14 | 502063080 | 3.5416 | 4 | 3.5496 | 3.5416 | 0 | 3.5576 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 3.564 | 3.564 | 11.3119 | 0 | PROCESSED | 57541.3990509259 | 2016-06-02 09:34:38 | 54912 | 2009-03-22 00:00:00 | 54546.1411689815 | 2008-03-21 03:23:17 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063080/ | Quick Look | ![]() |
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8 | NGC 4051 | 180.8556 | 44.5807 | 180.217538 | 44.859022 | 159.275193 | 40.404023 | 148.68917976 | 70.06918189 | 135.3482 | 53684.8015509259 | 2005-11-10 19:14:14 | 53687.4315277778 | 2005-11-13 10:21:24 | 700004010 | 119.578 | 150 | 119.61 | 119.61 | 119.586 | 119.578 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 120.0047 | 120.0047 | 227.1918 | 3 | PROCESSED | 57528.0225810185 | 2016-05-20 00:32:31 | 54247 | 2007-05-27 00:00:00 | 54037.5713078704 | 2006-10-29 13:42:41 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001012 | We propose to obtain a broad band spectrum of the narrow-line Seyfert 1 (NLS1) NGC 4051. NLS1s are often presumed that they host a relatively small black hole with a very high accretion rate. Such a class would have played an important role in the growth of black holes in a cosmological context. We will measure the intrinsic photon index, amount of reflection, and high energy cutoff for the first time to investigate an accretion disk under a high accretion rate and compare them with conventional broad-line Seyferts. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YUICHI TERASHIMA | JAP | 0 | SWG | THE ACCRETION IN THE NARROW-LINE SEYFERT 1 NGC 4051 PROBED BY A BROAD BAND SPECTRUM | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700004010/ | Quick Look | ![]() |
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9 | HR 9024 | 357.4125 | 36.4308 | 356.782155 | 36.152799 | 14.165064 | 34.009987 | 109.27773456 | -24.79729068 | 49.8624 | 53939.0616782407 | 2006-07-23 01:28:49 | 53940.6016087963 | 2006-07-24 14:26:19 | 401032010 | 58.7757 | 60 | 58.7997 | 58.7757 | 58.7837 | 58.7917 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 56.0116 | 56.0116 | 133.0398 | 1 | PROCESSED | 57535.042025463 | 2016-05-27 01:00:31 | 54401 | 2007-10-28 00:00:00 | 53950.2624074074 | 2006-08-03 06:17:52 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011022 | Suzaku-XIS is the best available instrument to study the Fe fluorescence emission from late-type evolved stars. Fe fluorescence is produced by illumination of the photosphere by ionizing coronal X-rays and its intensity depends on the height of the X-ray source. We propose to observe Fe fluorescence in the single G-type giant HR 9024 and in the active RS CVn system II Peg to obtain a direct geometrical constraint on the scale height of their coronal structures. These two stars have the brightest Fe fluorescence features of all the late-type stars observed by the Chandra-HETGS and their different stellar parameters (stellar radius, gravity, multiplicity,..) and evolutionary stage will allow us to probe the typical coronal scale for significantly different conditions. | GALACTIC POINT SOURCES | 4 | B | PAOLA TESTA | USA | 1 | AO1 | GEOMETRY DIAGNOSTICS FROM FE FLUORESCENT EMISSION IN LATE-TYPE EVOLVED STARS | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401032010/ | Quick Look | ![]() |
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10 | BETA LYR | 282.5098 | 33.3716 | 282.047998 | 33.312385 | 288.857806 | 55.996493 | 63.19266924 | 14.79477853 | 53.4974 | 53867.1260185185 | 2006-05-12 03:01:28 | 53867.6252199074 | 2006-05-12 15:00:19 | 401036020 | 21.4962 | 20 | 21.4962 | 21.4962 | 21.4962 | 21.4962 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 19.1642 | 19.1642 | 43.1199 | 2 | PROCESSED | 57534.2764814815 | 2016-05-26 06:38:08 | 54401 | 2007-10-28 00:00:00 | 53914.2784143518 | 2006-06-28 06:40:55 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011031 | The goal of our project is to determine the location and properties of the hard X-ray emitting gas in the massive B7II+B0V interacting binary Beta Lyr. Our experiment is designed to distinguish between X-rays originating in the mass transfer stream and those originating in the extended circumbinary envelope. Modeling of XIS spectra will allow us to constrain the plasma temperature and emission measure, while the light curve with three exposures and high count rates will probe variability at around the 1% level over both the orbital timescale (13 days) and dynamical flow timescales (hours). Our request is for 20 ksec exposures at 3 different orbital phases to catch the system in and out of eclipse. | GALACTIC POINT SOURCES | 4 | A | RICHARD IGNACE | USA | 1 | AO1 | AN X-RAY STUDY OF HOT PLASMA IN THE INTERACTING BINARY BETA LYRAE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401036020/ | Quick Look | ![]() |
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11 | 4U 1705-44 | 257.2295 | -44.1004 | 256.326357 | -44.0367 | 260.194477 | -21.092135 | 343.32321952 | -2.34240238 | 264.0794 | 53976.2429166667 | 2006-08-29 05:49:48 | 53976.7731712963 | 2006-08-29 18:33:22 | 401046010 | 18.3155 | 20 | 18.3155 | 18.3155 | 18.3155 | 18.3155 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 15.3715 | 15.3715 | 45.8099 | 0 | PROCESSED | 57535.3889236111 | 2016-05-27 09:20:03 | 54526 | 2008-03-01 00:00:00 | 54021.306087963 | 2006-10-13 07:20:46 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011112 | We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state. | GALACTIC POINT SOURCES | 4 | A | ANDREW YOUNG | USA | 1 | AO1 | REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401046010/ | Quick Look | ![]() |
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12 | 4U 1636-536 | 250.2262 | -53.7541 | 249.22979 | -53.657603 | 256.460667 | -31.236861 | 332.91086545 | -4.81751491 | 91.2457 | 54140.3877546296 | 2007-02-09 09:18:22 | 54140.99125 | 2007-02-09 23:47:24 | 401050010 | 24.232 | 19 | 24.232 | 24.232 | 0 | 24.232 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 21.6895 | 21.6895 | 52.136 | 0 | PROCESSED | 57537.3410069445 | 2016-05-29 08:11:03 | 54525 | 2008-02-29 00:00:00 | 54151.5052893518 | 2007-02-20 12:07:37 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011117 | Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. | GALACTIC POINT SOURCES | 4 | A | JEROEN HOMAN | USA | 1 | AO1 | THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401050010/ | Quick Look | ![]() |
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13 | IGRJ16195-4945 | 244.8541 | -49.816 | 243.916706 | -49.695602 | 251.909406 | -27.940354 | 333.49117084 | 0.29973526 | 284.0301 | 53998.8508333333 | 2006-09-20 20:25:12 | 53999.7231481482 | 2006-09-21 17:21:20 | 401056010 | 39.1486 | 40 | 39.1486 | 39.1486 | 39.1486 | 39.1486 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 42.2652 | 42.2652 | 75.3579 | 1 | PROCESSED | 57535.652662037 | 2016-05-27 15:39:50 | 54526 | 2008-03-01 00:00:00 | 54020.9227199074 | 2006-10-12 22:08:43 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011132 | INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. | GALACTIC POINT SOURCES | 4 | A | RANDALL SMITH | USA | 1 | AO1 | HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401056010/ | Quick Look | ![]() |
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14 | CYGNUS X-1 | 299.6124 | 35.133 | 299.141904 | 34.996436 | 313.652571 | 54.178807 | 71.28577556 | 3.01567368 | 256.2202 | 54038.1501273148 | 2006-10-30 03:36:11 | 54038.8225 | 2006-10-30 19:44:24 | 401059010 | 27.7068 | 30 | 27.7068 | 27.7378 | 27.7068 | 27.7068 | 2 | 1 | 2 | 2 | 1 | 0 | 0 | 27.6892 | 27.6892 | 58.0839 | 0 | PROCESSED | 57535.9949768518 | 2016-05-27 23:52:46 | 54526 | 2008-03-01 00:00:00 | 54063.4924884259 | 2006-11-24 11:49:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011141 | We request three, 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku will bring three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 200-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history. | GALACTIC POINT SOURCES | 4 | B | MICHAEL NOWAK | USA | 1 | AO1 | ENHANCING THE LONG TERM MONITORING CAMPAIGN OF CYGNUS X-1 IN THE SUZAKU ERA | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401059010/ | Quick Look | ![]() |
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15 | EV LAC | 341.7127 | 44.3232 | 341.158134 | 44.059332 | 6.045133 | 46.919235 | 100.60502245 | -13.08073089 | 256.1601 | 54432.9692013889 | 2007-11-28 23:15:39 | 54434.4655208333 | 2007-11-30 11:10:21 | 402032010 | 68.9493 | 100 | 68.9493 | 69.1333 | 0 | 69.1275 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 65.0113 | 65.0113 | 129.2328 | 2 | PROCESSED | 57540.7939236111 | 2016-06-01 19:03:15 | 54808 | 2008-12-08 00:00:00 | 54441.0876851852 | 2007-12-07 02:06:16 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021013 | We propose a 100 ks Suzaku XIS observation of the dMe flare star EV Lac to measure coronal element abundances during quiescence and flares of different sizes. EV Lac undergoes frequent small flares, and is known to have undergone a very large flare at ~300 times the quiescent count rate in 2000. Coronal abundance changes shed light on the process of chromospheric evaporation under conditions different to those on the Sun. Depending on the size and spectrum of the flare, we may also be able to detect a hard burst of emission that would serve as a time marker for particle acceleration during the flare. | GALACTIC POINT SOURCES | 4 | C | UNA HWANG | USA | 2 | AO2 | FLARE AND QUIESENT CONORAL ELEMENT ABUNDANCES IN EV LAC | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402032010/ | Quick Look | ![]() |
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16 | VY AQR | 318.0426 | -8.8307 | 317.372404 | -9.036659 | 317.753092 | 7.00586 | 41.59091784 | -35.22055705 | 252.6652 | 54414.6528587963 | 2007-11-10 15:40:07 | 54415.3855787037 | 2007-11-11 09:15:14 | 402043010 | 25.4473 | 20 | 25.4473 | 25.4473 | 0 | 25.4473 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.3605 | 22.3605 | 63.2999 | 2 | PROCESSED | 57540.476712963 | 2016-06-01 11:26:28 | 54790 | 2008-11-20 00:00:00 | 54423.1702314815 | 2007-11-19 04:05:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021105 | Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose short Suzaku observations of dwarf novae with secure, parallax-based distance estimates that have not been the subject of pointed, imaging, X-ray observations in the 0.5-10 keV band. This will be an important check of potential biases in earlier studies. | GALACTIC POINT SOURCES | 4 | C | KOJI MUKAI | USA | 2 | AO2 | BUILDING UP AN UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A PARALLAX SELECTED SAMPLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402043010/ | Quick Look | ![]() |
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17 | HOLMBERG IX X-1 | 149.4869 | 69.0752 | 148.468802 | 69.313718 | 119.773156 | 51.703341 | 141.91661656 | 41.06840873 | 124.5 | 56224.1252199074 | 2012-10-24 03:00:19 | 56226.4168981482 | 2012-10-26 10:00:20 | 707019030 | 106.9454 | 500 | 106.9454 | 106.9534 | 0 | 106.9614 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 105.0119 | 105.0119 | 197.9478 | 1 | PROCESSED | 57607.8725462963 | 2016-08-07 20:56:28 | 56018 | 2012-04-01 00:00:00 | 56240.5429050926 | 2012-11-09 13:01:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071251 | Recent X-ray observations have found evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in a super-Eddington state. Current data are unable to deliver a clear answer, but the diagnostics possible in a long observation will be decisive. We request a 500 ks observation of the ULX Holmberg IX X-1 to place crucial constraints on atomic features that would signal a super-Eddington flow. Detecting or ruling out atomic features naturally requires a deep exposure. The strong spectral constraints derived will reveal the nature of the accreting black holes in these systems. A definitive statement on the existence of 100-1000 Msun black holes or extreme accretion states will be an important Suzaku legacy. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JON MILLER | USA | 7 | AO7 | A DECISIVE LEGACY OBSERVATION OF AN ULTRALUMINOUS X-RAY SOURCE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707019030/ | Quick Look | ![]() |
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18 | 4U1705-44 | 257.2229 | -44.1035 | 256.319735 | -44.039768 | 260.189733 | -21.095668 | 343.31790137 | -2.34044351 | 107.4157 | 54543.8610532407 | 2008-03-18 20:39:55 | 54544.5210532407 | 2008-03-19 12:30:19 | 402051040 | 20.0744 | 15 | 20.0744 | 20.0744 | 0 | 20.0824 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 13.4113 | 13.4113 | 57.0179 | 1 | PROCESSED | 57541.899525463 | 2016-06-02 21:35:19 | 54922 | 2009-04-01 00:00:00 | 54553.1912268518 | 2008-03-28 04:35:22 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021113 | We recently proposed a solution to the problem of model ambiguity for the spectra of atoll-type neutron stars. This work was performed on X-ray transient, and we need to test the model on the main population of persistent atolls. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. We propose to supplement the Suzaku monitoring archive begun in AO-1 by targeting the two persistent atolls with the greatest X-ray variability. | GALACTIC POINT SOURCES | 4 | A | RONALD REMILLARD | USA | 2 | AO2 | X-RAY SPECTRA OF ATOLL-TYPE NEUTRON STARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402051040/ | Quick Look | ![]() |
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19 | 2S 0921-630 | 140.6655 | -63.298 | 140.375275 | -63.083061 | 195.139147 | -68.890832 | 281.84446964 | -9.33525426 | 8.3442 | 54335.887025463 | 2007-08-23 21:17:19 | 54336.9932175926 | 2007-08-24 23:50:14 | 402059010 | 43.131 | 40 | 43.131 | 43.131 | 0 | 43.131 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.1622 | 37.1622 | 95.5598 | 0 | PROCESSED | 57539.6661805556 | 2016-05-31 15:59:18 | 54721 | 2008-09-12 00:00:00 | 54350.5504861111 | 2007-09-07 13:12:42 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021118 | 2S 0921-630 is a bright, long-period LMXB that is thought to contain an accretion disk corona. Observations with both the Chandra HETGS and XMM-Newton spectrometers revealed line emission from a photoionized plasma. The spectral features are consistent with the predictions for emission from an accretion disk corona. However, with the present data it is impossible to determine whether the emission originates in the corona or in a localized region of the disk. We propose to observer 2S 0921-630 with Suzaku at four orbital phases in order to localize and identify the emitting plasma. The simultaneous HXD coverage will also allow us to constrain the underlying continuum and allow more sensitive study of the high energy region of the spectrum. | GALACTIC POINT SOURCES | 4 | A | JEAN COTTAM | USA | 2 | AO2 | PHASE-RESOLVED SPECTROSCOPY OF 2S 0921-630 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402059010/ | Quick Look | ![]() |
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20 | 2S 0921-630 | 140.666 | -63.2982 | 140.375774 | -63.08326 | 195.139946 | -68.890744 | 281.84477381 | -9.33523447 | 8.344 | 54338.0511226852 | 2007-08-26 01:13:37 | 54339.16 | 2007-08-27 03:50:24 | 402060010 | 40.3423 | 40 | 40.3503 | 40.3423 | 0 | 40.3503 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 35.6464 | 35.6464 | 95.7999 | 2 | PROCESSED | 57539.6728703704 | 2016-05-31 16:08:56 | 54721 | 2008-09-12 00:00:00 | 54350.5629398148 | 2007-09-07 13:30:38 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021118 | 2S 0921-630 is a bright, long-period LMXB that is thought to contain an accretion disk corona. Observations with both the Chandra HETGS and XMM-Newton spectrometers revealed line emission from a photoionized plasma. The spectral features are consistent with the predictions for emission from an accretion disk corona. However, with the present data it is impossible to determine whether the emission originates in the corona or in a localized region of the disk. We propose to observer 2S 0921-630 with Suzaku at four orbital phases in order to localize and identify the emitting plasma. The simultaneous HXD coverage will also allow us to constrain the underlying continuum and allow more sensitive study of the high energy region of the spectrum. | GALACTIC POINT SOURCES | 4 | A | JEAN COTTAM | USA | 2 | AO2 | PHASE-RESOLVED SPECTROSCOPY OF 2S 0921-630 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402060010/ | Quick Look | ![]() |
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21 | IGR J17391-3021 | 264.795 | -30.3419 | 263.992133 | -30.314694 | 265.466386 | -6.982553 | 358.06793122 | 0.44854091 | 89.216 | 54518.4950115741 | 2008-02-22 11:52:49 | 54519.3961226852 | 2008-02-23 09:30:25 | 402066010 | 36.4657 | 30 | 36.5457 | 36.5937 | 0 | 36.4657 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31.2591 | 31.2591 | 77.8198 | 1 | PROCESSED | 57541.7105671296 | 2016-06-02 17:03:13 | 54892 | 2009-03-02 00:00:00 | 54525.5064699074 | 2008-02-29 12:09:19 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021122 | We propose to observe 3 INTEGRAL-discovered High Mass X-ray Binaries (IGR HMXBs) to search for X-ray pulsations and to study their broadband spectra. Over the past few years, INTEGRAL has found a surprising number of HMXBs, and the large number of new, locally absorbed supergiant HMXBs indicate that these wind-accretors are more common than previously thought. In addition to high column densities, some of these systems have other extreme properties such as slowly rotating neutron stars (NSs) or rapid X-ray flares. For the systems we propose to observe, detection of pulsations is important for establishing the presence of a NS and for constraining the spin period distribution for HMXB NSs. As these are strong hard X-ray emitters, we will take advantage of Suzaku's broadband capabilities. | GALACTIC POINT SOURCES | 4 | B | JOHN TOMSICK | USA | 2 | AO2 | LOOKING FOR SIGNATURES OF HIGH MAGNETIC FIELD NEUTRON STARS IN INTEGRAL HMXBS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402066010/ | Quick Look | ![]() |
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22 | CIRCINUS X-1 | 230.1633 | -57.1695 | 229.194668 | -56.989293 | 244.120639 | -37.250007 | 322.11384942 | 0.03740334 | 115.206 | 54530.1953240741 | 2008-03-05 04:41:16 | 54531.5523032407 | 2008-03-06 13:15:19 | 402070010 | 46.4113 | 43 | 46.4113 | 46.4113 | 0 | 46.4113 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.8213 | 41.8213 | 117.196 | 0 | PROCESSED | 57541.8053125 | 2016-06-02 19:19:39 | 54916 | 2009-03-26 00:00:00 | 54550.2459953704 | 2008-03-25 05:54:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021128 | We propose a 100ks Suzaku observation of Circinus X-1 through the zero (dipping) phase to facilitate 2 important and independent science goals. (1) For the binary, we wish to better understand the viewing geometry, and investigate physical changes in the binary behavior as it relates to observed spectral changes through periastron passage. (2) Conduct a large angle scattering study of the X-ray halo surrounding Circinus X-1 to diagnose ISM grain properties (the line-of-sight position, size distribution, and grain density) near us, in complement with our Chandra halo studies at small angles on grain properties near the source. | GALACTIC POINT SOURCES | 4 | A | JULIA LEE | USA | 2 | AO2 | CIRCINUS X-1 NEAR PERIASTRON: PROBING BINARY PHYSICS AND ISM GRAINS ALONG THE LINE OF SIGHT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402070010/ | Quick Look | ![]() |
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23 | CYG X-1 | 299.5451 | 35.2618 | 299.075532 | 35.125519 | 313.637974 | 54.318601 | 71.3671857 | 3.12971485 | 59.9371 | 54237.8204050926 | 2007-05-17 19:41:23 | 54238.6480787037 | 2007-05-18 15:33:14 | 402072020 | 33.3568 | 30 | 33.3568 | 33.3649 | 0 | 33.3568 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 32.5637 | 32.5637 | 71.5039 | 1 | PROCESSED | 57538.696724537 | 2016-05-30 16:43:17 | 54695 | 2008-08-17 00:00:00 | 54245.0149884259 | 2007-05-25 00:21:35 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021133 | We request two additional 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku will bring three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 200-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history. | GALACTIC POINT SOURCES | 4 | A | MICHAEL NOWAK | USA | 2 | AO2 | CONTINUING TO ENHANCE THE LONG TERM MONITORING CAMPAIGN OF CYGNUS X-1 IN THE SUZAKU ERA | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402072020/ | Quick Look | ![]() |
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24 | CAS A | 350.8761 | 58.8091 | 350.310124 | 58.534509 | 27.390357 | 54.841399 | 111.74552355 | -2.13963884 | 214.5537 | 53783.6003472222 | 2006-02-17 14:24:30 | 53783.9218055556 | 2006-02-17 22:07:24 | 100043020 | 14.155 | 10 | 14.155 | 14.155 | 14.155 | 14.155 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 17.3713 | 17.3713 | 27.768 | 0 | PROCESSED | 57533.0311805556 | 2016-05-25 00:44:54 | 54247 | 2007-05-27 00:00:00 | 54041.4627893518 | 2006-11-02 11:06:25 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001097 | We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip | CALIBRATION | 1 | A | HIRONORI MATSUMOTO | JAP | 0 | SWG | XIS FLIGHT CAIBRATION PLAN | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100043020/ | Quick Look | ![]() |
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25 | TAU SCO | 248.9736 | -28.2151 | 248.194076 | -28.113426 | 251.450456 | -6.117318 | 351.53721955 | 12.80675658 | 279.3712 | 54723.4207291667 | 2008-09-14 10:05:51 | 54723.8119675926 | 2008-09-14 19:29:14 | 403034030 | 12.2902 | 10 | 12.2982 | 12.2982 | 0 | 12.2902 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.0282 | 11.0282 | 33.7999 | 0 | PROCESSED | 57543.8133564815 | 2016-06-04 19:31:14 | 55148 | 2009-11-13 00:00:00 | 54780.4631597222 | 2008-11-10 11:06:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031121 | We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars. | GALACTIC POINT SOURCES | 4 | A | RICHARD IGNACE | USA | 3 | AO3 | X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403034030/ | Quick Look | ![]() |
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26 | ETA CARINAE | 161.2297 | -59.7314 | 160.743721 | -59.468116 | 202.194195 | -58.967017 | 287.60304523 | -0.67930865 | 294 | 54627.0775 | 2008-06-10 01:51:36 | 54627.649525463 | 2008-06-10 15:35:19 | 403035010 | 35.4479 | 30 | 35.4639 | 35.4479 | 0 | 35.4639 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.2102 | 27.2102 | 49.4159 | 1 | PROCESSED | 57542.7628819445 | 2016-06-03 18:18:33 | 55003 | 2009-06-21 00:00:00 | 54637.2680092593 | 2008-06-20 06:25:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031124 | X-ray observations of Eta Carinae near the 2003 periastron passage confirmed that the X-ray emission primarily arises from collision of winds in a binary system, but raised fundamental questions about the cause of the 3 month-long X-ray minimum and an excess above ~10 keV (possibly up to 50 keV) in addition to the thermal emission with kT ~3-5 keV. These features would originate from plasma extremely embedded in the primary winds and acceleration of high energy particles at the wind colliding region. To resolve these features clearly, broad band Suzaku observations around the periastron passage are crucial. We propose four 30 ksec Suzaku observations of Eta Carinae during AO3, which will cover the next X-ray maximum (in late 2008) and minimum (in early 2009). | GALACTIC POINT SOURCES | 4 | A | KENJI HAMAGUCHI | USA | 3 | AO3 | X-RAY EMISSION FROM ETA CARINAE DURING THE X-RAY MAXIMUM AND MINIMUM | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403035010/ | Quick Look | ![]() |
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27 | ETA CARINAE | 161.3639 | -59.6742 | 160.876523 | -59.410706 | 202.202933 | -58.878505 | 287.63630523 | -0.59715454 | 170.6228 | 54877.528287037 | 2009-02-15 12:40:44 | 54878.4119675926 | 2009-02-16 09:53:14 | 403038010 | 35.5525 | 30 | 35.5685 | 35.5525 | 0 | 35.5605 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31.1193 | 31.1193 | 76.3239 | 1 | PROCESSED | 57545.5564814815 | 2016-06-06 13:21:20 | 55328 | 2010-05-12 00:00:00 | 54893.4307407407 | 2009-03-03 10:20:16 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031124 | X-ray observations of Eta Carinae near the 2003 periastron passage confirmed that the X-ray emission primarily arises from collision of winds in a binary system, but raised fundamental questions about the cause of the 3 month-long X-ray minimum and an excess above ~10 keV (possibly up to 50 keV) in addition to the thermal emission with kT ~3-5 keV. These features would originate from plasma extremely embedded in the primary winds and acceleration of high energy particles at the wind colliding region. To resolve these features clearly, broad band Suzaku observations around the periastron passage are crucial. We propose four 30 ksec Suzaku observations of Eta Carinae during AO3, which will cover the next X-ray maximum (in late 2008) and minimum (in early 2009). | GALACTIC POINT SOURCES | 4 | A | KENJI HAMAGUCHI | USA | 3 | AO3 | X-RAY EMISSION FROM ETA CARINAE DURING THE X-RAY MAXIMUM AND MINIMUM | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403038010/ | Quick Look | ![]() |
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28 | SS73 17 | 152.7399 | -57.7545 | 152.30201 | -57.507445 | 193.309145 | -60.825813 | 282.81739372 | -1.29143094 | 80.1552 | 54775.6877430556 | 2008-11-05 16:30:21 | 54776.3072453704 | 2008-11-06 07:22:26 | 403043010 | 24.907 | 20 | 24.907 | 24.907 | 0 | 24.907 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.8091 | 20.8091 | 53.5199 | 0 | PROCESSED | 57544.3629282407 | 2016-06-05 08:42:37 | 55157 | 2009-11-22 00:00:00 | 54791.6362847222 | 2008-11-21 15:16:15 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031145 | SS73 17 was an innocuous Mira-type symbiotic star until INTEGRAL and Swift discovered its bright hard X-ray emission. Suzaku observations showed it emits three bright iron lines, with almost no emission in the 0.5-2 keV bandpass. The PI has an approved 100 ksec Chandra HETG observation in 2008 to determine the origin of the iron lines and measure any weak emission lines. With simultaneous Suzaku observations we will also measure the hard X-ray emission from the source, both to constrain the continuum and detect any non-thermal component. The effective areas of the XIS and HXD will constrain the broadband emission process much better than the HETG data. Combined with simultaneous optical observations of the Mira-type star we will determine the origin of this star's unusual emission. | GALACTIC POINT SOURCES | 4 | A | RANDALL SMITH | USA | 3 | AO3 | SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS OF THE SYMBIOTIC STAR SS73 17 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403043010/ | Quick Look | ![]() |
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29 | 1A1118-61 | 170.3215 | -61.8847 | 169.770459 | -61.610411 | 210.906306 | -57.212373 | 292.5244731 | -0.84831529 | 142.606 | 54859.2344328704 | 2009-01-28 05:37:35 | 54859.8925810185 | 2009-01-28 21:25:19 | 403050010 | 44.2125 | 45 | 44.2125 | 44.2125 | 0 | 44.2125 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.9154 | 30.9154 | 56.8599 | 0 | PROCESSED | 57545.3633680556 | 2016-06-06 08:43:15 | 55328 | 2010-05-12 00:00:00 | 54880.5326273148 | 2009-02-18 12:46:59 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031155 | We propose to perform Target of Opportunity Observations of one accreting neutron star in outburst during Suzaku AO3. The aim of the observations is to observe the source at a level of 40 and 200mCrab, to determine the properties of the cyclotron line in this system and to determine its broad band spectrum. | GALACTIC POINT SOURCES | 4 | A | KATJA POTTSCHMIDT | USA | 3 | AO3-TOO | SEARCHING FOR CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403050010/ | Quick Look | ![]() |
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30 | CYG X-1 | 299.5797 | 35.2714 | 299.110135 | 35.134972 | 313.689122 | 54.31814 | 71.39012673 | 3.11059703 | 84.4565 | 54574.6816898148 | 2008-04-18 16:21:38 | 54575.4238425926 | 2008-04-19 10:10:20 | 403065010 | 33.9435 | 30 | 33.9435 | 33.9782 | 0 | 33.9703 | 1 | 1 | 0 | 2 | 1 | 0 | 0 | 28.9556 | 28.9556 | 64.118 | 0 | PROCESSED | 57542.3725231482 | 2016-06-03 08:56:26 | 54957 | 2009-05-06 00:00:00 | 54587.2117476852 | 2008-05-01 05:04:55 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031172 | We request two 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku brings three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 100-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history. | GALACTIC POINT SOURCES | 4 | A | MICHAEL NOWAK | USA | 3 | AO3 | CONTINUING TO ENHANCE THE LONG TERM MONITORING CAMPAIGN IN THE SUZAKU ERA | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403065010/ | Quick Look | ![]() |
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31 | V773 TAU | 63.5591 | 28.1916 | 62.7857 | 28.065974 | 66.717215 | 6.863448 | 168.22897578 | -16.34488481 | 264.3183 | 55255.9666550926 | 2010-02-28 23:11:59 | 55258.750162037 | 2010-03-03 18:00:14 | 404037010 | 115.4057 | 120 | 115.4057 | 115.4057 | 0 | 115.4057 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95.563 | 95.563 | 240.4667 | 1 | PROCESSED | 57550.8499189815 | 2016-06-11 20:23:53 | 55637 | 2011-03-17 00:00:00 | 55271.499537037 | 2010-03-16 11:59:20 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041203 | Young stars display magnetic activity at the extreme of that produced in nearby active stars and the Sun, making them useful tools to probe the dominant physical processes controlling such activity. The unique features of V773 Tau's X-ray and radio properties (frequent X-ray flaring of highly energetic flares, extreme nonthermal radio emission) mark it as one of the most active young stars. We seek coordinated Suzaku and mm wavelength observations to probe the interplay between the hot plasma and the stellar environment. We focus on utilizing the unique capabilities of Suzaku, namely the spectral resolution and sensitivity at 5--10 keV, to elucidate the properties of its hot plasma and its potential effects on the stellar environment such as detecting Fe fluorescence. | GALACTIC POINT SOURCES | 4 | C | RACHEL OSTEN | USA | 4 | AO4 | X-RAY EMISSION AND THE STELLAR ENVIRONMENT AROUND THE PRE-MAIN SEQUENCE BINARY V773 TAU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404037010/ | Quick Look | ![]() |
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32 | ETA CARINAE | 161.2575 | -59.6351 | 160.770713 | -59.371773 | 202.076586 | -58.890955 | 287.57052339 | -0.58758586 | 87.8919 | 55156.1883449074 | 2009-11-21 04:31:13 | 55157.3196643518 | 2009-11-22 07:40:19 | 404039010 | 49.3887 | 45 | 49.3887 | 49.3887 | 0 | 49.3887 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.2553 | 34.2553 | 97.7201 | 0 | PROCESSED | 57549.5287152778 | 2016-06-10 12:41:21 | 55542 | 2010-12-12 00:00:00 | 55176.3651388889 | 2009-12-11 08:45:48 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041204 | The collision of winds in the supermassive binary Eta Car produces hot plasma detectable by Suzaku to 40 keV. This emission provides key clues to the way extremely massive stars lose mass. We propose to observe this hard X-ray emission with Suzaku after the periastron passage in order to measure the intrinsic luminosity of the wind-wind shock to determine the density of the wind near the shock boundary, and to measure the absorbing column to indicate the density profile in the distorted wind of the primary star. In addition HXD observations will measure any excess emission up to energies of 40 keV to constrain the amount of particle acceleration in the shock by the first order Fermi process and to help resolve the discrepancy between published BeppoSAX and INTEGRAL measurements. | GALACTIC POINT SOURCES | 4 | A | KENJI HAMAGUCHI | USA | 4 | AO4 | HARD X-RAY EMISSION, PARTICLE ACCELERATION AND MASS LOSS FROM ETA CAR | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404039010/ | Quick Look | ![]() |
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33 | GRS 1758-258 | 270.2971 | -25.679 | 269.522467 | -25.678561 | 270.258372 | -2.238361 | 4.56169204 | -1.32563061 | 89.3817 | 55263.8983333333 | 2010-03-08 21:33:36 | 55266.0711111111 | 2010-03-11 01:42:24 | 404060010 | 82.6827 | 80 | 82.6827 | 82.6827 | 0 | 82.6827 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71.1789 | 71.1789 | 187.7097 | 1 | PROCESSED | 57550.8664583333 | 2016-06-11 20:47:42 | 55647 | 2011-03-27 00:00:00 | 55279.5468402778 | 2010-03-24 13:07:27 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041244 | We propose an 80 ks observation to obtain a broadband spectrum of the Galactic microquasar GRS 1758-258 while in the low-hard state with Suzaku. Here we aim to constrain the nature and geometry of the accretion flow via measurements of the various disc reflection features, which are detectable for the first time due to the unique capabilities of Suzaku. As this system is known to power large radio jets, its study will also aid our understanding of the conditions necessary for the formation of relativistic outflows and how these relate to the accretion geometry in the low-hard state. | GALACTIC POINT SOURCES | 4 | B | MARK REYNOLDS | USA | 4 | AO4 | CONSTRAINING DISC REFLECTION IN THE MICROQUASAR GRS 1758-258 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404060010/ | Quick Look | ![]() |
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34 | LMC X-1 | 84.947 | -69.7479 | 85.058791 | -69.772179 | 298.110491 | -86.30257 | 280.20680376 | -31.50316575 | 10.0004 | 55033.776724537 | 2009-07-21 18:38:29 | 55036.8953587963 | 2009-07-24 21:29:19 | 404061010 | 129.8679 | 120 | 129.8679 | 129.8679 | 0 | 129.8679 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 132.5976 | 132.5976 | 269.3956 | 4 | PROCESSED | 57548.0199537037 | 2016-06-09 00:28:44 | 55419 | 2010-08-11 00:00:00 | 55048.6509143518 | 2009-08-05 15:37:19 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041245 | We propose to measure the spins of two black holes, LMC X-1 and LMC X-3, using two independent methods concurrently: modeling the thermal spectrum of the accretion disk and modeling the profile of the Fe K line. Suzaku is the only mission capable of achieving both of our main objectives: (1) to make the first Fe K spin measurements of these LMC sources, and (2) to explore whether the two methods deliver consistent results. The XIS will provide full coverage of the continuum spectrum and handily resolve the broad Fe line, while the HXD PIN will strongly constrain the Compton power-law component, which is important to both methods. For both of these LMC sources, we confidently argue that the spins obtained by modeling the continuum spectrum will be of exceptional precision and reliability. | GALACTIC POINT SOURCES | 4 | A | JEFFREY MCCLINTOCK | USA | 4 | AO4 | MEASURING BLACK-HOLE SPINS IN THE LMC USING BOTH THE THERMAL X-RAY CONTINUUM AND FE K LINE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404061010/ | Quick Look | ![]() |
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35 | LMC X-3 | 84.7128 | -64.0821 | 84.643099 | -64.107952 | 45.920225 | -86.688866 | 273.5746003 | -32.09166858 | 184.4521 | 55186.5265162037 | 2009-12-21 12:38:11 | 55190.9105555556 | 2009-12-25 21:51:12 | 404062010 | 154.4242 | 150 | 154.434 | 154.434 | 0 | 154.4242 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 101.1721 | 101.1721 | 352.1458 | 2 | PROCESSED | 57550.1364930556 | 2016-06-11 03:16:33 | 55587 | 2011-01-26 00:00:00 | 55218.7384375 | 2010-01-22 17:43:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041245 | We propose to measure the spins of two black holes, LMC X-1 and LMC X-3, using two independent methods concurrently: modeling the thermal spectrum of the accretion disk and modeling the profile of the Fe K line. Suzaku is the only mission capable of achieving both of our main objectives: (1) to make the first Fe K spin measurements of these LMC sources, and (2) to explore whether the two methods deliver consistent results. The XIS will provide full coverage of the continuum spectrum and handily resolve the broad Fe line, while the HXD PIN will strongly constrain the Compton power-law component, which is important to both methods. For both of these LMC sources, we confidently argue that the spins obtained by modeling the continuum spectrum will be of exceptional precision and reliability. | GALACTIC POINT SOURCES | 4 | C | JEFFREY MCCLINTOCK | USA | 4 | AO4 | MEASURING BLACK-HOLE SPINS IN THE LMC USING BOTH THE THERMAL X-RAY CONTINUUM AND FE K LINE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404062010/ | Quick Look | ![]() |
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36 | EG AND | 11.168 | 40.673 | 10.482613 | 40.399604 | 27.902454 | 32.653699 | 121.54657283 | -22.18054863 | 225.2111 | 55597.6281018518 | 2011-02-05 15:04:28 | 55600.0030092593 | 2011-02-08 00:04:20 | 405034010 | 100.5333 | 100 | 100.5333 | 100.5413 | 0 | 100.5493 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 84.6589 | 84.6589 | 205.1719 | 3 | PROCESSED | 57600.9241666667 | 2016-07-31 22:10:48 | 55983 | 2012-02-26 00:00:00 | 55614.2972106482 | 2011-02-22 07:07:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051211 | The goals of this proposal are to use Suzaku XIS observations to : 1) determine whether EG And, BX Mon, and BF Cyg are members of the recently recognized class of hard X-ray emitting symbiotic stars; and 2) if they are, compare the nature of any absorption, the optical depth of the boundary layer, and the accretion rate to those of the well established hard X-ray symbiotics. Understanding the accretion processes in symbiotic stars is a crucial step in determining the role they play as progenitors of type Ia supernovae. | GALACTIC POINT SOURCES | 4 | C | THOMAS NELSON | USA | 5 | AO5 | EXPLORING THE ACCRETION DISK BOUNDARY LAYERS OF SYMBIOTIC STARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405034010/ | Quick Look | ![]() |
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37 | 4U 1626-67 | 248.0734 | -67.4643 | 246.814526 | -67.35746 | 258.330198 | -44.907314 | 321.7866399 | -13.09493758 | 285.8172 | 55445.5409259259 | 2010-09-06 12:58:56 | 55446.2376273148 | 2010-09-07 05:42:11 | 405044010 | 20.0335 | 20 | 20.0335 | 20.0575 | 0 | 20.0457 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.5372 | 19.5372 | 60.1799 | 0 | PROCESSED | 57553.3082175926 | 2016-06-14 07:23:50 | 55822 | 2011-09-18 00:00:00 | 55456.2336574074 | 2010-09-17 05:36:28 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051234 | Recent X-ray observations by Fermi/GBM and Swift/BAT of 4U 1626-67 discovered a new torque reversal of this source after 18 years of steady spinning down. Centered on Feb 4 2008, a dramatic increase in the X-ray flux was also observed. The lack of correlation between the X-ray flux and the torque applied to the neutron star before the transition, challenges our understanding of the physical mechanisms operating in this system. The main goal of this proposal is to look for changes in the long term flux behavior, energy spectra, pulse profile, line features and power spectra with the current evolution in 4U1626-67 s spin-up rate. In addition, we wish to determine whether the absence of the QPO observed just after the torque reversal persist. | GALACTIC POINT SOURCES | 4 | A | MARK FINGER | USA | 5 | AO5 | THE ACCRETING X-RAY PULSAR 4U 1626-67 AFTER A NEW TORQUE REVERSAL | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405044010/ | Quick Look | ![]() |
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38 | 4U 1957+11 | 299.8589 | 11.6979 | 299.267976 | 11.560536 | 304.903477 | 31.592045 | 51.30303986 | -9.34292333 | 251.3459 | 55501.8275462963 | 2010-11-01 19:51:40 | 55502.7001157407 | 2010-11-02 16:48:10 | 405057030 | 35.3491 | 35 | 35.3571 | 35.3491 | 0 | 35.3571 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.1697 | 27.1697 | 75.362 | 0 | PROCESSED | 57553.9520601852 | 2016-06-14 22:50:58 | 55881 | 2011-11-16 00:00:00 | 55515.3015046296 | 2010-11-15 07:14:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051254 | We propose three observations of the black hole candidate 4U 1957+11. It is one of only two persistently soft state BHC, and has the highest fitted temperature, and highest fitted spin parameter, of any observed BHC. The question arises of whether this high spin is a good estimate of the true spin, or whether this high temperature is evidence of a low level or corona or wind. The multiple Suzaku observations will allow us to track how the disk parameters change, and offer us a 40% chance of observing a state with a large coronal component. The latter might be indicative of launching of a disk wind. | GALACTIC POINT SOURCES | 4 | B | MICHAEL NOWAK | USA | 5 | AO5 | 4U1957+11: THE MOST RAPIDLY SPINNING BLACK HOLE? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405057030/ | Quick Look | ![]() |
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39 | TYCHO SNR HXD BKGD | 9.2173 | 64.3076 | 8.488109 | 64.032592 | 44.61366 | 53.051862 | 121.35322514 | 1.48051733 | 84.2005 | 53915.6541782407 | 2006-06-29 15:42:01 | 53916.7606944444 | 2006-06-30 18:15:24 | 500025010 | 51.0088 | 50 | 51.0088 | 51.0088 | 51.0088 | 51.0088 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 48.7224 | 48.7224 | 95.5939 | 2 | PROCESSED | 57534.8010300926 | 2016-05-26 19:13:29 | 54302 | 2007-07-21 00:00:00 | 54052.5940509259 | 2006-11-13 14:15:26 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001099 | We propose to observe Tycho's Supernova Remnant with Suzaku. The proposal has two main goals: (1) to measure the energy spectrum of the entire remnant above 10 keV with the HXD, and (2) to study the 0.5-10 keV band spectrum as a function of position with the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | JOHN HUGHES | JAP | 0 | SWG | SUZAKU STUDY OF TYCHO'S SUPERNOVA REMNANT | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500025010/ | Quick Look | ![]() |
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40 | HD162020 | 267.6631 | -40.3218 | 266.786356 | -40.308311 | 268.128314 | -16.895672 | 350.73730077 | -6.73005667 | 259.9987 | 55829.424212963 | 2011-09-25 10:10:52 | 55829.6543865741 | 2011-09-25 15:42:19 | 406038030 | 11.481 | 10 | 11.481 | 11.481 | 0 | 11.481 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.5402 | 8.5402 | 19.8799 | 0 | PROCESSED | 57603.2407638889 | 2016-08-03 05:46:42 | 56225 | 2012-10-25 00:00:00 | 55858.0790162037 | 2011-10-24 01:53:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061202 | Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. | GALACTIC POINT SOURCES | 4 | A | IGNAZIO PILLITTERI | USA | 6 | AO6 | STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406038030/ | Quick Look | ![]() |
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41 | 4 DRA | 187.5655 | 69.216 | 187.018636 | 69.492063 | 136.915856 | 61.202296 | 125.72551845 | 47.79722512 | 145.5318 | 55874.1707291667 | 2011-11-09 04:05:51 | 55875.0619328704 | 2011-11-10 01:29:11 | 406041010 | 42.258 | 40 | 42.258 | 42.258 | 0 | 42.258 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.7925 | 39.7925 | 76.998 | 2 | PROCESSED | 57603.7210532407 | 2016-08-03 17:18:19 | 56260 | 2012-11-29 00:00:00 | 55890.6961458333 | 2011-11-25 16:42:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061212 | 4 Dra is a weakly symbiotic star that exhibited strong variability in ROSAT observations. Our Suzaku Cycle 5 observation confirms it to be an absorbed hard X-ray source, powered by accretion. It is thus a nearby, lower accretion rate analogue of the hard X-ray bright symbiotic stars such as T CrB and CH Cyg. During Suzaku Cycle 6, 4 Dra is near apastron and near the inferior conjunction of the accreting white dwarf: both these should reduce the absorption due to the M giant, while absorption by the accretion flow near the white dwarf should remain roughly comparable. We therefore propose a second Suzaku observation of 4 Dra to constrain the relative contributions of these two X-ray absorbers, and to obtain a high signal-to-noise spectrum of a symbiotic star boundary layer near 1 keV. | GALACTIC POINT SOURCES | 4 | C | KOJI MUKAI | USA | 6 | AO6 | A SUZAKU OBSERVATION OF 4 DRA NEAR INFERIOR CONJUNCTION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406041010/ | Quick Look | ![]() |
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42 | 4U 1954+31 | 298.9334 | 32.0803 | 298.445315 | 31.946656 | 311.138232 | 51.470698 | 68.38077131 | 1.91321277 | 261.2562 | 55857.3373263889 | 2011-10-23 08:05:45 | 55858.7203009259 | 2011-10-24 17:17:14 | 406046010 | 60.216 | 60 | 60.224 | 60.232 | 0 | 60.216 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 57.9008 | 57.9008 | 119.4679 | 0 | PROCESSED | 57603.6159953704 | 2016-08-03 14:47:02 | 56241 | 2012-11-10 00:00:00 | 55874.1069328704 | 2011-11-09 02:33:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061226 | We propose the first Suzaku observation of a symbiotic X-ray binary 4U 1954+31. This object has an extraordinarily long spin period, ~5 hour, attributed to the neutron star (NS) rotation, making 4U 1954+31 the slowest-rotating accreting NS binary. It raises a question about its binary evolution, since a slowly rotating NS orbiting an M-type giant is quite unique. As to its large variability, the popular clumpy wind model has not yet become a smoking-gun, and we propose an alternative hypothesis that the NS is a magnetar descendent captured by an M-type giant in their closer encounter. Known X-ray properties of 4U~1954+31 will be revisited in a view of gated accretion onto the strongly magnetized NS. A 60 ks Suzaku observation can examine these scenarios. | GALACTIC POINT SOURCES | 4 | B | TERUAKI ENOTO | USA | 6 | AO6 | THE SLOWEST ROTATING PULSAR 4U 1954+31 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406046010/ | Quick Look | ![]() |
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43 | BV CEN | 202.8234 | -54.9803 | 202.03184 | -54.72288 | 225.050111 | -41.512019 | 308.67903183 | 7.44609562 | 120.7167 | 56329.0246875 | 2013-02-06 00:35:33 | 56329.4856018518 | 2013-02-06 11:39:16 | 407047010 | 33.38 | 30 | 33.388 | 33.388 | 0 | 33.38 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 30.8692 | 30.8692 | 39.8159 | 0 | PROCESSED | 57610.5262268518 | 2016-08-10 12:37:46 | 56715 | 2014-02-27 00:00:00 | 56349.4846990741 | 2013-02-26 11:37:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071212 | The mass of an accreting white dwarf is a key parameter governing its X-ray emission. We expect that the higher the mass, the higher the temperature and luminosity. Existing data appear consistent with this expectation, given the considerable uncertainties usually associated with the white dwarf masses of individual systems. Here we propose Suzaku observations of 5 dwarf novae for which very high or very low white dwarf mass estimates have been published. These targets provide the best opportunity of further establishing the mass-temperature correlation. Moreover, if the mass estimates are reliable, these targets are of interest from evolutionary considerations - how did these systems form with such high/low mass white dwarfs, and what are their ultimate fates? | GALACTIC POINT SOURCES | 4 | C | KOJI MUKAI | USA | 7 | AO7 | DWARF NOVAE WITH EXTREME WHITE DWARF MASSES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407047010/ | Quick Look | ![]() |
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44 | HERCULES X-1 | 254.4612 | 35.329 | 254.010606 | 35.404605 | 245.997214 | 57.479973 | 58.13300626 | 37.51795138 | 268.1998 | 56194.4317708333 | 2012-09-24 10:21:45 | 56195.0641087963 | 2012-09-25 01:32:19 | 407051030 | 23.5894 | 20 | 23.5931 | 23.5931 | 0 | 23.5894 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23.4769 | 23.4769 | 54.634 | 0 | PROCESSED | 57607.1945601852 | 2016-08-07 04:40:10 | 56689 | 2014-02-01 00:00:00 | 56323.5148726852 | 2013-01-31 12:21:25 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071224 | This proposal is for the continuation of successful Suzaku observations of Her X-1. The proposal is led by the NuSTAR team, extended with experts on X-ray binary pulsars with cyclotron lines. We propose three 20 ks simultaneous Suzaku and NuSTAR observations of Her X-1. Joint observations will substantial increase the science that can be addressed, allowing a systematic study of the fundamental cyclotron line (~40 keV) as a function of time, X-ray flux, 35 day phase, and 1.24 s pulse phase. The combined data will probe fundamental physics in this system, including the structure of the magnetic field in the polar caps, the physics of sub-Eddington accretion, and physical processes inside the neutron star. | GALACTIC POINT SOURCES | 4 | B | BRIAN GREFENSTETTE | USA | 7 | AO7 | STUDY OF THE CYCLOTRON LINE FEATURE IN HERCULES X-1: THE PROFILE AND THE SHORT- AND LONG-TERM VARIABILITY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407051030/ | Quick Look | ![]() |
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45 | 4U1538-522 | 235.6015 | -52.3857 | 234.665107 | -52.226494 | 246.064673 | -31.762519 | 327.42188954 | 2.16239803 | 275.2972 | 56149.0031134259 | 2012-08-10 00:04:29 | 56149.7349537037 | 2012-08-10 17:38:20 | 407068010 | 45.9554 | 40 | 45.9554 | 45.9554 | 0 | 45.9554 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.05 | 40.05 | 63.212 | 0 | PROCESSED | 57606.8269444444 | 2016-08-06 19:50:48 | 56640 | 2013-12-14 00:00:00 | 56272.688900463 | 2012-12-11 16:32:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071233 | Observations of accreting pulsars in High Mass X-ray Binaries (HMXBs) provide us with important information about the physical processes in the stellar wind of the high mass donor star, the coupling between the accreting material and the neutron star's magnetic field, and the physics of the strongly magnetized accretion column above the neutron star. In this proposal we ask for a 40 ks observation of the accreting HMXB 4U1538-522 to conduct the most sensitive study to date of the wide range of characteristics of the broad band (0.1-100 keV) spectrum over a quarter of a binary orbit and with pulse phase. When one considers the ~50% duty cycle of Suzaku observations, the proposed observation will yield coverage of a quarter of the binary orbit. | GALACTIC POINT SOURCES | 4 | A | RICHARD ROTHSCHILD | USA | 7 | AO7 | THE FIRST SUZAKU OBSERVATION OF 4U1538-522 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407068010/ | Quick Look | ![]() |
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46 | SWIFT J2319.4+2619 | 349.8819 | 26.2473 | 349.265885 | 25.973522 | 2.029717 | 27.934963 | 98.48369948 | -32.22425134 | 253.9963 | 56633.8796875 | 2013-12-07 21:06:45 | 56634.8786111111 | 2013-12-08 21:05:12 | 408030010 | 41.2758 | 40 | 41.2758 | 41.2758 | 0 | 41.2758 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 38.149 | 38.149 | 86.2879 | 2 | PROCESSED | 57613.5369328704 | 2016-08-13 12:53:11 | 57039 | 2015-01-17 00:00:00 | 56672.6300578704 | 2014-01-15 15:07:17 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081213 | Polars are a subclass of magnetic cataclysmic variables in which a strongly magnetic white dwarf accretes matter from a late-type, Roche-lobe filling mass donor. They are usually soft X-ray bright and hard X-ray dim, due to either buried shocks or strong cyclotron cooling, depending on system parameters. However, a small subset of polars have been detected as bright hard X-ray sources in INTEGRAL and Swift BAT surveys. As a part of an effort to understand the hard-to-soft X-ray luminosity ratios of polars in general, and specifically to understand what combination of parameters make some polars hard X-ray bright, we propose Suzaku observations of two poorly studied BAT polars, Swift J2319.4+2619 and IW Eri, supported by ground-based observations including optical polarimetry. | GALACTIC POINT SOURCES | 4 | C | KOJI MUKAI | USA | 8 | AO8 | THE HARD X-RAY BRIGHT POLARS SWIFT J2319.4+2619 AND IW ERI | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408030010/ | Quick Look | ![]() |
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47 | SERPENS X-1 | 279.9874 | 5.0445 | 279.370748 | 4.997683 | 281.283069 | 28.094693 | 36.12473115 | 4.84817413 | 93.4997 | 56729.1215277778 | 2014-03-13 02:55:00 | 56731.6459606482 | 2014-03-15 15:30:11 | 408033020 | 1.2154 | 120 | 6.5666 | 24.0772 | 0 | 1.2154 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82.3578 | 82.3578 | 218.0879 | 4 | PROCESSED | 57614.078912037 | 2016-08-14 01:53:38 | 57198 | 2015-06-25 00:00:00 | 56747.822037037 | 2014-03-31 19:43:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081222 | Much recent work has been focused on Fe K emission lines in neutron star low-mass X-ray binaries (LMXBs). Suzaku and XMM observations appear to have revealed asymmetric line profiles characteristic of relativistic effects present at the innermost accretion disk. However, the nature of these lines are still hotly debated, with recent work suggesting that pile-up can artificially broaden lines. In order to address this critical issue, we propose a 250 ks Suzaku observation of the NS LMXB, Ser X-1. The broadband capabilities of Suzaku will allow for a robust model of the continuum either side of the Fe K line, while all CCDs will be operated in fast clocking modes to achieve pile-up free spectra. This Suzaku observation will help settle the nature of broad Fe K emission lines in NS LMXBs. | GALACTIC POINT SOURCES | 4 | B | EDWARD CACKETT | USA | 8 | AO8 | THE NATURE OF BROAD FE KALPHA EMISSION LINES IN NEUTRON STAR LOW-MASS X-RAY BINARIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408033020/ | Quick Look | ![]() |
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48 | SERPENS X-1 | 279.9877 | 5.0424 | 279.371038 | 4.995582 | 281.28322 | 28.092576 | 36.12298663 | 4.84695852 | 81.3009 | 56757.3507060185 | 2014-04-10 08:25:01 | 56757.8959259259 | 2014-04-10 21:30:08 | 408033030 | 0.388 | 25 | 1.8071 | 6.4595 | 0 | 0.388 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 23.0266 | 23.0266 | 47.0979 | 0 | PROCESSED | 57614.2331481482 | 2016-08-14 05:35:44 | 57198 | 2015-06-25 00:00:00 | 56821.7352430556 | 2014-06-13 17:38:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081222 | Much recent work has been focused on Fe K emission lines in neutron star low-mass X-ray binaries (LMXBs). Suzaku and XMM observations appear to have revealed asymmetric line profiles characteristic of relativistic effects present at the innermost accretion disk. However, the nature of these lines are still hotly debated, with recent work suggesting that pile-up can artificially broaden lines. In order to address this critical issue, we propose a 250 ks Suzaku observation of the NS LMXB, Ser X-1. The broadband capabilities of Suzaku will allow for a robust model of the continuum either side of the Fe K line, while all CCDs will be operated in fast clocking modes to achieve pile-up free spectra. This Suzaku observation will help settle the nature of broad Fe K emission lines in NS LMXBs. | GALACTIC POINT SOURCES | 4 | B | EDWARD CACKETT | USA | 8 | AO8 | THE NATURE OF BROAD FE KALPHA EMISSION LINES IN NEUTRON STAR LOW-MASS X-RAY BINARIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408033030/ | Quick Look | ![]() |
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49 | ETA CARINAE | 161.2798 | -59.6805 | 160.793117 | -59.417138 | 202.155622 | -58.91379 | 287.60165846 | -0.62249687 | 316.5996 | 56857.6091435185 | 2014-07-19 14:37:10 | 56859.2363425926 | 2014-07-21 05:40:20 | 409026010 | 53.2665 | 45 | 53.2665 | 56.7325 | 0 | 56.7485 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.9866 | 28.9866 | 138.1737 | 0 | PROCESSED | 57615.4364814815 | 2016-08-15 10:28:32 | 57264 | 2015-08-30 00:00:00 | 56898.3302777778 | 2014-08-29 07:55:36 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091202 | Eta Carinae is an extremely massive binary system whose strong winds produce a variety of high-energy X-ray and possibly gamma-ray emission. Earlier XMM-Newton, Suzaku and INTEGRAL observations found interesting features in the extremely hard X-ray band: i) a flat spectral component above 9 keV toward the flux maximum; ii) strong 15-20 keV emission during an occultation of the wind-wind colliding plasma; iii) stable power-law emission above 25 keV. These features are signs of the highest energy processes yet detected in any colliding wind binary. Broad band X-ray observations around periastron are essential to understanding those features. We therefore propose Suzaku observations at 5 key phases around the next periastron passage of eta Carinae in 2014.6. | GALACTIC POINT SOURCES | 4 | A | KENJI HAMAGUCHI | USA | 9 | AO9 | PROBING THE HIGHEST ENERGY PHENOMENA OF ETA CARINAE AROUND PERIASTRON IN 2014 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409026010/ | Quick Look | ![]() |
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50 | M82 N2 | 148.2738 | 70.273 | 147.216273 | 70.508377 | 118.122269 | 52.466944 | 140.95732372 | 40.02876632 | 282.8972 | 57162.9827546296 | 2015-05-20 23:35:10 | 57164.434224537 | 2015-05-22 10:25:17 | 810043010 | 59.8084 | 60 | 59.8084 | 61.9021 | 0 | 61.9021 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 34.13 | 0 | PROCESSED | 57618.7218287037 | 2016-08-18 17:19:26 | 57548 | 2016-06-09 00:00:00 | 57177.3762847222 | 2015-06-04 09:01:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 101442 | We propose to carry out Suzaku observations of the starburst galaxy M82. We will search for X-ray emission from winds and shock heated clouds out to its possible outer boundary of ~45 kpc. We will also constrain the density and temperature profiles of the gas/wind emission out to large radii. These data can place important constraints on theoretical models of starburst galaxies and their environments. We will test models such as the Chevalier & Clegg adiabatic wind model, shocked clouds in a wind, etc. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KA-WAH WONG | USA | 10 | AO10 | SEARCH FOR THE OUTER BOUNDARY OF THE STARBURST GALAXY: M82 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/810043010/ | Quick Look | ![]() |
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51 | A1831 | 209.8007 | 27.9693 | 209.233208 | 28.211522 | 195.74505 | 37.218341 | 40.05378223 | 74.96810077 | 288.1207 | 53937.1181828704 | 2006-07-21 02:50:11 | 53937.5106481482 | 2006-07-21 12:15:20 | 801077010 | 18.0796 | 18 | 18.0796 | 18.0796 | 18.0796 | 18.0796 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17.0891 | 17.0891 | 33.8979 | 1 | PROCESSED | 57535.0011805556 | 2016-05-27 00:01:42 | 54401 | 2007-10-28 00:00:00 | 53943.553599537 | 2006-07-27 13:17:11 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801077010/ | Quick Look | ![]() |
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52 | VII ZW 403 | 172.0164 | 79.0077 | 171.163549 | 79.283023 | 114.484764 | 62.884943 | 127.82558857 | 37.31615306 | 108.8488 | 56627.0107638889 | 2013-12-01 00:15:30 | 56628.7884027778 | 2013-12-02 18:55:18 | 708039010 | 88.6616 | 87 | 88.6616 | 88.6616 | 0 | 88.6616 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 87.3974 | 87.3974 | 153.5578 | 1 | PROCESSED | 57613.4969328704 | 2016-08-13 11:55:35 | 57008 | 2014-12-17 00:00:00 | 56639.6396990741 | 2013-12-13 15:21:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081443 | The source of energetic photons that reionized the early universe remains uncertain. Recently, it has been proposed that X-ray binaries in early galaxies made a significant contribution to reionization. Early galaxies had low metallicity and the best local analogs are blue compact dwarf galaxies (BCDs) with low metallicity. We propose to observe two such galaxies known to be luminous in X-rays and accurately measure their spectra with the Suzaku XIS. These observations are important to our understanding of reionization and the formation of early galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | PHILIP KAARET | USA | 8 | AO8 | X-RAYS FROM LOW-METALLICITY BLUE COMPACT DWARF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708039010/ | Quick Look | ![]() |
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53 | 3C 390.3 | 280.4556 | 79.7798 | 281.326844 | 79.727189 | 82.097994 | 76.490616 | 111.44649344 | 27.08887917 | 37.561 | 56436.3002777778 | 2013-05-24 07:12:24 | 56438.6036921296 | 2013-05-26 14:29:19 | 708034010 | 100.3668 | 100 | 100.3668 | 100.3668 | 0 | 100.3668 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 109.3267 | 109.3267 | 198.9817 | 3 | PROCESSED | 57611.4065740741 | 2016-08-11 09:45:28 | 56816 | 2014-06-08 00:00:00 | 56449.7081365741 | 2013-06-06 16:59:43 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081431 | We propose simultaneous Suzaku (100 ks) and NuSTAR observations of the broad-line radio galaxy 3C 390.3, to measure Fe K-alpha emission and Compton reflection from the accretion disk. This is crucial for understanding the geometry of the accretion disk and its relation to the production of a powerful, relativistic radio jet. The combination of accurate Compton reflection parameters measured with NuSTAR and a simultaneous estimate of the accretion disk inner radius from Fe K-alpha with Suzaku will place strong constraints on accretion disk models for radio loud AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | PATRICK OGLE | USA | 8 | AO8 | ACCRETION AND BLACK HOLE SPIN IN THE POWERFUL, RADIO-LOUD AGN 3C 390.3 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708034010/ | Quick Look | ![]() |
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54 | NEP #4 | 270.0449 | 66.5788 | 270.046703 | 66.578557 | 56.874538 | 89.977746 | 96.40481628 | 29.79358389 | 165.3654 | 55193.4146875 | 2009-12-28 09:57:09 | 55194.4579166667 | 2009-12-29 10:59:24 | 504076010 | 49.8491 | 50 | 49.8571 | 49.8571 | 0 | 49.8491 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.5039 | 43.5039 | 90.114 | 0 | PROCESSED | 57550.0085648148 | 2016-06-11 00:12:20 | 54922 | 2009-04-01 00:00:00 | 55246.2930787037 | 2010-02-19 07:02:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | STEVEN SNOWDEN | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504076010/ | Quick Look | ![]() |
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55 | MRK 421 OFFSET | 165.3836 | 38.6302 | 164.685253 | 38.899103 | 150.412438 | 29.624722 | 179.31913311 | 64.35556561 | 121.9647 | 55146.4480092593 | 2009-11-11 10:45:08 | 55148.3176388889 | 2009-11-13 07:37:24 | 504087010 | 86.0144 | 75 | 86.0144 | 86.0144 | 0 | 86.0144 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64.8804 | 64.8804 | 161.5199 | 3 | PROCESSED | 57549.3389583333 | 2016-06-10 08:08:06 | 55531 | 2010-12-01 00:00:00 | 55160.2701041667 | 2009-11-25 06:28:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041324 | The OVII, OVIII, and NeIX absorption lines at z~0 have been discovered in the Chandra/XMM spectra of several bright AGNs, but the location of these absorptions has been debated since their discoveries. Here we request Suzaku observations of the soft X-ray background emission in the vicinity of Mrk 421, to conduct a joint analysis of the emission data with the extensive Chandra absorption data. This analysis will naturally yield an effective length of the absorbing/emitting gas. We have performed pilot studies and obtained a scale length of several kpc for the hot absorbing/emitting gas toward LMC X-3 and Mrk 421. The requested Suzaku observations are particular important to check these results and to further test the models we have developed in our study. | GALACTIC DIFFUSE EMISSION | 5 | B | YANGSEN YAO | USA | 4 | AO4 | A JOINT X-RAY ABSORPTION AND EMISSION STUDY OF THE HOT GAS TOWARD MRK 421 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504087010/ | Quick Look | ![]() |
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56 | A1800 | 207.3618 | 28.0973 | 206.789109 | 28.345144 | 193.256107 | 36.394356 | 40.59651819 | 77.12066844 | 302.3644 | 53936.635625 | 2006-07-20 15:15:18 | 53937.1140509259 | 2006-07-21 02:44:14 | 801078010 | 20.0437 | 17 | 20.0473 | 20.0553 | 20.0553 | 20.0437 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 19.0003 | 19.0003 | 41.3319 | 0 | PROCESSED | 57535.0036458333 | 2016-05-27 00:05:15 | 54401 | 2007-10-28 00:00:00 | 53943.5299652778 | 2006-07-27 12:43:09 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801078010/ | Quick Look | ![]() |
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57 | GX 301-2 | 186.689 | -62.7212 | 185.98909 | -62.444416 | 221.478022 | -52.575765 | 300.10817936 | 0.01514837 | 109.0098 | 54836.4396296296 | 2009-01-05 10:33:04 | 54838.0419328704 | 2009-01-07 01:00:23 | 403044020 | 61.8136 | 50 | 61.8136 | 61.8136 | 0 | 61.8136 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54.9922 | 54.9922 | 138.3981 | 2 | PROCESSED | 57545.1371064815 | 2016-06-06 03:17:26 | 55328 | 2010-05-12 00:00:00 | 54851.4303125 | 2009-01-20 10:19:39 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031152 | We propose the first observation of the bright neutron star GX 301-2 with Suzaku. The aim of the proposed 60 ks observation is a study of the broadband spectrum of the source in unprecedented detail and quality. This will allow us to analyze the structure (including density and clumpiness) of the intense wind of the optical companion and the gas stream flowing from Wray 977 to the neutron star. Spectral data will be used to study the evolution of nH and the iron line with very high time resolution. Furthermore, we will perform phase resolved spectroscopy to study the spectral variation of the cyclotron line with pulse phase. | GALACTIC POINT SOURCES | 4 | A | RICHARD ROTHSCHILD | USA | 3 | AO3 | BROAD-BAND STUDY OF GX 301-2 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403044020/ | Quick Look | ![]() |
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58 | GX 339-4 | 255.7095 | -48.7885 | 254.761689 | -48.717523 | 259.577896 | -25.861992 | 338.94163546 | -4.32765826 | 281.8009 | 54733.942650463 | 2008-09-24 22:37:25 | 54736.0968055556 | 2008-09-27 02:19:24 | 403067010 | 104.994 | 100 | 105.018 | 104.994 | 0 | 104.994 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 114.7759 | 114.7759 | 186.0917 | 2 | PROCESSED | 57544.0505092593 | 2016-06-05 01:12:44 | 55148 | 2009-11-13 00:00:00 | 54780.5803935185 | 2008-11-10 13:55:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031174 | Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with our multi-wavelength, radio to X-ray, program, Suzaku observations can constrain theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions. | GALACTIC POINT SOURCES | 4 | A | JOHN TOMSICK | USA | 3 | AO3-TOO | CONSTRAINING MODELS FOR BLACK HOLE ACCRETION IN THE HARD STATE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403067010/ | Quick Look | ![]() |
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59 | COMET_8P_TUTTLE-P1-5 | 28.1493 | 7.0036 | 27.492979 | 6.757378 | 28.646774 | -4.267305 | 148.58110255 | -52.79544349 | 248.5006 | 54470.7825810185 | 2008-01-05 18:46:55 | 54470.8487384259 | 2008-01-05 20:22:11 | 502062050 | 1.6746 | 2 | 1.6746 | 1.6746 | 0 | 1.6746 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1.703 | 1.703 | 5.6861 | 0 | PROCESSED | 57540.9980208333 | 2016-06-01 23:57:09 | 54908 | 2009-03-18 00:00:00 | 54542.2043055556 | 2008-03-17 04:54:12 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062050/ | Quick Look | ![]() |
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60 | COMET_8P_TUTTLE-P2_13 | 40.3641 | -37.3366 | 39.860845 | -37.549577 | 20.8839 | -49.581867 | 243.65335896 | -64.71445889 | 253.6857 | 54491.6297106482 | 2008-01-26 15:06:47 | 54491.762662037 | 2008-01-26 18:18:14 | 502063130 | 6.5907 | 6.7 | 6.6147 | 6.5987 | 0 | 6.5907 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 5.0221 | 5.0221 | 11.4799 | 0 | PROCESSED | 57541.4103356482 | 2016-06-02 09:50:53 | 54912 | 2009-03-22 00:00:00 | 54546.2204861111 | 2008-03-21 05:17:30 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063130/ | Quick Look | ![]() |
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61 | BULGE 2 | 270.6176 | -29.5847 | 269.818763 | -29.585758 | 270.530563 | -6.144879 | 1.30042786 | -3.49803376 | 83.2679 | 53801.7493981482 | 2006-03-07 17:59:08 | 53802.0689699074 | 2006-03-08 01:39:19 | 500002010 | 13.028 | 10 | 13.052 | 13.044 | 13.036 | 13.028 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 10.6741 | 10.6741 | 27.5999 | 1 | PROCESSED | 57533.1394444444 | 2016-05-25 03:20:48 | 54247 | 2007-05-27 00:00:00 | 54041.664525463 | 2006-11-02 15:56:55 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001014 | Leading . | GALACTIC DIFFUSE EMISSION | 5 | A | DAN MCCAMMON | JAP | 0 | SWG | THE SOFT GALACTIC BULGE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500002010/ | Quick Look | ![]() |
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62 | URSA MINOR | 227.2517 | 67.2307 | 227.099638 | 67.419875 | 158.023499 | 73.538029 | 104.9865755 | 44.80382561 | 40.7921 | 54195.7731944444 | 2007-04-05 18:33:24 | 54196.7557175926 | 2007-04-06 18:08:14 | 802052010 | 70.8823 | 67 | 70.8903 | 70.8823 | 0 | 70.8903 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 59.5872 | 59.5872 | 84.876 | 1 | PROCESSED | 57538.0737731482 | 2016-05-30 01:46:14 | 54695 | 2008-08-17 00:00:00 | 54203.3200462963 | 2007-04-13 07:40:52 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021405 | We propose 50 ksec Suzaku observations of the Ursa Minor and Draco dwarf spheroidal galaxies. These dense, dark-matter-dominated systems are carefully selected as the strongest potential sources of line emission from radiatively decaying keV dark matter of any astrophysical object. The low-level, stable Suzaku background makes it the most sensitive instrument to-date for this purpose. At the very least, constraints that enter a significant new regime are derived: non-detections are still of great importance. In the best case, the long sought-after identity of dark matter will be discovered, pointing the way to physics beyond the Standard Model. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MICHAEL LOEWENSTEIN | USA | 2 | AO2 | SEARCH FOR WARM DARK MATTER WITH SUZAKU OBSERVATIONS OF DWARF SPHEROIDAL GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802052010/ | Quick Look | ![]() |
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63 | BOOTES GROUP 1 | 218.7136 | 35.7235 | 218.197903 | 35.941461 | 200.235171 | 47.529275 | 60.71261374 | 66.41229506 | 153.2269 | 54440.1222106482 | 2007-12-06 02:55:59 | 54441.2015972222 | 2007-12-07 04:50:18 | 802054010 | 42.2242 | 38 | 42.2242 | 42.2242 | 0 | 42.2242 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.3023 | 41.3023 | 93.254 | 0 | PROCESSED | 57540.8293518518 | 2016-06-01 19:54:16 | 54815 | 2008-12-15 00:00:00 | 54448.2273842593 | 2007-12-14 05:27:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021424 | We propose four 30 ksec Suzaku pointings (120 ksec total) to obtain Lx and Tx for 4 distant (0.15 < z < 0.35) galaxy groups discovered in a contiguous, 9.3 sq. deg Chandra survey in Bootes. Our targets are spatially resolved by Chandra and are chosen to minimize point-source contamination of the Suzaku group spectra. The XIS data will significantly expand the sample of groups with known temperature in this redshift range, and so will improve constraints on group evolution mechanisms. We will use the existing, deep multicolor imaging and 20,000-object spectroscopic catalog for Bootes to study the effect of local environment on group properties, as well as the relationship between optically-selected and X-ray selected groups, for the first time in this redshift range. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MARSHALL BAUTZ | USA | 2 | AO2 | SUZAKU SPECTROSCOPY OF DISTANT GALAXY GROUPS IN BOOTES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802054010/ | Quick Look | ![]() |
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64 | A2665 | 357.7161 | 6.1352 | 357.076736 | 5.857083 | 0.350497 | 6.536022 | 96.94047732 | -53.65177278 | 245.9817 | 54078.2252893518 | 2006-12-09 05:24:25 | 54078.562037037 | 2006-12-09 13:29:20 | 801076010 | 13.944 | 15 | 13.944 | 13.944 | 0 | 13.944 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.6073 | 11.6073 | 29.0879 | 0 | PROCESSED | 57536.2715393518 | 2016-05-28 06:31:01 | 54695 | 2008-08-17 00:00:00 | 54089.271412037 | 2006-12-20 06:30:50 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801076010/ | Quick Look | ![]() |
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65 | PKS 1345+12 | 206.9131 | 12.3498 | 206.299989 | 12.598696 | 200.201065 | 21.844458 | 347.38894416 | 70.20282736 | 113.9421 | 54472.3082407407 | 2008-01-07 07:23:52 | 54473.6799768518 | 2008-01-08 16:19:10 | 702053010 | 52.9844 | 50 | 52.9844 | 52.9844 | 0 | 52.9844 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.2034 | 45.2034 | 118.5038 | 4 | PROCESSED | 57541.3141782407 | 2016-06-02 07:32:25 | 54854 | 2009-01-23 00:00:00 | 54483.4984375 | 2008-01-18 11:57:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021341 | We wish to take advantage of the sensitivity of Suzaku above 10 keV to constrain the energy source -- starburst or black-hole driven activity -- in three of the brightest warm transitional ultraluminous infrared galaxies, PKS 1345+12, Mrk 463, and 3C 273. These objects are arguably the best local laboratories to study the basic physical processes involved in creating massive early type hosts on the one hand, and feeding embedded supermassive black holes on the other hand, in major galaxy mergers. The Suzaku data will be used to search for the high-energy signature of deeply buried active black holes and to look for short time scale variability, another signature of black-hole driven activity. These data will be combined with our A01 spectra and be part of S. Teng's PhD thesis at UMD. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | SYLVAIN VEILLEUX | USA | 2 | AO2 | SPECTRA OF THE BRIGHTEST WARM ULTRALUMINOUS INFRARED GALAXIES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702053010/ | Quick Look | ![]() |
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66 | HD162020 | 267.6599 | -40.3316 | 266.783075 | -40.318096 | 268.125938 | -16.905511 | 350.72753331 | -6.73286722 | 269.5018 | 55820.4672453704 | 2011-09-16 11:12:50 | 55820.6918634259 | 2011-09-16 16:36:17 | 406038020 | 8.896 | 10 | 8.896 | 8.896 | 0 | 8.896 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.8519 | 7.8519 | 19.3999 | 0 | PROCESSED | 57603.1676851852 | 2016-08-03 04:01:28 | 56218 | 2012-10-18 00:00:00 | 55851.4444097222 | 2011-10-17 10:39:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061202 | Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. | GALACTIC POINT SOURCES | 4 | A | IGNAZIO PILLITTERI | USA | 6 | AO6 | STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406038020/ | Quick Look | ![]() |
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67 | ABELL 3571 | 206.8624 | -32.8524 | 206.14186 | -32.603207 | 216.960537 | -20.284209 | 316.31343933 | 28.55973438 | 103.8412 | 56666.0275 | 2014-01-09 00:39:36 | 56666.7772453704 | 2014-01-09 18:39:14 | 808094010 | 38.279 | 60 | 38.279 | 38.279 | 0 | 38.279 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.0047 | 39.0047 | 64.776 | 0 | PROCESSED | 57613.7763425926 | 2016-08-13 18:37:56 | 57096 | 2015-03-15 00:00:00 | 56730.4916435185 | 2014-03-14 11:47:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081531 | Abell 3571 is one of the brightest cluster in the X-ray sky and one of the main clusters in the Shapley supercluster. We have recently found evidence that it may be passing through a violent (~2000 km/s) merger in the line of sight (los). If corroborated it would be the closest template for the systems of this kind allowing us to study and characterize los mergers. We request a short observation of 60 ksec to corroborate the velocity gradients found with Chandra for this cluster, using the improved spectral resolution and gain stability of Suzaku s XISs. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | RENATO DUPKE | USA | 8 | AO8 | ABELL 3571. THE CLOSEST LINE OF SIGHT MERGER? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808094010/ | Quick Look | ![]() |
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68 | COMET_8P_TUTTLE-P2_16 | 40.5411 | -37.7213 | 40.040278 | -37.933718 | 20.796624 | -49.987507 | 244.42429467 | -64.47300408 | 253.9693 | 54492.0297106482 | 2008-01-27 00:42:47 | 54492.162662037 | 2008-01-27 03:54:14 | 502063160 | 3.7705 | 4 | 3.7705 | 3.7705 | 0 | 3.7705 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3.9881 | 3.9881 | 11.4799 | 0 | PROCESSED | 57541.4170833333 | 2016-06-02 10:00:36 | 54912 | 2009-03-22 00:00:00 | 54546.2311574074 | 2008-03-21 05:32:52 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063160/ | Quick Look | ![]() |
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69 | A3376 WEST RELIC | 90.0363 | -39.9917 | 89.629297 | -39.992531 | 90.071049 | -63.433501 | 246.43145562 | -26.38385089 | 126.3601 | 54034.3950231482 | 2006-10-26 09:28:50 | 54035.9176388889 | 2006-10-27 22:01:24 | 800011020 | 62.2648 | 60 | 62.2648 | 62.2648 | 62.2648 | 62.2648 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 55.5629 | 55.5629 | 131.5378 | 2 | PROCESSED | 57535.9705902778 | 2016-05-27 23:17:39 | 54694 | 2008-08-16 00:00:00 | 54090.2671643518 | 2006-12-21 06:24:43 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001039 | We propose a 150 ks observation of the giant radio relic in the west of the A3376 cluster. A3376 is a low temperature (4.5 keV) cluster with possible excess hard X-ray emission in 2.7 sigma significance by Beppo-SAX, and also with a pair of giant radio relics. This target is best suited for cluster hard excess survey with HXD. Following the first observation planned around October 2005 located near the east relic, the observation of the west relic 23 arcmin away can bring us the first spacial information on cluster excess hard X-rays. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAZUHIRO NAKAZAWA | JAP | 0 | SWG | SEARCH FOR EXCESS HARD X-RAY EMISSION FROM ABELL 3376 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800011020/ | Quick Look | ![]() |
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70 | AO 0235+164 | 39.665 | 16.613 | 38.972105 | 16.397631 | 42.455706 | 1.088366 | 156.77598662 | -39.11106084 | 252.4352 | 56310.722337963 | 2013-01-18 17:20:10 | 56311.7418634259 | 2013-01-19 17:48:17 | 707021010 | 43.1028 | 40 | 43.1108 | 43.1188 | 0 | 43.1028 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38.3583 | 38.3583 | 88.0698 | 0 | PROCESSED | 57608.5604166667 | 2016-08-08 13:27:00 | 56709 | 2014-02-21 00:00:00 | 56342.5387731482 | 2013-02-19 12:55:50 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071402 | We request observations of the variable blazar AO 0235+164, to be conducted simultaneously with Fermi and optical and radio telescopes, towards a multi-band campaign. This object has complex X-ray spectrum due to absorption by an intervening galaxy, and Suzaku will be essential in unraveling the effects and composition of that absorber, and for the first time, provide a robust measurement of the underlying blazar X-ray continuum, which, together with the Swift UVOT spectrum, will allow to verify the signature of the bulk-Compton component, due to cold electrons propagating in the relativistic jet. At the highest priority, we request 40 ks for a precise spectral measurement; at a lower priority, we wish to monitor the source for the total of 5 days, with the request of additional 160 ks. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GRZEGORZ MADEJSKI | USA | 7 | AO7 | SUZAKU OBSERVATIONS OF THE GAMMA-RAY BLAZAR AO 0235+164 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707021010/ | Quick Look | ![]() |
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71 | COMET_8P_TUTTLE-P1-8 | 28.3076 | 6.2429 | 27.652953 | 5.997039 | 28.526064 | -5.034788 | 149.32011202 | -53.43313536 | 248.4984 | 54470.9825 | 2008-01-05 23:34:48 | 54471.0487384259 | 2008-01-06 01:10:11 | 502062080 | 3.219 | 3.2 | 3.219 | 3.219 | 0 | 3.219 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3.374 | 3.374 | 5.664 | 0 | PROCESSED | 57541.0065046296 | 2016-06-02 00:09:22 | 54908 | 2009-03-18 00:00:00 | 54542.2264583333 | 2008-03-17 05:26:06 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062080/ | Quick Look | ![]() |
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72 | MARKARIAN 79 | 115.6357 | 49.8015 | 114.696355 | 49.919868 | 108.437878 | 27.988088 | 168.6115046 | 28.38007803 | 283.4884 | 54193.9134953704 | 2007-04-03 21:55:26 | 54195.7655439815 | 2007-04-05 18:22:23 | 702044010 | 83.7038 | 82 | 83.7118 | 83.7038 | 0 | 83.7118 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82.1042 | 82.1042 | 160.0059 | 0 | PROCESSED | 57538.0894444444 | 2016-05-30 02:08:48 | 54695 | 2008-08-17 00:00:00 | 54203.4223842593 | 2007-04-13 10:08:14 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021313 | Recently, deep observations of a number of Seyfert AGN with XMM-Newton and Suzaku have established variable and relativistic iron lines as robust features in roughly half of all deep Seyfert spectra. In these sources, the spin of the black hole can be constrained directly through fits to the relativistic iron line. A sample of excellent spectra from well-chosen AGN will facilitate a better understanding of the innermost regime near to black holes, and make correlations with parameters like radio luminosity, star formation rate, and galaxy and black hole mass possible for the first time. We propose to obtain observations of 4 under-exposed Seyfert AGN with promising evidence for broad lines to robustly constrain their spin parameters. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | JON MILLER | USA | 2 | AO2 | REVEALING BLACK HOLE SPIN IN RELATIVISTIC SEYFERT AGN | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702044010/ | Quick Look | ![]() |
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73 | ERIDANUS HOLE | 67.1401 | -17.0746 | 66.578414 | -17.184035 | 61.759444 | -38.302767 | 213.43674881 | -39.09232011 | 64.2755 | 54311.0359606482 | 2007-07-30 00:51:47 | 54313.2161921296 | 2007-08-01 05:11:19 | 502076010 | 103.7523 | 100 | 103.7523 | 103.7523 | 0 | 103.7523 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92.2091 | 92.2091 | 188.3518 | 2 | PROCESSED | 57539.4003356482 | 2016-05-31 09:36:29 | 54710 | 2008-09-01 00:00:00 | 54340.7341898148 | 2007-08-28 17:37:14 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021224 | We propose a study of the X-ray Emission from the Local Bubble (LB) and the Galactic Halo pointing toward the neutral hydrogen cloud MBM20 and a nearby low hydrogen column density, high latitude line of sight (called the Eridanus Hole). MBM20 absorbs about 75% of the foreground emission in the keV energy band, while the Eridanus Hole absorbs only 8%. The shadow of the cloud will be used to study the energy distribution of the X-ray foreground in the energy range 0.4-2 keV, to separate O VII and O VIII lines and study the composition and evolution of the LB. The comparison with the spectrum from the Eridanus Hole will be used to estimate the background emission due to the galactic halo and extragalactic source. | GALACTIC DIFFUSE EMISSION | 5 | B | MASSIMILIANO GALEAZZI | USA | 2 | AO2 | STUDYING THE PROPERTIES OF THE LOCAL BUBBLE AND GALACTIC HALO TOWARD MBM20 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502076010/ | Quick Look | ![]() |
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74 | RCS212414-6325.8 | 321.0509 | -63.4275 | 320.054735 | -63.642547 | 299.532953 | -45.130077 | 330.62476764 | -40.84164156 | 79.2319 | 55691.4113541667 | 2011-05-10 09:52:21 | 55691.979375 | 2011-05-10 23:30:18 | 806082010 | 36.3224 | 35 | 36.3304 | 36.3304 | 0 | 36.3224 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.914 | 26.914 | 49.0679 | 1 | PROCESSED | 57602.0065046296 | 2016-08-02 00:09:22 | 56068 | 2012-05-21 00:00:00 | 55701.1927546296 | 2011-05-20 04:37:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061533 | Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 19 optically-selected clusters of galaxies, half at z~0.3 and half at z~0.8. Here we propose 6 additional observations in order to uniformly span a total redshift range of 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | AMALIA HICKS | USA | 6 | AO6 | AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806082010/ | Quick Look | ![]() |
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75 | GRB060105 | 297.6095 | 46.3384 | 297.227077 | 46.210211 | 319.460988 | 65.110067 | 80.2506255 | 9.98748628 | 191.1906 | 53740.5089351852 | 2006-01-05 12:12:52 | 53741.5002083333 | 2006-01-06 12:00:18 | 900001010 | 42.2208 | 40 | 42.2208 | 42.2208 | 42.2208 | 42.2208 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 37.718 | 37.718 | 85.6419 | 2 | PROCESSED | 57532.6415856482 | 2016-05-24 15:23:53 | 54247 | 2007-05-27 00:00:00 | 54039.776712963 | 2006-10-31 18:38:28 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001008 | (i) Early break in lightcurve of X-ray afterglows using HXD. Recent Swift/XRT observations reveal that early X-ray afterglows of GRB has flat portion with very shallow decay. It may suggest continuous energy input from the central engine. The transition from its phase to general afterglow may display hard-to-soft evolution reflecting the cooling frequency. Thus multi wavelength observation will provide a key to the physics of central engine activity. (ii) Emission lines in the afterglows. The confirmation of line existence should be a matter of great importance because there remains unanswered questions. Some data may indicate a prominent iron line but others seem to suggest significant lower energy lines instead without iron lines. | EXTRAGALACTIC COMPACT SOURCES | 9 | A | TOSHIO MURAKAMI | JAP | 0 | SWG-TOO | TOO OBSERVATIONS OF GAMMA-RAY BURSTS | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/900001010/ | Quick Look | ![]() |
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76 | AB DOR | 82.2835 | -65.427 | 82.246883 | -65.464502 | 16.282788 | -86.671062 | 275.26967334 | -33.00819219 | 154.6774 | 54060.0265277778 | 2006-11-21 00:38:12 | 54061.4586111111 | 2006-11-22 11:00:24 | 401031010 | 53.4517 | 80 | 53.4517 | 53.4597 | 0 | 53.4614 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.0334 | 48.0334 | 123.708 | 1 | PROCESSED | 57536.170462963 | 2016-05-28 04:05:28 | 54502 | 2008-02-06 00:00:00 | 54133.0222916667 | 2007-02-02 00:32:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011021 | We propose to observe the rapidly rotating star AB Doradus for 80 ks with Suzaku Our main goals are to detect non-thermal hard X-rays and fluorescent Fe at 6.4 keV with the HXD and the XIS during a stellar flare. Such a spectral feature can be induced by non-thermal electrons in the impulsive flare phase, or by X-rays of the very hot flare plasma. The hard X-ray detectors will be used to detect non-thermal bremsstrahlung expected when a beam of non-thermal electrons (typically observed in the radio) impacts the dense chromosphere. We will also study the coronal element composition and its temporal evolution during the flare. Finally, we will attempt coordination with the Australian Telescope to monitor the non-thermal electron population, without any timing constraint for Suzaku. | GALACTIC POINT SOURCES | 4 | B | MARC AUDARD | USA | 1 | AO1 | NON-THERMAL HARD X-RAYS AND FLUORESCENT FE IN STELLAR FLARES | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401031010/ | Quick Look | ![]() |
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77 | ABELL 1795 Far North | 207.223 | 26.9995 | 206.646903 | 27.247656 | 193.71055 | 35.352954 | 35.63943573 | 77.21561208 | 130.4264 | 53715.3208796296 | 2005-12-11 07:42:04 | 53715.9730092593 | 2005-12-11 23:21:08 | 800012030 | 30.6406 | 30 | 30.6486 | 30.6406 | 30.6639 | 30.6566 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 27.8833 | 27.8833 | 56.3379 | 1 | PROCESSED | 57532.4195833333 | 2016-05-24 10:04:12 | 54247 | 2007-05-27 00:00:00 | 54039.1003703704 | 2006-10-31 02:24:32 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001056 | We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MARK BAUTZ | JAP | 0 | SWG | TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800012030/ | Quick Look | ![]() |
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78 | RT CRU | 188.7055 | -64.6161 | 187.980233 | -64.340558 | 224.663135 | -53.421751 | 301.15157727 | -1.80180428 | 281.609 | 54283.5270023148 | 2007-07-02 12:38:53 | 54284.2433333333 | 2007-07-03 05:50:24 | 402040010 | 50.8806 | 50 | 50.8806 | 50.8806 | 0 | 50.8806 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.8506 | 42.8506 | 61.8879 | 0 | PROCESSED | 57539.0744328704 | 2016-05-31 01:47:11 | 54695 | 2008-08-17 00:00:00 | 54328.4668055556 | 2007-08-16 11:12:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021102 | Symbiotic stars are interacting binaries in which a white dwarf (WD) accretes from the wind of a red giant. Their X-ray emission is typically very soft. Recently, however, 4 symbiotics have been detected out to almost 100 keV. Suzaku observations of two of these sources revealed that the hard X-rays emanated from an extremely hot thermal plasma. One means of producing such hot gas is accretion onto a near Chandrasekhar-mass WD. We propose to use the unique capabilities of Suzaku to test this hypothesis. We will use broad-band X-ray spectral fitting to determine the temperature of the hot plasma, hard X-ray timing studies to search for or constrain rapid variations due to either magnetic or non-magnetic accretion, and Fe line diagnostics to investigate the role of scattering. | GALACTIC POINT SOURCES | 4 | B | JENNIFER SOKOLOSKI | USA | 2 | AO2 | ARE HARD X-RAY SYMBIOTICS PROGENITORS OF TYPE IA SUPERNOVAE? | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402040010/ | Quick Look | ![]() |
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79 | ASAS J002511+1217.2 | 6.2997 | 12.2847 | 5.652783 | 12.007819 | 10.667541 | 8.77612 | 112.91544003 | -50.07604687 | 234.9156 | 54841.6813773148 | 2009-01-10 16:21:11 | 54842.5468055556 | 2009-01-11 13:07:24 | 403039010 | 33.256 | 30 | 33.256 | 33.256 | 0 | 33.256 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29.873 | 29.873 | 74.752 | 1 | PROCESSED | 57545.1348726852 | 2016-06-06 03:14:13 | 55328 | 2010-05-12 00:00:00 | 54851.4143055556 | 2009-01-20 09:56:36 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031144 | Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose to continue our ongoing program to observe dwarf novae with secure, parallax-based distance estimates. | GALACTIC POINT SOURCES | 4 | C | KOJI MUKAI | USA | 3 | AO3 | BUILDING UP AND UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A CONTINUATION IN SUZAKU CYCLE 3 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403039010/ | Quick Look | ![]() |
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80 | IRAS 00182-7112 | 5.1458 | -70.9276 | 4.573856 | -71.205097 | 312.979414 | -61.496651 | 306.55074146 | -45.98323945 | 33.8687 | 56050.171087963 | 2012-05-03 04:06:22 | 56052.8759143518 | 2012-05-05 21:01:19 | 707036010 | 93.959 | 90 | 93.967 | 93.959 | 0 | 93.959 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86.5766 | 86.5766 | 233.6819 | 1 | PROCESSED | 57605.3998263889 | 2016-08-05 09:35:45 | 56435 | 2013-05-23 00:00:00 | 56068.6299537037 | 2012-05-21 15:07:08 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071441 | We propose to observe with the Hard X-ray Detector onboard Suzaku the two Ultraluminous Infrared Galaxies IRAS 00182-7112 and IRAS 12127-1412, both of which are known to harbour very luminous and highly obscured active galactic nuclei (AGN). An AGN reflection component arising from ionized gas is clearly identified at 2 10 keV: the detection of the direct AGN emission above 10 keV and the measure of the reflection efficiency would provide fundamental information on both the physical structure of Compton-thick AGN embedded in a nuclear starburst and their feedback on the surrounding environment. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | EMANUELE NARDINI | USA | 7 | AO7 | THE PHYSICAL STRUCTURE OF COMPTON-THICK AGN/ULIRGS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707036010/ | Quick Look | ![]() |
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81 | HD162020 | 267.6618 | -40.3275 | 266.785008 | -40.314005 | 268.127379 | -16.901388 | 350.73183598 | -6.73206134 | 259.9987 | 55824.6498958333 | 2011-09-20 15:35:51 | 55825.1632407407 | 2011-09-21 03:55:04 | 406037030 | 16.23 | 15 | 16.238 | 16.238 | 0 | 16.23 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.3784 | 13.3784 | 44.3459 | 1 | PROCESSED | 57603.1988078704 | 2016-08-03 04:46:17 | 56218 | 2012-10-18 00:00:00 | 55851.4474884259 | 2011-10-17 10:44:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061202 | Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. | GALACTIC POINT SOURCES | 4 | A | IGNAZIO PILLITTERI | USA | 6 | AO6 | STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406037030/ | Quick Look | ![]() |
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82 | J081618.99+482328.4 | 124.0768 | 48.3841 | 123.174595 | 48.53824 | 114.890427 | 27.844597 | 171.01809871 | 33.69777889 | 298.4793 | 54917.0925462963 | 2009-03-27 02:13:16 | 54919.0946643518 | 2009-03-29 02:16:19 | 703042010 | 90.9224 | 90 | 90.9224 | 90.9224 | 0 | 90.9224 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81.0739 | 81.0739 | 172.9637 | 2 | PROCESSED | 57545.9726736111 | 2016-06-06 23:20:39 | 55329 | 2010-05-13 00:00:00 | 54930.3718055556 | 2009-04-09 08:55:24 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031337 | We have discovered polar broad absorption-line quasars (BALQSOs) from their radio variabilities. We know their inclination angles. Our results derived from the archival Chandra data of one polar BALQSO indicate that the X-ray emissions are from the jet and the X-ray absorbing gas is located at tens of parsecs above the accretion disk corona. We want to confirm these results at high confidence level using better signal to noise ratio data from a big observatory, like SUZAKU. In addition, we propose to observe three more polar BALQSOs, which have wide range of radio/UV/X-ray properties. Our primary science goal of this proposal is to determine the radial distribution of the X-ray absorbing gas in 4 polar BALQSOs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | KAJAL GHOSH | USA | 3 | AO3 | PROBING THE INNER STRUCTURE OF AGNS USING THE POLAR BALQSOS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703042010/ | Quick Look | ![]() |
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83 | XTE J1946+274 | 296.4201 | 27.2906 | 295.90791 | 27.167842 | 305.811743 | 47.50074 | 63.14511565 | 1.35338176 | 267.925 | 55480.9086805556 | 2010-10-11 21:48:30 | 55482.2446064815 | 2010-10-13 05:52:14 | 405041010 | 50.7317 | 45 | 50.7317 | 50.7317 | 0 | 50.7317 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.5571 | 46.5571 | 115.3739 | 1 | PROCESSED | 57553.7260185185 | 2016-06-14 17:25:28 | 55867 | 2011-11-02 00:00:00 | 55491.1017476852 | 2010-10-22 02:26:31 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051231 | We propose to perform Target of Opportunity Observations of one accreting neutron star out of a sample of five in outburst during Suzaku's AO-5. The aim is to observe the source for 45 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) in this system and to constrain the broad band spectrum. | GALACTIC POINT SOURCES | 4 | A | KATJA POTTSCHMIDT | USA | 5 | AO5-TOO | CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405041010/ | Quick Look | ![]() |
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84 | A2495 | 342.5777 | 10.9124 | 341.95313 | 10.647232 | 348.269753 | 16.897696 | 81.20126485 | -41.9387619 | 237.1467 | 54061.4694097222 | 2006-11-22 11:15:57 | 54062.0787037037 | 2006-11-23 01:53:20 | 801080010 | 18.0313 | 18 | 18.0313 | 18.3673 | 0 | 18.1193 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.3891 | 16.3891 | 52.6339 | 3 | PROCESSED | 57536.1381365741 | 2016-05-28 03:18:55 | 54695 | 2008-08-17 00:00:00 | 54088.9563194444 | 2006-12-19 22:57:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801080010/ | Quick Look | ![]() |
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85 | BULGE 3 | 274.7046 | -31.4846 | 273.893726 | -31.505472 | 274.041648 | -8.109784 | 1.3002625 | -7.49777303 | 80.4025 | 53800.3437962963 | 2006-03-06 08:15:04 | 53801.7474421296 | 2006-03-07 17:56:19 | 500001010 | 51.8468 | 50 | 51.8548 | 51.8548 | 51.8548 | 51.8468 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 45.0783 | 45.0783 | 121.2459 | 0 | PROCESSED | 57533.1540972222 | 2016-05-25 03:41:54 | 54247 | 2007-05-27 00:00:00 | 54041.7128703704 | 2006-11-02 17:06:32 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001014 | Leading . | GALACTIC DIFFUSE EMISSION | 5 | A | DAN MCCAMMON | JAP | 0 | SWG | THE SOFT GALACTIC BULGE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500001010/ | Quick Look | ![]() |
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86 | SN1006 NW | 225.6364 | -41.8003 | 224.819551 | -41.604176 | 235.339658 | -23.546444 | 327.59294648 | 14.70833496 | 115.0008 | 53766.4881365741 | 2006-01-31 11:42:55 | 53767.55375 | 2006-02-01 13:17:24 | 500017010 | 53.0194 | 50 | 53.0194 | 53.0277 | 53.0273 | 53.0273 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 60.4123 | 60.4123 | 92.0679 | 0 | PROCESSED | 57532.8347685185 | 2016-05-24 20:02:04 | 54247 | 2007-05-27 00:00:00 | 54040.7669675926 | 2006-11-01 18:24:26 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001062 | We propose two Suzaku pointings of the Galactic supernova remnant (SNR) that exploded as a supernova in 1006. The main goal of the project is to use the XIS measure the abundances of low-Z elements in the ejecta. | GALACTIC DIFFUSE EMISSION | 5 | A | JOHN HUGHES | JAP | 0 | SWG | THE EJECTA IN SN1006 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500017010/ | Quick Look | ![]() |
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87 | FG25 | 234.9579 | 30.7058 | 234.452539 | 30.866616 | 221.876556 | 48.458584 | 48.772653 | 53.18955534 | 294.6599 | 56136.7541898148 | 2012-07-28 18:06:02 | 56137.0821875 | 2012-07-29 01:58:21 | 807049010 | 10.6393 | 10 | 10.6393 | 10.6393 | 0 | 10.6393 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.074 | 11.074 | 28.3281 | 0 | PROCESSED | 57606.6807523148 | 2016-08-06 16:20:17 | 56527 | 2013-08-23 00:00:00 | 56161.2376736111 | 2012-08-22 05:42:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071511 | Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ELENA D'ONGHIA | USA | 7 | AO7 | SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807049010/ | Quick Look | ![]() |
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88 | A 2218 OFFSETB | 249.9091 | 65.2119 | 249.835523 | 65.307656 | 180.044789 | 81.713752 | 96.37864193 | 38.09205953 | 233.3309 | 53670.1916319444 | 2005-10-27 04:35:57 | 53670.4620833333 | 2005-10-27 11:05:24 | 800020010 | 14.9215 | 15 | 14.9375 | 14.9335 | 14.9215 | 14.9415 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 14.1931 | 14.1931 | 23.3561 | 0 | PROCESSED | 57527.6596180556 | 2016-05-19 15:49:51 | 54247 | 2007-05-27 00:00:00 | 54036.8343981482 | 2006-10-28 20:01:32 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001096 | To confirm the presence of redshifted oxygen lines from the WHIM surrounding A2218, we propose observations of 2 positions. One is a 35 ksec pointing on A2218 to raise the photon statistics of the oxygen feature, and the other is a 15 ksec pointing at about 1 degree west of the cluster to know the amplitude of the intensity variation of the Galactic oxygen lines. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | TAKAYA OHASHI | JAP | 0 | SWG | SEARCH FOR OXYGEN LINES FROM WARM IGM | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800020010/ | Quick Look | ![]() |
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89 | SMC X-1 | 19.2828 | -73.4495 | 18.951598 | -73.712645 | 312.330174 | -66.477022 | 300.41169288 | -43.55280074 | 39.2778 | 55706.0851851852 | 2011-05-25 02:02:40 | 55706.6745833333 | 2011-05-25 16:11:24 | 706030050 | 17.8463 | 18 | 17.8463 | 18.1823 | 0 | 18.1001 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 16.6829 | 16.6829 | 50.9139 | 0 | PROCESSED | 57602.111099537 | 2016-08-02 02:39:59 | 56092 | 2012-06-14 00:00:00 | 55725.1651736111 | 2011-06-13 03:57:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JOSEPH NEILSEN | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030050/ | Quick Look | ![]() |
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90 | COMA NW5 | 194.3037 | 29.1454 | 193.700799 | 29.41548 | 180.283789 | 32.183117 | 91.00313756 | 87.61452721 | 319.9965 | 55733.4693865741 | 2011-06-21 11:15:55 | 55734.0682407407 | 2011-06-22 01:38:16 | 806042010 | 21.0972 | 20 | 21.1201 | 21.1132 | 0 | 21.0972 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.4401 | 20.4401 | 51.724 | 0 | PROCESSED | 57602.3799537037 | 2016-08-02 09:07:08 | 55652 | 2011-04-01 00:00:00 | 55768.342025463 | 2011-07-26 08:12:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806042010/ | Quick Look | ![]() |
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91 | COMA SW5.5 | 193.6448 | 27.0863 | 193.037174 | 27.357142 | 180.762937 | 30.083449 | 29.67661506 | 89.29968791 | 314.5983 | 55735.866400463 | 2011-06-23 20:47:37 | 55736.3037037037 | 2011-06-24 07:17:20 | 806048010 | 15.2345 | 15 | 15.245 | 15.2345 | 0 | 15.2345 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.4375 | 16.4375 | 37.776 | 0 | PROCESSED | 57602.4025347222 | 2016-08-02 09:39:39 | 55652 | 2011-04-01 00:00:00 | 55794.9965625 | 2011-08-21 23:55:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806048010/ | Quick Look | ![]() |
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92 | RXCJ0605 | 91.7111 | -35.2772 | 91.267409 | -35.26998 | 92.696732 | -58.702768 | 241.82465393 | -23.81756849 | 309.9841 | 55323.0313194444 | 2010-05-07 00:45:06 | 55323.8550810185 | 2010-05-07 20:31:19 | 805065030 | 42.4239 | 40 | 42.4319 | 42.4319 | 0 | 42.4239 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.146 | 39.146 | 71.1619 | 0 | PROCESSED | 57551.4298263889 | 2016-06-12 10:18:57 | 55287 | 2010-04-01 00:00:00 | 55341.5040393518 | 2010-05-25 12:05:49 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805065030/ | Quick Look | ![]() |
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93 | MRK 766 | 184.6154 | 29.8184 | 183.986779 | 30.095968 | 171.206094 | 28.943476 | 190.63186084 | 82.27243688 | 133.2599 | 54055.0242361111 | 2006-11-16 00:34:54 | 54057.363900463 | 2006-11-18 08:44:01 | 701035010 | 97.8693 | 150 | 98.1756 | 97.8693 | 0 | 98.1676 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 96.8931 | 96.8931 | 202.1299 | 2 | PROCESSED | 57536.189525463 | 2016-05-28 04:32:55 | 54800 | 2008-11-30 00:00:00 | 54132.8396990741 | 2007-02-01 20:09:10 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011328 | X-ray spectroscopy of Mkn 766 has revealed ionised Fe emission that varies with the continuum on 10 ks timescales: direct evidence for ionised reflection from the accretion disk. This bright NLSy1 also shows extreme spectral variability, with the low state being dominated by a hard, constant reflection component, probably from cool distant material. We propose to measure the spectrum above 10 keV; the hot component should vary with the continuum, the cold distant component should be constant, and we can measure their relative contributions to test the predictions of the lower-energy analysis. This source is complex and needs the high-energy spectrum from Suzaku: it seems likely that previous complex behavior of several Seyferts can be described by these components | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TRACEY TURNER | USA | 1 | AO1 | DECOMPOSITION OF SEYFERT SPECTRA: TRACKING THE INNER DISK IN MKN 766 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701035010/ | Quick Look | ![]() |
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94 | MRK 1 | 19.06 | 33.0289 | 18.361574 | 32.765252 | 30.564721 | 23.029207 | 128.90716196 | -29.55492804 | 249.7486 | 54111.5318171296 | 2007-01-11 12:45:49 | 54114.5836111111 | 2007-01-14 14:00:24 | 701047010 | 126.4441 | 120 | 126.4441 | 126.4441 | 0 | 126.4441 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 126.0122 | 126.0122 | 263.6237 | 2 | PROCESSED | 57637.5831944445 | 2016-09-06 13:59:48 | 54702 | 2008-08-24 00:00:00 | 54133.1552314815 | 2007-02-02 03:43:32 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011336 | The supermassive black holes of active galactic nuclei (AGN) are fundamentally connected to the stars of their host galaxies, but it is not clear whether this relationship is evident at X-ray energies. We will test the prediction that prolific star formation is responsible for the soft X-ray emission from a Compton thick AGN that also contains a powerful circumnuclear starburst. The AGN's deep obscuration facilitates the soft X-ray measurements, and Compton thick AGN are generally significant, both as a large fraction of the local AGN population and for their contribution to the X-ray background. Furthermore, we will use the direct measurement of the intrinsic AGN luminosity to test unified AGN models and the validity of indirect luminosity indicators. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | NANCY LEVENSON | USA | 1 | AO1 | TESTING THE STARBURST-AGN CONNECTION AND MEASURING DEEPLY OBSCURED AGN | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701047010/ | Quick Look | ![]() |
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95 | CAS A | 350.8729 | 58.8094 | 350.30695 | 58.534812 | 27.388607 | 54.842749 | 111.74406014 | -2.13880346 | 214.7372 | 53768.5363657407 | 2006-02-02 12:52:22 | 53768.833599537 | 2006-02-02 20:00:23 | 100043010 | 0 | 10 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 10.3268 | 10.3268 | 25.6739 | 1 | PROCESSED | 57532.8451736111 | 2016-05-24 20:17:03 | 54247 | 2007-05-27 00:00:00 | 54040.7488888889 | 2006-11-01 17:58:24 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001097 | We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip | CALIBRATION | 1 | A | HIRONORI MATSUMOTO | JAP | 0 | SWG | XIS FLIGHT CAIBRATION PLAN | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100043010/ | Quick Look | ![]() |
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96 | NGC 1365 | 53.3976 | -36.1412 | 52.920229 | -36.30818 | 36.797911 | -53.03906 | 237.95777124 | -54.60123537 | 60.7695 | 55392.8956597222 | 2010-07-15 21:29:45 | 55399.3676273148 | 2010-07-22 08:49:23 | 705031020 | 302.1753 | 450 | 302.1753 | 302.1833 | 0 | 302.1833 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 251.0612 | 251.0612 | 425.5339 | 2 | PROCESSED | 57552.8844791667 | 2016-06-13 21:13:39 | 55287 | 2010-04-01 00:00:00 | 55413.8216435185 | 2010-08-05 19:43:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051112 | We propose 3 observations (~4 days each) of the Seyfert galaxy NGC 1365, at 2-week intervals. We aim to use eclipses to unambiguously identify the broad Fe K line, examine variability of the HXD/PIN excess, and to search for changes in the physical properties of the ionized absorber in this bright, nearby AGN. Shorter observations of this galaxy with XMM-Newton, Chandra and Suzaku showcase several remarkable physical traits: (1) FeXXV and FeXXVI K-shell absorption lines (the highest s/n detection so far among AGN), (2) rapidly varying cold absorption, (3) a highly significant relativistic Fe K emission line, and (4) a factor ~4 excess flux at high energies. The proposed observations will provide legacy spectra for what is arguably the single most physically-revealing obscured AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | LAURA BRENNEMAN | USA | 5 | AO5 | A LONG LOOK AT NGC 1365: DISC TOMOGRAPHY, IONIZED ABSORPTION AND HIGH ENERGY EXCESS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705031020/ | Quick Look | ![]() |
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97 | ESO 511-G030 | 214.8456 | -26.6457 | 214.126189 | -26.416188 | 221.40386 | -12.022179 | 326.23004886 | 32.21661925 | 292.391 | 56156.7622337963 | 2012-08-17 18:17:37 | 56157.7960416667 | 2012-08-18 19:06:18 | 707023030 | 51.9172 | 270 | 51.9252 | 51.9252 | 0 | 51.9172 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 52.011 | 52.011 | 89.3158 | 3 | PROCESSED | 57606.8813194444 | 2016-08-06 21:09:06 | 56640 | 2013-12-14 00:00:00 | 56272.6998148148 | 2012-12-11 16:47:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071413 | The study of "bare" Seyfert 1 AGN is essential to measure the true properties of the inner regions of the accretion disk. The nearby Seyfert ESO 511-G30 is a prime candidate for fulfilling this role due to its broad Fe K component and lack of any intrinsic warm absorption. It is also one of the X-ray brightest bare Seyferts featured in the Swift 58 month BAT catalogue as yet unobserved with Suzaku. We propose a 270 ks Suzaku observation of ESO 511-G30 to unambiguously constrain the properties of the accretion disk and subsequently the black hole spin. In addition, the HXD data will allow us to measure the Compton reflection hump, while the excellent soft X-ray spectral resolution of XIS will allow the origin of the soft excess to be determined. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JAMES REEVES | USA | 7 | AO7 | MEASURING THE ACCRETION DISK AND BLACK HOLE PROPERTIES OF ESO 511-G30 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707023030/ | Quick Look | ![]() |
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98 | PUP A : INTERIOR | 125.5916 | -42.8951 | 125.161363 | -42.733897 | 147.106586 | -59.478577 | 260.333956 | -3.34905821 | 276.8883 | 53842.5813541667 | 2006-04-17 13:57:09 | 53842.9127199074 | 2006-04-17 21:54:19 | 501088010 | 20.2709 | 20 | 20.2924 | 20.2949 | 20.2789 | 20.2709 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 19.9519 | 19.9519 | 28.6239 | 0 | PROCESSED | 57533.5042476852 | 2016-05-25 12:06:07 | 54401 | 2007-10-28 00:00:00 | 53906.8948611111 | 2006-06-20 21:28:36 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011246 | We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present. | GALACTIC DIFFUSE EMISSION | 5 | A | UNA HWANG | USA | 1 | AO1 | MAPPING OXYGEN IN PUPPIS A | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501088010/ | Quick Look | ![]() |
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99 | OFF-FIELD2 | 312.2284 | -9.8925 | 311.551158 | -10.078408 | 311.903273 | 7.617962 | 37.42106637 | -30.55240738 | 73.668 | 56784.946724537 | 2014-05-07 22:43:17 | 56787.0627314815 | 2014-05-10 01:30:20 | 509043010 | 80.156 | 80 | 80.156 | 80.156 | 0 | 80.156 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69.6142 | 69.6142 | 182.8079 | 1 | PROCESSED | 57615.1427430556 | 2016-08-15 03:25:33 | 56748 | 2014-04-01 00:00:00 | 56861.5828240741 | 2014-07-23 13:59:16 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091321 | Our special vantage point in our Galaxy allows us to study the Galactic warm-hot halo along several sightlines and determine its physical properties. The combination of absorption and emission measurements provides a powerful tool in this regard. Instead of average emission and absorption measures used in previous studies, one immediate step forward would be to use emission measures close to absorption sightlines. With proposed observations we will determine emission measures close to five sightlines in which we have the most accurate absorption measurements with Chandra. This will break the degeneracy between density and path-length and robustly measure the extent and mass of the warm-hot halo, placing strongest constraints yet on the fraction of missing baryons in the warm-hot plasma. | GALACTIC DIFFUSE EMISSION | 5 | A | ANJALI GUPTA | USA | 9 | AO9 | CIRCUM-GALACTIC MEDIUM OF THE MILKY WAY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509043010/ | Quick Look | ![]() |
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100 | A 2218 CENTER | 249.0052 | 66.205 | 248.955095 | 66.304813 | 172.75657 | 81.615548 | 97.72589248 | 38.11630228 | 233.3294 | 53669.4904050926 | 2005-10-26 11:46:11 | 53670.1905555556 | 2005-10-27 04:34:24 | 800019010 | 31.9354 | 35 | 31.9434 | 31.9434 | 31.9354 | 31.9434 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 28.9371 | 28.9371 | 60.4879 | 1 | PROCESSED | 57527.6471990741 | 2016-05-19 15:31:58 | 54247 | 2007-05-27 00:00:00 | 54036.9596990741 | 2006-10-28 23:01:58 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001096 | To confirm the presence of redshifted oxygen lines from the WHIM surrounding A2218, we propose observations of 2 positions. One is a 35 ksec pointing on A2218 to raise the photon statistics of the oxygen feature, and the other is a 15 ksec pointing at about 1 degree west of the cluster to know the amplitude of the intensity variation of the Galactic oxygen lines. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | TAKAYA OHASHI | JAP | 0 | SWG | SEARCH FOR OXYGEN LINES FROM WARM IGM | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800019010/ | Quick Look | ![]() |
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101 | ABELL 2259 | 260.1834 | 27.7413 | 259.686949 | 27.789931 | 256.20097 | 50.711544 | 50.50845469 | 31.05916058 | 109.9997 | 57082.4117476852 | 2015-03-01 09:52:55 | 57083.6002199074 | 2015-03-02 14:24:19 | 809081020 | 42.5928 | 42.5 | 42.5928 | 43.0168 | 0 | 43.0568 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.687650463 | 2016-08-17 16:30:13 | 57465 | 2016-03-18 00:00:00 | 57097.407037037 | 2015-03-16 09:46:08 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091526 | Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but not many were studied for "regular" non-cool core clusters. We propose a 170 ks Suzaku observation of a regular non-cool core cluster Abell 2259. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KA-WAH WONG | USA | 9 | AO9 | REGULAR NON-COOL CORE GALAXY CLUSTER OUT TO THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809081020/ | Quick Look | ![]() |
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102 | SPT-CL J0000-5748 | 0.2511 | -57.8123 | 359.609856 | -58.090789 | 327.861661 | -51.025666 | 315.62746494 | -58.05556131 | 46.7517 | 55694.989849537 | 2011-05-13 23:45:23 | 55696.1169097222 | 2011-05-15 02:48:21 | 806074010 | 50.3986 | 50 | 50.3986 | 50.3986 | 0 | 50.3986 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.4563 | 42.4563 | 97.3498 | 0 | PROCESSED | 57602.0636921296 | 2016-08-02 01:31:43 | 56072 | 2012-05-25 00:00:00 | 55705.1979166667 | 2011-05-24 04:45:00 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061531 | We propose observations of four high-redshift galaxy clusters to constrain the metal enrichment history of the intra-cluster medium (ICM). The clusters, two at z ~ 1.0 and two at z ~ 0.75, are chosen from an initial mass-limited sample identified by the South Pole Telescope (SPT) cluster project, and they are among the most massive high-redshift clusters known. Chandra observations have verified the absence of point sources in these targets. The proposed Suzaku observations will increase the X-ray cluster counts by a factor of four, they will yield the most precise ICM abundance measurements at these redshifts to date, and they will provide a path-finder for future Suzaku studies of large, representative samples of high-redshift clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ERIC MILLER | USA | 6 | AO6 | THE METAL ABUNDANCE OF HIGH-REDSHIFT GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806074010/ | Quick Look | ![]() |
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103 | ETA CARINAE | 161.2306 | -59.7313 | 160.744613 | -59.468015 | 202.194654 | -58.966617 | 287.60339978 | -0.67900846 | 291.9998 | 54992.8234143518 | 2009-06-10 19:45:43 | 54994.2918865741 | 2009-06-12 07:00:19 | 404038010 | 51.2259 | 45 | 51.2259 | 51.2339 | 0 | 51.2339 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.1186 | 49.1186 | 126.8398 | 0 | PROCESSED | 57547.5667361111 | 2016-06-08 13:36:06 | 55378 | 2010-07-01 00:00:00 | 55006.2447569444 | 2009-06-24 05:52:27 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041204 | The collision of winds in the supermassive binary Eta Car produces hot plasma detectable by Suzaku to 40 keV. This emission provides key clues to the way extremely massive stars lose mass. We propose to observe this hard X-ray emission with Suzaku after the periastron passage in order to measure the intrinsic luminosity of the wind-wind shock to determine the density of the wind near the shock boundary, and to measure the absorbing column to indicate the density profile in the distorted wind of the primary star. In addition HXD observations will measure any excess emission up to energies of 40 keV to constrain the amount of particle acceleration in the shock by the first order Fermi process and to help resolve the discrepancy between published BeppoSAX and INTEGRAL measurements. | GALACTIC POINT SOURCES | 4 | A | KENJI HAMAGUCHI | USA | 4 | AO4 | HARD X-RAY EMISSION, PARTICLE ACCELERATION AND MASS LOSS FROM ETA CAR | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404038010/ | Quick Look | ![]() |
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104 | Z235 | 10.9622 | 24.4059 | 10.298374 | 24.132304 | 19.875378 | 18.073678 | 120.72614401 | -38.43334342 | 59.0539 | 53944.0060185185 | 2006-07-28 00:08:40 | 53944.6148032407 | 2006-07-28 14:45:19 | 801083010 | 20.0335 | 20 | 20.0415 | 20.0415 | 20.0415 | 20.0335 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 19.5263 | 19.5263 | 52.5899 | 1 | PROCESSED | 57535.0666782407 | 2016-05-27 01:36:01 | 54401 | 2007-10-28 00:00:00 | 53955.6800925926 | 2006-08-08 16:19:20 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801083010/ | Quick Look | ![]() |
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105 | CYGNUS X-1 | 299.5777 | 35.2112 | 299.107757 | 35.074782 | 313.651801 | 54.261993 | 71.33781217 | 3.08063246 | 52.2303 | 57169.4748148148 | 2015-05-27 11:23:44 | 57170.7827893518 | 2015-05-28 18:47:13 | 410018010 | 11.0177 | 50 | 11.0177 | 12.2057 | 0 | 11.7469 | 4 | 3 | 0 | 3 | 1 | 0 | 0 | 26.1315 | 26.1315 | 110.7598 | 0 | PROCESSED | 57618.8568171296 | 2016-08-18 20:33:49 | 57626 | 2016-08-26 00:00:00 | 57183.6630902778 | 2015-06-10 15:54:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 101725 | We propose to observe Cygnus X-1 with NuSTAR (for 30 ks) and Suzaku (for 50 ks) in any spectral state in order to measure the reflection component and constrain the properties of the inner accretion disk, including the location of the inner radius, the geometry of the hard X-ray source, and the inclination. Observations made in the first two years of the NuSTAR mission have raised the interesting possibility that the inner disk inclination may differ from the orbital inclination, and this could occur if the black hole spin is misaligned. The proposed NuSTAR/Suzaku observation would be at the orbital phase where absorption due to stellar wind material is at a minimum, providing a clean measurement of the iron line profile and a significant improvement over the existing observations. | GALACTIC POINT SOURCES | 4 | A | JOHN TOMSICK | USA | 10 | AO10 | THE INNER ACCRETION DISK AROUND THE RAPIDLY ROTATING BLACK HOLE IN CYGNUS X-1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/410018010/ | Quick Look | ![]() |
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106 | NGC 2992 | 146.4207 | -14.2696 | 145.81924 | -14.038457 | 154.003817 | -26.061971 | 249.65504756 | 28.81616071 | 88.7924 | 53693.8781597222 | 2005-11-19 21:04:33 | 53694.9759722222 | 2005-11-20 23:25:24 | 700005020 | 37.4935 | 120 | 37.6565 | 39.6915 | 37.4935 | 37.8205 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 33.8991 | 33.8991 | 94.8479 | 1 | PROCESSED | 57528.0334490741 | 2016-05-20 00:48:10 | 54247 | 2007-05-27 00:00:00 | 54037.7316087963 | 2006-10-29 17:33:31 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001013 | NGC 2992 is a nearby Seyfert 1.9 galaxy showing long-term (20 yrs) large amplitude (factor of 20) variability. This object showed switching between Compton-thick and -thin. Recent RXTE monitoring has shown that this object is highly variable on shorter time scales (2 weeks). We propose three Suzaku observations to monitor the variability of absorption column, broad band continuum shape, and Fe line intensity to understand the cause of the remarkable variability. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YUICHI TERASHIMA | JAP | 0 | SWG | THE SPECTRAL VARIABILITY IN NGC 2992: FE-LINE, REFLECTION, AND COMPTON-THIN/THICK SWITCHING | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700005020/ | Quick Look | ![]() |
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107 | SWIFTJ1010.1-5747 | 152.7309 | -57.8539 | 152.293849 | -57.606865 | 193.450641 | -60.897616 | 282.8705066 | -1.37559689 | 290.7012 | 53891.2175 | 2006-06-05 05:13:12 | 53891.5544560185 | 2006-06-05 13:18:25 | 401055010 | 19.1717 | 20 | 19.1717 | 19.1717 | 19.1717 | 19.1717 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17.8778 | 17.8778 | 29.0879 | 0 | PROCESSED | 57534.4906944444 | 2016-05-26 11:46:36 | 54401 | 2007-10-28 00:00:00 | 53926.1075347222 | 2006-07-10 02:34:51 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011132 | INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. | GALACTIC POINT SOURCES | 4 | A | RANDALL SMITH | USA | 1 | AO1 | HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401055010/ | Quick Look | ![]() |
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108 | A3376 WEST RELIC | 90.0415 | -39.9946 | 89.634521 | -39.995405 | 90.079962 | -63.436398 | 246.43569548 | -26.38071178 | 132.0018 | 53681.5938078704 | 2005-11-07 14:15:05 | 53684.7883912037 | 2005-11-10 18:55:17 | 800011010 | 126.9969 | 150 | 126.9969 | 127.1809 | 127.0769 | 127.0289 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 112.9113 | 112.9113 | 230.9397 | 3 | PROCESSED | 57528.0013541667 | 2016-05-20 00:01:57 | 54247 | 2007-05-27 00:00:00 | 54037.6050231482 | 2006-10-29 14:31:14 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001039 | We propose a 150 ks observation of the giant radio relic in the west of the A3376 cluster. A3376 is a low temperature (4.5 keV) cluster with possible excess hard X-ray emission in 2.7 sigma significance by Beppo-SAX, and also with a pair of giant radio relics. This target is best suited for cluster hard excess survey with HXD. Following the first observation planned around October 2005 located near the east relic, the observation of the west relic 23 arcmin away can bring us the first spacial information on cluster excess hard X-rays. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAZUHIRO NAKAZAWA | JAP | 0 | SWG | SEARCH FOR EXCESS HARD X-RAY EMISSION FROM ABELL 3376 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800011010/ | Quick Look | ![]() |
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109 | E0102-72 | 16.027 | -72.0223 | 15.622199 | -72.290248 | 314.64413 | -65.039289 | 301.54815221 | -45.07189388 | 294.0751 | 53768.8467592593 | 2006-02-02 20:19:20 | 53769.4065393518 | 2006-02-03 09:45:25 | 100044030 | 20.8277 | 20 | 20.8357 | 20.8437 | 20.8437 | 20.8277 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20.2688 | 20.2688 | 48.36 | 1 | PROCESSED | 57532.8615740741 | 2016-05-24 20:40:40 | 54247 | 2007-05-27 00:00:00 | 53905.6764351852 | 2006-06-19 16:14:04 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001097 | We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip | CALIBRATION | 1 | A | HIRONORI MATSUMOTO | JAP | 0 | SWG | XIS FLIGHT CAIBRATION PLAN | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100044030/ | Quick Look | ![]() |
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110 | ETA CARINAE | 161.248 | -59.6859 | 160.761598 | -59.422588 | 202.142 | -58.929196 | 287.58997588 | -0.63475906 | 156.124 | 53769.4163194444 | 2006-02-03 09:59:30 | 53769.9481944444 | 2006-02-03 22:45:24 | 100045010 | 21.3678 | 20 | 21.3678 | 21.3678 | 21.3678 | 21.3678 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 18.1458 | 18.1458 | 45.9459 | 1 | PROCESSED | 57532.9369907407 | 2016-05-24 22:29:16 | 54247 | 2007-05-27 00:00:00 | 54040.9846643518 | 2006-11-01 23:37:55 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001097 | We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip | CALIBRATION | 1 | A | HIRONORI MATSUMOTO | JAP | 0 | SWG | XIS FLIGHT CAIBRATION PLAN | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100045010/ | Quick Look | ![]() |
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111 | BULGE 6 | 282.6839 | -33.8925 | 281.860158 | -33.951684 | 280.687841 | -10.9215 | 1.99857856 | -14.59644221 | 88.3467 | 53802.7373032407 | 2006-03-08 17:41:43 | 53803.0466087963 | 2006-03-09 01:07:07 | 500003010 | 14.2617 | 10 | 14.2617 | 14.2617 | 14.2617 | 14.2617 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 11.414 | 11.414 | 26.7159 | 1 | PROCESSED | 57533.1570833333 | 2016-05-25 03:46:12 | 54247 | 2007-05-27 00:00:00 | 54041.7424305556 | 2006-11-02 17:49:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001014 | Leading . | GALACTIC DIFFUSE EMISSION | 5 | A | DAN MCCAMMON | JAP | 0 | SWG | THE SOFT GALACTIC BULGE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500003010/ | Quick Look | ![]() |
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112 | X1630-472 | 248.4772 | -47.3405 | 247.556757 | -47.236251 | 254.058584 | -25.081993 | 336.93627828 | 0.30053306 | 75.5959 | 53794.9708333333 | 2006-02-28 23:18:00 | 53795.6968055556 | 2006-03-01 16:43:24 | 400010030 | 21.5216 | 200 | 21.5216 | 21.5216 | 21.5216 | 21.5216 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 19.0328 | 19.0328 | 62.718 | 0 | PROCESSED | 57533.1079050926 | 2016-05-25 02:35:23 | 54247 | 2007-05-27 00:00:00 | 54041.5956018518 | 2006-11-02 14:17:40 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001058 | We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active. | GALACTIC POINT SOURCES | 4 | A | JEAN COTTAM | JAP | 0 | SWG-TOO | FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400010030/ | Quick Look | ![]() |
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113 | JUPITER | 226.5948 | -16.1928 | 225.896045 | -16.000249 | 228.688969 | 1.24261 | 343.98613419 | 35.70433361 | 118.4906 | 53791.7941319445 | 2006-02-25 19:03:33 | 53792.7940277778 | 2006-02-26 19:03:24 | 401001020 | 37.704 | 36 | 37.704 | 37.704 | 37.704 | 37.704 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 32.7781 | 32.7781 | 86.36 | 1 | PROCESSED | 57533.0943981482 | 2016-05-25 02:15:56 | 54401 | 2007-10-28 00:00:00 | 53905.5035416667 | 2006-06-19 12:05:06 | 3.0.22.43 | 6 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011003 | We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure. | GALACTIC POINT SOURCES | 4 | C | RONALD ELSNER | USA | 1 | AO1 | JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401001020/ | Quick Look | ![]() |
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114 | SIGMA^2 CRB | 243.6552 | 33.7881 | 243.181435 | 33.91264 | 231.394365 | 53.752123 | 54.56402364 | 46.14689859 | 281.1207 | 53969.4764467593 | 2006-08-22 11:26:05 | 53972.1925231482 | 2006-08-25 04:37:14 | 401034010 | 109.1604 | 110 | 109.1904 | 109.1604 | 109.1684 | 109.1764 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 98.8376 | 98.8376 | 234.6539 | 3 | PROCESSED | 57535.3877777778 | 2016-05-27 09:18:24 | 54526 | 2008-03-01 00:00:00 | 54021.2578587963 | 2006-10-13 06:11:19 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011025 | Suzaku is a powerful instrument for studying the hot (>100 MK) coronal quiescent and flare emission from RS CVn binaries. We propose to obtain 110 ksec (3 day elapsed time) observations of the RS CVn systems Sigma^2 CrB (F6V + G0V) and Sigma Gem (K0III +?). Our goals are i) to better characterize their hard (> 10 keV) emission, ii) to understand the origin of coronal thermal and nonthermal plasma by studying the evolution of the coronal thermal structure, and iii) to investigate the persistent and flaring nonthermal electron population using a combination of X-ray and radio cm+mm continuum data. Such studies require the long duty cycle of Suzaku observations and its high sensitivity, particularly the greatly enhanced capability in the 10-25 keV region provided by HXD. | GALACTIC POINT SOURCES | 4 | B | ALEXANDER BROWN | USA | 1 | AO1 | SUZAKU OBSERVATIONS OF THERMAL AND NONTHERMAL CORONAL EMISSION ON THE RS CVN BINARIES SIGMA^2 CRB AND SIGMA GEM | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401034010/ | Quick Look | ![]() |
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115 | 4U 1820-30 | 275.9207 | -30.3623 | 275.117497 | -30.389079 | 275.135384 | -7.027059 | 2.78792233 | -7.91550172 | 265.9754 | 53992.9234606482 | 2006-09-14 22:09:47 | 53993.6605902778 | 2006-09-15 15:51:15 | 401047010 | 25.7008 | 37 | 25.7008 | 25.8109 | 25.7239 | 25.7148 | 2 | 1 | 2 | 2 | 1 | 0 | 0 | 31.8782 | 31.8782 | 63.6339 | 1 | PROCESSED | 57535.6012962963 | 2016-05-27 14:25:52 | 54526 | 2008-03-01 00:00:00 | 54021.2227083333 | 2006-10-13 05:20:42 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011113 | The potential well around low-magnetic field neutron stars is very similar to that around Schwarzschild black holes. Doppler shifts expected at the inner disk around such neutron stars should be very similar, and should produce relativistic FeK-alpha emission lines like those observed in some black hole systems. To date, however, relativistically broadened FeK-alpha emission lines have not been clearly detected in neutron star systems, in part because their lines are generally weaker than those found in black hole systems. We propose to observe the neutron star binaries 4U 1820-30, Cygnus X-2, and Serpens X-1 for 37 ksec each in Suzaku Cycle 1, to confirm possible evidence of relativistic broadening. Relativistic phenomena and accretion studies are central to NASA's ``SEU'' theme. | GALACTIC POINT SOURCES | 4 | B | JON MILLER | USA | 1 | AO1 | A SUZAKU STUDY OF BROAD IRON LINES IN NEUTRON STAR BINARIES | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401047010/ | Quick Look | ![]() |
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116 | 4U 1636-536 | 250.2259 | -53.7533 | 249.229501 | -53.656802 | 256.460315 | -31.236099 | 332.911352 | -4.8168543 | 100.7755 | 54188.4720717593 | 2007-03-29 11:19:47 | 54188.7856944445 | 2007-03-29 18:51:24 | 401050050 | 12.2418 | 38 | 12.2498 | 12.2418 | 0 | 12.2498 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 11.804 | 11.804 | 27.088 | 0 | PROCESSED | 57537.9973148148 | 2016-05-29 23:56:08 | 54695 | 2008-08-17 00:00:00 | 54200.4687731482 | 2007-04-10 11:15:02 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011117 | Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. | GALACTIC POINT SOURCES | 4 | A | JEROEN HOMAN | USA | 1 | AO1 | THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401050050/ | Quick Look | ![]() |
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117 | 4U1907+09 | 287.4013 | 9.8378 | 286.806482 | 9.755913 | 290.334973 | 32.058259 | 43.74739314 | 0.48531727 | 60.2599 | 53857.2580324074 | 2006-05-02 06:11:34 | 53858.7322222222 | 2006-05-03 17:34:24 | 401057010 | 58.4403 | 60 | 58.4403 | 58.4563 | 58.4483 | 58.4563 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 38.8215 | 38.8215 | 127.3539 | 1 | PROCESSED | 57533.6690509259 | 2016-05-25 16:03:26 | 54401 | 2007-10-28 00:00:00 | 53913.4367476852 | 2006-06-27 10:28:55 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011133 | We propose 60ksec of Suzaku observations of the high mass X-ray binary 4U1907+09, to study the little known spectrum of the source below 2keV and to measure its behavior during its frequent dips, where matter ceases to accrete onto the magnetic poles of the neutron star. Making use of Suzaku's unique broad band capabilities, we will also perform pulse phase spectroscopy of the cyclotron line and study the parameters of the fundamental and first harmonic cyclotron lines, as 4U1907+09 is one of the few accreting neutron stars where two cyclotron lines lie within the energy range of the XIS and HXD-PIN detectors. The scientific aims of this proposal address questions within NASA's Goals and Research Focus Area ``Structure and Evolution of the Universe''. | GALACTIC POINT SOURCES | 4 | A | KATJA POTTSCHMIDT | USA | 1 | AO1 | THE BROAD BAND SPECTRUM OF 4U1907+09 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401057010/ | Quick Look | ![]() |
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118 | BZ UMA | 133.4243 | 57.801 | 132.45894 | 57.99062 | 117.906758 | 38.491504 | 159.01672768 | 38.83001001 | 307.4767 | 54549.9926388889 | 2008-03-24 23:49:24 | 54550.4446064815 | 2008-03-25 10:40:14 | 402046010 | 29.7466 | 20 | 29.7546 | 29.7546 | 0 | 29.7466 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24.9212 | 24.9212 | 39.0459 | 0 | PROCESSED | 57541.9622106482 | 2016-06-02 23:05:35 | 54933 | 2009-04-12 00:00:00 | 54566.2225231482 | 2008-04-10 05:20:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021105 | Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose short Suzaku observations of dwarf novae with secure, parallax-based distance estimates that have not been the subject of pointed, imaging, X-ray observations in the 0.5-10 keV band. This will be an important check of potential biases in earlier studies. | GALACTIC POINT SOURCES | 4 | C | KOJI MUKAI | USA | 2 | AO2 | BUILDING UP AN UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A PARALLAX SELECTED SAMPLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402046010/ | Quick Look | ![]() |
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119 | 4U1705-44 | 257.2347 | -44.0965 | 256.331587 | -44.032824 | 260.198067 | -21.087901 | 343.32858118 | -2.34307771 | 294.8341 | 54381.763275463 | 2007-10-08 18:19:07 | 54382.2015509259 | 2007-10-09 04:50:14 | 402051020 | 21.9713 | 15 | 21.9793 | 21.981 | 0 | 21.9713 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15.688 | 15.688 | 37.856 | 1 | PROCESSED | 57540.198125 | 2016-06-01 04:45:18 | 54770 | 2008-10-31 00:00:00 | 54402.6586226852 | 2007-10-29 15:48:25 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021113 | We recently proposed a solution to the problem of model ambiguity for the spectra of atoll-type neutron stars. This work was performed on X-ray transient, and we need to test the model on the main population of persistent atolls. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. We propose to supplement the Suzaku monitoring archive begun in AO-1 by targeting the two persistent atolls with the greatest X-ray variability. | GALACTIC POINT SOURCES | 4 | A | RONALD REMILLARD | USA | 2 | AO2 | X-RAY SPECTRA OF ATOLL-TYPE NEUTRON STARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402051020/ | Quick Look | ![]() |
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120 | AQL X-1 | 287.8179 | 0.5789 | 287.179626 | 0.495179 | 289.378971 | 22.828716 | 35.71351779 | -4.14685757 | 277.9777 | 54376.9927777778 | 2007-10-03 23:49:36 | 54377.3516087963 | 2007-10-04 08:26:19 | 402053020 | 15.1326 | 15 | 15.1406 | 15.1423 | 0 | 15.1326 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.8908 | 11.8908 | 30.9999 | 1 | PROCESSED | 57540.1490277778 | 2016-06-01 03:34:36 | 54771 | 2008-11-01 00:00:00 | 54403.9157175926 | 2007-10-30 21:58:38 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021114 | We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. | GALACTIC POINT SOURCES | 4 | A | RONALD REMILLARD | USA | 2 | AO2-TOO | X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402053020/ | Quick Look | ![]() |
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121 | IGR J16207-5129 | 245.1891 | -51.5041 | 244.232474 | -51.385129 | 252.515963 | -29.556446 | 332.45561032 | -1.05025433 | 89.5006 | 54526.8661111111 | 2008-03-01 20:47:12 | 54527.7502199074 | 2008-03-02 18:00:19 | 402065020 | 32.6127 | 30 | 32.7095 | 32.7133 | 0 | 32.6127 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.3312 | 28.3312 | 76.3759 | 0 | PROCESSED | 57541.7496180556 | 2016-06-02 17:59:27 | 54901 | 2009-03-11 00:00:00 | 54535.208599537 | 2008-03-10 05:00:23 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021122 | We propose to observe 3 INTEGRAL-discovered High Mass X-ray Binaries (IGR HMXBs) to search for X-ray pulsations and to study their broadband spectra. Over the past few years, INTEGRAL has found a surprising number of HMXBs, and the large number of new, locally absorbed supergiant HMXBs indicate that these wind-accretors are more common than previously thought. In addition to high column densities, some of these systems have other extreme properties such as slowly rotating neutron stars (NSs) or rapid X-ray flares. For the systems we propose to observe, detection of pulsations is important for establishing the presence of a NS and for constraining the spin period distribution for HMXB NSs. As these are strong hard X-ray emitters, we will take advantage of Suzaku's broadband capabilities. | GALACTIC POINT SOURCES | 4 | B | JOHN TOMSICK | USA | 2 | AO2 | LOOKING FOR SIGNATURES OF HIGH MAGNETIC FIELD NEUTRON STARS IN INTEGRAL HMXBS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402065020/ | Quick Look | ![]() |
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122 | KT PER | 24.2933 | 50.9468 | 23.514247 | 50.69234 | 43.593687 | 37.546222 | 130.24865907 | -11.27406186 | 260.9001 | 54843.8957060185 | 2009-01-12 21:29:49 | 54844.5334953704 | 2009-01-13 12:48:14 | 403041010 | 29.1957 | 20 | 29.1957 | 29.1957 | 0 | 29.1957 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.1658 | 28.1658 | 55.0899 | 0 | PROCESSED | 57545.1649537037 | 2016-06-06 03:57:32 | 55328 | 2010-05-12 00:00:00 | 54854.0547916667 | 2009-01-23 01:18:54 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031144 | Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose to continue our ongoing program to observe dwarf novae with secure, parallax-based distance estimates. | GALACTIC POINT SOURCES | 4 | C | KOJI MUKAI | USA | 3 | AO3 | BUILDING UP AND UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A CONTINUATION IN SUZAKU CYCLE 3 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403041010/ | Quick Look | ![]() |
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123 | IGRJ16393-4643 | 249.7688 | -46.7009 | 248.852096 | -46.602507 | 254.906032 | -24.312906 | 338.00177501 | 0.07896045 | 111.6627 | 55267.9865740741 | 2010-03-12 23:40:40 | 55269.4508564815 | 2010-03-14 10:49:14 | 404056010 | 50.54 | 50 | 50.564 | 50.54 | 0 | 50.564 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.2565 | 42.2565 | 126.4678 | 1 | PROCESSED | 57550.8754166667 | 2016-06-11 21:00:36 | 55647 | 2011-03-27 00:00:00 | 55279.4686689815 | 2010-03-24 11:14:53 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041234 | Stellar winds play a critical role in several as yet poorly understood astrophysical processes. One of the best laboratories for studying winds is in wind fed Supergiant High Mass X-ray binaries. Using the neutron star (NS) as a backlight, variable absorption in X-rays measures column density variations in the secondary star wind. A recent explosion in the number of known HMXBs has defined two additional subclasses of HMXBs, potentially related through geometry and wind properties: 1) heavily obscured sources and 2) so-called Supergiant Fast X-ray Transients (SFXTs). We propose observations of 2 obscured sgHMXBs and 2 SFXTs to monitor the column density. This will test wind models and probe whether these subclasses are related to one another and to classical HMXBs through wind parameters. | GALACTIC POINT SOURCES | 4 | C | DAVID MORRIS | USA | 4 | AO4 | PROBING DONOR STAR WIND STRUCTURE IN HMXBS THROUGH VARIABLE ABSORPTION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404056010/ | Quick Look | ![]() |
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124 | LOCKMANHOLE | 163.4063 | 57.6108 | 162.636897 | 57.876997 | 137.149157 | 45.549363 | 148.98193179 | 53.14624927 | 119.611 | 53688.2372337963 | 2005-11-14 05:41:37 | 53689.8300694444 | 2005-11-15 19:55:18 | 100046010 | 76.9806 | 100 | 76.9806 | 77.0446 | 77.0126 | 77.0206 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 94.5107 | 94.5107 | 137.6079 | 3 | PROCESSED | 57528.0048148148 | 2016-05-20 00:06:56 | 54247 | 2007-05-27 00:00:00 | 54037.5889814815 | 2006-10-29 14:08:08 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001098 | We propose a 100 ks observation of LockmanHole with Suzaku. The main purpose is to obtain a template dataset of HXD background. | CALIBRATION | 1 | A | MOTOHIDE KOKUBUN | JAP | 0 | SWG | BACKGROUND ESTABLISHMENT OF HXD | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100046010/ | Quick Look | ![]() |
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125 | CH UMA | 151.7457 | 67.5324 | 150.779554 | 67.776446 | 122.251575 | 50.881841 | 142.91256562 | 42.65793237 | 289.9979 | 56048.5009490741 | 2012-05-01 12:01:22 | 56049.4815046296 | 2012-05-02 11:33:22 | 407043010 | 45.2045 | 40 | 45.2045 | 45.2045 | 0 | 45.2045 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.3751 | 43.3751 | 84.6981 | 0 | PROCESSED | 57605.3249652778 | 2016-08-05 07:47:57 | 56435 | 2013-05-23 00:00:00 | 56068.6246180556 | 2012-05-21 14:59:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071212 | The mass of an accreting white dwarf is a key parameter governing its X-ray emission. We expect that the higher the mass, the higher the temperature and luminosity. Existing data appear consistent with this expectation, given the considerable uncertainties usually associated with the white dwarf masses of individual systems. Here we propose Suzaku observations of 5 dwarf novae for which very high or very low white dwarf mass estimates have been published. These targets provide the best opportunity of further establishing the mass-temperature correlation. Moreover, if the mass estimates are reliable, these targets are of interest from evolutionary considerations - how did these systems form with such high/low mass white dwarfs, and what are their ultimate fates? | GALACTIC POINT SOURCES | 4 | A | KOJI MUKAI | USA | 7 | AO7 | DWARF NOVAE WITH EXTREME WHITE DWARF MASSES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407043010/ | Quick Look | ![]() |
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126 | A2572B | 349.6066 | 18.7294 | 348.98329 | 18.45586 | 358.210513 | 21.259827 | 94.21850787 | -38.90117923 | 59.1565 | 53922.7742939815 | 2006-07-06 18:34:59 | 53923.3002199074 | 2006-07-07 07:12:19 | 801073010 | 24.0595 | 21 | 24.0755 | 24.0595 | 24.0675 | 24.0755 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 21.4951 | 21.4951 | 45.3979 | 1 | PROCESSED | 57534.8583912037 | 2016-05-26 20:36:05 | 54401 | 2007-10-28 00:00:00 | 53930.6043055556 | 2006-07-14 14:30:12 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801073010/ | Quick Look | ![]() |
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127 | COMA W SHOCK1 | 194.1832 | 28.2738 | 193.578654 | 28.544023 | 180.637957 | 31.358455 | 77.58391557 | 88.36116739 | 275.406 | 56475.3084143518 | 2013-07-02 07:24:07 | 56475.66125 | 2013-07-02 15:52:12 | 808090010 | 16.692 | 15 | 16.692 | 16.716 | 0 | 16.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.638 | 13.638 | 30.4759 | 1 | PROCESSED | 57611.6582407407 | 2016-08-11 15:47:52 | 56897 | 2014-08-28 00:00:00 | 56524.6518518518 | 2013-08-20 15:38:40 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081529 | Our analysis of Suzaku data of the Coma Cluster revealed an intriguing correlation between the outer edge of its radio halo and the thermodynamic properties of the gas. This correlation seems to be the most pronounced in the western direction where the temperature drops from about 10keV in the annulus spanning 35'-41' to only 1.7keV in the annulus spanning 50'-60'. The Planck Collaboration found a marked local steepening of the radial gradient of the SZ signal at this location and interpret this feature as a shock with a Mach number of about 2. Unfortunately, we currently lack X-ray coverage towards the W in this critical range of 41'-50'. We therefore propose two additional pointings with a total exposure time of 30ks, that will allow us to resolve the temperature gradient in this region. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | AURORA SIMIONESCU | USA | 8 | AO8 | THE MISSING PUZZLE PIECE IN THE COMA SHOCK FRONT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808090010/ | Quick Look | ![]() |
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128 | AE AQUARII | 310.0612 | -0.931 | 309.416636 | -1.108991 | 312.236832 | 16.82972 | 45.23545862 | -24.46836188 | 250.6241 | 54033.2319907407 | 2006-10-25 05:34:04 | 54034.3829282407 | 2006-10-26 09:11:25 | 400001020 | 47.9743 | 50 | 47.9743 | 48.5956 | 48.1316 | 48.3103 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 45.5384 | 45.5384 | 99.4239 | 1 | PROCESSED | 57526.8238773148 | 2016-05-18 19:46:23 | 54526 | 2008-03-01 00:00:00 | 54109.7083449074 | 2007-01-09 17:00:01 | 3.0.22.43 | 9 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001004 | We have a new idea that a magnetized white dwarf can be a particle-acceleration cite to emit non thermal emission. In order to understand the particle acceleration process in rotation-powered objects, it is important to measure the hard X-ray emission from magnetized white dwarfs, in addition to that from well-known neutron stars. Here, we propose a 100ksec observation of a magnetic cataclysmic valiable, AE Aqurii. It is difficult for INTEGRAL mission, and is challenging even for the HXD, but it will be a ``first detection'' of the non-thermal emission in the hard X-ray band from a white dwarf with Suzaku. | GALACTIC POINT SOURCES | 4 | A | YUKIKATSU TERADA | JAP | 0 | SWG | SEARCH FOR THE NON-THERMAL EMISSION FROM MAGNETIZED WHITE DWARF WITH SUZAKU | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400001020/ | Quick Look | ![]() |
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129 | GX 349+2 | 256.4194 | -36.3657 | 255.579957 | -36.298328 | 258.779942 | -13.451385 | 349.14166441 | 2.79326977 | 78.9359 | 53813.9267708333 | 2006-03-19 22:14:33 | 53814.6043402778 | 2006-03-20 14:30:15 | 400003020 | 28.1177 | 50 | 28.1177 | 28.1317 | 28.1204 | 28.1204 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25.6573 | 25.6573 | 58.538 | 0 | PROCESSED | 57533.2767939815 | 2016-05-25 06:38:35 | 54247 | 2007-05-27 00:00:00 | 54042.1657407407 | 2006-11-03 03:58:40 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001026 | We propose Suzaku observations of two luminous low-mass X-ray binaries (Z sources), GX 349+2 and Cyg X-2, to investigate the origin of the hard tails of Z sources, of which the spectral photon indices are reported to become occasionally less than unity. With the high sensitivity of the HXD, we detect the spectral shape up to several 100 keV and reveal existence of particle acceleration caused by high radiation pressure. | GALACTIC POINT SOURCES | 4 | A | HIROMITSU TAKAHASHI | JAP | 0 | SWG | SUZAKU OBSERVATIONS OF THE HARD TAILS OF LUMINOUS LOW-MASS X-RAY BINARIES (Z SOURCES) | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400003020/ | Quick Look | ![]() |
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130 | IW ERIDANI | 66.4802 | -19.763 | 65.931423 | -19.87535 | 60.255555 | -40.808034 | 216.43667954 | -40.61449502 | 63.2719 | 56870.0005092593 | 2014-08-01 00:00:44 | 56870.9730902778 | 2014-08-01 23:21:15 | 409030010 | 39.4581 | 40 | 39.4581 | 39.8021 | 0 | 39.8341 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.4481134259 | 2016-08-16 10:45:17 | 57270 | 2015-09-05 00:00:00 | 56902.7186574074 | 2014-09-02 17:14:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091211 | Cataclysmic variables (CVs) detected in the INTEGRAL and Swift BAT hard X-ray surveys are predominantly magnetic systems of the intermediate polar subtype. However, as the survey sensitivity improves, an increasing number of polars are also detected as hard X-ray sources, even though the majority of polars are soft X-ray bright and hard X-ray faint. Over the long term, we hope to understand why most polars are soft X-ray dominated, and why a subset is hard X-ray bright. Here we propose Suzaku observations of four poorly studied BAT-detected polars, 1RXS J032540.0-081442, Swift J2319.4+2619, IW Eri, and IGR J14536-5522, supported by ground-based observations including optical polarimetry, to determine their system parameters. | GALACTIC POINT SOURCES | 4 | A | KOJI MUKAI | USA | 9 | AO9 | HARD X-RAY BRIGHT POLARS: WHY ARE THEY DIFFERENT? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409030010/ | Quick Look | ![]() |
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131 | XB1916-053 | 289.7007 | -5.2492 | 289.035593 | -5.341539 | 290.517676 | 16.79898 | 31.34828117 | -8.46968862 | 261.8039 | 56944.6811574074 | 2014-10-14 16:20:52 | 56948.5140740741 | 2014-10-18 12:20:16 | 409032010 | 155.8851 | 300 | 155.8851 | 155.8851 | 0 | 155.8851 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 8.7968 | 8.7968 | 19.7276 | 0 | PROCESSED | 57616.6949768518 | 2016-08-16 16:40:46 | 56748 | 2014-04-01 00:00:00 | 57017.41125 | 2014-12-26 09:52:12 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091221 | XB1916-053 is a prototypical dipping low mass X-ray binary (LMXB) with a dip recurrence period of 3000.6+-0.2s. However, extensive optical observations also show a longer stable period of 3027s. The former is most likely the orbital period, and the latter the superhump period caused by the precession of an elliptical accretion disk at a period of 3.9 days, representing the beat period between optical and X-ray periods. The morphology of the X-ray dips does indeed change dramatically over several days, but existing data suggest a somewhat longer period for the dip morphology cycle of 4.7 days. Here we propose a 300ks Suzaku observation of XB1916-053 with as few interruptions as possible, to conduct a definitive timing and spectroscopic study of its disk emission and dipping activity. | GALACTIC POINT SOURCES | 4 | B | ALAN SMALE | USA | 9 | AO9 | THE PRECESSING DISK IN THE DIPPING X-RAY BINARY XB1916-053 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409032010/ | Quick Look | ![]() |
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132 | SCT X-1 | 278.8598 | -7.62 | 278.182099 | -7.661259 | 279.107067 | 15.540876 | 24.33170335 | 0.06100641 | 260.9954 | 56952.1146412037 | 2014-10-22 02:45:05 | 56953.1389814815 | 2014-10-23 03:20:08 | 409033020 | 38.5811 | 34 | 38.5811 | 38.6687 | 0 | 38.6767 | 3 | 3 | 0 | 3 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6602314815 | 2016-08-16 15:50:44 | 57373 | 2015-12-17 00:00:00 | 57006.4003240741 | 2014-12-15 09:36:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091222 | We propose to observe the accreting 112s pulsar Scutum X-1 with Suzaku for 50ks. The optical companion is a late type giant or supergiant, making this a rare, persistent, non-OB-type wind accreting, Symbiotic X-ray Binary (SyXB). After initial flaring in the 1970s, the source generally exhibited low flux levels and has only rarely been observed. We will constrain the broadband spectrum, check for signs of wind accretion (variable absorption, log-normal count rate distribution), search for an iron fluorescence line, update the pulse period evolution, and compare to other Suzaku observations of SyXBs, especially to a quiescent observation of the prototype SyXB 4U 1954+31. | GALACTIC POINT SOURCES | 4 | A | KATJA POTTSCHMIDT | USA | 9 | AO9 | THE SYMBIOTIC X-RAY BINARY SCUTUM X-1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409033020/ | Quick Look | ![]() |
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133 | X1630-472 | 248.4828 | -47.3401 | 247.56235 | -47.235876 | 254.062648 | -25.080987 | 336.93914719 | 0.29801709 | 78.3341 | 53774.6318981482 | 2006-02-08 15:09:56 | 53775.1390972222 | 2006-02-09 03:20:18 | 400010010 | 22.1902 | 200 | 22.1902 | 22.1902 | 22.1902 | 22.1902 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 22.247 | 22.247 | 43.816 | 0 | PROCESSED | 57532.9380787037 | 2016-05-24 22:30:50 | 54247 | 2007-05-27 00:00:00 | 54040.9540856482 | 2006-11-01 22:53:53 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001058 | We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active. | GALACTIC POINT SOURCES | 4 | A | JEAN COTTAM | JAP | 0 | SWG-TOO | FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400010010/ | Quick Look | ![]() |
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134 | MRK 509 | 311.0374 | -10.7203 | 310.356339 | -10.901854 | 310.541946 | 7.132317 | 35.97290357 | -29.85106035 | 73.7532 | 57143.3705671296 | 2015-05-01 08:53:37 | 57144.6814930556 | 2015-05-02 16:21:21 | 410017010 | 54.2728 | 50 | 54.2757 | 54.2757 | 0 | 54.2728 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.0659722222 | 2016-08-18 01:35:00 | 57593 | 2016-07-24 00:00:00 | 57225.3881944445 | 2015-07-22 09:19:00 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 101708 | We propose combined Suzaku 50~ks and NuSTAR 200~ks observations of the bright Seyfert 1 galaxy Mrk~509 for the purpose of making a detailed study of the spectrum of radiation reflected from the accretion disk. Our chief aim is to constrain both the spin of the black hole and the properties of the corona that illuminates the disk. The combination of NuSTAR's high-sensitivity in the hard X-ray band, the soft-band coverage of Suzaku, and our state-of-the-art relativistic reflection models will allow us to break degeneracies between different scenarios currently proposed to explain the broadband spectrum of this exceptionally bright and much-studied source. | GALACTIC POINT SOURCES | 4 | A | JAVIER GARCIA | USA | 10 | AO10 | OBSERVING THE STRONG-FIELD REGION OF THE AGN IN MRK~509 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/410017010/ | Quick Look | ![]() |
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135 | 73P/SW3 | 279.6627 | 33.4734 | 279.203358 | 33.427762 | 284.650097 | 56.423756 | 62.35168426 | 17.03145652 | 46.5564 | 53862.4804282407 | 2006-05-07 11:31:49 | 53862.5419444444 | 2006-05-07 13:00:24 | 500012020 | 3.248 | 5 | 3.248 | 3.248 | 3.248 | 3.248 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.1119 | 2.1119 | 5.2799 | 0 | PROCESSED | 57533.7332407407 | 2016-05-25 17:35:52 | 54256 | 2007-06-05 00:00:00 | 54042.2282175926 | 2006-11-03 05:28:38 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500012020/ | Quick Look | ![]() |
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136 | 73P/SW3 | 316.717 | 24.6807 | 316.164001 | 24.478965 | 328.484877 | 39.12074 | 71.53645371 | -15.07849931 | 72.7087 | 53868.1752314815 | 2006-05-13 04:12:20 | 53868.2085532407 | 2006-05-13 05:00:19 | 500013010 | 2.353 | 20 | 2.353 | 2.353 | 2.353 | 2.353 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.595 | 2.595 | 2.8719 | 0 | PROCESSED | 57534.2831597222 | 2016-05-26 06:47:45 | 54256 | 2007-06-05 00:00:00 | 54042.2312268518 | 2006-11-03 05:32:58 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013010/ | Quick Look | ![]() |
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137 | 73P/SW3 | 317.1042 | 24.5187 | 316.549923 | 24.315676 | 328.827114 | 38.838912 | 71.64340536 | -15.45205291 | 72.7099 | 53868.2091666667 | 2006-05-13 05:01:12 | 53868.2752199074 | 2006-05-13 06:36:19 | 500013020 | 3.225 | 20 | 3.225 | 3.225 | 3.225 | 3.225 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3.467 | 3.467 | 5.7039 | 0 | PROCESSED | 57534.2879398148 | 2016-05-26 06:54:38 | 54256 | 2007-06-05 00:00:00 | 54042.2634027778 | 2006-11-03 06:19:18 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013020/ | Quick Look | ![]() |
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138 | 73P/SW3 | 319.1503 | 23.6322 | 318.589279 | 23.422515 | 330.602424 | 37.314629 | 72.21442919 | -17.44595626 | 72.7095 | 53868.5425 | 2006-05-13 13:01:12 | 53868.6085532407 | 2006-05-13 14:36:19 | 500013070 | 3.0624 | 20 | 3.0624 | 3.0624 | 3.0624 | 3.0624 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.088 | 2.088 | 5.688 | 1 | PROCESSED | 57534.3049074074 | 2016-05-26 07:19:04 | 54256 | 2007-06-05 00:00:00 | 54042.3037268518 | 2006-11-03 07:17:22 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013070/ | Quick Look | ![]() |
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139 | 73P/SW3 | 17.8447 | -9.1515 | 17.217751 | -9.416998 | 12.842123 | -15.443966 | 138.54867442 | -71.41609802 | 59.3994 | 53893.7363888889 | 2006-06-07 17:40:24 | 53893.8023032407 | 2006-06-07 19:15:19 | 500014020 | 3.2369 | 35 | 3.2369 | 3.2369 | 3.2369 | 3.2369 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.478 | 2.478 | 5.6879 | 0 | PROCESSED | 57534.5816435185 | 2016-05-26 13:57:34 | 54267 | 2007-06-16 00:00:00 | 54052.5079861111 | 2006-11-13 12:11:30 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014020/ | Quick Look | ![]() |
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140 | 73P/SW3 | 18.0085 | -9.2093 | 17.381763 | -9.474557 | 12.972897 | -15.560645 | 139.0853548 | -71.43220951 | 59.4015 | 53893.9358333333 | 2006-06-07 22:27:36 | 53894.0023032407 | 2006-06-08 00:03:19 | 500014050 | 3.235 | 35 | 3.235 | 3.235 | 3.235 | 3.235 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.5041 | 2.5041 | 5.7359 | 0 | PROCESSED | 57534.5878125 | 2016-05-26 14:06:27 | 54267 | 2007-06-16 00:00:00 | 54052.5317361111 | 2006-11-13 12:45:42 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014050/ | Quick Look | ![]() |
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141 | 73P/SW3 | 18.1094 | -9.2436 | 17.482792 | -9.508708 | 13.054019 | -15.631304 | 139.41528011 | -71.44015907 | 59.3996 | 53894.0691666667 | 2006-06-08 01:39:36 | 53894.1356365741 | 2006-06-08 03:15:19 | 500014070 | 2.2209 | 35 | 2.2209 | 2.2209 | 2.2209 | 2.2209 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1.939 | 1.939 | 5.7359 | 1 | PROCESSED | 57534.589849537 | 2016-05-26 14:09:23 | 54267 | 2007-06-16 00:00:00 | 54052.5472800926 | 2006-11-13 13:08:05 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014070/ | Quick Look | ![]() |
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142 | 73P/SW3 | 18.2503 | -9.299 | 17.623885 | -9.563897 | 13.164284 | -15.736856 | 139.88257526 | -71.45759255 | 59.3985 | 53894.2691435185 | 2006-06-08 06:27:34 | 53894.3356134259 | 2006-06-08 08:03:17 | 500014100 | 1.3121 | 35 | 1.3121 | 1.3121 | 1.3121 | 1.3121 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1.322 | 1.322 | 5.742 | 0 | PROCESSED | 57534.5960185185 | 2016-05-26 14:18:16 | 54267 | 2007-06-16 00:00:00 | 54052.5405324074 | 2006-11-13 12:58:22 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014100/ | Quick Look | ![]() |
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143 | 73P/SW3 | 18.435 | -9.3697 | 17.808837 | -9.63432 | 13.309685 | -15.873419 | 140.49459076 | -71.47695116 | 59.4003 | 53894.5358333333 | 2006-06-08 12:51:36 | 53894.6016087963 | 2006-06-08 14:26:19 | 500014140 | 1.977 | 35 | 1.977 | 1.977 | 1.977 | 1.977 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1.951 | 1.951 | 5.6719 | 0 | PROCESSED | 57534.60375 | 2016-05-26 14:29:24 | 54267 | 2007-06-16 00:00:00 | 54052.5450231482 | 2006-11-13 13:04:50 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014140/ | Quick Look | ![]() |
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144 | MBM12 | 44.0042 | 19.487 | 43.295962 | 19.285573 | 47.250431 | 2.610049 | 159.18888296 | -34.46916863 | 253.4644 | 53769.9600578704 | 2006-02-03 23:02:29 | 53772.6460416667 | 2006-02-06 15:30:18 | 500015010 | 102.9371 | 100 | 102.9371 | 102.9371 | 102.9371 | 102.9371 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 93.6709 | 93.6709 | 232.0499 | 1 | PROCESSED | 57532.9850694444 | 2016-05-24 23:38:30 | 54247 | 2007-05-27 00:00:00 | 54041.1327662037 | 2006-11-02 03:11:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001059 | Suzaku can potentially determine the time since the nearby supernova that created (or reheated) the Local Hot Bubble (LHB) by measuring the ratio of the O VII/O VIII lines emitted by the LHB. The LHB temperature is ~10^6 K, and in equilibrium we would expect no O VIII emission. However, the LHB is almost certainly not in equilibrium, and it is quite possible that significant O^{+7} is still recombining (and emitting O VIII) following its creation in the most recent local supernova 2-4 Myr ago. We propose to measure these lines from the LHB using the nearby molecular cloud MBM12 as a curtain to shadow more distant emission. Even if O VIII is not detected, the O VII measurement will be the first unambiguous measurement of a line from the LHB. | GALACTIC DIFFUSE EMISSION | 5 | A | RANDALL SMITH | JAP | 0 | SWG | DATING THE LOCAL HOT BUBBLE WITH SUZAKU | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500015010/ | Quick Look | ![]() |
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145 | CYGNUS LOOP NE4 | 313.5005 | 32.369 | 312.987812 | 32.178281 | 329.006135 | 47.302265 | 75.72495347 | -7.98937114 | 221.2023 | 53704.2368287037 | 2005-11-30 05:41:02 | 53704.7661342593 | 2005-11-30 18:23:14 | 500023010 | 25.0049 | 20 | 25.0049 | 25.2689 | 25.0067 | 25.0689 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25.1249 | 25.1249 | 45.726 | 1 | PROCESSED | 57532.3510763889 | 2016-05-24 08:25:33 | 54247 | 2007-05-27 00:00:00 | 54038.67625 | 2006-10-30 16:13:48 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001093 | We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 0 | SWG | CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500023010/ | Quick Look | ![]() |
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146 | G156.2+5.7NW | 74.223 | 52.4174 | 73.2357 | 52.339427 | 79.010107 | 29.577951 | 155.48379099 | 5.80912082 | 273.883 | 54147.6530902778 | 2007-02-16 15:40:27 | 54148.7558333333 | 2007-02-17 18:08:24 | 501075010 | 50.5468 | 50 | 50.5468 | 50.5468 | 0 | 50.5468 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.1958 | 46.1958 | 95.2599 | 0 | PROCESSED | 57537.3885763889 | 2016-05-29 09:19:33 | 54695 | 2008-08-17 00:00:00 | 54153.2775 | 2007-02-22 06:39:36 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011235 | G156.2+5.7 (RX J04591+5147) is thought to be a 26,000 yr old Type Ia remnant expanding in a low density medium. Ginga and ASCA observations reveal a hard emission component, interpreted as arising from shock-accelerated electrons, making this the oldest SNR in which shock acceleration has been found. Recent reanalysis of the ASCA data leaves ambiguity about the existence of this component. The importance of understanding the evolution of shock acceleration in SNRs makes vital confirming the existence of the hard component and localizing it. We propose 50 ks XIS observations of 3 locations to localize the hard component. Given its angular size, lack of small high contrast features, 0.4 keV thermal component with strong lines, and hard component, G156.2+5.7 is an ideal Suzaku target. | GALACTIC DIFFUSE EMISSION | 5 | C | ROBERT PETRE | USA | 1 | AO1 | A SEARCH FOR HARD X-RAY EMISSION FROM THE EVOLVED SNR G156.2+5.7 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501075010/ | Quick Look | ![]() |
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147 | SNR G93.3+6.9 CENTER | 312.9805 | 55.373 | 312.634427 | 55.183848 | 352.046818 | 66.979241 | 93.25121789 | 6.97467523 | 40.9208 | 53905.2215509259 | 2006-06-19 05:19:02 | 53905.6480787037 | 2006-06-19 15:33:14 | 501079010 | 20.5372 | 20 | 20.5452 | 20.5452 | 20.5452 | 20.5372 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20.008 | 20.008 | 36.8159 | 0 | PROCESSED | 57534.7200347222 | 2016-05-26 17:16:51 | 54401 | 2007-10-28 00:00:00 | 53926.792962963 | 2006-07-10 19:01:52 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011242 | The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. | GALACTIC DIFFUSE EMISSION | 5 | B | Q. DANIEL WANG | USA | 1 | AO1 | G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501079010/ | Quick Look | ![]() |
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148 | SNR G93.3+6.9 S1 | 313.1088 | 55.5284 | 312.76382 | 55.338789 | 352.457306 | 67.040407 | 93.41888838 | 7.01647125 | 40.6424 | 53905.6486458333 | 2006-06-19 15:34:03 | 53905.9696064815 | 2006-06-19 23:16:14 | 501080010 | 15.875 | 15 | 15.875 | 15.8902 | 15.891 | 15.883 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 12.7588 | 12.7588 | 27.7279 | 1 | PROCESSED | 57534.7111805556 | 2016-05-26 17:04:06 | 54401 | 2007-10-28 00:00:00 | 53926.199212963 | 2006-07-10 04:46:52 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011242 | The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. | GALACTIC DIFFUSE EMISSION | 5 | B | Q. DANIEL WANG | USA | 1 | AO1 | G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501080010/ | Quick Look | ![]() |
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149 | SNR G93.3+6.9 S4 | 312.7524 | 55.2472 | 312.406034 | 55.058863 | 351.58456 | 66.978212 | 93.07038921 | 6.99620044 | 39.4008 | 53906.7271296296 | 2006-06-20 17:27:04 | 53907.0550347222 | 2006-06-21 01:19:15 | 501083010 | 15.3662 | 15 | 15.3662 | 15.3662 | 15.3662 | 15.3662 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 14.4694 | 14.4694 | 28.3279 | 1 | PROCESSED | 57534.7341550926 | 2016-05-26 17:37:11 | 54401 | 2007-10-28 00:00:00 | 53926.117662037 | 2006-07-10 02:49:26 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011242 | The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. | GALACTIC DIFFUSE EMISSION | 5 | B | Q. DANIEL WANG | USA | 1 | AO1 | G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501083010/ | Quick Look | ![]() |
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150 | X1630-472 | 248.5405 | -47.3458 | 247.619879 | -47.241836 | 254.106265 | -25.080324 | 336.96147829 | 0.2654214 | 120.3 | 53817.4260300926 | 2006-03-23 10:13:29 | 53817.9313425926 | 2006-03-23 22:21:08 | 400010060 | 21.6541 | 200 | 21.6621 | 21.6541 | 21.6541 | 21.6541 | 2 | 1 | 2 | 2 | 1 | 0 | 0 | 22.7619 | 22.7619 | 43.6559 | 1 | PROCESSED | 57533.3033796296 | 2016-05-25 07:16:52 | 54247 | 2007-05-27 00:00:00 | 54042.1043287037 | 2006-11-03 02:30:14 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001058 | We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active. | GALACTIC POINT SOURCES | 4 | A | JEAN COTTAM | JAP | 0 | SWG-TOO | FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400010060/ | Quick Look | ![]() |
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151 | COMET_8P_TUTTLE-P1-9 | 28.3593 | 5.9969 | 27.705197 | 5.751157 | 28.487543 | -5.283181 | 149.56477648 | -53.63811023 | 248.4989 | 54471.0491666667 | 2008-01-06 01:10:48 | 54471.1154050926 | 2008-01-06 02:46:11 | 502062090 | 3.2186 | 3.2 | 3.2186 | 3.2186 | 0 | 3.2186 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2.439 | 2.439 | 5.664 | 0 | PROCESSED | 57541.0088425926 | 2016-06-02 00:12:44 | 54908 | 2009-03-18 00:00:00 | 54542.2348611111 | 2008-03-17 05:38:12 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062090/ | Quick Look | ![]() |
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152 | COMET_8P_TUTTLE-P1-11 | 28.4619 | 5.5053 | 27.808889 | 5.259792 | 28.409931 | -5.779338 | 150.05998726 | -54.04643055 | 248.5015 | 54471.1825 | 2008-01-06 04:22:48 | 54471.2487384259 | 2008-01-06 05:58:11 | 502062110 | 3.219 | 3.2 | 3.219 | 3.219 | 0 | 3.219 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2.0356 | 2.0356 | 5.688 | 0 | PROCESSED | 57541.2689699074 | 2016-06-02 06:27:19 | 54908 | 2009-03-18 00:00:00 | 54542.2871990741 | 2008-03-17 06:53:34 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062110/ | Quick Look | ![]() |
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153 | COMET_8P_TUTTLE-P1-12 | 28.5143 | 5.2526 | 27.861852 | 5.007213 | 28.369731 | -6.034275 | 150.31791041 | -54.25562458 | 248.4993 | 54471.2491666667 | 2008-01-06 05:58:48 | 54471.3154050926 | 2008-01-06 07:34:11 | 502062120 | 3.2196 | 3.2 | 3.2196 | 3.2196 | 0 | 3.2196 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2.162 | 2.162 | 5.696 | 0 | PROCESSED | 57541.268587963 | 2016-06-02 06:26:46 | 54908 | 2009-03-18 00:00:00 | 54542.261400463 | 2008-03-17 06:16:25 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062120/ | Quick Look | ![]() |
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154 | COMET_8P_TUTTLE-P2_03 | 39.7649 | -35.9737 | 39.253357 | -36.188553 | 21.195094 | -48.151161 | 240.80897167 | -65.5250468 | 257.7596 | 54490.2964351852 | 2008-01-25 07:06:52 | 54490.4293287037 | 2008-01-25 10:18:14 | 502063030 | 6.0389 | 6 | 6.0549 | 6.0389 | 0 | 6.0549 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 6.6011 | 6.6011 | 11.4639 | 0 | PROCESSED | 57541.3810532407 | 2016-06-02 09:08:43 | 54912 | 2009-03-22 00:00:00 | 54546.1040046296 | 2008-03-21 02:29:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063030/ | Quick Look | ![]() |
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155 | COMET_8P_TUTTLE-P2_04 | 39.8249 | -36.1145 | 39.31419 | -36.329166 | 21.162848 | -48.298537 | 241.11100541 | -65.44459708 | 257.8515 | 54490.4297106482 | 2008-01-25 10:18:47 | 54490.562662037 | 2008-01-25 13:30:14 | 502063040 | 6.6876 | 6.7 | 6.6876 | 6.7191 | 0 | 6.6876 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.3887 | 7.3887 | 11.4799 | 0 | PROCESSED | 57541.3859375 | 2016-06-02 09:15:45 | 54912 | 2009-03-22 00:00:00 | 54546.1129513889 | 2008-03-21 02:42:39 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063040/ | Quick Look | ![]() |
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156 | COMET_8P_TUTTLE-P2_05 | 39.8852 | -36.2545 | 39.375324 | -36.468978 | 21.131041 | -48.445251 | 241.40935004 | -65.36366996 | 257.9439 | 54490.5630439815 | 2008-01-25 13:30:47 | 54490.6959953704 | 2008-01-25 16:42:14 | 502063050 | 6.6974 | 6.7 | 6.6976 | 6.6976 | 0 | 6.6974 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6.1619 | 6.1619 | 11.4799 | 0 | PROCESSED | 57541.3887847222 | 2016-06-02 09:19:51 | 54912 | 2009-03-22 00:00:00 | 54546.126712963 | 2008-03-21 03:02:28 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063050/ | Quick Look | ![]() |
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157 | COMET_8P_TUTTLE-P2_10 | 40.1849 | -36.9375 | 39.679167 | -37.15104 | 20.975454 | -49.162155 | 242.83840601 | -64.95862507 | 253.4045 | 54491.2297106482 | 2008-01-26 05:30:47 | 54491.362662037 | 2008-01-26 08:42:14 | 502063100 | 5.7304 | 5 | 5.7384 | 5.7384 | 0 | 5.7304 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 6.2091 | 6.2091 | 11.4739 | 0 | PROCESSED | 57541.4028472222 | 2016-06-02 09:40:06 | 54912 | 2009-03-22 00:00:00 | 54546.1949884259 | 2008-03-21 04:40:47 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063100/ | Quick Look | ![]() |
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158 | COMET_8P_TUTTLE-P2_12 | 40.3045 | -37.2045 | 39.80042 | -37.417664 | 20.914316 | -49.442898 | 243.38522043 | -64.79583615 | 253.5926 | 54491.4963773148 | 2008-01-26 11:54:47 | 54491.6293287037 | 2008-01-26 15:06:14 | 502063120 | 6.6082 | 6.7 | 6.6082 | 6.6082 | 0 | 6.6242 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6.4698 | 6.4698 | 11.4799 | 0 | PROCESSED | 57541.4099884259 | 2016-06-02 09:50:23 | 54912 | 2009-03-22 00:00:00 | 54546.2619675926 | 2008-03-21 06:17:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063120/ | Quick Look | ![]() |
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159 | COMET_8P_TUTTLE-P2_14 | 40.423 | -37.4668 | 39.920562 | -37.679591 | 20.853678 | -49.718838 | 243.91615364 | -64.63380941 | 253.7796 | 54491.7630439815 | 2008-01-26 18:18:47 | 54491.8959953704 | 2008-01-26 21:30:14 | 502063140 | 6.5627 | 6.7 | 6.5627 | 6.5867 | 0 | 6.5627 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3.833 | 3.833 | 11.4799 | 0 | PROCESSED | 57541.4134143518 | 2016-06-02 09:55:19 | 54912 | 2009-03-22 00:00:00 | 54546.2568518518 | 2008-03-21 06:09:52 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063140/ | Quick Look | ![]() |
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160 | COMET_8P_TUTTLE-P2_15 | 40.4836 | -37.5961 | 39.981983 | -37.8087 | 20.825541 | -49.855587 | 244.17467378 | -64.55180166 | 253.8725 | 54491.8963773148 | 2008-01-26 21:30:47 | 54492.0293287037 | 2008-01-27 00:42:14 | 502063150 | 3.4717 | 4 | 3.4797 | 3.4717 | 0 | 3.4877 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2.3461 | 2.3461 | 11.4799 | 1 | PROCESSED | 57541.4238657407 | 2016-06-02 10:10:22 | 54912 | 2009-03-22 00:00:00 | 54546.2153587963 | 2008-03-21 05:10:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063150/ | Quick Look | ![]() |
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161 | G332.5-5.6 CENTER | 250.7335 | -54.5135 | 249.725841 | -54.419293 | 256.94436 | -31.940577 | 332.53119736 | -5.54004522 | 262.5079 | 54330.694224537 | 2007-08-18 16:39:41 | 54331.8731944444 | 2007-08-19 20:57:24 | 502066010 | 70.1488 | 80 | 70.1488 | 70.1488 | 0 | 70.1568 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 71.4907 | 71.4907 | 101.8399 | 0 | PROCESSED | 57539.62875 | 2016-05-31 15:05:24 | 54721 | 2008-09-12 00:00:00 | 54354.4910300926 | 2007-09-11 11:47:05 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021216 | We propose to observe G332.5-5.6, a puzzling supernova remnant with several unusual features: high radio polarization, central emission with bilaterally symmetric limbs, and evidence for enhanced nitrogen suggesting interaction with processed circumstellar material. Very little is known about G332.5-5.6, so our observations will provide information on the remnant shock speed, age, and evolutionary state; on the possible presence of nonthermal emission, either due to a pulsar in the center or to shock-accelerated electrons in the limbs; and on abundances, which might identify ejecta emission and allow the classification of the supernova. | GALACTIC DIFFUSE EMISSION | 5 | B | STEPHEN REYNOLDS | USA | 2 | AO2 | G332.5-5.6: AN UNUSUAL SUPERNOVA REMNANT WITH CIRCUMSTELLAR INTERACTION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502066010/ | Quick Look | ![]() |
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162 | B1920+10(1) | 293.0298 | 10.9618 | 292.438521 | 10.854204 | 297.004439 | 32.268855 | 47.34140504 | -3.87470613 | 252.2888 | 54772.350462963 | 2008-11-02 08:24:40 | 54774.137662037 | 2008-11-04 03:18:14 | 503090010 | 73.6033 | 70 | 73.6124 | 73.6033 | 0 | 73.6113 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 66.6682 | 66.6682 | 154.4039 | 3 | PROCESSED | 57544.3491550926 | 2016-06-05 08:22:47 | 55154 | 2009-11-19 00:00:00 | 54788.4472337963 | 2008-11-18 10:44:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031204 | A bow-shock pulsar wind nebula with an exceptionally long tail has been detected in X-ray observations of the pulsar PSR B1929+10. Recent observations suggest that such long structures may be associated with many other pulsars. Being the longest extended structures observed around Galactic compact objects. The physical processes responsible for the formation of such tails are not well understood, and the existing numerical models may only be valid at small distances from the pulsar. To determine the major factors governing the post-shock wind, we propose to observe the tail of PSR B1929+10, measure its full extent, map the surface brightness distribution, and perform spatially resolved spectroscopy. We will also measure the pulsar spectrum to study the properties of its polar caps. | GALACTIC DIFFUSE EMISSION | 5 | C | ZDENKA MISANOVIC | USA | 3 | AO3 | STUDYING THE LONG PULSAR TAIL OF THE PSR B1929+10 WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503090010/ | Quick Look | ![]() |
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163 | HESS J1023-575 | 155.5616 | -57.7533 | 155.104313 | -57.500238 | 195.408014 | -59.737737 | 284.06754503 | -0.45248582 | 284.3289 | 54617.1411458333 | 2008-05-31 03:23:15 | 54617.4515509259 | 2008-05-31 10:50:14 | 503092010 | 13.826 | 10 | 13.826 | 13.826 | 0 | 13.826 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.0573 | 11.0573 | 26.8159 | 1 | PROCESSED | 57542.6773842593 | 2016-06-03 16:15:26 | 54999 | 2009-06-17 00:00:00 | 54633.6961458333 | 2008-06-16 16:42:27 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031207 | We propose to search the neighborhood of two extended TeV sources to determine if there are X-ray sources that are potentially pulsar wind nebulae powering them. One source is near the colliding wind binary RCW 49, which has been suggested as the accelerator, and would therefore represent a new source class if there is no other plausible accelerator in the neighborhood. The other is a very bright source first detected by MILAGRO in the Galactic plane, which has been shown to be a large, extended source by HESS. While there is in each case a proposed X-ray counterpart, only a part of each nebula has been imaged in hard X-rays, and so it is unknown if there are other, more plausible counterparts. | GALACTIC DIFFUSE EMISSION | 5 | B | MALLORY ROBERTS | USA | 3 | AO3 | SEARCHING FOR X-RAY COUNTERPARTS OF TWO GALACTIC TEV SOURCES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503092010/ | Quick Look | ![]() |
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164 | GCL2 | 264.8888 | -28.9255 | 264.094972 | -28.898771 | 265.497098 | -5.564174 | 359.31035513 | 1.13376438 | 106.9569 | 54905.2789467593 | 2009-03-15 06:41:41 | 54905.9169444444 | 2009-03-15 22:00:24 | 503100010 | 25.7179 | 25 | 25.7179 | 25.7179 | 0 | 25.7179 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24.146 | 24.146 | 55.1199 | 1 | PROCESSED | 57545.8116666667 | 2016-06-06 19:28:48 | 55329 | 2010-05-13 00:00:00 | 54917.3744675926 | 2009-03-27 08:59:14 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031234 | We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity. | GALACTIC DIFFUSE EMISSION | 5 | B | FARHAD YUSEF-ZADEH | USA | 3 | AO3 | A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503100010/ | Quick Look | ![]() |
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165 | GCL3 | 265.2728 | -28.8569 | 264.479303 | -28.83203 | 265.832305 | -5.484097 | 359.5469331 | 0.88519 | 106.9023 | 54906.6133912037 | 2009-03-16 14:43:17 | 54907.3252777778 | 2009-03-17 07:48:24 | 503101010 | 33.8911 | 25 | 33.8991 | 33.8991 | 0 | 33.8911 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.8309 | 30.8309 | 61.4979 | 0 | PROCESSED | 57545.8349652778 | 2016-06-06 20:02:21 | 55329 | 2010-05-13 00:00:00 | 54917.3115393518 | 2009-03-27 07:28:37 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031234 | We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity. | GALACTIC DIFFUSE EMISSION | 5 | B | FARHAD YUSEF-ZADEH | USA | 3 | AO3 | A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503101010/ | Quick Look | ![]() |
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166 | NEP #2 | 270.0521 | 66.5655 | 270.053494 | 66.565223 | 19.553337 | 89.984047 | 96.38949161 | 29.79071779 | 194.6438 | 55172.5015162037 | 2009-12-07 12:02:11 | 55173.6411342593 | 2009-12-08 15:23:14 | 504072010 | 48.6977 | 50 | 48.6977 | 48.6977 | 0 | 48.6977 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38.4582 | 38.4582 | 98.456 | 1 | PROCESSED | 57549.730775463 | 2016-06-10 17:32:19 | 54922 | 2009-04-01 00:00:00 | 55190.01875 | 2009-12-25 00:27:00 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | STEVEN SNOWDEN | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504072010/ | Quick Look | ![]() |
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167 | HESS J1809-193A | 273.0012 | -19.0034 | 272.264617 | -19.016192 | 272.836277 | 4.407781 | 11.60922783 | -0.25253702 | 270.0939 | 55083.2051967593 | 2009-09-09 04:55:29 | 55084.4828009259 | 2009-09-10 11:35:14 | 504077010 | 52.1109 | 50 | 52.1745 | 52.1908 | 0 | 52.1109 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 44.109 | 44.109 | 110.376 | 1 | PROCESSED | 57548.5474189815 | 2016-06-09 13:08:17 | 55475 | 2010-10-06 00:00:00 | 55109.4207638889 | 2009-10-05 10:05:54 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041303 | We propose a detailed study of the extended VHE source HESS J1809-193 neighboring young PSR J1809-1917 with a known X-ray pulsar-wind nebula (PWN). As the chance coincidence is very unlikely, there should be a connection between the two. Furthermore, previous short Chandra observations of this field have revealed a large-scale asymmetric PWN extending toward the center of the TeV source. Thus, this is an excellent case for testing whether the unidentified TeV sources near young pulsars are, in fact, relic PWNe crushed by the asymmetric SNR reverse shock. We will probe the nature of the X-ray emission by measuring the surface brightness and spatially-resolved spectra across the large extent of the TeV source. Suzaku XIS is ideally suited for this purpose because of its low background. | GALACTIC DIFFUSE EMISSION | 5 | A | OLEG KARGALTSEV | USA | 4 | AO4 | CRUSHED PLERION HESS J1809-193: TEV TO X-RAY CONNECTION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504077010/ | Quick Look | ![]() |
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168 | G156.2+5.7 (S) | 74.9073 | 51.0204 | 73.935792 | 50.94566 | 79.297666 | 28.139899 | 156.85145441 | 5.28162006 | 265.6871 | 55259.9832407407 | 2010-03-04 23:35:52 | 55261.1495833333 | 2010-03-06 03:35:24 | 504080010 | 52.6413 | 50 | 52.6493 | 52.6413 | 0 | 52.6493 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.6566 | 47.6566 | 100.7578 | 0 | PROCESSED | 57550.7899189815 | 2016-06-11 18:57:29 | 55689 | 2011-05-08 00:00:00 | 55323.2891666667 | 2010-05-07 06:56:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041311 | The large Galactic (R=50') supernova remnant (SNR) G156.2+5.7 is one of the few evolved SNRs with possible X-ray non-thermal (hard-tail) emission. Based on our recent observations with the Suzaku XIS, we found an indication of correlation between the X-ray hard-tail emission and radio emission. In addition, we confirmed the existence of metal-rich ejecta in the central portion, but found no evidence of ejecta in the rim regions. To investigate the correlation between the X-ray hard-tail emission and the radio emission, and the distributions of the X-ray emitting ejecta in this SNR, we propose to extend our observations with the Suzaku XIS. We request three pointings with a total exposure time of 150 ks. | GALACTIC DIFFUSE EMISSION | 5 | C | SATORU KATSUDA | USA | 4 | AO4 | REVEALING X-RAY HARD-TAIL AND EJECTA STRUCTURES IN THE EVOLVED SNR G156.2+5.7 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504080010/ | Quick Look | ![]() |
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169 | 330.2+1.0 | 240.2338 | -51.5878 | 239.290441 | -51.447552 | 249.060918 | -30.286354 | 330.14022152 | 0.98429318 | 285.0004 | 55081.4851273148 | 2009-09-07 11:38:35 | 55082.1453472222 | 2009-09-08 03:29:18 | 504083020 | 30.8896 | 30 | 30.8896 | 30.8896 | 0 | 30.8971 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.0764 | 27.0764 | 57.0379 | 0 | PROCESSED | 57548.4451736111 | 2016-06-09 10:41:03 | 55458 | 2010-09-19 00:00:00 | 55092.1620949074 | 2009-09-18 03:53:25 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041312 | Observations of G330.2+1.0 have revealed that it is a rare supernova remnant whose X-ray emission is dominated by synchrotron radiation. The available X-ray data provides rather poor constraints on the physical properties of the remnant. We propose to perform a deep Suzaku observation to obtain good spectral data. Joint spectral analyses of Suzaku and radio data will enable us to accurately and precisely measure the synchrotron spectral index and cutoff frequency, the electron temperature, the emission measure, and, perhaps, the relative elemental abundances. As a result, it will be possible to compute accurate and precise values for the spectral index and maximum energy of the nonthermal electrons, the strength of the magnetic field, and the ambient density, age, and shock velocity. | GALACTIC DIFFUSE EMISSION | 5 | B | GLENN ALLEN | USA | 4 | AO4 | MULTIWAVELENGTH SPECTROSCOPY OF 330.2 1.0 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504083020/ | Quick Look | ![]() |
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170 | NGC 6888 | 302.9954 | 38.2382 | 302.538596 | 38.087534 | 320.045193 | 56.092572 | 75.36419968 | 2.38310331 | 253.873 | 55139.4126388889 | 2009-11-04 09:54:12 | 55141.3127777778 | 2009-11-06 07:30:24 | 504085010 | 77.349 | 75 | 77.461 | 77.349 | 0 | 77.461 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 62.1002 | 62.1002 | 164.1558 | 0 | PROCESSED | 57549.1334837963 | 2016-06-10 03:12:13 | 55518 | 2010-11-18 00:00:00 | 55152.1455671296 | 2009-11-17 03:29:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041321 | Fast winds from massive stars create large cavities in the surrounding interstellar medium filled with hot gas, known as Wind-Blown Bubbles (WBB). We propose to obtain XIS imaging spectroscopy of the prototype WBB NGC 6888. Thanks to the XIS excellent sensitivity and energy resolution in the soft X-ray band, we will: (i) obtain a high quality CCD spectrum which can be used to constrain the temperature of the hot plasma and the efficiency of thermal conduction across the bubble wall, (ii) determine the spatial distribution and properties of X-ray emitting plasma, (iii) therefore, test and refine shock physics models of bubbles by a direct confrontation of their results with observations. | GALACTIC DIFFUSE EMISSION | 5 | A | SVETOZAR ZHEKOV | USA | 4 | AO4 | X-RAYS FROM THE PROTOTYPE WIND-BLOWN BUBBLE NGC 6888 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504085010/ | Quick Look | ![]() |
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171 | MRK 421 OFFSET | 166.8026 | 37.7335 | 166.111285 | 38.004105 | 152.017379 | 29.315723 | 180.50489089 | 65.69633084 | 129.0398 | 55144.0655092593 | 2009-11-09 01:34:20 | 55145.8091087963 | 2009-11-10 19:25:07 | 504086010 | 75.2595 | 75 | 75.2675 | 75.2595 | 0 | 75.2675 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.94 | 51.94 | 150.6288 | 2 | PROCESSED | 57549.2648148148 | 2016-06-10 06:21:20 | 55542 | 2010-12-12 00:00:00 | 55176.2291319444 | 2009-12-11 05:29:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041324 | The OVII, OVIII, and NeIX absorption lines at z~0 have been discovered in the Chandra/XMM spectra of several bright AGNs, but the location of these absorptions has been debated since their discoveries. Here we request Suzaku observations of the soft X-ray background emission in the vicinity of Mrk 421, to conduct a joint analysis of the emission data with the extensive Chandra absorption data. This analysis will naturally yield an effective length of the absorbing/emitting gas. We have performed pilot studies and obtained a scale length of several kpc for the hot absorbing/emitting gas toward LMC X-3 and Mrk 421. The requested Suzaku observations are particular important to check these results and to further test the models we have developed in our study. | GALACTIC DIFFUSE EMISSION | 5 | B | YANGSEN YAO | USA | 4 | AO4 | A JOINT X-RAY ABSORPTION AND EMISSION STUDY OF THE HOT GAS TOWARD MRK 421 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504086010/ | Quick Look | ![]() |
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172 | 0548-70.4 | 86.9619 | -70.4173 | 87.103378 | -70.431737 | 284.612052 | -85.985846 | 280.90214015 | -30.75163284 | 12.6051 | 55378.8779861111 | 2010-07-01 21:04:18 | 55381.6286689815 | 2010-07-04 15:05:17 | 505065010 | 103.6746 | 100 | 103.6746 | 103.6746 | 0 | 103.6746 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 156.9716 | 156.9716 | 237.6358 | 1 | PROCESSED | 57552.5583912037 | 2016-06-13 13:24:05 | 55287 | 2010-04-01 00:00:00 | 55434.3854513889 | 2010-08-26 09:15:03 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051102 | Type Ia SNe play a central role in modern astrophysics, and yet we know little about their progenitors. Some of these progenitors are expected to significantly modify ambient medium around them prior to SN explosions. A standard Type Ia SNR model, a white dwarf explosion in a uniform ambient medium, fails to account for bright Fe-rich ejecta and faint blast waves seen in majority of Type Ia SNRs in the Magellanic Clouds. A promising explanation involves presence of dense circumstellar medium (CSM) around their progenitors. We propose a Suzaku study of 4 mature Type Ia SNRs in the LMC, with the goal of determining chemical abundances, temperatures and ionization ages within their ejecta. This will allow us to construct dynamical SNR models, and learn about their CSM and progenitors. | GALACTIC DIFFUSE EMISSION | 5 | B | KAZIMIERZ BORKOWSKI | USA | 5 | AO5 | TYPE IA REMNANTS IN THE LARGE MAGELLANIC CLOUD: WHAT PROGENITORS? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505065010/ | Quick Look | ![]() |
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173 | VELA SNR CB2 | 130.2058 | -44.7742 | 129.776213 | -44.595251 | 154.639113 | -59.522265 | 263.81853128 | -1.77251278 | 293.5729 | 55318.5746412037 | 2010-05-02 13:47:29 | 55318.9238425926 | 2010-05-02 22:10:20 | 505069010 | 19.3805 | 20 | 19.4125 | 19.4045 | 0 | 19.3805 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.8298 | 18.8298 | 30.1679 | 0 | PROCESSED | 57551.3535763889 | 2016-06-12 08:29:09 | 55696 | 2011-05-15 00:00:00 | 55330.2121643518 | 2010-05-14 05:05:31 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051304 | The Vela SNR is known to have ejecta bullets outside the main shell. In addition to these bullets, signatures of ejecta inside the main shell have been uncovered in recent X-ray studies. Mostly, these are rich in light metals such as O, Ne, or Mg, whereas no Fe-rich ejecta had yet been detected. Based on archival XMM-Newton data, we found a possible Fe-rich ejecta bullet headed roughly in the opposite direction of Vela pulsar's motion. This would provide us with a window into the core-collapse SN explosion of the Vela SNR. Since its electron temperature is very low (~0.1 keV), the good Suzaku XIS response below 0.5 keV is suitable to study this object. We propose to observe it in four pointings. The requested exposure time is 20 ks each, resulting in a total exposure time of 80 ks. | GALACTIC DIFFUSE EMISSION | 5 | B | SATORU KATSUDA | USA | 5 | AO5 | IRON-RICH EJECTA BULLET IN THE VELA SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505069010/ | Quick Look | ![]() |
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174 | VELA PWN E5 | 130.8405 | -45.4455 | 130.413883 | -45.264192 | 156.083116 | -59.869195 | 264.62375514 | -1.83200273 | 304.5067 | 55712.7368402778 | 2011-05-31 17:41:03 | 55712.9570601852 | 2011-05-31 22:58:10 | 506048010 | 15.9196 | 15 | 15.9196 | 15.9196 | 0 | 15.9436 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.9129 | 11.9129 | 19.0159 | 0 | PROCESSED | 57602.1724305556 | 2016-08-02 04:08:18 | 56093 | 2012-06-15 00:00:00 | 55726.0610185185 | 2011-06-14 01:27:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | B | SATORU KATSUDA | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506048010/ | Quick Look | ![]() |
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175 | VELA PWN E7 | 131.6969 | -45.5129 | 131.268004 | -45.328458 | 157.17001 | -59.613979 | 265.05012769 | -1.40367097 | 303.5042 | 55713.2300925926 | 2011-06-01 05:31:20 | 55713.4688310185 | 2011-06-01 11:15:07 | 506050010 | 13.0454 | 15 | 13.0494 | 13.0454 | 0 | 13.0534 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.0751 | 11.0751 | 20.622 | 0 | PROCESSED | 57602.181875 | 2016-08-02 04:21:54 | 56093 | 2012-06-15 00:00:00 | 55726.0999768518 | 2011-06-14 02:23:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | B | SATORU KATSUDA | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506050010/ | Quick Look | ![]() |
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176 | G236+38 OFF | 149.4117 | 1.4719 | 148.767122 | 1.710754 | 151.004118 | -10.298746 | 237.07053965 | 41.11953464 | 293.1755 | 55719.6375462963 | 2011-06-07 15:18:04 | 55721.2780092593 | 2011-06-09 06:40:20 | 506056010 | 70.8135 | 70 | 70.8215 | 70.8295 | 0 | 70.8135 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64.4444 | 64.4444 | 141.7278 | 0 | PROCESSED | 57602.2364583333 | 2016-08-02 05:40:30 | 56127 | 2012-07-19 00:00:00 | 55757.6968518518 | 2011-07-15 16:43:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061321 | Interstellar clouds cast shadows in the soft X-ray background (SXRB). Observations of these shadows enable us to disentangle the various components of the SXRB. Unfortunately, to date, shadowing observations with XMM or Suzaku have only been published for three directions, all in the southern Galactic hemisphere. We propose two new pairs of on- and off-cloud shadowing observations, in order to sample the northern Galactic hemisphere. Our particular goal is to obtain accurate X-ray spectra of the Galactic halo, which we will compare with the predictions of models of galactic fountains and infalling extragalactic material. | GALACTIC DIFFUSE EMISSION | 5 | B | DAVID HENLEY | USA | 6 | AO6 | UNDERSTANDING THE ORIGIN OF THE GALACTIC HALO USING SHADOWING OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506056010/ | Quick Look | ![]() |
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177 | RX J1713 SOUTHEAST | 258.9281 | -40.015 | 258.058505 | -39.959445 | 261.147328 | -16.912866 | 347.36958165 | -0.95677146 | 84 | 56711.6431018518 | 2014-02-23 15:26:04 | 56713.2190046296 | 2014-02-25 05:15:22 | 508067010 | 80.0774 | 80 | 80.0854 | 80.0854 | 0 | 80.0774 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74.9291 | 74.9291 | 118.0069 | 0 | PROCESSED | 57613.9112152778 | 2016-08-13 21:52:09 | 57173 | 2015-05-31 00:00:00 | 56806.6951851852 | 2014-05-29 16:41:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081313 | Detecting thermal emission and determining the ambient density are the missing keys to constrain hadronic acceleration in X-ray synchrotron-dominated SNRs. In the prototypical CR accelerator RX J1713.7-3946, X-ray thermal emission has been sought for over a decade, without success. Deep Suzaku observations will constrain either the conditions of the ambient medium in which the SNR is evolving, or the SN progenitor type (core-collapse or thermonuclear) and nucleosynthesis yield. | GALACTIC DIFFUSE EMISSION | 5 | A | FABIO ACERO | USA | 8 | AO8 | STUDY OF THE THERMAL EMISSION IN THE SYNCHROTRON DOMINATED SNR RX J1713.7-3946 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508067010/ | Quick Look | ![]() |
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178 | MBM36-OFF | 238.9304 | -1.7878 | 238.282545 | -1.642781 | 237.109098 | 18.17526 | 7.39248129 | 37.0792042 | 270.0134 | 56533.8916319444 | 2013-08-29 21:23:57 | 56535.9634606482 | 2013-08-31 23:07:23 | 508074010 | 74.1565 | 80 | 74.1645 | 74.1645 | 0 | 74.1565 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 64.2521 | 64.2521 | 178.982 | 1 | PROCESSED | 57612.4561574074 | 2016-08-12 10:56:52 | 56970 | 2014-11-09 00:00:00 | 56603.6967476852 | 2013-11-07 16:43:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081322 | We propose the observation of three off-cloud targets near the targets of the Solar Wind Charge Exchange (SWCX) Key Project to study the properties of the Diffuse X-ray Background below 1 keV, with particular focus on the characterization of the Galactic Halo. The Key Project targets are at a distance of a few hundreds pc from the Sun and their high density portions shields about 90% of X-rays at the O VII energy, our proposed targets, instead, shield only about 50% of the Galactic Halo emission. The contrast between on- and off-cloud allows us to disentangle the foreground and background emissions. In particular we will focus on the properties of the galactic halo, which dominates the oxygen background emission. | GALACTIC DIFFUSE EMISSION | 5 | A | EUGENIO URSINO | USA | 8 | AO8 | PROPERTIES OF THE GALACTIC HALO THROUGH SHADOW OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508074010/ | Quick Look | ![]() |
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179 | HB9-EAST | 75.4362 | 46.2793 | 74.514835 | 46.207153 | 79.087021 | 23.389602 | 160.82107477 | 2.65100841 | 76.7663 | 56929.6809722222 | 2014-09-29 16:20:36 | 56930.7918518518 | 2014-09-30 19:00:16 | 509033010 | 51.0581 | 50 | 51.0581 | 51.0581 | 0 | 51.0581 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6020949074 | 2016-08-16 14:27:01 | 57358 | 2015-12-02 00:00:00 | 56986.4031481482 | 2014-11-25 09:40:32 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091312 | We propose to conduct two pointed observations of the Galactic supernova remnant (SNR) HB9 (G160.9+2.6) with Suzaku. HB9 is a member of the class of Galactic SNRs which are distinguished by their contrasting radio and X-ray morphologies. Prior X-ray observations of HB9 have suggested that the SNR may have a hard component to its X-ray emission, but the true nature of this emission and its origin (a background AGN, intercluster gas associated with the cluster that harbors the AGN or the SNR itself) remains elusive. Our proposed observations will help identify the true nature of the hard emission as well as search for spectral variations (and possible overionization) in the properties of the X-ray emitting plasma associated with the SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | THOMAS PANNUTI | USA | 9 | AO9 | SUZAKU OBSERVATIONS OF THE GALACTIC SUPERNOVA REMNANT HB9 (G160.9+2.6) | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509033010/ | Quick Look | ![]() |
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180 | G93.3+6.9 SE RIM | 313.3308 | 55.275 | 312.981985 | 55.084608 | 352.240038 | 66.77051 | 93.30192448 | 6.7583673 | 52.5 | 56812.4202314815 | 2014-06-04 10:05:08 | 56814.806412037 | 2014-06-06 19:21:14 | 509039010 | 108.0493 | 100 | 108.0493 | 108.0493 | 0 | 108.0493 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.2124074074 | 2016-08-15 05:05:52 | 57205 | 2015-07-02 00:00:00 | 56835.7633912037 | 2014-06-27 18:19:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091316 | We propose three relatively long observations (totaling 280 ksec) of the high Galactic latitude supernova remnant G093.3+6.9, previously observed in AO-1 with a series of short exposures. This remnant is of particular interest because it is expanding in a low-density medium, appears sub-energetic, and has mixed-morphology, with central thermal X-ray emission surrounded by a radio synchrotron shell. Fits to the spectrum suggest a Type Ia SNR, but the possible presence of a pulsar wind nebula challenges that interpretation. The new pointings will significantly improve the statistics for key regions (rims and background), allowing us to type the remnant, determine its age, study its energetics, place limits on nonthermal X-ray emission, and better characterize the PWN. | GALACTIC DIFFUSE EMISSION | 5 | C | MICHAEL STAGE | USA | 9 | AO9 | G093.3+6.9: SUPERNOVA PHYSICS IN A LOW-DENSITY MEDIUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509039010/ | Quick Look | ![]() |
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181 | OFF-FIELD3 | 339.5497 | 30.5758 | 338.966926 | 30.315472 | 354.778732 | 35.902508 | 91.73533627 | -24.10496467 | 65.4693 | 56819.1115625 | 2014-06-11 02:40:39 | 56821.2502199074 | 2014-06-13 06:00:19 | 509044010 | 97.3343 | 80 | 97.3343 | 97.3343 | 0 | 97.3343 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38.618 | 38.618 | 77.04 | 0 | PROCESSED | 57615.247974537 | 2016-08-15 05:57:05 | 56748 | 2014-04-01 00:00:00 | 56834.8146527778 | 2014-06-26 19:33:06 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091321 | Our special vantage point in our Galaxy allows us to study the Galactic warm-hot halo along several sightlines and determine its physical properties. The combination of absorption and emission measurements provides a powerful tool in this regard. Instead of average emission and absorption measures used in previous studies, one immediate step forward would be to use emission measures close to absorption sightlines. With proposed observations we will determine emission measures close to five sightlines in which we have the most accurate absorption measurements with Chandra. This will break the degeneracy between density and path-length and robustly measure the extent and mass of the warm-hot halo, placing strongest constraints yet on the fraction of missing baryons in the warm-hot plasma. | GALACTIC DIFFUSE EMISSION | 5 | C | ANJALI GUPTA | USA | 9 | AO9 | CIRCUM-GALACTIC MEDIUM OF THE MILKY WAY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509044010/ | Quick Look | ![]() |
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182 | FERMI_JET_COCOON_3 | 314.5039 | -35.288 | 313.721159 | -35.481827 | 306.823334 | -17.363917 | 8.28342789 | -40.13197139 | 258.2411 | 56980.5600694445 | 2014-11-19 13:26:30 | 56980.9689583333 | 2014-11-19 23:15:18 | 509049010 | 18.6742 | 20 | 18.6742 | 18.6742 | 0 | 18.6742 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7925347222 | 2016-08-16 19:01:15 | 57362 | 2015-12-06 00:00:00 | 56995.6103240741 | 2014-12-04 14:38:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091322 | The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way. | GALACTIC DIFFUSE EMISSION | 5 | C | MATTHEW MILLER | USA | 9 | AO9 | OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509049010/ | Quick Look | ![]() |
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183 | FERMI_JET_COCOON_4 | 313.0188 | -30.9125 | 312.254939 | -31.101111 | 306.880758 | -12.815318 | 13.57103518 | -38.16097703 | 249.0341 | 56968.206412037 | 2014-11-07 04:57:14 | 56968.8473958333 | 2014-11-07 20:20:15 | 509050010 | 21.6767 | 20 | 21.6767 | 21.8127 | 0 | 21.8207 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7496412037 | 2016-08-16 17:59:29 | 57358 | 2015-12-02 00:00:00 | 56982.4333333333 | 2014-11-21 10:24:00 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091322 | The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way. | GALACTIC DIFFUSE EMISSION | 5 | C | MATTHEW MILLER | USA | 9 | AO9 | OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509050010/ | Quick Look | ![]() |
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184 | FERMI_JET_COCOON_6 | 319.6218 | -32.8375 | 318.863263 | -33.048426 | 311.821395 | -16.319347 | 12.30967968 | -44.01160773 | 252.671 | 56969.3646296296 | 2014-11-08 08:45:04 | 56970.0259375 | 2014-11-09 00:37:21 | 509052010 | 21.3583 | 20 | 21.3583 | 21.3583 | 0 | 21.3583 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7516782407 | 2016-08-16 18:02:25 | 57358 | 2015-12-02 00:00:00 | 56982.4382407407 | 2014-11-21 10:31:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091322 | The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way. | GALACTIC DIFFUSE EMISSION | 5 | C | MATTHEW MILLER | USA | 9 | AO9 | OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509052010/ | Quick Look | ![]() |
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185 | DIFFUSE1B | 201.171 | 8.6653 | 200.545653 | 8.925438 | 196.184358 | 16.273856 | 327.54408522 | 69.93225444 | 119.3004 | 57014.7841898148 | 2014-12-23 18:49:14 | 57015.2196759259 | 2014-12-24 05:16:20 | 509059010 | 20.7335 | 20 | 20.7335 | 20.7415 | 0 | 20.7335 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.558275463 | 2016-08-17 13:23:55 | 57475 | 2016-03-28 00:00:00 | 57107.4265162037 | 2015-03-26 10:14:11 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091324 | In the course of a program to fit spatial models to the Galactic hot gas content, we discovered a few fields that were highly discrepant in the strength of their O VII and/or O VIII line strengths. These are rare emission regions, occurring in fewer than 1% of the fields and they are not due to known extended emission regions (SNR, galaxy clusters, etc.). These emission anomalies probably signify locations of unusual physics, such as shocks, conductive heating, or local heat injection. We propose observations to determine the angular extent of these unusual regions and to better define the intensities of the O VII and O VIII lines. These observations will help identify the relevant physical process and the nature of the phenomenon causing them. | GALACTIC DIFFUSE EMISSION | 5 | C | JOEL BREGMAN | USA | 9 | AO9 | UNIDENTIFIED BRIGHT X-RAY BACKGROUND REGIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509059010/ | Quick Look | ![]() |
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186 | 3C120 | 68.2993 | 5.3535 | 67.634764 | 5.249056 | 67.434072 | -16.404208 | 190.3755878 | -27.39480435 | 262.4873 | 53789.4598726852 | 2006-02-23 11:02:13 | 53790.8748958333 | 2006-02-24 20:59:51 | 700001030 | 40.9073 | 160 | 40.9073 | 40.9073 | 40.9073 | 40.9073 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 38.4817 | 38.4817 | 77.876 | 2 | PROCESSED | 57533.073900463 | 2016-05-25 01:46:25 | 54247 | 2007-05-27 00:00:00 | 54041.5149189815 | 2006-11-02 12:21:29 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001003 | Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 0 | SWG | BROAD-BAND MONITORING OF 3C120 IN VARIOUS ACCRETING STATES | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700001030/ | Quick Look | ![]() |
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187 | MCG-6-30-15 | 203.9713 | -34.2978 | 203.254904 | -34.042659 | 215.172989 | -22.546967 | 313.28925681 | 27.67845448 | 102.4359 | 53762.928275463 | 2006-01-27 22:16:43 | 53765.368275463 | 2006-01-30 08:50:19 | 700007030 | 96.6919 | 300 | 96.6919 | 96.6919 | 96.6999 | 96.6999 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 89.8194 | 89.8194 | 210.8019 | 5 | PROCESSED | 57532.8529861111 | 2016-05-24 20:28:18 | 54247 | 2007-05-27 00:00:00 | 54040.8156828704 | 2006-11-01 19:34:35 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001035 | The broad iron line in the Seyfert 1 galaxy MCG-6-30-15 shows that most of the power is released at 2--4 gravitational radii enabling the strong gravity, accretion flow and energy release in that exciting regime to be studied. The spectral variability of the source decomposes into a highly variable power law and a reflection-dominated component, containing the iron line and Compton hump, which varies significantly but with much less amplitude. This can be explained by the extreme gravitational light bending occuring in this region. We propose to observe MCG--6-30-15 for 4 x 50~ks in order to determine for the first time the variability of the reflection over a wide range of energies from below 1 keV to above 40 keV and timescales . | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ANDREW FABIAN | JAP | 0 | SWG | REFLECTION, ABSORPTION AND STRONG GRAVITY AROUND THE SPINNING BLACK HOLE IN MCG--6-30-15 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700007030/ | Quick Look | ![]() |
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188 | 0836+714 | 130.267 | 70.829 | 129.006808 | 71.006559 | 109.318804 | 50.076677 | 143.62710847 | 34.4182022 | 294.8268 | 53809.7578125 | 2006-03-15 18:11:15 | 53810.5836111111 | 2006-03-16 14:00:24 | 700010010 | 55.6261 | 50 | 55.6341 | 55.6341 | 55.6261 | 55.6341 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 47.4058 | 47.4058 | 71.3419 | 1 | PROCESSED | 57533.2238541667 | 2016-05-25 05:22:21 | 54247 | 2007-05-27 00:00:00 | 54041.9651851852 | 2006-11-02 23:09:52 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001061 | We propose two 50 ks observations, one for each of two EGRET blazars, 1510-089 (OR -017) and 0836+710 (4C +71.07). Both objects show extremely hard X-ray spectra, with photon indices about 1.3. The blazar 1510-089 ($z = 0.361$) is among a few OVV quasars showing prominent soft X-ray excess. The blazar 0836+710 ($z = 2.172)$ is the brightest X-ray source among the high redshift ($z>2$) quasars, and its very hard X-ray spectrum extends down to soft X-rays. Studying spectral shape and variability in the soft X-ray band relative to variability in the mid X-ray and optical bands can help to reveal nature of the soft X-ray excess of unknown origin, and multifrequency variability studies can provide constraints on the structure of jets on subparsec scales. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GREG MADEJSKI | JAP | 0 | SWG | TESTING THE SHOCK-IN-JET MODEL FOR NONTHERMAL FLARES IN BLAZARS VIA SUZAKU OBSERVATIONS | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700010010/ | Quick Look | ![]() |
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189 | SWIFT J0746.3+2548 | 116.6142 | 25.8792 | 115.852151 | 26.002245 | 113.853224 | 4.615293 | 194.5201067 | 22.91801121 | 97.0095 | 53678.357974537 | 2005-11-04 08:35:29 | 53680.5862847222 | 2005-11-06 14:04:15 | 700011010 | 99.4284 | 100 | 99.5235 | 100.4524 | 99.4284 | 99.7235 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 87.6995 | 87.6995 | 192.472 | 4 | PROCESSED | 57527.9575694445 | 2016-05-19 22:58:54 | 54247 | 2007-05-27 00:00:00 | 54037.5799074074 | 2006-10-29 13:55:04 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001087 | Recently the BAT gamma-ray detector onboard Swift satellite has discovered very flat hard X-ray sources with photon index ~ 1.5 above 100 keV. The x-ray spectrum obtained with the XRT on Swiftis highly variable on time scales < 90 minutes. This variability and flat continuum spectrum suggests that this source is classified as a blazar. If this association is real, we have a precious chance to obtain spectrum upto several hundred keV in the source frame of the source. This wide range is of particularly importanceto study the blazar spectrum, or the electron distribution. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TADAYUKI TAKAHASHI | JAP | 0 | SWG | SUZAKU OBSERVATION OF A HIGH REDSHIFT BLAZAR RECENTLY DISCOVERED BY THE BAT ON SWIFT | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700011010/ | Quick Look | ![]() |
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190 | BO 375 | 11.4476 | 41.6573 | 10.75946 | 41.384162 | 28.671168 | 33.427051 | 121.80050832 | -21.20204189 | 232.9596 | 54135.3691666667 | 2007-02-04 08:51:36 | 54135.7592476852 | 2007-02-04 18:13:19 | 701028010 | 12.7798 | 13 | 12.7798 | 12.7798 | 0 | 12.7798 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.8386 | 12.8386 | 33.664 | 1 | PROCESSED | 57536.9599189815 | 2016-05-28 23:02:17 | 54695 | 2008-08-17 00:00:00 | 54151.4930324074 | 2007-02-20 11:49:58 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011120 | There are over 400 very luminous (Lx > 1e38-1e40 erg/s) globular cluster X-ray sources in nearby galaxies. None are present in our Galaxy, and their nature is unknown. They may be accreting black holes, however, this is quite controversial and it is contrary to theoretical expectations. The distance is too large to make accurate studies of any of them that could reveal their nature. Luckily, there is one such very luminous source, Bo 375, in a globular cluster in M31. We propose to perform ten 10 ksec Suzaku observations of Bo 375. We expect that from the long-term lightcurve, broad-band energy spectra, and power spectra, we will be able to determine the nature of this object and thereby possibly the nature of the many very luminous globular cluster X-ray sources in nearby galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ALBERT KONG | USA | 1 | AO1 | PROBING THE NATURE OF A VERY LUMINOUS GLOBULAR CLUSTER X-RAY SOURCE IN M31 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701028010/ | Quick Look | ![]() |
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191 | BO 375 | 11.4497 | 41.6556 | 10.761554 | 41.382464 | 28.671878 | 33.424815 | 121.80214792 | -21.2037783 | 231.6187 | 54137.6100810185 | 2007-02-06 14:38:31 | 54137.9737731482 | 2007-02-06 23:22:14 | 701028020 | 15.5371 | 13 | 15.5371 | 15.5371 | 0 | 15.5371 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14.942 | 14.942 | 31.4159 | 0 | PROCESSED | 57537.3176967593 | 2016-05-29 07:37:29 | 54695 | 2008-08-17 00:00:00 | 54151.4987731482 | 2007-02-20 11:58:14 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011120 | There are over 400 very luminous (Lx > 1e38-1e40 erg/s) globular cluster X-ray sources in nearby galaxies. None are present in our Galaxy, and their nature is unknown. They may be accreting black holes, however, this is quite controversial and it is contrary to theoretical expectations. The distance is too large to make accurate studies of any of them that could reveal their nature. Luckily, there is one such very luminous source, Bo 375, in a globular cluster in M31. We propose to perform ten 10 ksec Suzaku observations of Bo 375. We expect that from the long-term lightcurve, broad-band energy spectra, and power spectra, we will be able to determine the nature of this object and thereby possibly the nature of the many very luminous globular cluster X-ray sources in nearby galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ALBERT KONG | USA | 1 | AO1 | PROBING THE NATURE OF A VERY LUMINOUS GLOBULAR CLUSTER X-RAY SOURCE IN M31 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701028020/ | Quick Look | ![]() |
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192 | BO 375 | 11.4497 | 41.6556 | 10.761554 | 41.382464 | 28.671878 | 33.424815 | 121.80214792 | -21.2037783 | 231.4176 | 54142.8248032407 | 2007-02-11 19:47:43 | 54143.2167824074 | 2007-02-12 05:12:10 | 701028030 | 15.0878 | 13 | 15.0878 | 15.0878 | 0 | 15.0878 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.7164 | 15.7164 | 33.8379 | 1 | PROCESSED | 57537.3535069444 | 2016-05-29 08:29:03 | 54695 | 2008-08-17 00:00:00 | 54153.1806828704 | 2007-02-22 04:20:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011120 | There are over 400 very luminous (Lx > 1e38-1e40 erg/s) globular cluster X-ray sources in nearby galaxies. None are present in our Galaxy, and their nature is unknown. They may be accreting black holes, however, this is quite controversial and it is contrary to theoretical expectations. The distance is too large to make accurate studies of any of them that could reveal their nature. Luckily, there is one such very luminous source, Bo 375, in a globular cluster in M31. We propose to perform ten 10 ksec Suzaku observations of Bo 375. We expect that from the long-term lightcurve, broad-band energy spectra, and power spectra, we will be able to determine the nature of this object and thereby possibly the nature of the many very luminous globular cluster X-ray sources in nearby galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ALBERT KONG | USA | 1 | AO1 | PROBING THE NATURE OF A VERY LUMINOUS GLOBULAR CLUSTER X-RAY SOURCE IN M31 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701028030/ | Quick Look | ![]() |
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193 | NGC 3783 | 174.7611 | -37.7364 | 174.141196 | -37.45925 | 192.677729 | -36.170962 | 287.45850943 | 22.95048745 | 293.6402 | 53910.7726388889 | 2006-06-24 18:32:36 | 53912.8571412037 | 2006-06-26 20:34:17 | 701033010 | 75.7193 | 75 | 75.7193 | 75.7193 | 75.7193 | 75.7193 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 68.2993 | 68.2993 | 180.0237 | 0 | PROCESSED | 57534.7899652778 | 2016-05-26 18:57:33 | 54401 | 2007-10-28 00:00:00 | 53926.8847453704 | 2006-07-10 21:14:02 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011325 | We propose a 75 ksec Suzaku observation of the bright Seyfert 1 NGC 3783. Absorption due to photo-ionized material in the line of sight is well-established in this source, but can lead to degeneracy during modeling: is 3-6 keV continuum curvature due to photo-ionized absorption or a relativistically broad Fe K component? The simultaneous broadband XIS/HXD coverage is needed to define the continuum emission over a wide bandpass and disentangle the various emitting and absorbing components. We can then study the ionized absorber components, establish whether or not broad Fe K emission exists, and constrain reflection components, including the Compton shoulder. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | ALEX MARKOWITZ | USA | 1 | AO1 | PROBING FE K EMISSION AND IONIZED ABSORPTION IN NGC 3783 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701033010/ | Quick Look | ![]() |
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194 | MRK 273 | 206.1319 | 55.8192 | 205.671114 | 56.069559 | 168.560084 | 59.024421 | 108.09580624 | 59.75355315 | 290.8776 | 53923.3108333333 | 2006-07-07 07:27:36 | 53925.3356481482 | 2006-07-09 08:03:20 | 701050010 | 79.9046 | 80 | 79.9126 | 79.9046 | 79.9206 | 79.9206 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 82.8076 | 82.8076 | 174.9059 | 3 | PROCESSED | 57534.931400463 | 2016-05-26 22:21:13 | 54401 | 2007-10-28 00:00:00 | 53930.7076851852 | 2006-07-14 16:59:04 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011341 | We wish to take advantage of the unprecedented sensitivity of Suzaku Observatory to very hard X-rays (> 10 keV) to constrain the energy source -- starburst or black-hole driven activity -- in two of the nearest and brightest ultraluminous infrared galaxies, Mrk 273 and F05189-2524. These objects are arguably the best local laboratories to study the basic physical processes involved in creating massive early type hosts on the one hand, and feeding embedded supermassive black holes on the other hand, in major galaxy mergers. The Suzaku data will be used to search for the high-energy signature of deeply buried active black holes and to look for short timescale variability, another signature of black-hole driven activity. These data will be part of S. Teng's PhD thesis at Maryland. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | SYLVAIN VEILLEUX | USA | 1 | AO1 | THE DOMINANT ENERGY SOURCE OF ULTRALUMINOUS INFRARED GALAXIES | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701050010/ | Quick Look | ![]() |
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195 | APM 08279+5255 | 127.9265 | 52.7635 | 126.994318 | 52.932793 | 116.239859 | 32.72128 | 165.74397918 | 36.24189551 | 118.0523 | 54020.1580902778 | 2006-10-12 03:47:39 | 54022.3134143518 | 2006-10-14 07:31:19 | 701057010 | 102.3328 | 100 | 102.3408 | 102.3408 | 102.3328 | 102.3408 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 96.0187 | 96.0187 | 186.1858 | 3 | PROCESSED | 57535.8953125 | 2016-05-27 21:29:15 | 54702 | 2008-08-24 00:00:00 | 54053.9467013889 | 2006-11-14 22:43:15 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011353 | Motivated by the detection of a relativistic outflow of highly ionized gas in previous XMM-Newton and Chandra observations of the lensed quasar APM08279+5255 we propose to monitor this object with three 100ks observations with the aim of improving our understanding of the significance of such outflows in regulating black hole growth and in influencing structure formation. The main scientific goals are : (a) verify the present interpretations of Fe line features in this quasar, (b) monitor the time variability of the Fe absorption features and thus constrain the acceleration mechanism, (c) constrain the kinematic, ionization and absorbing properties of the outflow, and (d) show whether the low-energy ionized absorber is part of the relativistic outflow. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GEORGE CHARTAS | USA | 1 | AO1 | VIEWS OF RELATIVISTIC WINDS THROUGH NATURAL LENSES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701057010/ | Quick Look | ![]() |
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196 | 1ES 1101-232 | 165.8976 | -23.5471 | 165.286971 | -23.277424 | 177.035323 | -27.087344 | 273.21266184 | 33.02701002 | 279.8544 | 53880.6859606482 | 2006-05-25 16:27:47 | 53882.2161921296 | 2006-05-27 05:11:19 | 701071010 | 62.4327 | 55 | 62.4407 | 62.4407 | 62.4407 | 62.4327 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 50.1033 | 50.1033 | 132.1939 | 0 | PROCESSED | 57534.4584027778 | 2016-05-26 11:00:06 | 54401 | 2007-10-28 00:00:00 | 53927.4165393518 | 2006-07-11 09:59:49 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011376 | Detecting absorption effects in TeV blazar spectra from TeV photon collisions on the extragalactic IR background (EBL) is a powerful tool to probe the EBL. It requires a thorough understanding of the intrinsic blazar spectra. We propose XIS and HXD observations, with emphasis on the hard X-rays, for the 3 most distant HESS blazars, coordinated with HESS observations. Thanks to Suzaku's sensitivity in a broad energy range, we expect to set tight limits on the models' parameter space, and constrain emission and acceleration scenarios by studying the shape and evolution of the particle distribution, most sensitively conducted in the important hard X-ray energy range. In coordination with TeV observations, it allows us to disentangle EBL absorption effects from the blazar intrinsic spectra. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ANITA REIMER | USA | 1 | AO1 | CHALLENGING JET MODELS OF THE MOST DISTANT TEV-BLAZARS | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701071010/ | Quick Look | ![]() |
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197 | NGC5548 | 214.4933 | 25.1285 | 213.926392 | 25.358693 | 201.994196 | 36.40686 | 31.9338138 | 70.49848107 | 305.6607 | 54289.4186921296 | 2007-07-08 10:02:55 | 54290.1182175926 | 2007-07-09 02:50:14 | 702042040 | 30.6996 | 30 | 30.6996 | 30.6996 | 0 | 30.6996 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 28.8279 | 28.8279 | 60.4319 | 1 | PROCESSED | 57539.1330324074 | 2016-05-31 03:11:34 | 54695 | 2008-08-17 00:00:00 | 54328.4843402778 | 2007-08-16 11:37:27 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021307 | We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARTIN ELVIS | USA | 2 | AO2 | NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702042040/ | Quick Look | ![]() |
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198 | NGC5548 | 214.4959 | 25.1277 | 213.928994 | 25.357885 | 201.997272 | 36.407089 | 31.932758 | 70.49602002 | 293.6791 | 54296.5817013889 | 2007-07-15 13:57:39 | 54297.4168865741 | 2007-07-16 10:00:19 | 702042050 | 30.0197 | 30 | 30.0277 | 30.0357 | 0 | 30.0197 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.3004 | 26.3004 | 58.971 | 1 | PROCESSED | 57539.274849537 | 2016-05-31 06:35:47 | 54707 | 2008-08-29 00:00:00 | 54340.3894328704 | 2007-08-28 09:20:47 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021307 | We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARTIN ELVIS | USA | 2 | AO2 | NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702042050/ | Quick Look | ![]() |
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199 | NGC5548 | 214.4979 | 25.1264 | 213.930994 | 25.35658 | 201.999984 | 36.406639 | 31.92993093 | 70.49400067 | 281.7605 | 54317.0262268518 | 2007-08-05 00:37:46 | 54318.0211111111 | 2007-08-06 00:30:24 | 702042080 | 38.7757 | 210 | 38.7837 | 38.7917 | 0 | 38.7757 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 32.6497 | 32.6497 | 85.9519 | 0 | PROCESSED | 57539.4187037037 | 2016-05-31 10:02:56 | 54714 | 2008-09-05 00:00:00 | 54347.3528472222 | 2007-09-04 08:28:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021307 | We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARTIN ELVIS | USA | 2 | AO2 | NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702042080/ | Quick Look | ![]() |
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200 | FAIRALL 9 | 20.9481 | -58.8141 | 20.470954 | -59.074601 | 340.57309 | -59.156739 | 295.06951561 | -57.81752905 | 48.1772 | 54258.155462963 | 2007-06-07 03:43:52 | 54260.5766666667 | 2007-06-09 13:50:24 | 702043010 | 167.7983 | 164 | 167.7983 | 167.8063 | 0 | 167.8143 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 136.4834 | 136.4834 | 209.1758 | 2 | PROCESSED | 57538.9238425926 | 2016-05-30 22:10:20 | 54773 | 2008-11-03 00:00:00 | 54265.5470717593 | 2007-06-14 13:07:47 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021313 | Recently, deep observations of a number of Seyfert AGN with XMM-Newton and Suzaku have established variable and relativistic iron lines as robust features in roughly half of all deep Seyfert spectra. In these sources, the spin of the black hole can be constrained directly through fits to the relativistic iron line. A sample of excellent spectra from well-chosen AGN will facilitate a better understanding of the innermost regime near to black holes, and make correlations with parameters like radio luminosity, star formation rate, and galaxy and black hole mass possible for the first time. We propose to obtain observations of 4 under-exposed Seyfert AGN with promising evidence for broad lines to robustly constrain their spin parameters. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JON MILLER | USA | 2 | AO2 | REVEALING BLACK HOLE SPIN IN RELATIVISTIC SEYFERT AGN | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702043010/ | Quick Look | ![]() |
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201 | NGC 1052 | 40.2309 | -8.2134 | 39.616406 | -8.42693 | 35.027708 | -22.668341 | 181.91154484 | -57.92833515 | 49.7745 | 54297.4313888889 | 2007-07-16 10:21:12 | 54299.87875 | 2007-07-18 21:05:24 | 702058010 | 100.6691 | 100 | 100.6691 | 100.6691 | 0 | 100.6691 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 83.4998 | 83.4998 | 211.4278 | 2 | PROCESSED | 57539.327037037 | 2016-05-31 07:50:56 | 54707 | 2008-08-29 00:00:00 | 54339.9136458333 | 2007-08-27 21:55:39 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021355 | Accretion onto supermassive black holes is thought to play a major role in the production of relativistic jets. Our understanding of jet production remains elusive, however, because we cannot image the accretion flow. Fortunately, the Fe K line offers a direct probe of accretion. As part of a multi-mission monitoring program of the radio loud AGN NGC 1052, we propose two 100 ksec Suzaku observations to obtain best-quality X-ray spectra at two epochs to determine the true continuum shape and thus probe the relativistic iron line, determine line and continuum variability patterns and possibly investigate how the structure of the accretion disk changes when there are jet ejection events. Our aim is to determine what leads supermassive black holes to launch powerful jets. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KIMBERLY WEAVER | USA | 2 | AO2 | PROBING THE DISK-JET CONNECTION IN AGN WITH AN INTENSIVE MULTIWAVELENGTH MONITORING CAMPAIGN OF NGC 1052 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702058010/ | Quick Look | ![]() |
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202 | Q1946+7658 | 296.1546 | 77.0965 | 296.596903 | 76.972833 | 64.242641 | 76.919523 | 109.22346589 | 23.50098326 | 3.7704 | 54294.4255902778 | 2007-07-13 10:12:51 | 54294.6432175926 | 2007-07-13 15:26:14 | 702060010 | 13.1636 | 13 | 13.1636 | 13.1636 | 0 | 13.1636 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.9282 | 13.9282 | 18.7759 | 0 | PROCESSED | 57539.2591782407 | 2016-05-31 06:13:13 | 54706 | 2008-08-28 00:00:00 | 54339.4067824074 | 2007-08-27 09:45:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021361 | The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | GEORGE CHARTAS | USA | 2 | AO2 | AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702060010/ | Quick Look | ![]() |
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203 | Q1334-0033 | 204.1954 | -0.819 | 203.55335 | -0.564423 | 202.702904 | 8.620784 | 326.07775276 | 59.99926461 | 306.9566 | 54295.3551736111 | 2007-07-14 08:31:27 | 54295.7084953704 | 2007-07-14 17:00:14 | 702067010 | 13.9621 | 15 | 13.9621 | 13.9621 | 0 | 13.9621 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.0064 | 13.0064 | 30.5199 | 0 | PROCESSED | 57539.262337963 | 2016-05-31 06:17:46 | 54710 | 2008-09-01 00:00:00 | 54340.4777430556 | 2007-08-28 11:27:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021361 | The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | GEORGE CHARTAS | USA | 2 | AO2 | AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702067010/ | Quick Look | ![]() |
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204 | Q1548+0917 | 237.6002 | 9.1581 | 236.997547 | 9.308492 | 232.970531 | 28.527987 | 18.5566992 | 44.16075413 | 106.1242 | 54513.4560763889 | 2008-02-17 10:56:45 | 54514.16 | 2008-02-18 03:50:24 | 702068010 | 32.1133 | 23 | 32.1213 | 32.1213 | 0 | 32.1133 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 29.4756 | 29.4756 | 60.8159 | 0 | PROCESSED | 57541.5745601852 | 2016-06-02 13:47:22 | 54889 | 2009-02-27 00:00:00 | 54522.1462731482 | 2008-02-26 03:30:38 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021361 | The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | GEORGE CHARTAS | USA | 2 | AO2 | AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702068010/ | Quick Look | ![]() |
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205 | MRK 417 | 162.3659 | 22.9016 | 161.688757 | 23.166381 | 154.921054 | 14.241178 | 214.84390845 | 62.11471123 | 281.9359 | 54238.6593402778 | 2007-05-18 15:49:27 | 54239.5730555556 | 2007-05-19 13:45:12 | 702078010 | 41.5066 | 40 | 41.5066 | 41.5066 | 0 | 41.5066 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.3385 | 39.3385 | 78.9239 | 0 | PROCESSED | 57538.6952662037 | 2016-05-30 16:41:11 | 54695 | 2008-08-17 00:00:00 | 54245.0002430556 | 2007-05-25 00:00:21 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021374 | Though Compton thick AGN are expected to constitute a sizable fraction of the Seyfert population (Maiolino et al 1998 and Risaliti et al 1999), the fraction and the signatures of Compton thick AGN is unknown. The SWIFT BAT all-sky AGN survey has detected a complete sample of AGN with flux > 1-3e-11 erg/cm^2/s in the 15-200 keV band. At this energy range, the effects of heavy obscuration are minimal and thus BAT will allow us to determine the true fraction of Compton-thick sources. However, the BAT spectra are not simultaneous with XRT and XRT does not have the spectral resolution (with 10 ks) necessary to characterize a heavily absorbed 0.3-10 keV spectrum. We propose HXD nominal Suzaku observations of 4 possible Compton thick sources for which we recently obtained XMM 10 ks follow-ups. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RICHARD MUSHOTZKY | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF POSSIBLY COMPTON THICK AGN FROM THE SWIFT BAT SURVEY | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702078010/ | Quick Look | ![]() |
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206 | NGC 1142 | 43.7827 | -0.1295 | 43.142852 | -0.331581 | 41.283841 | -16.101856 | 175.79604248 | -49.86350093 | 73.9096 | 54302.4506481482 | 2007-07-21 10:48:56 | 54303.4308333333 | 2007-07-22 10:20:24 | 702079010 | 40.5697 | 40 | 40.5697 | 40.5697 | 0 | 40.5697 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36.5404 | 36.5404 | 84.6799 | 1 | PROCESSED | 57539.2980902778 | 2016-05-31 07:09:15 | 54706 | 2008-08-28 00:00:00 | 54339.1106828704 | 2007-08-27 02:39:23 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021374 | Though Compton thick AGN are expected to constitute a sizable fraction of the Seyfert population (Maiolino et al 1998 and Risaliti et al 1999), the fraction and the signatures of Compton thick AGN is unknown. The SWIFT BAT all-sky AGN survey has detected a complete sample of AGN with flux > 1-3e-11 erg/cm^2/s in the 15-200 keV band. At this energy range, the effects of heavy obscuration are minimal and thus BAT will allow us to determine the true fraction of Compton-thick sources. However, the BAT spectra are not simultaneous with XRT and XRT does not have the spectral resolution (with 10 ks) necessary to characterize a heavily absorbed 0.3-10 keV spectrum. We propose HXD nominal Suzaku observations of 4 possible Compton thick sources for which we recently obtained XMM 10 ks follow-ups. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RICHARD MUSHOTZKY | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF POSSIBLY COMPTON THICK AGN FROM THE SWIFT BAT SURVEY | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702079010/ | Quick Look | ![]() |
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207 | MCG +04-48-002 | 307.1488 | 25.8021 | 306.615298 | 25.635019 | 318.241154 | 43.22286 | 67.06317106 | -7.53431612 | 93.9583 | 54208.4668634259 | 2007-04-18 11:12:17 | 54209.4134143518 | 2007-04-19 09:55:19 | 702081010 | 41.2988 | 40 | 41.3068 | 41.2988 | 0 | 41.3068 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.7466 | 37.7466 | 81.7699 | 2 | PROCESSED | 57538.398275463 | 2016-05-30 09:33:31 | 54695 | 2008-08-17 00:00:00 | 54217.0231712963 | 2007-04-27 00:33:22 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021374 | Though Compton thick AGN are expected to constitute a sizable fraction of the Seyfert population (Maiolino et al 1998 and Risaliti et al 1999), the fraction and the signatures of Compton thick AGN is unknown. The SWIFT BAT all-sky AGN survey has detected a complete sample of AGN with flux > 1-3e-11 erg/cm^2/s in the 15-200 keV band. At this energy range, the effects of heavy obscuration are minimal and thus BAT will allow us to determine the true fraction of Compton-thick sources. However, the BAT spectra are not simultaneous with XRT and XRT does not have the spectral resolution (with 10 ks) necessary to characterize a heavily absorbed 0.3-10 keV spectrum. We propose HXD nominal Suzaku observations of 4 possible Compton thick sources for which we recently obtained XMM 10 ks follow-ups. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RICHARD MUSHOTZKY | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF POSSIBLY COMPTON THICK AGN FROM THE SWIFT BAT SURVEY | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702081010/ | Quick Look | ![]() |
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208 | TYPE2AGN | 216.4026 | 35.2819 | 215.878545 | 35.506676 | 198.09088 | 46.269263 | 60.85487771 | 68.34395808 | 307.3753 | 54292.1781712963 | 2007-07-11 04:16:34 | 54292.6183333333 | 2007-07-11 14:50:24 | 702090010 | 19.8387 | 19 | 19.8467 | 19.8547 | 0 | 19.8387 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.87 | 20.87 | 38.0159 | 0 | PROCESSED | 57539.1533912037 | 2016-05-31 03:40:53 | 54706 | 2008-08-28 00:00:00 | 54339.0120833333 | 2007-08-27 00:17:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021376 | We propose to use Suzaku's large collecting area and excellent energy response to measure accurate X-ray spectra for 9 XBONGs and 8 luminous Type 2 AGN selected from very large samples of identified XBONGs and Type 2 AGN found in our Chandra XBootes survey. We have obtained optical spectra for 258 XBONGs and identified ~700 X-ray luminous Type 2 AGN at z>0.7. With known source positions and X-ray fluxes, we select sources that are relatively bright with little or no contamination from other X-ray sources. Thus we will measure individual spectra for these bright sources. We propose eight 15 ksec Suzaku XIS observations to measure the absorption in 8 luminous z > 0.8 Type 2 AGN and eight 10 ksec observations to measure the absorption and iron emission for nine XBONGs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | CHRISTINE JONES | USA | 2 | AO2 | OBSCURED AGN AND XBONGS IN BOOTES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702090010/ | Quick Look | ![]() |
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209 | NGC3227 | 155.8768 | 19.8688 | 155.194236 | 20.122176 | 150.387557 | 9.143202 | 216.98485011 | 55.4460253 | 111.8565 | 54790.7083333333 | 2008-11-20 17:00:00 | 54792.374525463 | 2008-11-22 08:59:19 | 703022040 | 64.5679 | 50 | 64.5759 | 64.5679 | 0 | 64.5759 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.622 | 46.622 | 143.9478 | 1 | PROCESSED | 57544.506412037 | 2016-06-05 12:09:14 | 54557 | 2008-04-01 00:00:00 | 54812.4380324074 | 2008-12-12 10:30:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031013 | We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARTIN ELVIS | USA | 3 | AO3 | NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703022040/ | Quick Look | ![]() |
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210 | NGC3227 | 155.8768 | 19.8687 | 155.194236 | 20.122076 | 150.387594 | 9.143109 | 216.98501654 | 55.44599229 | 109.926 | 54802.6028125 | 2008-12-02 14:28:03 | 54803.7231365741 | 2008-12-03 17:21:19 | 703022060 | 51.4105 | 50 | 51.4105 | 51.4105 | 0 | 51.4105 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.6836 | 39.6836 | 96.7818 | 1 | PROCESSED | 57544.6321875 | 2016-06-05 15:10:21 | 54557 | 2008-04-01 00:00:00 | 54812.4432407407 | 2008-12-12 10:38:16 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031013 | We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARTIN ELVIS | USA | 3 | AO3 | NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703022060/ | Quick Look | ![]() |
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211 | SN 2006JD | 120.5331 | 0.8102 | 119.888824 | 0.950282 | 122.553341 | -19.245849 | 220.45612728 | 16.05834455 | 284.354 | 54578.4377777778 | 2008-04-22 10:30:24 | 54579.6807175926 | 2008-04-23 16:20:14 | 703026010 | 54.1968 | 50 | 54.2048 | 54.1968 | 0 | 54.2048 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52.0488 | 52.0488 | 107.3398 | 1 | PROCESSED | 57542.379837963 | 2016-06-03 09:06:58 | 54957 | 2009-05-06 00:00:00 | 54588.1523611111 | 2008-05-02 03:39:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031241 | Supernovae (SNe) 2005kd and 2006jd are some of the brightest SNe ever detected in X-rays. The high X-ray luminosities (>E41 erg/s) are the results of the SN shock interacting with dense material in the environment of the SNe. We propose one Suzaku observation of each SN to obtain high-quality spectra that will be used to measure the temperature of the forward and reverse shock and to establish the rate of decline in comparison with existing Swift, Chandra and XMM-Newton data. The data will further be used to measure the circumstellar matter density and mass-loss rate of the progenitors to probe the nature of the SN progenitors. Our science objectives rely on Suzaku's uniqueness, i.e. the large collecting area, good spectral resolution, and the high sensitivity in the hard X-ray band. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | STEFAN IMMLER | USA | 3 | AO3 | SUZAKU OBSERVATIONS OF X-RAY BRIGHT SUPERNOVAE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703026010/ | Quick Look | ![]() |
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212 | ESO 103- G 035 | 279.5941 | -65.4238 | 278.351287 | -65.467222 | 275.354112 | -42.161198 | 329.78379096 | -23.17817546 | 291.5832 | 54761.6331597222 | 2008-10-22 15:11:45 | 54764.1717476852 | 2008-10-25 04:07:19 | 703031010 | 91.442 | 80 | 91.442 | 91.45 | 0 | 91.45 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81.0096 | 81.0096 | 219.282 | 2 | PROCESSED | 57544.3339467593 | 2016-06-05 08:00:53 | 55148 | 2009-11-13 00:00:00 | 54782.4220023148 | 2008-11-12 10:07:41 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031322 | X-ray observations of Seyfert 2 have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by the AGN Unification Scheme. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (80 ksec each) of three bright Compton-thin Seyfert 2 galaxies, selected from the Swift/BAT survey, with a hard X-ray flux exceeding 9e-11cgs, to form a flux-limited sample. The unprecedented bandpass of Suzaku offers a unique tool to investigate the X-ray emission of these sources, allowing us to put strong constraints on the reprocessing matter in Seyfert 2s. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | VALENTINA BRAITO | USA | 3 | AO3 | THE NATURE OF THE X-RAY ABSORBER IN SEYFERT 2 GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703031010/ | Quick Look | ![]() |
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213 | Q0551-3637 | 88.2027 | -36.6207 | 87.768974 | -36.630505 | 87.117827 | -60.044705 | 242.37463259 | -26.91966553 | 321.5977 | 54600.5596643518 | 2008-05-14 13:25:55 | 54601.2044444444 | 2008-05-15 04:54:24 | 703036020 | 21.6143 | 22 | 21.6143 | 21.6143 | 0 | 21.6183 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.2831 | 18.2831 | 55.684 | 1 | PROCESSED | 57542.5389236111 | 2016-06-03 12:56:03 | 54979 | 2009-05-28 00:00:00 | 54613.0157060185 | 2008-05-27 00:22:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031334 | Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GEORGE CHARTAS | USA | 3 | AO3 | A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703036020/ | Quick Look | ![]() |
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214 | Q0329-385 | 52.7815 | -38.4067 | 52.316664 | -38.576045 | 34.470474 | -54.910107 | 241.941352 | -54.89845774 | 23.7676 | 54633.4249421296 | 2008-06-16 10:11:55 | 54634.1898611111 | 2008-06-17 04:33:24 | 703038010 | 30.203 | 29 | 30.219 | 30.203 | 0 | 30.219 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.2925 | 25.2925 | 66.082 | 1 | PROCESSED | 57542.8370601852 | 2016-06-03 20:05:22 | 55010 | 2009-06-28 00:00:00 | 54644.1762615741 | 2008-06-27 04:13:49 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031334 | Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GEORGE CHARTAS | USA | 3 | AO3 | A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703038010/ | Quick Look | ![]() |
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215 | ESO 548-G081 | 55.4927 | -21.1949 | 54.941134 | -21.353755 | 46.730142 | -39.596754 | 213.74761618 | -50.8353425 | 69.3236 | 55046.3350462963 | 2009-08-03 08:02:28 | 55047.1946064815 | 2009-08-04 04:40:14 | 704026010 | 39.4112 | 40 | 39.4192 | 39.4192 | 0 | 39.4112 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36.1429 | 36.1429 | 74.2599 | 0 | PROCESSED | 57548.0531481482 | 2016-06-09 01:16:32 | 55427 | 2010-08-19 00:00:00 | 55060.8071875 | 2009-08-17 19:22:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041402 | The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | LISA WINTER | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704026010/ | Quick Look | ![]() |
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216 | MCG +04-22-042 | 140.9461 | 22.9693 | 140.230202 | 23.184366 | 136.125191 | 7.311314 | 205.9821846 | 43.11036681 | 106.3587 | 55157.3309259259 | 2009-11-22 07:56:32 | 55158.2634143518 | 2009-11-23 06:19:19 | 704028010 | 40.962 | 40 | 40.994 | 40.962 | 0 | 40.986 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 35.8969 | 35.8969 | 80.5599 | 0 | PROCESSED | 57549.5187384259 | 2016-06-10 12:26:59 | 55542 | 2010-12-12 00:00:00 | 55176.1858101852 | 2009-12-11 04:27:34 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041402 | The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | LISA WINTER | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704028010/ | Quick Look | ![]() |
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217 | 1H0323+342 | 51.1507 | 34.2411 | 50.363828 | 34.065013 | 57.518057 | 15.07869 | 155.67406743 | -18.71640786 | 76.7168 | 55038.1604513889 | 2009-07-26 03:51:03 | 55040.2084722222 | 2009-07-28 05:00:12 | 704034010 | 84.0884 | 80 | 84.0884 | 84.2404 | 0 | 84.3524 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74.2979 | 74.2979 | 176.9379 | 0 | PROCESSED | 57548.0010532407 | 2016-06-09 00:01:31 | 55419 | 2010-08-11 00:00:00 | 55050.8162847222 | 2009-08-07 19:35:27 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041408 | Recent radio observations reveal blazar-like properties in some radio-loud narrow line Seyfert-1 AGNs. 1H0323+342, classified as this class of AGNs, shows prominent hard X-ray emission with a hard photon index. Since the spectrum in hard X-ray is reminiscent of blazar, its X-ray spectrum seems to have different components originated from disk and jet. Thanks to sensitive X-ray detectors extending to the hard X-ray band, Suzaku observation is expected to resolve a possible multi-component structure in the spectrum. Since beamed radiation from jet is highly variable, spectral temporal behavior is also vital information to distinguish the emission origin. As this source is located relatively nearby (z=0.061), the source is an excellent target to investigate the emission from disk and jet. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MASAAKI HAYASHIDA | USA | 4 | AO4 | SUZAKU OBSERVATION OF 1H0323+342: A PECULIAR SEYFERT-1 --PROBING THE DISK AND JET CONNECTION IN AGN-- | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704034010/ | Quick Look | ![]() |
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218 | MCG0208 | 43.0963 | -8.5129 | 42.484335 | -8.717227 | 37.842662 | -23.868775 | 185.55840319 | -55.88722126 | 57.4541 | 55016.0987037037 | 2009-07-04 02:22:08 | 55017.2134722222 | 2009-07-05 05:07:24 | 704045010 | 42.9115 | 40 | 42.9435 | 42.9115 | 0 | 42.9195 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36.7878 | 36.7878 | 96.286 | 5 | PROCESSED | 57547.7724768518 | 2016-06-08 18:32:22 | 55395 | 2010-07-18 00:00:00 | 55027.1160532407 | 2009-07-15 02:47:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041414 | We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | EZEQUIEL TREISTER | USA | 4 | AO4 | THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704045010/ | Quick Look | ![]() |
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219 | SDSS J1352+4239 | 208.1832 | 42.6476 | 207.663098 | 42.893525 | 184.337785 | 49.439251 | 88.11360974 | 70.09649039 | 316.6443 | 54984.9959375 | 2009-06-02 23:54:09 | 54985.7502199074 | 2009-06-03 18:00:19 | 704050010 | 32.0745 | 30 | 32.0825 | 32.0745 | 0 | 32.0825 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29.5021 | 29.5021 | 65.1639 | 0 | PROCESSED | 57547.4324652778 | 2016-06-08 10:22:45 | 55364 | 2010-06-17 00:00:00 | 54994.4273032407 | 2009-06-12 10:15:19 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041422 | BALQSOs can be used to probe geometric and evolutionary models of quasars and AGN feedback. Recent studies have found larger (~2X) BALQSO fractions in NIR selected samples compared to those in optical samples and have suggested that the NIR samples of BALQSOs better represent the general population of BALQSOs. We propose to observe three bright, red 2MASS selected BALQSOs with Suzaku, to complement archival X-ray observations of BALQSOs that may have been biased by their selection on optical properties only. Combined with the archival sample, we will measure the average X-ray properties of BALQSOs. By comparing the hard X-ray to K_s band flux ratios at a range of optical to infrared colors, we will test the robustness of NIR selection and the origin of the large NIR BALQSO fraction. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | XINYU DAI | USA | 4 | AO4 | X-RAY PROPERTIES OF 2MASS SELECTED BALQSOS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704050010/ | Quick Look | ![]() |
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220 | SDSS J0943+5417 | 145.8252 | 54.2751 | 144.963883 | 54.504193 | 127.754031 | 37.9036 | 161.23003018 | 46.41565232 | 274.2141 | 54975.5889236111 | 2009-05-24 14:08:03 | 54976.3473611111 | 2009-05-25 08:20:12 | 704052010 | 34.2264 | 30 | 34.2264 | 34.2264 | 0 | 34.2264 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.0591 | 32.0591 | 65.5179 | 2 | PROCESSED | 57546.6638773148 | 2016-06-07 15:55:59 | 55358 | 2010-06-11 00:00:00 | 54992.6588888889 | 2009-06-10 15:48:48 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041422 | BALQSOs can be used to probe geometric and evolutionary models of quasars and AGN feedback. Recent studies have found larger (~2X) BALQSO fractions in NIR selected samples compared to those in optical samples and have suggested that the NIR samples of BALQSOs better represent the general population of BALQSOs. We propose to observe three bright, red 2MASS selected BALQSOs with Suzaku, to complement archival X-ray observations of BALQSOs that may have been biased by their selection on optical properties only. Combined with the archival sample, we will measure the average X-ray properties of BALQSOs. By comparing the hard X-ray to K_s band flux ratios at a range of optical to infrared colors, we will test the robustness of NIR selection and the origin of the large NIR BALQSO fraction. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | XINYU DAI | USA | 4 | AO4 | X-RAY PROPERTIES OF 2MASS SELECTED BALQSOS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704052010/ | Quick Look | ![]() |
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221 | CEN A S LOBE NO. 2 | 200.3949 | -45.1401 | 199.658837 | -44.878468 | 217.502785 | -33.539168 | 308.49497877 | 17.40582221 | 289.0008 | 55419.7766087963 | 2010-08-11 18:38:19 | 55420.9641087963 | 2010-08-12 23:08:19 | 705033010 | 81.3878 | 80 | 81.3958 | 81.3878 | 0 | 81.4038 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 68.1085 | 68.1085 | 102.5858 | 0 | PROCESSED | 57552.9708564815 | 2016-06-13 23:18:02 | 55812 | 2011-09-08 00:00:00 | 55445.267662037 | 2010-09-06 06:25:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051401 | We propose a set of four pointings (200 ks), to study the X-ray emission from the Southern giant lobe of the radio galaxy Cen A. Those lobes clearly separated from the central source, have been detected as a source of diffuse gamma-ray emission by the Fermi Telescope. The goal of the Suzaku observations is two-fold: first, to measure the diffuse component of the non-thermal X-ray emission with both the XIS and the HXD in order to determine the details of the distribution of the radiating relativistic particles (and B field), and second, to measure the thermal emission from the lobes (using primarily the XIS), to determine temperature and density of the X-ray emitting plasma, which, via consideration of pressure balance, will determine the content of energetic protons (cosmic rays). | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GRZEGORZ MADEJSKI | USA | 5 | AO5 | SUZAKU OBSERVATIONS OF THE SOUTHERN LOBE OF CEN A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705033010/ | Quick Look | ![]() |
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222 | 1RXS J111706.3+20141 | 169.2749 | 20.2432 | 168.614437 | 20.516401 | 162.09404 | 14.35752 | 225.56577108 | 67.37465885 | 120.2309 | 55510.3081944444 | 2010-11-10 07:23:48 | 55511.1543402778 | 2010-11-11 03:42:15 | 705036010 | 34.2125 | 32 | 34.2125 | 34.2125 | 0 | 34.2125 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31.5366 | 31.5366 | 73.0979 | 0 | PROCESSED | 57554.0402199074 | 2016-06-15 00:57:55 | 55903 | 2011-12-08 00:00:00 | 55537.0979050926 | 2010-12-07 02:20:59 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051402 | High frequency peaked BL Lacs are a peculiar subclass of Blazars characterized by non-thermal emission across the whole electromagnetic spectrum. Their spectral energy distributions (SEDs) include two main components: a low-energy component with power peaking in the range from the UV to the X-ray band, and a substantial high-energy component often dominated by gamma-rays. We propose 3 observations (32 ks each) of a selected sample of HBLs to study the behavior of the first component, widely interpreted as synchrotron radiation. First, we will be able to disentangle between different spectral shapes of the synchrotron SED of HBLs. Second, we will use the proposed observations to investigate the properties of the most representative sample of TeV candidate HBLs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | FRANCESCO MASSARO | USA | 5 | AO5 | X-RAY CURVED SPECTRA IN HIGH FREQUENCY PEAKED BL LACS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705036010/ | Quick Look | ![]() |
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223 | 3C111 | 64.5838 | 38.0329 | 63.747646 | 37.911608 | 69.36811 | 16.396021 | 161.66828978 | -8.81804056 | 76.1726 | 55453.9599768518 | 2010-09-14 23:02:22 | 55455.7432986111 | 2010-09-16 17:50:21 | 705040030 | 80.3659 | 80 | 80.3819 | 80.3659 | 0 | 80.3819 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.9533 | 70.9533 | 154.0639 | 2 | PROCESSED | 57553.468599537 | 2016-06-14 11:14:47 | 55835 | 2011-10-01 00:00:00 | 55469.3718287037 | 2010-09-30 08:55:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051412 | Using our Suzaku observations we discovered ultra-fast outflows (UFOs) in radio-loud Broad-Line Radio Galaxies, with velocities v/c~0.04--0.15 and carrying a mass of the same order as the accretion mass. The bright BLRG 3C~111 was selected for an in-depth study of its UFO through its predicted variability on timescales of approximately one week. We propose 3 Suzaku pointings of 80~ks each separated by one week to determine the gas geometrical, physical, and dynamical characteristics and start addressing its role for the jet-disk connection in radio-loud AGN. Additionally, we will obtain a simultaneous radio-to-GeV Spectral Energy Distribution and model the relative contributions of the accretion and non-thermal components. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RITA SAMBRUNA | USA | 5 | AO5 | PROBING THE ULTRA-FAST OUTFLOW IN 3C 111 WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705040030/ | Quick Look | ![]() |
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224 | MKN 590 | 33.6477 | -0.7713 | 33.009436 | -1.003927 | 31.140057 | -13.460103 | 163.51612886 | -56.94122484 | 251.1273 | 55587.0949652778 | 2011-01-26 02:16:45 | 55588.2146990741 | 2011-01-27 05:09:10 | 705043020 | 40.9139 | 150 | 40.9219 | 40.9219 | 0 | 40.9139 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.8699 | 37.8699 | 96.7339 | 1 | PROCESSED | 57600.7810763889 | 2016-07-31 18:44:45 | 55988 | 2012-03-02 00:00:00 | 55621.2137731482 | 2011-03-01 05:07:50 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051433 | We propose a 150 ks Suzaku long-look to study the Compton reflection component, soft excess, ionized emission and possible ionized reflection of the Seyfert 1.2 AGN Mkn 590, which has an unobscured line of sight or "bare nucleus" and as of yet unquantified reflection. We aim to accurately constrain the geometry of the circumnuclear material and determine the ionization states of both the Compton-thin and Compton-thick material surrounding the black hole by studying the origin of the soft excess, determining the likelihood of ionized reflection and accurately measuring the intensity of neutral, H-like and He-like Fe emission lines. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | ELIZABETH RIVERS | USA | 5 | AO5 | QUANTIFYING THE COMPTON REFLECTION AND IONIZED EMISSION IN MKN 590 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705043020/ | Quick Look | ![]() |
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225 | NGC 4945 | 196.3636 | -49.4659 | 195.633608 | -49.198211 | 217.017818 | -38.639251 | 305.27160994 | 13.34216317 | 120.2557 | 55590.0873842593 | 2011-01-29 02:05:50 | 55591.1182175926 | 2011-01-30 02:50:14 | 705047050 | 46.1076 | 40 | 46.1076 | 46.1076 | 0 | 46.1076 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54.0907 | 54.0907 | 89.0518 | 0 | PROCESSED | 57600.8100810185 | 2016-07-31 19:26:31 | 55969 | 2012-02-12 00:00:00 | 55602.2238194445 | 2011-02-10 05:22:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051442 | We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GUIDO RISALITI | USA | 5 | AO5 | HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705047050/ | Quick Look | ![]() |
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226 | SWIFTJ2344.6-424322 | 356.1059 | -42.7624 | 355.44614 | -43.040118 | 336.666972 | -37.094539 | 339.65324523 | -69.27134863 | 225.0657 | 55505.2812731482 | 2010-11-05 06:45:02 | 55506.5570601852 | 2010-11-06 13:22:10 | 705049010 | 61.7416 | 60 | 61.7416 | 61.7416 | 0 | 61.7416 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50.3941 | 50.3941 | 110.2118 | 1 | PROCESSED | 57553.9985532407 | 2016-06-14 23:57:55 | 55885 | 2011-11-20 00:00:00 | 55518.3162847222 | 2010-11-18 07:35:27 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051443 | We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195 keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log(L_x) > 45.5 erg/sec) absorbed type II QSOs in the local universe and the most ripe for study with Suzaku. The newly discovered source SWIFT J2344.6-4233 at a redshift of z=0.6 is the most luminous object in the BAT sample with log(L_x) = 46.5 erg/sec. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | WAYNE BAUMGARTNER | USA | 5 | AO5 | SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705049010/ | Quick Look | ![]() |
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227 | SMC X-1 | 19.2724 | -73.4484 | 18.941012 | -73.711562 | 312.330249 | -66.473862 | 300.41553375 | -43.55429702 | 25.8573 | 55691.0197337963 | 2011-05-10 00:28:25 | 55691.4064814815 | 2011-05-10 09:45:20 | 706030040 | 17.9054 | 18 | 17.9214 | 17.9214 | 0 | 17.9054 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.8143 | 16.8143 | 33.4079 | 0 | PROCESSED | 57601.9922222222 | 2016-08-01 23:48:48 | 56068 | 2012-05-21 00:00:00 | 55701.1543981482 | 2011-05-20 03:42:20 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JOSEPH NEILSEN | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030040/ | Quick Look | ![]() |
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228 | SMC X-1 | 19.2675 | -73.4407 | 18.935881 | -73.70387 | 312.347206 | -66.469935 | 300.41598527 | -43.56211574 | 204.2035 | 55875.0768055556 | 2011-11-10 01:50:36 | 55875.6182291667 | 2011-11-10 14:50:15 | 706030080 | 19.8598 | 18 | 19.8881 | 19.8961 | 0 | 19.8598 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 19.2508 | 19.2508 | 46.772 | 0 | PROCESSED | 57603.7203587963 | 2016-08-03 17:17:19 | 56260 | 2012-11-29 00:00:00 | 55890.6941203704 | 2011-11-25 16:39:32 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JOSEPH NEILSEN | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030080/ | Quick Look | ![]() |
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229 | SMC X-1 | 19.2681 | -73.4483 | 18.936643 | -73.711469 | 312.329443 | -66.472676 | 300.41718915 | -43.55456404 | 342.3682 | 56005.2598611111 | 2012-03-19 06:14:12 | 56005.8452546296 | 2012-03-19 20:17:10 | 706030100 | 18.5821 | 18 | 18.6263 | 18.6343 | 0 | 18.5821 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 20.3061 | 20.3061 | 50.5719 | 0 | PROCESSED | 57604.9618055556 | 2016-08-04 23:05:00 | 56399 | 2013-04-17 00:00:00 | 56022.2021296296 | 2012-04-05 04:51:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JOSEPH NEILSEN | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030100/ | Quick Look | ![]() |
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230 | III ZW 2 | 2.6244 | 10.9839 | 1.981573 | 10.705729 | 6.801457 | 9.029508 | 106.97577765 | -50.61513425 | 67.4163 | 55726.9877893518 | 2011-06-14 23:42:25 | 55728.9792708333 | 2011-06-16 23:30:09 | 706031010 | 81.466 | 80 | 81.466 | 81.466 | 0 | 81.466 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74.3629 | 74.3629 | 172.0397 | 3 | PROCESSED | 57602.3450925926 | 2016-08-02 08:16:56 | 56127 | 2012-07-19 00:00:00 | 55757.7040046296 | 2011-07-15 16:53:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061411 | Fermi-LAT has revealed gamma-ray emission from Seyfert galaxies in its 1st catalog. Optical and X-ray spectra of Seyferts generally provide important clues to the nature of the accretion process, and thus those objects are promising targets to investigate the connection of the jet to the central source. Here, we propose Suzaku observations of three Seyfert-type AGNs from our gamma-ray candidate list: those objects are also present in the Swift-BAT catalog. Those are III Zw 2, NGC 6814 and ESO 323-G077 and we request pointings of 80 ks, 40 ks and 40 ks respectively. All three candidates appear to be associated with AGN, but show different radio or IR properties. Suzaku data will give us crucial information to investigate the origin of high-energy emission from those Seyfert objects. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MASAAKI HAYASHIDA | USA | 6 | AO6 | SUZAKU OBSERVATIONS OF SEYFERT GALAXIES AS GAMMA-RAY SOURCE CANDIDATES SELECTED FROM THE SWIFT-BAT CATALOG | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706031010/ | Quick Look | ![]() |
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231 | ESO 323-G077 | 196.6073 | -40.4236 | 195.900559 | -40.156267 | 212.090645 | -30.55227 | 306.0162391 | 22.35835315 | 295.8925 | 55762.647337963 | 2011-07-20 15:32:10 | 55763.4168287037 | 2011-07-21 10:00:14 | 706033010 | 44.1222 | 40 | 44.1222 | 44.1222 | 0 | 44.1222 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.9258 | 40.9258 | 66.4819 | 0 | PROCESSED | 57602.6188310185 | 2016-08-02 14:51:07 | 56212 | 2012-10-12 00:00:00 | 55845.2395949074 | 2011-10-11 05:45:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061411 | Fermi-LAT has revealed gamma-ray emission from Seyfert galaxies in its 1st catalog. Optical and X-ray spectra of Seyferts generally provide important clues to the nature of the accretion process, and thus those objects are promising targets to investigate the connection of the jet to the central source. Here, we propose Suzaku observations of three Seyfert-type AGNs from our gamma-ray candidate list: those objects are also present in the Swift-BAT catalog. Those are III Zw 2, NGC 6814 and ESO 323-G077 and we request pointings of 80 ks, 40 ks and 40 ks respectively. All three candidates appear to be associated with AGN, but show different radio or IR properties. Suzaku data will give us crucial information to investigate the origin of high-energy emission from those Seyfert objects. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MASAAKI HAYASHIDA | USA | 6 | AO6 | SUZAKU OBSERVATIONS OF SEYFERT GALAXIES AS GAMMA-RAY SOURCE CANDIDATES SELECTED FROM THE SWIFT-BAT CATALOG | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706033010/ | Quick Look | ![]() |
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232 | 1622-297 | 246.5282 | -29.8629 | 245.741591 | -29.750241 | 249.573082 | -8.070344 | 348.81494865 | 13.309894 | 287.0011 | 55828.8879166667 | 2011-09-24 21:18:36 | 55829.1800810185 | 2011-09-25 04:19:19 | 706044010 | 8.7781 | 10 | 8.7781 | 8.7781 | 0 | 8.7781 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 8.7513 | 8.7513 | 25.198 | 0 | PROCESSED | 57603.2321064815 | 2016-08-03 05:34:14 | 56236 | 2012-11-05 00:00:00 | 55868.9351851852 | 2011-11-03 22:26:40 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061601 | We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | SVETLANA JORSTAD | USA | 6 | AO6 | EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706044010/ | Quick Look | ![]() |
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233 | 4C38.41 | 248.824 | 38.1186 | 248.386993 | 38.220121 | 236.373082 | 59.10929 | 61.06470824 | 42.32788618 | 255.0463 | 55829.1891666667 | 2011-09-25 04:32:24 | 55829.4148032407 | 2011-09-25 09:57:19 | 706045010 | 8.9239 | 10 | 8.9319 | 8.9319 | 0 | 8.9239 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.5353 | 9.5353 | 19.4719 | 0 | PROCESSED | 57603.2349305556 | 2016-08-03 05:38:18 | 56225 | 2012-10-25 00:00:00 | 55875.6235185185 | 2011-11-10 14:57:52 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061601 | We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | SVETLANA JORSTAD | USA | 6 | AO6 | EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706045010/ | Quick Look | ![]() |
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234 | HOLMBERG IX X-1 | 149.4435 | 69.0486 | 148.425456 | 69.287009 | 119.776016 | 51.672601 | 141.95726659 | 41.07139178 | 311.5635 | 56030.7575810185 | 2012-04-13 18:10:55 | 56034.6807175926 | 2012-04-17 16:20:14 | 707019010 | 182.5274 | 500 | 182.5274 | 182.5274 | 0 | 182.5274 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 208.6236 | 208.6236 | 338.9339 | 3 | PROCESSED | 57605.2861342593 | 2016-08-05 06:52:02 | 56018 | 2012-04-01 00:00:00 | 56044.4614699074 | 2012-04-27 11:04:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071251 | Recent X-ray observations have found evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in a super-Eddington state. Current data are unable to deliver a clear answer, but the diagnostics possible in a long observation will be decisive. We request a 500 ks observation of the ULX Holmberg IX X-1 to place crucial constraints on atomic features that would signal a super-Eddington flow. Detecting or ruling out atomic features naturally requires a deep exposure. The strong spectral constraints derived will reveal the nature of the accreting black holes in these systems. A definitive statement on the existence of 100-1000 Msun black holes or extreme accretion states will be an important Suzaku legacy. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JON MILLER | USA | 7 | AO7 | A DECISIVE LEGACY OBSERVATION OF AN ULTRALUMINOUS X-RAY SOURCE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707019010/ | Quick Look | ![]() |
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235 | HOLMBERG IX X-1 | 149.4877 | 69.0751 | 148.469613 | 69.31362 | 119.77363 | 51.703415 | 141.9165022 | 41.0686989 | 124.501 | 56221.770162037 | 2012-10-21 18:29:02 | 56224.1252083333 | 2012-10-24 03:00:18 | 707019020 | 107.4958 | 320 | 107.4958 | 107.4958 | 0 | 107.4958 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 106.8673 | 106.8673 | 203.4479 | 1 | PROCESSED | 57607.8555324074 | 2016-08-07 20:31:58 | 56018 | 2012-04-01 00:00:00 | 56330.5864930556 | 2013-02-07 14:04:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071251 | Recent X-ray observations have found evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in a super-Eddington state. Current data are unable to deliver a clear answer, but the diagnostics possible in a long observation will be decisive. We request a 500 ks observation of the ULX Holmberg IX X-1 to place crucial constraints on atomic features that would signal a super-Eddington flow. Detecting or ruling out atomic features naturally requires a deep exposure. The strong spectral constraints derived will reveal the nature of the accreting black holes in these systems. A definitive statement on the existence of 100-1000 Msun black holes or extreme accretion states will be an important Suzaku legacy. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JON MILLER | USA | 7 | AO7 | A DECISIVE LEGACY OBSERVATION OF AN ULTRALUMINOUS X-RAY SOURCE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707019020/ | Quick Look | ![]() |
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236 | HOLMBERG IX X-1 | 149.4867 | 69.0744 | 148.468616 | 69.312918 | 119.773774 | 51.702635 | 141.91753226 | 41.06881922 | 124.4999 | 56226.4169097222 | 2012-10-26 10:00:21 | 56228.7717708333 | 2012-10-28 18:31:21 | 707019040 | 110.0175 | 500 | 110.0383 | 110.0175 | 0 | 110.0175 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 105.7961 | 105.7961 | 203.426 | 2 | PROCESSED | 57607.8756018518 | 2016-08-07 21:00:52 | 56018 | 2012-04-01 00:00:00 | 56240.5502430556 | 2012-11-09 13:12:21 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071251 | Recent X-ray observations have found evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in a super-Eddington state. Current data are unable to deliver a clear answer, but the diagnostics possible in a long observation will be decisive. We request a 500 ks observation of the ULX Holmberg IX X-1 to place crucial constraints on atomic features that would signal a super-Eddington flow. Detecting or ruling out atomic features naturally requires a deep exposure. The strong spectral constraints derived will reveal the nature of the accreting black holes in these systems. A definitive statement on the existence of 100-1000 Msun black holes or extreme accretion states will be an important Suzaku legacy. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JON MILLER | USA | 7 | AO7 | A DECISIVE LEGACY OBSERVATION OF AN ULTRALUMINOUS X-RAY SOURCE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707019040/ | Quick Look | ![]() |
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237 | NGC 4151 | 182.642 | 39.4132 | 182.010684 | 39.69131 | 164.095796 | 36.629182 | 155.04475012 | 75.06022062 | 134.3454 | 56242.8428472222 | 2012-11-11 20:13:42 | 56245.9599537037 | 2012-11-14 23:02:20 | 707024010 | 150.2669 | 150 | 150.2829 | 150.2669 | 0 | 150.2829 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 150.5465 | 150.5465 | 269.2897 | 4 | PROCESSED | 57608.0679861111 | 2016-08-08 01:37:54 | 56702 | 2014-02-14 00:00:00 | 56330.6348032407 | 2013-02-07 15:14:07 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071417 | We propose simultaneous NuSTAR/Suzaku observations of NGC 4151 and IC 4329A. These pointings will achieve three goals: (1) They will provide the best-ever broad-band X-ray spectra of two of the brightest Seyfert galaxies in the 0.5-80 keV band; (2) They will enable broad-band, time-resolved X-ray spectroscopy of these fascinating and variable sources; (3) They will serve as invaluable calibration targets for the two observatories. The spectral coverage and sensitivity will enable the continuum, absorption and reflection components of each spectrum to be conclusively disentangled, allowing us to determine whether inner disk reflection signatures are present. We will also be able to break the degeneracy between the coronal temperature and optical depth in both AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | LAURA BRENNEMAN | USA | 7 | AO7 | SHEDDING NEW LIGHT ON THE BROAD-BAND X-RAY SPECTRA OF NGC 4151 AND IC 4329A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707024010/ | Quick Look | ![]() |
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238 | NGC 5252 | 204.5663 | 4.5481 | 203.934961 | 4.801923 | 201.032031 | 13.744519 | 331.30380316 | 64.80829028 | 117.6998 | 56287.8794791667 | 2012-12-26 21:06:27 | 56289.0952777778 | 2012-12-28 02:17:12 | 707028010 | 50.2701 | 45 | 50.2701 | 50.2921 | 0 | 50.2766 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.3367 | 43.3367 | 105.0278 | 0 | PROCESSED | 57608.3760300926 | 2016-08-08 09:01:29 | 56687 | 2014-01-30 00:00:00 | 56321.5462268518 | 2013-01-29 13:06:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071424 | A hard X-ray-selected (BAT) AGN sample shows a remarkable 70% of the local population of type 1 AGN to have extreme hard excesses above 20 keV, likely caused by Compton-thick gas in the line-of-sight, covering at least 50% of the source. We request six snapshot observations to complete a Suzaku survey of a BAT-flux-limited sample and make a complete and unbiased measurement of the incidence. Analysis of the new sources will be performed in conjunction with existing exposures, providing exciting new insight into the previously unknown structures in hard X-ray selected AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TRACEY TURNER | USA | 7 | AO7 | INVESTIGATING COMPTON-THICK ABSORBERS IN TYPE 1 AGN: OVERHAULING THE AGN PARADIGM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707028010/ | Quick Look | ![]() |
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239 | PDS 456 | 262.0802 | -14.261 | 261.369515 | -14.22093 | 262.220782 | 8.966234 | 10.39487872 | 11.16781955 | 96.2511 | 56344.8907407407 | 2013-02-21 21:22:40 | 56349.993912037 | 2013-02-26 23:51:14 | 707035010 | 182.299 | 450 | 182.299 | 182.299 | 0 | 182.299 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 160.3071 | 160.3071 | 440.8752 | 4 | PROCESSED | 57610.7549768518 | 2016-08-10 18:07:10 | 56018 | 2012-04-01 00:00:00 | 56363.6993981482 | 2013-03-12 16:47:08 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071431 | PDS 456 is the most luminous nearby (z=0.184) AGN, more typical of quasars at high redshift. A 2007 Suzaku observation resolved iron K absorption at 9 keV in the QSO frame, moving at near relativistic velocities (0.25c). A follow-up 2011 observation was highly absorbed and showed a direct response of the iron K absorber to a decrease in the ionizing flux, while the harder photons lag behind the soft, by 10^4 secs. We propose to monitor the remarkable spectral variability and outflow from PDS 456, through a deep 450ks Suzaku observation. We wish to:- (i) quantify the time lags and determine the location of the reprocessor, (ii) determine the origin and timescale of the absorber variability and (iii) measure the hard X-ray variability from a Compton thick absorber in PDS 456. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | JAMES REEVES | USA | 7 | AO7 | VARIABILITY AND REVERBERATION OF THE QUASAR WIND IN PDS 456 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707035010/ | Quick Look | ![]() |
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240 | PDS 456 | 262.0805 | -14.2617 | 261.369811 | -14.221632 | 262.221115 | 8.965551 | 10.39443055 | 11.16720212 | 96.2512 | 56354.8215972222 | 2013-03-03 19:43:06 | 56359.5001388889 | 2013-03-08 12:00:12 | 707035020 | 164.8107 | 450 | 164.8267 | 164.8107 | 0 | 164.8291 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 147.4496 | 147.4496 | 404.1815 | 2 | PROCESSED | 57610.8342824074 | 2016-08-10 20:01:22 | 56018 | 2012-04-01 00:00:00 | 56373.6804166667 | 2013-03-22 16:19:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071431 | PDS 456 is the most luminous nearby (z=0.184) AGN, more typical of quasars at high redshift. A 2007 Suzaku observation resolved iron K absorption at 9 keV in the QSO frame, moving at near relativistic velocities (0.25c). A follow-up 2011 observation was highly absorbed and showed a direct response of the iron K absorber to a decrease in the ionizing flux, while the harder photons lag behind the soft, by 10^4 secs. We propose to monitor the remarkable spectral variability and outflow from PDS 456, through a deep 450ks Suzaku observation. We wish to:- (i) quantify the time lags and determine the location of the reprocessor, (ii) determine the origin and timescale of the absorber variability and (iii) measure the hard X-ray variability from a Compton thick absorber in PDS 456. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | JAMES REEVES | USA | 7 | AO7 | VARIABILITY AND REVERBERATION OF THE QUASAR WIND IN PDS 456 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707035020/ | Quick Look | ![]() |
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241 | 0836+710 | 130.3582 | 70.9091 | 129.096 | 71.086996 | 109.311372 | 50.162038 | 143.52368034 | 34.42368753 | 111.9979 | 56213.6030787037 | 2012-10-13 14:28:26 | 56213.8223726852 | 2012-10-13 19:44:13 | 707042010 | 10.613 | 10 | 10.613 | 10.613 | 0 | 10.613 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.866 | 8.866 | 18.9279 | 0 | PROCESSED | 57607.7537615741 | 2016-08-07 18:05:25 | 56598 | 2013-11-02 00:00:00 | 56232.4320717593 | 2012-11-01 10:22:11 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071601 | We propose to perform two 2-week multi-frequency campaigns of observations of a sample of gamma-ray blazars during Fermi Cycle 5. The campaigns will involve: (1) gamma-ray monitoring with the Fermi LAT, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B, V, R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku and Swift; (6) mid-IR measurements with IRTF; and (7) near-IR photometric J, H, and K observations. The research aims i) to search for correlated variability on short timescales; ii) to compile SEDs at different states of gamma-ray and radio jet activitiy; and iii) to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | SVETLANA JORSTAD | USA | 7 | AO7 | MULTI-FREQUENCY CAMPAIGNS TO STUDY RAPID VARIABILITY IN GAMMA_RAY BLAZARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707042010/ | Quick Look | ![]() |
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242 | BL LAC | 330.6707 | 42.2941 | 330.154473 | 42.052039 | 354.261979 | 49.60384 | 92.59387966 | -10.42383814 | 77.7587 | 56431.6193981482 | 2013-05-19 14:51:56 | 56431.8724884259 | 2013-05-19 20:56:23 | 707044010 | 12.7426 | 10 | 12.7506 | 12.7426 | 0 | 12.7506 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.144 | 13.144 | 21.8319 | 0 | PROCESSED | 57611.320625 | 2016-08-11 07:41:42 | 56826 | 2014-06-18 00:00:00 | 56455.7300231482 | 2013-06-12 17:31:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071601 | We propose to perform two 2-week multi-frequency campaigns of observations of a sample of gamma-ray blazars during Fermi Cycle 5. The campaigns will involve: (1) gamma-ray monitoring with the Fermi LAT, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B, V, R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku and Swift; (6) mid-IR measurements with IRTF; and (7) near-IR photometric J, H, and K observations. The research aims i) to search for correlated variability on short timescales; ii) to compile SEDs at different states of gamma-ray and radio jet activitiy; and iii) to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | SVETLANA JORSTAD | USA | 7 | AO7 | MULTI-FREQUENCY CAMPAIGNS TO STUDY RAPID VARIABILITY IN GAMMA_RAY BLAZARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707044010/ | Quick Look | ![]() |
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243 | MKN 335 | 1.5767 | 20.2085 | 0.933785 | 19.930185 | 9.740922 | 17.859652 | 108.75946317 | -41.41793251 | 71.5257 | 56454.1494907407 | 2013-06-11 03:35:16 | 56457.9792824074 | 2013-06-14 23:30:10 | 708016010 | 143.995 | 300 | 144.027 | 143.995 | 0 | 144.027 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 129.5529 | 129.5529 | 330.8674 | 3 | PROCESSED | 57611.6156828704 | 2016-08-11 14:46:35 | 56383 | 2013-04-01 00:00:00 | 56470.7662037037 | 2013-06-27 18:23:20 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081411 | The idea of this proposal is trigger a 300ks observation with Suzaku of the Narrow Line Seyfert 1 Galaxy Mkn 335 during one of its low X-ray flux states. The goal here is to measure its underlying broad-band continuum with Suzaku during a low state and compare it with the 2006 high-state observations. Mkn 335 is one of the best examples of an AGN that went into a deep minimum X-ray flux state. Two competing models can explain these extreme low states: reflection models and partial covering absorber models. Both models still require a variable underlying intrinsic continuum. The science driver is to find out what is causing these low X-ray flux states that have been observed in several NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | DIRK GRUPE | USA | 8 | AO8-TOO | INTRINSIC LOW-STATE X-RAY LUMINOSITY OF THE NLS1 MKN 335 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708016010/ | Quick Look | ![]() |
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244 | MCG-5-23-16 | 146.9232 | -30.945 | 146.373955 | -30.712416 | 162.623211 | -41.142672 | 262.74537578 | 17.2400137 | 295.4404 | 56444.9213194444 | 2013-06-01 22:06:42 | 56448.2467361111 | 2013-06-05 05:55:18 | 708021010 | 159.5262 | 300 | 159.5582 | 159.5262 | 0 | 159.5582 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 155.1267 | 155.1267 | 287.3018 | 1 | PROCESSED | 57611.525787037 | 2016-08-11 12:37:08 | 56383 | 2013-04-01 00:00:00 | 56461.789537037 | 2013-06-18 18:56:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081416 | Significant recent developments in probing environments around AGN black holes has been achieved using X-ray reverberation. They were initially detected in the soft excess of several NLS1s, then recently, the first Fe K reverberation was also seen. In addition to measuring x-rays reverberating a few r_g from the event horizon, short/long delays from different radii have been separated for the first time in NGC4151. Here we propose to observe MCG-5-23-1 for 300 ks in order to study its iron K reverberation. It is optimally one of the brightest and most variable AGN in X-rays. Archival data already show very exciting signatures of Fe K reverberation. With new observations we aim to constrain the emitting region size and study the emission originating at different distances from of the hole. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ABDERAHMEN ZOGHBI | USA | 8 | AO8 | IRON K REVERBERATION IN MCG 5-23-16 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708021010/ | Quick Look | ![]() |
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245 | NGC 235A | 10.7176 | -23.5378 | 10.098982 | -23.81167 | 359.839777 | -25.738096 | 94.13393297 | -85.9211578 | 213.1719 | 56636.0921759259 | 2013-12-10 02:12:44 | 56636.4792939815 | 2013-12-10 11:30:11 | 708026010 | 19.8251 | 20 | 19.8331 | 19.8251 | 0 | 19.8409 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.2251 | 18.2251 | 33.4439 | 1 | PROCESSED | 57613.5511921296 | 2016-08-13 13:13:43 | 56383 | 2013-04-01 00:00:00 | 56646.6871412037 | 2013-12-20 16:29:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081419 | The BAT AGN sample constitutes an unprecedented all-sky hard X-ray survey of the local AGN population. However, to properly model the X-ray absorption & reflection, coverage below 10 keV is needed with CCD spectral resolution and adequate signal-to-noise. We propose to observe 11 AGN with Suzaku, which will increase the completeness of a flux-limited sample with such coverage from 85 to 158 sources. The 11 AGN only have severely underexposed Swift XRT coverage below 10 keV whereas the remaining sources have either Suzaku or XMM coverage. The Suzaku data have the additional advantage of sensitivity above 10 keV that helps to mitigate the long time-baseline of the BAT spectra. The new observations will create a significantly enhanced legacy data set that will provide value for years to come. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TAHIR YAQOOB | USA | 8 | AO8 | ROBUST CHARACTERIZATION OF ABSORPTION AND REFLECTION IN A LOCAL FLUX-LIMITED AGN POPULATION FROM THE SWIFT BAT SURVEY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708026010/ | Quick Look | ![]() |
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246 | CENTAURUS A | 201.3699 | -43.0194 | 200.636516 | -42.759434 | 217.141069 | -31.326977 | 309.51956362 | 19.416494 | 303.7255 | 56519.1824305556 | 2013-08-15 04:22:42 | 56519.4264930556 | 2013-08-15 10:14:09 | 708036010 | 10.6751 | 10 | 10.6751 | 10.6751 | 0 | 10.6911 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.0647 | 10.0647 | 21.0799 | 0 | PROCESSED | 57612.2554050926 | 2016-08-12 06:07:47 | 56954 | 2014-10-24 00:00:00 | 56587.7389351852 | 2013-10-22 17:44:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081433 | We request observations of the nucleus of the radio galaxy Centaurus A to study time variability of its broadband spectral energy distribution (SED) and constrain jet emission models of radio-loud AGN. Due to its proximity, Cen A can be studied in unique detail. Although frequently observed, no time-dependent, simultaneous SEDs covering the spectrum from radio to gamma-rays have been obtained for Cen A so far. Since AGN are highly variable, only quasi-contemporaneous SEDs allow us to constrain parameters of jet emission models. Combining our TANAMI radio Very Long Baseline Interferometry monitoring campaign and Fermi observations with simultaneous Suzaku spectra will fill the gap in energy and address the time-dependent behavior of jet emission and torus absorption with high accuracy. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | ROOPESH OJHA | USA | 8 | AO8 | SIMULTANEOUS SUZAKU AND MULTIWAVELENGTH OBSERVATIONS OF THE NUCLEUS OF CENTAURUS A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708036010/ | Quick Look | ![]() |
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247 | CENTAURUS A | 201.3033 | -43.0014 | 200.570255 | -42.741318 | 217.080563 | -31.331883 | 309.47108059 | 19.44109405 | 111.5377 | 56663.4710763889 | 2014-01-06 11:18:21 | 56663.6613888889 | 2014-01-06 15:52:24 | 708036020 | 7.3652 | 10 | 7.3652 | 7.3732 | 0 | 7.3732 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6.5444 | 6.5444 | 16.4399 | 0 | PROCESSED | 57613.7500462963 | 2016-08-13 18:00:04 | 57086 | 2015-03-05 00:00:00 | 56719.7206944444 | 2014-03-03 17:17:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081433 | We request observations of the nucleus of the radio galaxy Centaurus A to study time variability of its broadband spectral energy distribution (SED) and constrain jet emission models of radio-loud AGN. Due to its proximity, Cen A can be studied in unique detail. Although frequently observed, no time-dependent, simultaneous SEDs covering the spectrum from radio to gamma-rays have been obtained for Cen A so far. Since AGN are highly variable, only quasi-contemporaneous SEDs allow us to constrain parameters of jet emission models. Combining our TANAMI radio Very Long Baseline Interferometry monitoring campaign and Fermi observations with simultaneous Suzaku spectra will fill the gap in energy and address the time-dependent behavior of jet emission and torus absorption with high accuracy. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | ROOPESH OJHA | USA | 8 | AO8 | SIMULTANEOUS SUZAKU AND MULTIWAVELENGTH OBSERVATIONS OF THE NUCLEUS OF CENTAURUS A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708036020/ | Quick Look | ![]() |
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248 | ABELL 998 | 156.5862 | 67.9284 | 155.666008 | 68.182911 | 124.296815 | 52.261797 | 140.87284378 | 43.80315875 | 119.4303 | 56601.7924768518 | 2013-11-05 19:01:10 | 56602.9584722222 | 2013-11-06 23:00:12 | 708041010 | 60.2402 | 60 | 60.2402 | 60.2404 | 0 | 60.2562 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 51.856 | 51.856 | 100.7319 | 2 | PROCESSED | 57613.2563657407 | 2016-08-13 06:09:10 | 56980 | 2014-11-19 00:00:00 | 56614.6831944444 | 2013-11-18 16:23:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081533 | We propose to map out the core of the A981 supercluster with three Suzaku observations. The A981 supercluster contains four Abell richness class 2 clusters within a redshift range of 2,000 km/s. All four clusters also overlap within their virial radii, at least in projection. The low and steady background of the Suzaku telescope is ideal for studying the low surface brightness X-ray emission between the clusters. Such observations will determine if the clusters are interacting via the detection of merger-induced shocks or perturbed features in the outskirts of the individual clusters. Our proposed Suzaku observations will help elucidate the fundamental astrophysics that occurs during the formation of very massive clusters. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | LAURENCE DAVID | USA | 8 | AO8 | MAPPING THE ABELL 981 SUPER CLUSTER WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708041010/ | Quick Look | ![]() |
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249 | HOLMBERG IX X-1 | 149.4663 | 69.0509 | 148.44846 | 69.289367 | 119.784926 | 51.679022 | 141.94846823 | 41.07666025 | 284.4995 | 57158.2357291667 | 2015-05-16 05:39:27 | 57159.0827546296 | 2015-05-17 01:59:10 | 709015040 | 34.12 | 30 | 34.12 | 34.128 | 0 | 34.128 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.6575347222 | 2016-08-18 15:46:51 | 57536 | 2016-05-28 00:00:00 | 57168.6253935185 | 2015-05-26 15:00:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091251 | Broadband X-ray spectroscopy of ultraluminous X-ray sources (ULXs) with NuSTAR and Suzaku has begun to provide important information regarding the nature of these enigmatic sources. Recent NuSTAR observations of the extreme ULX Holmberg IX X-1 revealed unusual spectral variability, and different competing evolutionary scenarios can explain the available data. Resolving this degeneracy is critical to determining the nature of the accretion onto this source, and requires multi-epoch broadband spectroscopy probing a more diverse range of fluxes. We propose to undertake 4x30 ks coordinated Suzaku+NuSTAR observations of Holmberg IX X-1 to provide the additional spectra needed to robustly determine the nature of the observed evolution, providing a vital step in our understanding of extreme ULXs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | DOMINIC WALTON | USA | 9 | AO9 | MULTI-EPOCH BROADBAND X-RAY SPECTROSCOPY OF HOLMBERG IX X-1 WITH SUZAKU AND NUSTAR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709015040/ | Quick Look | ![]() |
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250 | HE0512-3329 | 78.5445 | -33.4308 | 78.084109 | -33.487216 | 72.678048 | -56.186874 | 236.61833373 | -33.85137764 | 251.0519 | 57071.9701388889 | 2015-02-18 23:17:00 | 57072.4937847222 | 2015-02-19 11:51:03 | 709020030 | 25.0955 | 26 | 25.0955 | 25.0955 | 0 | 25.0955 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6171296296 | 2016-08-17 14:48:40 | 57457 | 2016-03-10 00:00:00 | 57087.4623726852 | 2015-03-06 11:05:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091431 | The origin of AGN iron K alpha emission has been debated for two decades. We propose to constrain iron line emission sizes using quasar X-ray microlensing. Our Chandra Cycle 11 observations have shown that the iron line equivalent widths (EWs) in six lensed systems are significantly higher than those measured in local AGNs. This implies that the iron line emission is microlensed more strongly than the X-ray continuum and originates from very compact regions. We propose to confirm the high iron line EWs in lensed quasars by monitoring two more lenses, Q0142-100 and HE0512+3329 using Suzaku, with a total exposure time 115 kilo-seconds. This will provide independent constraints for settling the debate on the origin of the iron line emission. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | BIN CHEN | USA | 9 | AO9 | CONSTRAINING QUASAR IRON LINE EMISSION USING MICROLENSING | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709020030/ | Quick Look | ![]() |
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251 | ABELL2801 | 9.6433 | -29.1188 | 9.027926 | -29.393572 | 356.054774 | -30.312746 | 357.12193154 | -86.53506096 | 232.0377 | 53701.3547106482 | 2005-11-27 08:30:47 | 53702.1668865741 | 2005-11-28 04:00:19 | 800008010 | 34.89 | 25 | 34.89 | 34.89 | 34.89 | 34.89 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 30.1636 | 30.1636 | 70.1639 | 1 | PROCESSED | 57528.0891898148 | 2016-05-20 02:08:26 | 54247 | 2007-05-27 00:00:00 | 54038.3717361111 | 2006-10-30 08:55:18 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001025 | We propose to observe the central region of the Sculptor supercluster at z=0.11, in a search for the theoretically predicted Warm/Hot Intergalactic Medium (WHIM). The WHIM has been 'missing' observationally, until recent detection of the X-ray absorption due to the ionized light elements in the background quasar spectra. Still there is no confident detection of the expected soft X-ray emission. This is mainly because that the X-ray brightness is very low, compared to the Galactic diffuse emission in the soft X-ray band and/or the spectral sensitivity of previous experiments are limited. To separate the expected X-ray lines of the WHIM (mainly O VII) from the Galactic emission, we select an unique supercluster at z>0.1. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | TAKAYUKI TAMURA | JAP | 0 | SWG | THE SCULPTOR SUPERCLUSTER: SEARCH FOR THE WARM/HOT INTERGALACTIC MEDIUM | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800008010/ | Quick Look | ![]() |
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252 | ABELL 1795 Near North | 207.2221 | 26.7993 | 206.645445 | 27.047459 | 193.815884 | 35.172187 | 34.737463 | 77.20142043 | 130.7334 | 53714.7756481482 | 2005-12-10 18:36:56 | 53715.3203587963 | 2005-12-11 07:41:19 | 800012020 | 24.4106 | 25 | 24.4266 | 24.4106 | 24.4426 | 24.4346 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 25.1798 | 25.1798 | 47.0559 | 2 | PROCESSED | 57532.404375 | 2016-05-24 09:42:18 | 54247 | 2007-05-27 00:00:00 | 54038.8804166667 | 2006-10-30 21:07:48 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001056 | We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MARK BAUTZ | JAP | 0 | SWG | TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800012020/ | Quick Look | ![]() |
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253 | ABELL 1795 Near South | 207.2228 | 26.4007 | 206.645046 | 26.648859 | 194.026663 | 34.812966 | 32.94964182 | 77.16185549 | 129.833 | 53715.9739467593 | 2005-12-11 23:22:29 | 53716.5355787037 | 2005-12-12 12:51:14 | 800012040 | 26.074 | 25 | 26.098 | 26.0919 | 26.074 | 26.086 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25.7986 | 25.7986 | 48.522 | 1 | PROCESSED | 57532.4329282407 | 2016-05-24 10:23:25 | 54247 | 2007-05-27 00:00:00 | 54039.0706018518 | 2006-10-31 01:41:40 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001056 | We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MARK BAUTZ | JAP | 0 | SWG | TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800012040/ | Quick Look | ![]() |
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254 | NGC4388 | 186.4461 | 12.6674 | 185.812197 | 12.944186 | 180.780806 | 14.166666 | 279.11809751 | 74.34084148 | 119.622 | 53728.3779976852 | 2005-12-24 09:04:19 | 53731.250162037 | 2005-12-27 06:00:14 | 800017010 | 123.6341 | 100 | 123.9249 | 125.8143 | 123.6341 | 124.1523 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 111.8209 | 111.8209 | 248.128 | 3 | PROCESSED | 57532.5484143518 | 2016-05-24 13:09:43 | 54247 | 2007-05-27 00:00:00 | 54039.5984375 | 2006-10-31 14:21:45 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001077 | Large-scale X-ray nebulae up to a few tens of kpc have been often found in starburst galaxies, which is thermally heated up by the superwind from the starburst nucleus. Iwasawa et al. (2003) found a large X-ray nebula up to 16kpc around NGC4388, which is photoiionized by Seyfert nucleus. Thus, this result suggests that the hard X-ray emission from active galactic nucleus could be a prime heat source of nebula. The goals of this observation are (1) to see how far the X-ray nebula is extended, (2) to obtain its precise X-ray spectrum, (3) to determine what is the X-ray emission mechanism, and (4) to exam if the photoionization by AGN could be a prime heat source of the galactic halo. We determine the photon index and the high energy cut-off of the power-law component from the HXD spectrum. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | TAKESHI TSURU | JAP | 0 | SWG | VERY EXTENDED PHOTOIONIZED X-RAY NEBULA AROUND THE SEYFERT GALAXY NGC4388 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800017010/ | Quick Look | ![]() |
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255 | Z8276 | 266.0474 | 32.9693 | 265.586798 | 32.989586 | 263.998981 | 56.326696 | 57.88393681 | 27.65216461 | 308.1365 | 53961.1406134259 | 2006-08-14 03:22:29 | 53961.4723958333 | 2006-08-14 11:20:15 | 801079010 | 14.9374 | 14 | 14.9374 | 14.9374 | 14.9374 | 14.9374 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 15.462 | 15.462 | 28.658 | 0 | PROCESSED | 57535.267962963 | 2016-05-27 06:25:52 | 54391 | 2007-10-18 00:00:00 | 54018.6023842593 | 2006-10-10 14:27:26 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801079010/ | Quick Look | ![]() |
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256 | BOOTES GROUP 26 | 219.0541 | 33.7727 | 218.530502 | 33.989642 | 201.885156 | 45.915481 | 55.78379271 | 66.53529007 | 323.2958 | 54265.160787037 | 2007-06-14 03:51:32 | 54266.3092476852 | 2007-06-15 07:25:19 | 802055010 | 43.6657 | 38 | 43.6737 | 43.6817 | 0 | 43.6657 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38.8727 | 38.8727 | 99.2108 | 0 | PROCESSED | 57538.9553703704 | 2016-05-30 22:55:44 | 54695 | 2008-08-17 00:00:00 | 54271.4809837963 | 2007-06-20 11:32:37 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021424 | We propose four 30 ksec Suzaku pointings (120 ksec total) to obtain Lx and Tx for 4 distant (0.15 < z < 0.35) galaxy groups discovered in a contiguous, 9.3 sq. deg Chandra survey in Bootes. Our targets are spatially resolved by Chandra and are chosen to minimize point-source contamination of the Suzaku group spectra. The XIS data will significantly expand the sample of groups with known temperature in this redshift range, and so will improve constraints on group evolution mechanisms. We will use the existing, deep multicolor imaging and 20,000-object spectroscopic catalog for Bootes to study the effect of local environment on group properties, as well as the relationship between optically-selected and X-ray selected groups, for the first time in this redshift range. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MARSHALL BAUTZ | USA | 2 | AO2 | SUZAKU SPECTROSCOPY OF DISTANT GALAXY GROUPS IN BOOTES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802055010/ | Quick Look | ![]() |
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257 | PKS 0745-191 | 116.8852 | -19.2901 | 116.331446 | -19.165404 | 123.663194 | -39.639458 | 236.4397894 | 3.03527791 | 293.9994 | 54231.0124884259 | 2007-05-11 00:17:59 | 54231.8216898148 | 2007-05-11 19:43:14 | 802062010 | 32.0065 | 30 | 32.0065 | 32.0305 | 0 | 32.0145 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.7016 | 27.7016 | 69.9099 | 0 | PROCESSED | 57538.6154976852 | 2016-05-30 14:46:19 | 54695 | 2008-08-17 00:00:00 | 54238.8868518518 | 2007-05-18 21:17:04 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021440 | PKS 0745-191 is the X-ray brightest galaxy cluster beyond a redshift of 0.1. It has a smooth surface brightness profile and appears relaxed. Using the low background of Suzaku we will measure the temperature of the intracluster medium to the virial radius of the cluster. Its high temperature means that we will be unaffected by any loss of effective area at low energies. In addition the cluster is bright enough so that the bremsstrahlung emission will be easily detected using the PIN detector. This will allow us to search for any nonthermal component as well as accurately determining the high temperature components in the cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ANDREW YOUNG | USA | 2 | AO2 | PKS 0745-191: THE BRIGHTEST CLUSTER BEYOND Z=0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802062010/ | Quick Look | ![]() |
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258 | PKS 0745-191 | 117.1155 | -19.3739 | 116.561976 | -19.248204 | 123.963107 | -39.669924 | 236.62179243 | 3.1809503 | 294.0002 | 54233.2263773148 | 2007-05-13 05:25:59 | 54234.0369675926 | 2007-05-14 00:53:14 | 802062040 | 32.9092 | 30 | 32.9092 | 32.9092 | 0 | 32.9092 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 31.0085 | 31.0085 | 69.9999 | 0 | PROCESSED | 57538.6488541667 | 2016-05-30 15:34:21 | 54695 | 2008-08-17 00:00:00 | 54245.5354861111 | 2007-05-25 12:51:06 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021440 | PKS 0745-191 is the X-ray brightest galaxy cluster beyond a redshift of 0.1. It has a smooth surface brightness profile and appears relaxed. Using the low background of Suzaku we will measure the temperature of the intracluster medium to the virial radius of the cluster. Its high temperature means that we will be unaffected by any loss of effective area at low energies. In addition the cluster is bright enough so that the bremsstrahlung emission will be easily detected using the PIN detector. This will allow us to search for any nonthermal component as well as accurately determining the high temperature components in the cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ANDREW YOUNG | USA | 2 | AO2 | PKS 0745-191: THE BRIGHTEST CLUSTER BEYOND Z=0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802062040/ | Quick Look | ![]() |
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259 | NGC1961BACKGROUND | 85.5048 | 67.8763 | 84.182746 | 67.851301 | 87.633372 | 44.47331 | 145.2497599 | 18.81010884 | 72.0206 | 54748.602962963 | 2008-10-09 14:28:16 | 54749.1197222222 | 2008-10-10 02:52:24 | 803041010 | 24.1435 | 20 | 24.1435 | 24.1435 | 0 | 24.1435 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.099 | 20.099 | 44.6399 | 1 | PROCESSED | 57544.0915393518 | 2016-06-05 02:11:49 | 55148 | 2009-11-13 00:00:00 | 54780.6911342593 | 2008-11-10 16:35:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031401 | Galaxies are missing most of their baryons when compared to the cosmological baryon to dark matter ratio. The Milky Way is missing at least 70% of its baryons while lower mass galaxies retain less than 10% of their baryons. Theory suggests that these baryons were expelled by intense galactic winds during the primary star formation period. These galactic winds carry gas far beyond the virial radius of small and modest galaxies, but the most massive galaxies should retain much of this gas. We propose to test this picture by searching for the missing baryons surrounding the very massive spiral galaxy, NGC 1961, which has 10 times the stellar content of M31 and with v_rot = 450 km/sec. If successful, we will detect a significant fraction of the 5E11 Msun of its missing baryons. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JOEL BREGMAN | USA | 3 | AO3 | THE BARYONS CONTENT OF THE MOST MASSIVE SPIRAL GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803041010/ | Quick Look | ![]() |
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260 | ABELL S753 RELIC | 211.0241 | -34.0331 | 210.287956 | -33.79356 | 220.862622 | -20.093047 | 319.70505054 | 26.46102153 | 102.5257 | 54838.0480555556 | 2009-01-07 01:09:12 | 54841.6668287037 | 2009-01-10 16:00:14 | 803053010 | 137.5275 | 120 | 137.5355 | 137.5275 | 0 | 137.5355 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 99.5992 | 99.5992 | 312.6056 | 3 | PROCESSED | 57545.2410069444 | 2016-06-06 05:47:03 | 55328 | 2010-05-12 00:00:00 | 54851.4730787037 | 2009-01-20 11:21:14 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031432 | The cluster radio relic PKS B1400-33 in the poor cluster Abell S753 will be observed with the HXD/PIN to detect and characterize the nonthermal Inverse Compton emission. This is one of the brightest cluster radio relics known. Remarkably, it is associated with a relatively poor, cool cluster. Although it has many properties similar to other cluster radio relics, it is possible that it is an old radio lobe, displaced by motions or buoyancy. The HXD/PIN data will be a strong test of merger shock acceleration processes. The XIS observations will constrain the low energy nonthermal spectrum and determine the thermal gas properties near the relic, and allow a merger shock to be detected. The long exposure with the XIS will also provide accurate abundances for the gas in this cool cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CRAIG SARAZIN | USA | 3 | AO3 | PKS B1400-33 AND ABELL S753: A VERY BRIGHT RADIO RELIC IN A POOR CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803053010/ | Quick Look | ![]() |
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261 | A3112 | 49.4785 | -44.2477 | 49.044044 | -44.429449 | 25.501128 | -58.962889 | 252.95565297 | -56.08416767 | 11.0983 | 54609.240162037 | 2008-05-23 05:45:50 | 54611.0557638889 | 2008-05-25 01:20:18 | 803054010 | 67.4982 | 60 | 67.4982 | 67.4982 | 0 | 67.4982 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 59.0658 | 59.0658 | 156.8578 | 0 | PROCESSED | 57542.6456365741 | 2016-06-03 15:29:43 | 54988 | 2009-06-06 00:00:00 | 54620.3684490741 | 2008-06-03 08:50:34 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031434 | We propose to perform spatially resolved spectroscopy on the X-ray bright relaxed galaxy cluster Abell 3112, in order to characterize its soft/hard X-ray excess component. Abell 3112 is one of two clusters with very strong soft excess emission (the other being Abell S1101, observed in AO1). The indications provided by this observation will be crucial in order to assess, beyond doubt, the reality of the soft excess emission, previously observed by all soft X-ray missions since EUVE. The proposed observation will constrain the nature of the excess emitter, and address outstanding questions in observational cosmology: the {it missing baryon} problem, the density of matter in the universe and the non-thermal energy in galaxy clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MASSIMILIANO BONAMENTE | USA | 3 | AO3 | SOFT EXCESS, HARD EXCESS AND THERMAL EMISSION IN ABELL 3112 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803054010/ | Quick Look | ![]() |
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262 | SHAPLEY OFF-FILAMENT | 201.0894 | -30.5701 | 200.390777 | -30.309695 | 211.196223 | -20.080758 | 311.26734846 | 31.76827748 | 298.8248 | 54666.4273958333 | 2008-07-19 10:15:27 | 54670.1905439815 | 2008-07-23 04:34:23 | 803068010 | 143.4669 | 140 | 143.4749 | 143.4749 | 0 | 143.4669 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 110.8111 | 110.8111 | 325.0858 | 2 | PROCESSED | 57543.1803240741 | 2016-06-04 04:19:40 | 55073 | 2009-08-30 00:00:00 | 54707.3575694444 | 2008-08-29 08:34:54 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031451 | It is, in principle, possible to search for the signature of the Warm-Hot Intergalactic Medium (WHIM) in regions between clusters, where WHIM filaments are expected. However, the complexity of the filament network and the distance between clusters makes this approach very difficult (if not impossible), except in few cases where several clusters are sufficiently close together, such as within a supercluster. We propose an investigation using Suzaku of a region within the Shapley Supercluster where, following the cluster network, a filament is expected and a ROSAT PSPC investigation has found excess emission. Suzaku s characteristics will allow a clear detection and characterization of the filament. A second observation in an empty region nearby will be used as control field. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MASSIMILIANO GALEAZZI | USA | 3 | AO3 | FILAMENTARY X-RAY STRUCTURE IN THE SHAPLEY SUPERCLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803068010/ | Quick Look | ![]() |
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263 | SMC X-1 | 19.2661 | -73.446 | 18.934565 | -73.709172 | 312.334379 | -66.471359 | 300.41753301 | -43.55692043 | 64.0051 | 55740.5953819444 | 2011-06-28 14:17:21 | 55741.0960069444 | 2011-06-29 02:18:15 | 706030060 | 18.6682 | 18 | 18.7129 | 18.7049 | 0 | 18.6682 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 20.6764 | 20.6764 | 43.2479 | 0 | PROCESSED | 57602.4222800926 | 2016-08-02 10:08:05 | 56163 | 2012-08-24 00:00:00 | 55775.167974537 | 2011-08-02 04:01:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JOSEPH NEILSEN | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030060/ | Quick Look | ![]() |
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264 | NGC 669 | 26.8113 | 35.5683 | 26.082401 | 35.319076 | 38.038857 | 22.814409 | 135.52840833 | -25.9346715 | 67.5273 | 55017.2207523148 | 2009-07-05 05:17:53 | 55018.4377777778 | 2009-07-06 10:30:24 | 804049010 | 50.2528 | 50 | 50.2608 | 50.2528 | 0 | 50.2608 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 45.4023 | 45.4023 | 105.1199 | 11 | PROCESSED | 57547.7727430556 | 2016-06-08 18:32:45 | 55395 | 2010-07-18 00:00:00 | 55029.2656944444 | 2009-07-17 06:22:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041504 | Galaxies are missing most of their baryons when compared to the cosmological baryon to dark matter ratio: the Milky Way retained only 30% of its baryons while lower mass galaxies retain less than 10%. Probably, these baryons were expelled by intense galactic winds during the early star formation period at z = 1-3. These galactic winds can carry gas far beyond the virial radius of small and modest galaxies, but the most massive galaxies should retain much of this gas. We propose to test this picture by searching for the missing baryons surrounding two extremely massive spiral galaxies, with 6-8 times the stellar content of M31 and with v_rot = 370, 420 km/s. If successful, we will detect a significant fraction of the 3-4E11 Msun of the missing baryons as hot gas. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | JOEL BREGMAN | USA | 4 | AO4 | THE BARYON CONTENT OF MASSIVE SPIRAL GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804049010/ | Quick Look | ![]() |
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265 | RXJ1159+5531 | 179.953 | 55.611 | 179.309735 | 55.889319 | 149.803846 | 49.191232 | 137.55848692 | 60.02702904 | 317.8793 | 54953.4172222222 | 2009-05-02 10:00:48 | 54955.52875 | 2009-05-04 12:41:24 | 804051010 | 85.4892 | 75 | 85.4972 | 85.4892 | 0 | 85.4972 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82.4128 | 82.4128 | 182.4218 | 2 | PROCESSED | 57546.517974537 | 2016-06-07 12:25:53 | 55343 | 2010-05-27 00:00:00 | 54976.1055439815 | 2009-05-25 02:31:59 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041514 | We propose a 75ks observation of the galaxy group RXJ1159+5531 to place definitive constraints on its gas out to the virial radius (Rvir). These unprecedented measurements will enable us to study the entropy profile at scales near the region in which accretion shocks become important, and will reveal whether its flattening outside the core of the group extends as far as Rvir. Furthermore, we will obtain the mass profile and test the validity of the NFW model in the outer parts of the halo. Due to its high surface brightness and favourable distance, RXJ1159+5531 is the ideal target with which to carry out this study. It will constitute a textbook case for constraining the feedback and other nongravitational processes which shape the distribution of hot gas in galaxy groups. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | PHILIP HUMPHREY | USA | 4 | AO4 | GAS IN A GALAXY GROUP AT THE VIRIAL RADIUS: RXJ1159+5531, A TEXTBOOK EXAMPLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804051010/ | Quick Look | ![]() |
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266 | NGC741MOSAICE_P1 | 29.7199 | 5.461 | 29.066489 | 5.218433 | 29.574235 | -6.258595 | 152.014798 | -53.55912322 | 71.7248 | 55053.8433796296 | 2009-08-10 20:14:28 | 55054.0834837963 | 2009-08-11 02:00:13 | 804052010 | 10.8302 | 10 | 10.8342 | 10.8302 | 0 | 10.8381 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 7.8627 | 7.8627 | 20.74 | 0 | PROCESSED | 57548.1137847222 | 2016-06-09 02:43:51 | 55448 | 2010-09-09 00:00:00 | 55081.2096875 | 2009-09-07 05:01:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JOEL BREGMAN | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804052010/ | Quick Look | ![]() |
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267 | NGC741MOSAICS_P4 | 29.2193 | 5.0492 | 28.567063 | 4.805449 | 28.959637 | -6.470888 | 151.55342081 | -54.14565062 | 71.7599 | 55053.1534259259 | 2009-08-10 03:40:56 | 55053.3759143518 | 2009-08-10 09:01:19 | 804054040 | 10.589 | 10 | 10.597 | 10.589 | 0 | 10.589 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.9689 | 9.9689 | 19.1919 | 0 | PROCESSED | 57548.09625 | 2016-06-09 02:18:36 | 55451 | 2010-09-12 00:00:00 | 55084.9935763889 | 2009-09-10 23:50:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JOEL BREGMAN | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804054040/ | Quick Look | ![]() |
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268 | ABELL 426 E1 | 50.3027 | 41.5257 | 49.474155 | 41.346372 | 58.885391 | 22.278944 | 150.79331238 | -13.10366228 | 89.0025 | 55041.5144560185 | 2009-07-29 12:20:49 | 55041.7141666667 | 2009-07-29 17:08:24 | 804056010 | 9.696 | 10 | 9.696 | 9.696 | 0 | 9.696 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.856 | 7.856 | 17.2479 | 0 | PROCESSED | 57547.9587268518 | 2016-06-08 23:00:34 | 55419 | 2010-08-11 00:00:00 | 55050.256400463 | 2009-08-07 06:09:13 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804056010/ | Quick Look | ![]() |
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269 | ABELL 426 E5 | 51.7975 | 41.5108 | 50.964978 | 41.337079 | 60.044403 | 21.962427 | 151.74947693 | -12.48443224 | 87.0002 | 55042.7485069444 | 2009-07-30 17:57:51 | 55043.2932175926 | 2009-07-31 07:02:14 | 804060010 | 21.649 | 20 | 21.649 | 21.9423 | 0 | 21.929 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 22.1391 | 22.1391 | 47.0481 | 0 | PROCESSED | 57548.0130208333 | 2016-06-09 00:18:45 | 55427 | 2010-08-19 00:00:00 | 55060.702349537 | 2009-08-17 16:51:23 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804060010/ | Quick Look | ![]() |
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270 | ABELL 426 N3 | 49.4023 | 42.2033 | 48.571812 | 42.020646 | 58.391407 | 23.116315 | 149.83616068 | -12.90614214 | 59.9986 | 55062.4722106482 | 2009-08-19 11:19:59 | 55062.7542708333 | 2009-08-19 18:06:09 | 804065010 | 12.2498 | 10 | 12.2498 | 12.2498 | 0 | 12.2498 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.8582 | 11.8582 | 24.3619 | 0 | PROCESSED | 57548.2751157407 | 2016-06-09 06:36:10 | 55441 | 2010-09-02 00:00:00 | 55074.9931597222 | 2009-08-31 23:50:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804065010/ | Quick Look | ![]() |
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271 | ABELL 426 N7 | 48.6285 | 43.1676 | 47.793828 | 42.98212 | 58.096043 | 24.202758 | 148.81295674 | -12.39950143 | 59.9993 | 55064.6340509259 | 2009-08-21 15:13:02 | 55065.4329166667 | 2009-08-22 10:23:24 | 804069010 | 36.4901 | 30 | 36.4901 | 36.5101 | 0 | 36.5021 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.3696 | 30.3696 | 69.018 | 0 | PROCESSED | 57548.3120486111 | 2016-06-09 07:29:21 | 55441 | 2010-09-02 00:00:00 | 55075.0667708333 | 2009-09-01 01:36:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804069010/ | Quick Look | ![]() |
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272 | RCS0928+3646 | 142.0898 | 36.7798 | 141.319732 | 36.998258 | 132.498761 | 20.704213 | 186.98438508 | 46.37223207 | 116.6063 | 55148.3222800926 | 2009-11-13 07:44:05 | 55149.1064699074 | 2009-11-14 02:33:19 | 804080010 | 36.5167 | 30 | 36.5327 | 36.5167 | 0 | 36.5327 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.0584 | 27.0584 | 67.7439 | 1 | PROCESSED | 57549.3099652778 | 2016-06-10 07:26:21 | 55546 | 2010-12-16 00:00:00 | 55180.0365972222 | 2009-12-15 00:52:42 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041525 | Understanding relationships between baryons in galaxy clusters and the underlying dark matter distributions is crucial for using clusters as cosmological probes. Recent work indicates massive low-Lx clusters at all redshifts, in conflict with self-similarity predictions. The only way to quantify these findings is to observe a cluster sample chosen independently of X-ray properties. We propose to study 14 clusters at 0.15<z<0.45, for which robust velocity dispersions are measured. We were awarded Chandra observations of 8 high-dispersion, low-z targets. Suzaku s superior throughput is required to probe the low-dispersion, high-z side of the distribution. We propose XIS observations of the remaining 6 targets, allowing us to rigorously assess baryon content in an unbiased sample of clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | AMALIA HICKS | USA | 4 | AO4 | DECIPHERING CLUSTER OBSERVABLES: TRACING THE BARYONS IN CLUSTERS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804080010/ | Quick Look | ![]() |
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273 | A1795_FAR_NORTHEAST | 207.4803 | 26.8793 | 206.904436 | 27.126887 | 194.02783 | 35.343989 | 35.17669327 | 76.97815393 | 300.5693 | 55010.6105439815 | 2009-06-28 14:39:11 | 55011.5556712963 | 2009-06-29 13:20:10 | 804082010 | 40.0263 | 35 | 40.0263 | 40.0263 | 0 | 40.0263 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57547.6967476852 | 2016-06-08 16:43:19 | 55395 | 2010-07-18 00:00:00 | 55026.4466087963 | 2009-07-14 10:43:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041528 | The outer regions of clusters beyond 0.5 r200 contain a large amount of the dark matter, baryons and metals in the system, yet they are poorly understood. We propose to conduct a new test of cluster and structure formation by probing the distribution of dark matter and the thermodynamic history of the ICM in the outskirts of the cluster Abell 1795. Our previous Suzaku observations of Abell 1795 indicate deviations from hydrostatic equilibrium; we sample two disjoint regions beyond r500, detecting cluster emission in one but not the other (a difference of 5-sigma). With the proposed observations spanning r500-r200, we will obtain a more sensitive measurement of the azimuthally averaged temperature and density at this radius and search for variations over a wider range of azimuth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 4 | AO4 | ABELL 1795 WITH SUZAKU: A NEW WINDOW ON CLUSTER FORMATION AND STRUCTURE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804082010/ | Quick Look | ![]() |
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274 | A1795_FAR_WEST | 206.824 | 26.695 | 206.246184 | 26.94403 | 193.479611 | 34.924294 | 34.12189199 | 77.54661564 | 300.5663 | 55008.5840625 | 2009-06-26 14:01:03 | 55009.4634143518 | 2009-06-27 11:07:19 | 804084010 | 35.4763 | 35 | 35.4843 | 35.4763 | 0 | 35.4843 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.3466 | 30.3466 | 75.9378 | 1 | PROCESSED | 57547.7077662037 | 2016-06-08 16:59:11 | 55395 | 2010-07-18 00:00:00 | 55022.2936458333 | 2009-07-10 07:02:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041528 | The outer regions of clusters beyond 0.5 r200 contain a large amount of the dark matter, baryons and metals in the system, yet they are poorly understood. We propose to conduct a new test of cluster and structure formation by probing the distribution of dark matter and the thermodynamic history of the ICM in the outskirts of the cluster Abell 1795. Our previous Suzaku observations of Abell 1795 indicate deviations from hydrostatic equilibrium; we sample two disjoint regions beyond r500, detecting cluster emission in one but not the other (a difference of 5-sigma). With the proposed observations spanning r500-r200, we will obtain a more sensitive measurement of the azimuthally averaged temperature and density at this radius and search for variations over a wider range of azimuth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 4 | AO4 | ABELL 1795 WITH SUZAKU: A NEW WINDOW ON CLUSTER FORMATION AND STRUCTURE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804084010/ | Quick Look | ![]() |
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275 | A2204_FIELD_2 | 248.1003 | 5.3993 | 247.484152 | 5.504515 | 245.364183 | 26.985557 | 20.85022945 | 33.23419381 | 260.9996 | 55435.6212615741 | 2010-08-27 14:54:37 | 55436.6744675926 | 2010-08-28 16:11:14 | 805057010 | 39.7312 | 40 | 39.7392 | 39.7312 | 0 | 39.7421 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.3157 | 35.3157 | 90.9818 | 1 | PROCESSED | 57553.2244444445 | 2016-06-14 05:23:12 | 55287 | 2010-04-01 00:00:00 | 55449.2310416667 | 2010-09-10 05:32:42 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805057010/ | Quick Look | ![]() |
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276 | A1413_FIELD_1 | 178.851 | 23.2234 | 178.207267 | 23.50167 | 169.288709 | 20.757468 | 226.97411288 | 76.74388731 | 303.0003 | 55345.0808333333 | 2010-05-29 01:56:24 | 55346.139849537 | 2010-05-30 03:21:23 | 805059010 | 40.2041 | 40 | 40.2041 | 40.2041 | 0 | 40.2041 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.564 | 34.564 | 91.4919 | 1 | PROCESSED | 57551.6776041667 | 2016-06-12 16:15:45 | 55287 | 2010-04-01 00:00:00 | 55365.2529513889 | 2010-06-18 06:04:15 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805059010/ | Quick Look | ![]() |
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277 | NGC5129 OFF-CENTER2 | 201.1253 | 13.7341 | 200.509035 | 13.994301 | 194.045924 | 20.91983 | 334.52733324 | 74.54035563 | 127.8098 | 55548.7900810185 | 2010-12-18 18:57:43 | 55549.42875 | 2010-12-19 10:17:24 | 805073010 | 30.7651 | 30 | 30.7811 | 30.7651 | 0 | 30.7811 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.2475 | 25.2475 | 55.168 | 0 | PROCESSED | 57554.4510416667 | 2016-06-15 10:49:30 | 55960 | 2012-02-03 00:00:00 | 55593.1036805556 | 2011-02-01 02:29:18 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051512 | Using the composite data from dwarf galaxies to rich clusters, we find that the baryon fraction is mainly set by the system's potential well depth. The small scatter of baryon fractions as a function of the gravitational potential well depth indicates a universal baryon loss mechanism for these systems. However, the relation is most poorly constrained in the poor galaxy group regime below 1keV, where few individual measurements exists. Since most galaxies reside in these groups, it is also important to test whether the missing baryons from the galaxies are actually in these poor groups. We propose deep, off-center observations of two such groups, doubling the sample, to better delineate and understand the transition of the baryon loss from clusters to galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | XINYU DAI | USA | 5 | AO5 | BARYON LOSS IN POOR GALAXY GROUPS: DISTINGUISHING PRE-HEATING AND FEEDBACK MODELS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805073010/ | Quick Look | ![]() |
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278 | NGC5129 BACKGROUND | 201.7433 | 13.5725 | 201.127421 | 13.831619 | 194.704871 | 21.009611 | 336.16988197 | 74.1046924 | 116.4041 | 55547.7947106482 | 2010-12-17 19:04:23 | 55548.0397106482 | 2010-12-18 00:57:11 | 805074010 | 12.2767 | 10 | 12.2767 | 12.2847 | 0 | 12.2927 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.7811 | 10.7811 | 21.16 | 0 | PROCESSED | 57554.4321180556 | 2016-06-15 10:22:15 | 55960 | 2012-02-03 00:00:00 | 55592.9616435185 | 2011-01-31 23:04:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051512 | Using the composite data from dwarf galaxies to rich clusters, we find that the baryon fraction is mainly set by the system's potential well depth. The small scatter of baryon fractions as a function of the gravitational potential well depth indicates a universal baryon loss mechanism for these systems. However, the relation is most poorly constrained in the poor galaxy group regime below 1keV, where few individual measurements exists. Since most galaxies reside in these groups, it is also important to test whether the missing baryons from the galaxies are actually in these poor groups. We propose deep, off-center observations of two such groups, doubling the sample, to better delineate and understand the transition of the baryon loss from clusters to galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | XINYU DAI | USA | 5 | AO5 | BARYON LOSS IN POOR GALAXY GROUPS: DISTINGUISHING PRE-HEATING AND FEEDBACK MODELS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805074010/ | Quick Look | ![]() |
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279 | ESO3060170 OFFSET | 85.0343 | -41.2366 | 84.63691 | -41.261684 | 81.30371 | -64.529199 | 246.8664627 | -30.36071331 | 321.0164 | 55326.497025463 | 2010-05-10 11:55:43 | 55327.7204166667 | 2010-05-11 17:17:24 | 805076010 | 78.6782 | 80 | 78.6782 | 78.6862 | 0 | 78.6862 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69.7827 | 69.7827 | 105.6858 | 1 | PROCESSED | 57551.4828240741 | 2016-06-12 11:35:16 | 55707 | 2011-05-26 00:00:00 | 55341.5427893518 | 2010-05-25 13:01:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051513 | We propose 30 and 80 ksec observations of the X-ray brightest fossil group, ESO 3060170. The target pointings will reach to 75% of the virial radius from the center of the galaxy, in order to determine the temperature and metal abundances of group gas at large radii. This will allow us to determine the radial profiles of the gaseous iron mass to stellar light ratio, the relative distributions of ejecta from SN Ia and SN II, the entropy, the total mass to light ratio, and the dark matter concentration for this fossil group. The energy resolution and low background of the XIS instrument are crucial for this study, which will help constrain the evolutional history of this fossil group and tell us how fossil groups relate to normal groups and clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | YUANYUAN SU | USA | 5 | AO5 | HOW DO FOSSIL GROUPS OF GALAXIES DIFFER FROM NORMAL GROUPS? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805076010/ | Quick Look | ![]() |
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280 | PKS 0745-191 | 116.7033 | -18.9048 | 116.14781 | -18.780899 | 123.330634 | -39.304661 | 236.01965558 | 3.07990407 | 294.0011 | 55315.865462963 | 2010-04-29 20:46:16 | 55316.6418518518 | 2010-04-30 15:24:16 | 805084010 | 34.8356 | 35 | 34.8356 | 34.8356 | 0 | 34.8356 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29.5067 | 29.5067 | 67.0759 | 1 | PROCESSED | 57551.3211458333 | 2016-06-12 07:42:27 | 55696 | 2011-05-15 00:00:00 | 55330.1469675926 | 2010-05-14 03:31:38 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051526 | Suzaku has enabled us to make the first measurement of the temperature profile beyond the virial radius of any cluster. The gas in the outskirts of galaxy clusters presents information of astrophysical and cosmological importance. Measurements at the virial radius, where the dominant gas behavior switches from infall to equilibrium, can improve cluster mass estimates. Temperature and entropy profiles in the outskirts describe the accretion history and energy balance of clusters, near where they must match the background properties of the Universe. But these observations are just beginning. How do clusters grow? Are there large scale accretion shocks? To what extent are clusters relaxed? Here we propose to continue our study of PKS 0745-191 using Suzaku's unique capability to map this area. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATTHEW GEORGE | USA | 5 | AO5 | BEYOND THE VIRIAL RADIUS OF PKS 0745-191, THE BRIGHTEST CLUSTER PAST Z=0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805084010/ | Quick Look | ![]() |
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281 | T CRB | 239.8773 | 25.9106 | 239.353591 | 26.051383 | 230.095833 | 45.264151 | 42.36027985 | 48.16117824 | 268.9321 | 53984.9474652778 | 2006-09-06 22:44:21 | 53986.0911921296 | 2006-09-08 02:11:19 | 401043010 | 46.3033 | 50 | 46.3113 | 46.3113 | 46.3193 | 46.3033 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 45.4314 | 45.4314 | 98.8159 | 1 | PROCESSED | 57535.5107175926 | 2016-05-27 12:15:26 | 54526 | 2008-03-01 00:00:00 | 54053.4340856482 | 2006-11-14 10:25:05 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011106 | Hard X-ray emission up to ~100 keV has recently been detected with INTEGRAL and Swift from 3 exceptional symbiotic stars. These 3 objects are members of a subclass of symbiotics characterized by rapid optical flickering, and in some cases jets, recurrent nova eruptions, and high-mass white dwarfs possibly headed toward supernova Type Ia explosion. The origin of the hard X-ray emission from these accreting white dwarfs is a mystery. Broad-band X-ray observations, which only Suzaku can provide, are needed to bridge the gap between existing soft and hard X-ray spectra. We propose to perform such Suzaku observations of RT Cru, T CrB, and RS Oph to distinguish among thermal emission from a magnetic accretion column, non-thermal emission from a jet, or some unforeseen emission mechanism. | GALACTIC POINT SOURCES | 4 | A | JENNIFER SOKOLOSKI | USA | 1 | AO1 | THE NATURE OF HARD X-RAY SYMBIOTIC BINARIES | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401043010/ | Quick Look | ![]() |
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282 | RCS2343-3517 | 355.9933 | -35.2927 | 355.337628 | -35.570369 | 340.879701 | -30.492367 | 359.21699124 | -73.45928386 | 237.6557 | 55523.8239930556 | 2010-11-23 19:46:33 | 55525.0418171296 | 2010-11-25 01:00:13 | 805088010 | 48.3167 | 61 | 48.3167 | 48.3167 | 0 | 48.3167 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.1454 | 40.1454 | 105.1859 | 1 | PROCESSED | 57554.2088078704 | 2016-06-15 05:00:41 | 55903 | 2011-12-08 00:00:00 | 55537.0179861111 | 2010-12-07 00:25:54 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051527 | Understanding relationships between baryons in galaxy clusters and underlying dark matter distributions is crucial for using clusters as cosmological probes. Recent work indicates massive low-Lx clusters at all redshifts, in conflict with self-similarity predictions. The only way to quantify these findings is to observe a sample chosen independently of X-ray properties. We propose to study 13 clusters at 0.15<z<0.45, for which robust velocity dispersions are measured. We were awarded Suzaku/Chandra observations of 11 high-dispersion, low-z targets. Suzaku's superior throughput is required to complete the low-dispersion, high-z side of the distribution. We propose XIS observations of the remaining 2 targets, allowing us to rigorously assess baryon content in an unbiased sample of clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 5 | AO5 | DECIPHERING CLUSTER OBSERVABLES: TRACING THE BARYONS IN CLUSTERS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805088010/ | Quick Look | ![]() |
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283 | IGRJ16465-4507 | 251.6303 | -45.1738 | 250.724808 | -45.083948 | 256.064043 | -22.616175 | 340.00343338 | 0.10772124 | 284.9562 | 53987.3839814815 | 2006-09-09 09:12:56 | 53987.9203009259 | 2006-09-09 22:05:14 | 401052010 | 22.5279 | 20 | 22.5359 | 22.5279 | 22.5359 | 22.5359 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 24.6454 | 24.6454 | 46.332 | 0 | PROCESSED | 57535.4975925926 | 2016-05-27 11:56:32 | 54526 | 2008-03-01 00:00:00 | 54021.113287037 | 2006-10-13 02:43:08 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011132 | INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. | GALACTIC POINT SOURCES | 4 | A | RANDALL SMITH | USA | 1 | AO1 | HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401052010/ | Quick Look | ![]() |
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284 | ABELL 773 | 139.2619 | 51.6127 | 138.389122 | 51.822209 | 124.54102 | 33.911668 | 166.27594696 | 43.26641657 | 277.0001 | 55684.0736342593 | 2011-05-03 01:46:02 | 55684.909212963 | 2011-05-03 21:49:16 | 806027030 | 47.578 | 50 | 47.578 | 47.578 | 0 | 47.578 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.1095 | 44.1095 | 72.1819 | 0 | PROCESSED | 57601.9127083333 | 2016-08-01 21:54:18 | 55652 | 2011-04-01 00:00:00 | 55697.2793518518 | 2011-05-16 06:42:16 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061116 | We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 6 | AO6-LP | THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806027030/ | Quick Look | ![]() |
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285 | ABELL 1068 | 160.1718 | 40.1411 | 159.449793 | 40.402342 | 145.494968 | 29.227943 | 178.75085582 | 60.06234552 | 130.0011 | 55860.7020601852 | 2011-10-26 16:50:58 | 55861.8821527778 | 2011-10-27 21:10:18 | 806028010 | 51.9826 | 50 | 51.9906 | 51.9826 | 0 | 51.9826 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.5347 | 44.5347 | 101.9378 | 1 | PROCESSED | 57603.6168981482 | 2016-08-03 14:48:20 | 55652 | 2011-04-01 00:00:00 | 55874.1455324074 | 2011-11-09 03:29:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061116 | We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 6 | AO6-LP | THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806028010/ | Quick Look | ![]() |
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286 | ABELL 2667 | 358.0843 | -26.1324 | 357.438238 | -26.410641 | 347.261091 | -23.090967 | 33.89369276 | -76.76238411 | 64.8814 | 55725.7013773148 | 2011-06-13 16:49:59 | 55726.9814351852 | 2011-06-14 23:33:16 | 806029040 | 51.7936 | 50 | 51.7936 | 51.8161 | 0 | 51.8016 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.6427 | 43.6427 | 110.5818 | 1 | PROCESSED | 57602.3116319444 | 2016-08-02 07:28:45 | 55652 | 2011-04-01 00:00:00 | 55757.7024652778 | 2011-07-15 16:51:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061116 | We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 6 | AO6-LP | THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806029040/ | Quick Look | ![]() |
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287 | COMA E4 | 196.1292 | 27.8947 | 195.52895 | 28.162497 | 182.637315 | 31.793754 | 48.48781449 | 87.00057059 | 279.9984 | 55729.6868287037 | 2011-06-17 16:29:02 | 55730.3355671296 | 2011-06-18 08:03:13 | 806033010 | 20.2023 | 20 | 20.2023 | 20.2103 | 0 | 20.2183 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.516 | 20.516 | 56.0419 | 1 | PROCESSED | 57602.3427199074 | 2016-08-02 08:13:31 | 55652 | 2011-04-01 00:00:00 | 55770.1680092593 | 2011-07-28 04:01:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806033010/ | Quick Look | ![]() |
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288 | BEYOND VIRGO 1 | 187.7129 | 16.0953 | 187.082675 | 16.371354 | 180.479874 | 17.795652 | 278.48728746 | 77.9786094 | 118.4704 | 55905.1491666667 | 2011-12-10 03:34:48 | 55905.8431828704 | 2011-12-10 20:14:11 | 806060010 | 22.2598 | 20 | 22.2678 | 22.2678 | 0 | 22.2598 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.63 | 20.63 | 59.9539 | 1 | PROCESSED | 57604.1022569444 | 2016-08-04 02:27:15 | 56284 | 2012-12-23 00:00:00 | 55917.0698958333 | 2011-12-22 01:40:39 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061523 | To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NORBERT WERNER | USA | 6 | AO6 | LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806060010/ | Quick Look | ![]() |
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289 | BEYOND VIRGO 2 | 187.7135 | 16.3643 | 187.083459 | 16.640353 | 180.363309 | 18.040696 | 277.98453264 | 78.22684296 | 118.4711 | 55905.8436574074 | 2011-12-10 20:14:52 | 55906.3980439815 | 2011-12-11 09:33:11 | 806061010 | 21.4115 | 20 | 21.4275 | 21.4115 | 0 | 21.4335 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19.1816 | 19.1816 | 47.872 | 1 | PROCESSED | 57604.0951041667 | 2016-08-04 02:16:57 | 56284 | 2012-12-23 00:00:00 | 55917.0723842593 | 2011-12-22 01:44:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061523 | To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NORBERT WERNER | USA | 6 | AO6 | LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806061010/ | Quick Look | ![]() |
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290 | BEYOND VIRGO 6 | 187.7152 | 17.4312 | 187.085892 | 17.70725 | 179.897096 | 19.011602 | 275.76419982 | 79.20143703 | 118.777 | 55919.8968287037 | 2011-12-24 21:31:26 | 55920.9286574074 | 2011-12-25 22:17:16 | 806065010 | 39.5769 | 40 | 39.6169 | 39.5769 | 0 | 39.6169 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 33.7703 | 33.7703 | 89.136 | 2 | PROCESSED | 57604.2337962963 | 2016-08-04 05:36:40 | 56339 | 2013-02-16 00:00:00 | 55972.6645833333 | 2012-02-15 15:57:00 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061523 | To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NORBERT WERNER | USA | 6 | AO6 | LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806065010/ | Quick Look | ![]() |
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291 | LOCK-365 | 161.9095 | 57.7105 | 161.128548 | 57.974475 | 136.113511 | 45.200495 | 149.74973686 | 52.48617693 | 106.5217 | 55897.0768981482 | 2011-12-02 01:50:44 | 55900.1780439815 | 2011-12-05 04:16:23 | 806077010 | 149.9102 | 150 | 149.9422 | 149.9102 | 0 | 149.9422 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 131.1259 | 131.1259 | 267.9076 | 0 | PROCESSED | 57604.1079050926 | 2016-08-04 02:35:23 | 56065 | 2012-05-18 00:00:00 | 55914.3640393518 | 2011-12-19 08:44:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061532 | We propose Suzaku XIS observations of a sample of three high redshift galaxy clusters with 0.87 < z < 1.20 discovered by the 42 square degree Spitzer Adaptation of the Red Sequence Survey (SpARCS). This survey is currently the largest optical/IR survey for high redshift clusters, and includes significant multi-wavelength follow-up. Extensive Gemini spectroscopic observations have confirmed that all of our targets are rich, massive clusters with velocity dispersions ranging from 550-800 km/sec. Our Suzaku observations are designed to detect the extended intra-cluster medium in the cluster cores, provide first estimates of cluster X-ray luminosities, and broadly investigate the core gas densities of our targets. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 6 | AO6 | OBSERVING DISTANT GALAXY CLUSTERS FROM THE SPITZER SPARCS SURVEY WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806077010/ | Quick Look | ![]() |
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292 | AE AQUARII | 310.0457 | -0.9355 | 309.401118 | -1.113434 | 312.219972 | 16.829528 | 45.22275468 | -24.45710482 | 264.8759 | 53673.9022685185 | 2005-10-30 21:39:16 | 53676.043275463 | 2005-11-02 01:02:19 | 400001010 | 70.5289 | 100 | 70.5289 | 70.6169 | 70.5689 | 70.5449 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 59.4538 | 59.4538 | 184.9569 | 2 | PROCESSED | 57527.7308217593 | 2016-05-19 17:32:23 | 54247 | 2007-05-27 00:00:00 | 54036.9851388889 | 2006-10-28 23:38:36 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001004 | We have a new idea that a magnetized white dwarf can be a particle-acceleration cite to emit non thermal emission. In order to understand the particle acceleration process in rotation-powered objects, it is important to measure the hard X-ray emission from magnetized white dwarfs, in addition to that from well-known neutron stars. Here, we propose a 100ksec observation of a magnetic cataclysmic valiable, AE Aqurii. It is difficult for INTEGRAL mission, and is challenging even for the HXD, but it will be a ``first detection'' of the non-thermal emission in the hard X-ray band from a white dwarf with Suzaku. | GALACTIC POINT SOURCES | 4 | A | YUKIKATSU TERADA | JAP | 0 | SWG | SEARCH FOR THE NON-THERMAL EMISSION FROM MAGNETIZED WHITE DWARF WITH SUZAKU | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400001010/ | Quick Look | ![]() |
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293 | RCS051838-4324.9 | 79.6593 | -43.4168 | 79.277976 | -43.467716 | 71.171582 | -66.18535 | 248.71475233 | -34.61566895 | 286.4929 | 56016.4337268518 | 2012-03-30 10:24:34 | 56018.0001388889 | 2012-04-01 00:00:12 | 806083010 | 67.6666 | 75 | 67.6906 | 67.6666 | 0 | 67.6906 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57.511 | 57.511 | 135.2938 | 1 | PROCESSED | 57605.0718402778 | 2016-08-05 01:43:27 | 56399 | 2013-04-17 00:00:00 | 56027.1518287037 | 2012-04-10 03:38:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061533 | Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 19 optically-selected clusters of galaxies, half at z~0.3 and half at z~0.8. Here we propose 6 additional observations in order to uniformly span a total redshift range of 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 6 | AO6 | AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806083010/ | Quick Look | ![]() |
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294 | FG04 | 121.8798 | 33.9978 | 121.078663 | 34.143156 | 116.761327 | 13.47104 | 187.39667673 | 29.69857824 | 274.999 | 56053.6835648148 | 2012-05-06 16:24:20 | 56053.9411921296 | 2012-05-06 22:35:19 | 807053010 | 10.821 | 10 | 10.821 | 10.821 | 0 | 10.821 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.0766 | 11.0766 | 22.2559 | 0 | PROCESSED | 57605.3537268518 | 2016-08-05 08:29:22 | 56435 | 2013-05-23 00:00:00 | 56068.6337152778 | 2012-05-21 15:12:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071511 | Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ELENA D'ONGHIA | USA | 7 | AO7 | SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807053010/ | Quick Look | ![]() |
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295 | RXJ1416.4+2315 | 214.0475 | 23.1701 | 213.473378 | 23.401516 | 202.507315 | 34.451007 | 25.95045598 | 70.44211392 | 293.1172 | 56123.5919675926 | 2012-07-15 14:12:26 | 56124.3335300926 | 2012-07-16 08:00:17 | 807065010 | 23.7192 | 120 | 23.7272 | 23.7192 | 0 | 23.7272 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22.6028 | 22.6028 | 64.0639 | 1 | PROCESSED | 57606.624537037 | 2016-08-06 14:59:20 | 56598 | 2013-11-02 00:00:00 | 56144.9996180556 | 2012-08-05 23:59:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071514 | Our study of the fossil group RXJ 1159+5531 does not find the gas clumping invoked to explain unexpectedly flat entropy profiles and large gas fractions near r_vir in some clusters. Instead its ICM properties at r_vir are consistent with adiabatic cluster formation, which may reflect that hydrostatic equilibrium is very accurate in this highly evolved fossil group. To examine whether these results extend to other fossils and to more massive systems, we propose to observe the fossil cluster RXJ 1416.4+2315 (M_vir ~3 x 10^14 M_sun) to constrain its entropy and gas fraction out to r_vir (r_112). Since it is located at a redshift of 0.137, this target provides an efficient means to explore the outer ICM, where a large azimuthal portion (~80%) of r_vir can be observed in a single Suzaku field. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | DAVID BUOTE | USA | 7 | AO7 | RXJ1416.4+2315: A MASSIVE FOSSIL CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807065010/ | Quick Look | ![]() |
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296 | ANTLIA E4 | 158.9815 | -35.3293 | 158.412243 | -35.069878 | 177.109135 | -40.308725 | 274.02289995 | 19.82417732 | 279.0004 | 56094.1885532407 | 2012-06-16 04:31:31 | 56095.3688888889 | 2012-06-17 08:51:12 | 807069010 | 46.5031 | 45 | 46.5031 | 46.5195 | 0 | 46.5111 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38.6185 | 38.6185 | 101.9699 | 0 | PROCESSED | 57605.7108564815 | 2016-08-05 17:03:38 | 56477 | 2013-07-04 00:00:00 | 56111.0445023148 | 2012-07-03 01:04:05 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071521 | We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KA-WAH WONG | USA | 7 | AO7 | MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807069010/ | Quick Look | ![]() |
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297 | ABELL 2597 | 351.5123 | -12.2071 | 350.862263 | -12.482246 | 347.371921 | -7.852378 | 65.46064183 | -65.03980804 | 250.0004 | 56263.5374884259 | 2012-12-02 12:53:59 | 56264.7744907407 | 2012-12-03 18:35:16 | 807073030 | 50.2983 | 50 | 50.3063 | 50.2983 | 0 | 50.2983 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.3364 | 42.3364 | 106.8558 | 0 | PROCESSED | 57608.190625 | 2016-08-08 04:34:30 | 56018 | 2012-04-01 00:00:00 | 56279.6896180556 | 2012-12-18 16:33:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071522 | We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 7 | AO7 | COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807073030/ | Quick Look | ![]() |
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298 | RCS022456-0348.8 | 36.2382 | -3.8143 | 35.608784 | -4.039767 | 32.599151 | -17.199331 | 170.77871975 | -57.71972182 | 253.341 | 56324.4414814815 | 2013-02-01 10:35:44 | 56325.9579282407 | 2013-02-02 22:59:25 | 807078010 | 50.8118 | 49 | 50.8227 | 50.8147 | 0 | 50.8118 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.195 | 46.195 | 131.0078 | 0 | PROCESSED | 57610.5290509259 | 2016-08-10 12:41:50 | 56711 | 2014-02-23 00:00:00 | 56345.5401967593 | 2013-02-22 12:57:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071525 | Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 24 optically-selected clusters of galaxies out to z~1. Here we propose 5 additional observations in order to uniformly span our total mass-redshift space over the range 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 7 | AO7 | AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES II | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807078010/ | Quick Look | ![]() |
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299 | COMA NW3 | 194.5571 | 28.6697 | 193.954123 | 28.93948 | 180.77176 | 31.860187 | 79.10101688 | 87.84902047 | 319.997 | 55732.646099537 | 2011-06-20 15:30:23 | 55732.9793865741 | 2011-06-20 23:30:19 | 806040010 | 10.469 | 10 | 10.469 | 10.469 | 0 | 10.469 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.1768 | 10.1768 | 28.7899 | 0 | PROCESSED | 57602.3615856482 | 2016-08-02 08:40:41 | 55652 | 2011-04-01 00:00:00 | 55768.2657523148 | 2011-07-26 06:22:41 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806040010/ | Quick Look | ![]() |
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300 | ESO318-021 | 163.2697 | -40.3328 | 162.69794 | -40.066534 | 184.394245 | -42.926152 | 279.73310675 | 17.14745123 | 111.1499 | 56639.0964467593 | 2013-12-13 02:18:53 | 56643.3605902778 | 2013-12-17 08:39:15 | 808063010 | 152.2198 | 150 | 152.2198 | 152.2198 | 0 | 152.2198 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 132.9733 | 132.9733 | 368.3777 | 4 | PROCESSED | 57613.6558101852 | 2016-08-13 15:44:22 | 57050 | 2015-01-28 00:00:00 | 56680.7667476852 | 2014-01-23 18:24:07 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081503 | The mass profiles of elliptical galaxies are important probes of galaxy formation and cosmology. Only a few elliptical galaxies have detailed mass measurements from X-rays because of the lack of suitable targets in terms of total mass (< ~10^{13} m_sun) and relaxed dynamical states appropriate for hydrostatic analysis. We have identified a sample of (hot) gas-rich isolated elliptical galaxies, most of which were discovered from previously awarded XMM and Chandra snapshot programs to search for optimal targets for X-ray studies of mass profiles on the galaxy scale. We request Suzaku observations to map the detailed profiles of stars, dark matter, and hot gas in two of these galaxies which have (scheduled) complementary Chandra observations. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | DAVID BUOTE | USA | 8 | AO8 | THE DARK MATTER AND BARYON PROFILES OF ISOLATED ELLIPTICAL GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808063010/ | Quick Look | ![]() |
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301 | RXJ1416.4+2315 | 214.0623 | 23.3458 | 213.488767 | 23.577175 | 202.437112 | 34.617457 | 26.46691952 | 70.47697816 | 292.671 | 56496.6431712963 | 2013-07-23 15:26:10 | 56499.3349074074 | 2013-07-26 08:02:16 | 808064010 | 122.9317 | 120 | 122.9317 | 122.9317 | 0 | 122.9317 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 116.8226 | 116.8226 | 232.5474 | 2 | PROCESSED | 57612.032650463 | 2016-08-12 00:47:01 | 56953 | 2014-10-23 00:00:00 | 56587.4880671296 | 2013-10-22 11:42:49 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081511 | Our preliminary analysis of AO7 XIS data of the fossil cluster RXJ 1416.4+2315 does not find evidence for the gas clumping invoked to explain the flat entropy profiles and large gas fractions found near r_vir in several nearby clusters. Instead its ICM properties at r_vir are consistent with adiabatic cluster formation as we found previously for the fossil group/cluster RXJ 1159+5531, which may reflect that hydrostatic equilibrium is very accurate in these highly evolved fossil systems. Therefore, we propose a Suzaku observation in a different azimuthal direction to double the azimuthal coverage at r_vir (from ~30% to ~60%) in order to test for the presence of azimuthal ICM variations expected for clusters that grow by accretion along large-scale filaments. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | DAVID BUOTE | USA | 8 | AO8 | VERIFYING RELAXED ICM AT THE VIRIAL RADIUS IN A FOSSIL GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808064010/ | Quick Look | ![]() |
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302 | MKW-N2 | 181.1507 | 2.5267 | 180.510236 | 2.805064 | 180.047061 | 2.775514 | 276.44275792 | 62.96433079 | 120.2659 | 56663.6701967593 | 2014-01-06 16:05:05 | 56666.0195023148 | 2014-01-09 00:28:05 | 808067010 | 99.7883 | 100 | 99.7883 | 99.7883 | 0 | 99.7883 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 99.9362 | 99.9362 | 202.9537 | 4 | PROCESSED | 57613.8221643518 | 2016-08-13 19:43:55 | 57096 | 2015-03-15 00:00:00 | 56730.5704166667 | 2014-03-14 13:41:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081512 | We propose to observe the MKW4 group by leveraging existing observations to provide coverage from its center to its virial radius in two orthogonal directions. Three additional pointings, totaling 230 ksec, combined with two existing pointings, will allow us to determine radial profiles of gas temperature, density, entropy, pressure, and gas mass fraction, as well as their azimuthal variations. Comparing these properties to those of clusters will allow us to probe the role played by baryonic physics and assess the imprints of hierarchical structure formation. The stable and low background of the Suzaku XIS is crucial for the study of galaxy groups to their virial radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUANYUAN SU | USA | 8 | AO8 | PROBING A TYPICAL GALAXY GROUP TO ITS VIRAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808067010/ | Quick Look | ![]() |
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303 | A133_FIELD_2 | 15.4723 | -21.5865 | 14.860654 | -21.855252 | 5.175152 | -25.865615 | 146.72727626 | -83.96930246 | 231.9996 | 56646.6689583333 | 2013-12-20 16:03:18 | 56647.8294212963 | 2013-12-21 19:54:22 | 808082010 | 50.6406 | 50 | 50.6646 | 50.6566 | 0 | 50.6406 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.4338 | 46.4338 | 100.2559 | 1 | PROCESSED | 57613.6561921296 | 2016-08-13 15:44:55 | 57061 | 2015-02-08 00:00:00 | 56695.6286689815 | 2014-02-07 15:05:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081525 | We propose observations of the outskirts of Abell 133, a relaxed galaxy cluster that is the target of a Chandra X-ray Visionary Project. These modest Suzaku observations will leverage the 2.4 Msec of Chandra time spent deeply imaging the region beyond r_500 to search for ICM clumping. Such clumping has been invoked to explain the flat entropy profiles and excess inferred gas fraction beyond r_500 in several clusters observed recently with Suzaku. The proposed Suzaku observations combined with the unprecedented Chandra depth will create a fiducial dataset to compare to the existing Suzaku cluster outskirts data, and they will definitely determine whether the excess inferred gas fractions seen with Suzaku arise from gas clumping. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | ERIC MILLER | USA | 8 | AO8 | A DEFINITIVE STUDY OF GALAXY CLUSTER OUTSKIRTS WITH SUZAKU AND CHANDRA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808082010/ | Quick Look | ![]() |
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304 | ABELL 1689 (OFFSET) | 198.1816 | -1.2688 | 197.539227 | -1.003818 | 197.250037 | 5.95631 | 314.01012466 | 61.14421574 | 293.5484 | 56470.3775578704 | 2013-06-27 09:03:41 | 56473.3751273148 | 2013-06-30 09:00:11 | 808089010 | 105.7518 | 396 | 105.7598 | 105.7518 | 0 | 105.7518 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95.0477 | 95.0477 | 258.9556 | 4 | PROCESSED | 57611.7314930556 | 2016-08-11 17:33:21 | 56383 | 2013-04-01 00:00:00 | 56523.7467708333 | 2013-08-19 17:55:21 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081528 | Recent Suzaku results suggest that the surface brightness in galaxy cluster outskirts is higher than the predictions by self-similar models, indicating that the gas may be clumpy or may not be in collisional equilibrium near and beyond the virial radius. If this is the case, gas emission near cosmological accretion shocks should readily be detected. We propose to search for emission near the accretion shock radius where it is the only region unexplored in galaxy cluster studies in X-ray. These data can place important constraints on accretion models and large-scale structure formation theory. Physical properties at the true virial radius (R100) will also be measured to the highest precision to date. A very deep exposure and the low Suzaku background allow this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KA-WAH WONG | USA | 8 | AO8 | SEARCH FOR ACCRETION SHOCK IN A MASSIVE GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808089010/ | Quick Look | ![]() |
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305 | ABELL 1689 (OFFSET) | 198.1818 | -1.2687 | 197.539427 | -1.003718 | 197.250185 | 5.956479 | 314.01056832 | 61.14428006 | 293.5484 | 56473.3751388889 | 2013-06-30 09:00:12 | 56475.3022916667 | 2013-07-02 07:15:18 | 808089020 | 67.8003 | 396 | 67.8083 | 67.8003 | 0 | 67.8083 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 60.9649 | 60.9649 | 166.4698 | 5 | PROCESSED | 57611.6944907407 | 2016-08-11 16:40:04 | 56383 | 2013-04-01 00:00:00 | 56491.6594675926 | 2013-07-18 15:49:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081528 | Recent Suzaku results suggest that the surface brightness in galaxy cluster outskirts is higher than the predictions by self-similar models, indicating that the gas may be clumpy or may not be in collisional equilibrium near and beyond the virial radius. If this is the case, gas emission near cosmological accretion shocks should readily be detected. We propose to search for emission near the accretion shock radius where it is the only region unexplored in galaxy cluster studies in X-ray. These data can place important constraints on accretion models and large-scale structure formation theory. Physical properties at the true virial radius (R100) will also be measured to the highest precision to date. A very deep exposure and the low Suzaku background allow this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KA-WAH WONG | USA | 8 | AO8 | SEARCH FOR ACCRETION SHOCK IN A MASSIVE GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808089020/ | Quick Look | ![]() |
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306 | A1413 | 178.8303 | 23.6485 | 178.18646 | 23.926767 | 169.076487 | 21.133974 | 225.18767075 | 76.86550896 | 123.0348 | 53689.8362847222 | 2005-11-15 20:04:15 | 53692.5939699074 | 2005-11-18 14:15:19 | 800001010 | 107.8672 | 100 | 107.8672 | 108.0032 | 107.9472 | 107.9103 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 102.4315 | 102.4315 | 238.2397 | 7 | PROCESSED | 57528.0427546296 | 2016-05-20 01:01:34 | 54247 | 2007-05-27 00:00:00 | 54038.1136689815 | 2006-10-30 02:43:41 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001010 | No cluster has had its X-ray temperature measured out to the virial radius. Hence no cluster has had it total mass measured using X-ray methods. Typically these measurements extend only to 60% of the virial radius. We propose to perform these measurements for the first time and with high accuracy for the relaxed cluster A1413. The low Suzaku background permits us to make this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | J. HENRY | JAP | 0 | SWG | CLUSTER TEMPERATURE AND MASS MEASUREMENT TO THE VIRIAL RADIUS | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800001010/ | Quick Look | ![]() |
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307 | NGC 953 | 37.7955 | 29.584 | 37.059252 | 29.362946 | 44.923297 | 13.943505 | 147.58231113 | -28.46974369 | 250.5565 | 57059.5397222222 | 2015-02-06 12:57:12 | 57063.4376157407 | 2015-02-10 10:30:10 | 809055010 | 150.8191 | 150 | 150.8191 | 150.8671 | 0 | 150.8671 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6137037037 | 2016-08-17 14:43:44 | 56748 | 2014-04-01 00:00:00 | 57107.4400578704 | 2015-03-26 10:33:41 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091503 | The mass profiles of elliptical galaxies are important probes of galaxy formation and cosmology. Only a few elliptical galaxies have detailed mass measurements from X-rays because of the lack of suitable targets in terms of total mass (< ~10^13 m_sun) and relaxed dynamical states appropriate for hydrostatic analysis. We have identified a sample of (hot) gas-rich isolated elliptical galaxies, most of which were discovered from previously awarded XMM and Chandra snapshot programs to search for optimal targets for X-ray studies of mass profiles on the galaxy scale. We request Suzaku observations to map the detailed profiles of stars, dark matter, and hot gas in two of these galaxies which have complementary Chandra observations. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | DAVID BUOTE | USA | 9 | AO9 | THE DARK MATTER AND BARYON PROFILES OF ISOLATED ELLIPTICAL GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809055010/ | Quick Look | ![]() |
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308 | FG10 | 163.7228 | 55.3656 | 162.966111 | 55.632252 | 139.04941 | 43.748241 | 151.60913312 | 54.78459511 | 121.1085 | 56973.8939467593 | 2014-11-12 21:27:17 | 56975.0737615741 | 2014-11-14 01:46:13 | 809061010 | 61.1085 | 60 | 61.1085 | 61.2978 | 0 | 61.2978 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7792361111 | 2016-08-16 18:42:06 | 57444 | 2016-02-26 00:00:00 | 57076.4143865741 | 2015-02-23 09:56:43 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091512 | Optical and X-ray measurements of fossil galaxy systems (FGs) suggest that they are old and relaxed. If FGs are assembled at higher redshifts, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest group galaxy (BGG). We carry out the first systematic and multiwavelength study of a large sample of FGs, the FOssil Group Origins (FOGO) project. We propose to observe four bona fide fossil groups, most with T< 2 keV measuring Tx and Lx for objects at the mass scale of groups, which are rather unexplored. We will evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to our sample of fossil clusters completing the first X-ray selected sample of fossil systems ranging from the cluster to galaxy group scale. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | ELENA D'ONGHIA | USA | 9 | AO9 | SCALING RELATIONS OF FOSSIL GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809061010/ | Quick Look | ![]() |
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309 | ABELL 2259 | 259.9722 | 27.8097 | 259.476075 | 27.85934 | 255.895749 | 50.75928 | 50.52312942 | 31.25775464 | 109.9997 | 57081.1636458333 | 2015-02-28 03:55:39 | 57082.4113194445 | 2015-03-01 09:52:18 | 809081010 | 42.2203 | 42.5 | 42.2203 | 43.0443 | 0 | 43.1003 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6840509259 | 2016-08-17 16:25:02 | 57465 | 2016-03-18 00:00:00 | 57091.4611226852 | 2015-03-10 11:04:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091526 | Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but not many were studied for "regular" non-cool core clusters. We propose a 170 ks Suzaku observation of a regular non-cool core cluster Abell 2259. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KA-WAH WONG | USA | 9 | AO9 | REGULAR NON-COOL CORE GALAXY CLUSTER OUT TO THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809081010/ | Quick Look | ![]() |
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310 | ABELL 2259 | 260.1067 | 27.5543 | 259.609076 | 27.603301 | 256.126173 | 50.518333 | 50.27658806 | 31.07091189 | 109.9997 | 57083.6006018518 | 2015-03-02 14:24:52 | 57084.7258564815 | 2015-03-03 17:25:14 | 809081030 | 44.2468 | 42.5 | 44.2468 | 44.2548 | 0 | 44.2548 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.7027314815 | 2016-08-17 16:51:56 | 57475 | 2016-03-28 00:00:00 | 57107.4892476852 | 2015-03-26 11:44:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091526 | Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but not many were studied for "regular" non-cool core clusters. We propose a 170 ks Suzaku observation of a regular non-cool core cluster Abell 2259. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KA-WAH WONG | USA | 9 | AO9 | REGULAR NON-COOL CORE GALAXY CLUSTER OUT TO THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809081030/ | Quick Look | ![]() |
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311 | M82 N1 | 148.6748 | 70.0409 | 147.627175 | 70.277324 | 118.519213 | 52.349642 | 141.10131259 | 40.27429686 | 283.7057 | 57159.0836921296 | 2015-05-17 02:00:31 | 57160.4702546296 | 2015-05-18 11:17:10 | 809122010 | 59.5055 | 60 | 59.5055 | 59.5055 | 0 | 59.5135 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.6721759259 | 2016-08-18 16:07:56 | 57538 | 2016-05-30 00:00:00 | 57171.5244212963 | 2015-05-29 12:35:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091701 | We propose to carry out joint Chandra and Suzaku observations of the starburst galaxy M82. We will search for extended clumps similar to the Northern Cap out to 45 kpc. We will also constrain the density and temperature profiles of the tenuous wind emission out to large radii. These data can place important constraints on theoretical models of starburst galaxies and their environments. We will test models such as the Chevalier & Clegg adiabatic wind model, hydrostatic halo model, shocked clouds in a wind, etc. The excellent Chandra spatial resolution combining with the low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | S | KA-WAH WONG | USA | 9 | AO9 | SEARCH FOR THE OUTER BOUNDARY OF THE STARBURST GALAXY: M82 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809122010/ | Quick Look | ![]() |
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312 | ZETA OPH | 249.2878 | -10.5628 | 248.598836 | -10.46277 | 249.217592 | 11.396196 | 6.28378927 | 23.59180747 | 94.9452 | 54540.8758912037 | 2008-03-15 21:01:17 | 54543.8543287037 | 2008-03-18 20:30:14 | 402038010 | 105.5837 | 100 | 105.5917 | 105.5917 | 0 | 105.5837 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79.9813 | 79.9813 | 257.3178 | 2 | PROCESSED | 57541.9592708333 | 2016-06-02 23:01:21 | 54922 | 2009-04-01 00:00:00 | 54553.3785300926 | 2008-03-28 09:05:05 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021022 | Zeta Oph is a well known optical and UV variable star and is now known to displays both short (hours) and long (years) term X-ray variability. The short term variability has different periods for the soft and hard X-ray bands. The soft period being identical with the UV DAC reoccurrence period. The hard period is 40 percent smaller than the soft period and the source of it's variability is thus far unclear. Zeta Oph has been observed by several X-ray telescopes over a 22 year time span and the observations show significant variations in the total observed X-ray flux. We are requesting an XIS observation of this star to develop: 1) a greater understanding of the hard X-ray emission; 2) confirm the hard and soft periodicities, and; 3) provide further monitoring of the long term variability. | GALACTIC POINT SOURCES | 4 | C | WAYNE WALDRON | USA | 2 | AO2 | MULTIPLE X-RAY EMISSION PERIODICITY IN THE RAPIDLY ROTATING O-STAR, ZETA OPH | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402038010/ | Quick Look | ![]() |
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313 | 4U1705-44 | 257.2319 | -44.0961 | 256.328793 | -44.032411 | 260.195881 | -21.087692 | 343.32770356 | -2.34122442 | 265.637 | 54348.6112847222 | 2007-09-05 14:40:15 | 54349.0140509259 | 2007-09-06 00:20:14 | 402051010 | 13.3436 | 15 | 13.3436 | 13.3436 | 0 | 13.3436 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.3706 | 9.3706 | 34.7919 | 1 | PROCESSED | 57539.9453472222 | 2016-05-31 22:41:18 | 54773 | 2008-11-03 00:00:00 | 54356.2627430556 | 2007-09-13 06:18:21 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021113 | We recently proposed a solution to the problem of model ambiguity for the spectra of atoll-type neutron stars. This work was performed on X-ray transient, and we need to test the model on the main population of persistent atolls. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. We propose to supplement the Suzaku monitoring archive begun in AO-1 by targeting the two persistent atolls with the greatest X-ray variability. | GALACTIC POINT SOURCES | 4 | A | RONALD REMILLARD | USA | 2 | AO2 | X-RAY SPECTRA OF ATOLL-TYPE NEUTRON STARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402051010/ | Quick Look | ![]() |
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314 | AQL X-1 | 287.8182 | 0.5791 | 287.179926 | 0.495378 | 289.379323 | 22.828874 | 35.71383379 | -4.14703266 | 264.9589 | 54382.2112384259 | 2007-10-09 05:04:11 | 54382.6877893518 | 2007-10-09 16:30:25 | 402053030 | 19.7117 | 15 | 19.7197 | 19.7277 | 0 | 19.7117 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.5522 | 17.5522 | 41.162 | 0 | PROCESSED | 57540.2157291667 | 2016-06-01 05:10:39 | 54770 | 2008-10-31 00:00:00 | 54402.5719328704 | 2007-10-29 13:43:35 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021114 | We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. | GALACTIC POINT SOURCES | 4 | A | RONALD REMILLARD | USA | 2 | AO2-TOO | X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402053030/ | Quick Look | ![]() |
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315 | AQL X-1 | 287.8172 | 0.5775 | 287.178919 | 0.493782 | 289.378018 | 22.82742 | 35.71194856 | -4.14687642 | 265.833 | 54397.9824074074 | 2007-10-24 23:34:40 | 54398.5072222222 | 2007-10-25 12:10:24 | 402053060 | 21.3648 | 15 | 21.4608 | 21.4608 | 0 | 21.3648 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.4022 | 21.4022 | 45.3439 | 0 | PROCESSED | 57540.3340509259 | 2016-06-01 08:01:02 | 54776 | 2008-11-06 00:00:00 | 54407.3747222222 | 2007-11-03 08:59:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021114 | We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. | GALACTIC POINT SOURCES | 4 | A | RONALD REMILLARD | USA | 2 | AO2-TOO | X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402053060/ | Quick Look | ![]() |
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316 | AQL X-1 | 287.8217 | 0.5796 | 287.183429 | 0.495861 | 289.383158 | 22.828908 | 35.71588636 | -4.14991498 | 243.6715 | 54403.2743171296 | 2007-10-30 06:35:01 | 54403.66 | 2007-10-30 15:50:24 | 402053070 | 17.5362 | 15 | 17.5842 | 17.604 | 0 | 17.5362 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14.3322 | 14.3322 | 33.3199 | 0 | PROCESSED | 57540.3767824074 | 2016-06-01 09:02:34 | 54776 | 2008-11-06 00:00:00 | 54409.1320138889 | 2007-11-05 03:10:06 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021114 | We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. | GALACTIC POINT SOURCES | 4 | A | RONALD REMILLARD | USA | 2 | AO2-TOO | X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402053070/ | Quick Look | ![]() |
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317 | X1630-472 | 248.5414 | -47.3441 | 247.620794 | -47.24014 | 254.106628 | -25.078548 | 336.96314137 | 0.26612574 | 120.5775 | 53802.0758796296 | 2006-03-08 01:49:16 | 53802.7300231482 | 2006-03-08 17:31:14 | 400010040 | 21.2481 | 200 | 21.2481 | 21.2499 | 21.2499 | 21.2499 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 20.4778 | 20.4778 | 56.512 | 0 | PROCESSED | 57533.1620486111 | 2016-05-25 03:53:21 | 54247 | 2007-05-27 00:00:00 | 54041.7698726852 | 2006-11-02 18:28:37 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001058 | We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active. | GALACTIC POINT SOURCES | 4 | A | JEAN COTTAM | JAP | 0 | SWG-TOO | FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400010040/ | Quick Look | ![]() |
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318 | 4U2206+54 | 331.9811 | 54.5897 | 331.524827 | 54.344502 | 8.281106 | 58.879755 | 100.6432606 | -1.04691755 | 90.2357 | 54236.1620949074 | 2007-05-16 03:53:25 | 54237.812662037 | 2007-05-17 19:30:14 | 402069010 | 103.9768 | 100 | 103.9848 | 103.9906 | 0 | 103.9768 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 99.7842 | 99.7842 | 142.5819 | 1 | PROCESSED | 57538.7118402778 | 2016-05-30 17:05:03 | 54695 | 2008-08-17 00:00:00 | 54242.76625 | 2007-05-22 18:23:24 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021125 | 4U 2206+54 is a high mass X-ray binary which is suspected to contain a neutron star accreting from the wind of its companion BD +53 2790. However, there has been no confirmed detection of X-ray pulsations, and while several authors have reported hints of a cyclotron line in the energy spectra near 30 keV, none have reported significant detections. We propose Suzaku observations to search for long-period pulsations with the XIS, and possible confirmation of the cyclotron line using HXD/PIN. | GALACTIC POINT SOURCES | 4 | A | MARK FINGER | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF THE PECULIAR HMXB 4U 2206+54 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402069010/ | Quick Look | ![]() |
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319 | GRS 1915+105 | 288.7933 | 10.9535 | 288.203422 | 10.865162 | 292.134883 | 32.961388 | 45.37037141 | -0.21130356 | 67.354 | 54227.6113657407 | 2007-05-07 14:40:22 | 54229.0717476852 | 2007-05-09 01:43:19 | 402071010 | 65.6568 | 37 | 65.6568 | 65.8039 | 0 | 65.6728 | 1 | 2 | 0 | 1 | 1 | 0 | 0 | 56.8973 | 56.8973 | 126.168 | 1 | PROCESSED | 57538.6640972222 | 2016-05-30 15:56:18 | 54702 | 2008-08-24 00:00:00 | 54235.5321759259 | 2007-05-15 12:46:20 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021132 | We have discovered a connection between Fe line strength and QPO phase in RXTE observations of GRS 1915+105. This connection independently ties Fe lines to radii less than 100 R_Schw. QPO-phase-resolved Suzaku spectra will enable us to detect changes in the relativistic line profile (inner radius, equivalent width), to extend the connection to the broadband disk reflection spectrum, and to test models for the Fe line - QPO connection. Moreover, at CCD resolution, the connection can be used to over-constrain disk radii - a first step toward mapping the inner disk. We therefore request a 37 ksec TOO observation of GRS 1915+105. Understanding black hole accretion is fundamental to NASA's "SEU" theme. | GALACTIC POINT SOURCES | 4 | A | JON MILLER | USA | 2 | AO2-TOO | THE RELATIVISTIC IRON LINE - QPO CONNECTION IN GRS 1915+105 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402071010/ | Quick Look | ![]() |
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320 | VELA PWN NE2 | 130.6211 | -44.2844 | 130.186671 | -44.103918 | 154.655956 | -58.950029 | 263.6136326 | -1.23809583 | 141.8635 | 55917.0080439815 | 2011-12-22 00:11:35 | 55917.6126273148 | 2011-12-22 14:42:11 | 506042010 | 18.514 | 15 | 18.538 | 18.514 | 0 | 18.514 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.8755 | 16.8755 | 52.2259 | 0 | PROCESSED | 57604.2062962963 | 2016-08-04 04:57:04 | 56305 | 2013-01-13 00:00:00 | 55937.7869212963 | 2012-01-11 18:53:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | C | SATORU KATSUDA | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506042010/ | Quick Look | ![]() |
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321 | SGR C BGD | 265.7856 | -29.8854 | 264.98542 | -29.862996 | 266.313646 | -6.498142 | 358.90876565 | -0.03691694 | 81.9998 | 53789.4522106482 | 2006-02-23 10:51:11 | 53789.8349421296 | 2006-02-23 20:02:19 | 500019010 | 13.3073 | 10 | 13.3153 | 13.3153 | 13.3153 | 13.3073 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 12.2404 | 12.2404 | 33.0639 | 0 | PROCESSED | 57533.050462963 | 2016-05-25 01:12:40 | 54247 | 2007-05-27 00:00:00 | 54041.3629166667 | 2006-11-02 08:42:36 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001079 | We propose 100 ksec observation of the Sgr C cloud in the Galactic center region. The cloud emits strong 6.4-keV line, and is a candidate of X-ray reflection nebula; the molecular cloud which emits fluorescence and scattered X-rays irradiated by an external X-ray source. The past activity of Sgr~A$^*$, the Galactic nucleus, may be the origin of 6.4-keV line. We will study 6.4-keV line and verify the X-ray reflection scenario. The second objective is to study the distribution of high ionized and neutral iron lines in the GC region. Chandra observation indicates that H-like iron line is very strong in this region. With the higher energy resolution of XIS, we can confirm the Chandra results. High energy diffuse emission above 10 keV is also a important target by HXD. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI MURAKAMI | JAP | 0 | SWG | FOSSILS OF THE GALACTIC CENTER ACTIVITY | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500019010/ | Quick Look | ![]() |
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322 | 1H 0707-495 | 107.1586 | -49.5558 | 106.829982 | -49.474426 | 125.752559 | -70.871973 | 260.16951247 | -17.68246857 | 144.7199 | 53707.1759143518 | 2005-12-03 04:13:19 | 53710.0974537037 | 2005-12-06 02:20:20 | 700008010 | 97.2291 | 100 | 97.8529 | 100.3891 | 97.2291 | 97.8149 | 4 | 2 | 4 | 4 | 1 | 0 | 0 | 91.8008 | 91.8008 | 252.3688 | 4 | PROCESSED | 57532.4288194444 | 2016-05-24 10:17:30 | 54247 | 2007-05-27 00:00:00 | 54059.7078472222 | 2006-11-20 16:59:18 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001040 | We propose a 100 ks observation of the NLS1 1H 0707--495 in order to understand its remarkable and puzzling spectral and variability properties. The Suzaku data will help us to disentangle between the two interpretations adopted so far, namely partial covering and relativistically blurred reflection. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GIOVANNI MINIUTTI | JAP | 0 | SWG | THE EXTREME PROPERTIES OF THE NLS1 GALAXY 1H 0707-495 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700008010/ | Quick Look | ![]() |
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323 | MRK 501 | 253.4335 | 39.8281 | 253.015349 | 39.90842 | 242.48193 | 61.693142 | 63.68387876 | 38.89139128 | 70.9919 | 54913.7775347222 | 2009-03-23 18:39:39 | 54915.3328587963 | 2009-03-25 07:59:19 | 703046010 | 72.3342 | 65 | 72.3342 | 72.3342 | 0 | 72.3342 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64.8365 | 64.8365 | 134.3581 | 1 | PROCESSED | 57545.930462963 | 2016-06-06 22:19:52 | 55329 | 2010-05-13 00:00:00 | 54924.366724537 | 2009-04-03 08:48:05 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031343 | We propose to observe two bright TeV blazars with Suzaku, in coordination with VERITAS and MAGIC at TeV energies. The primary objective is to make use of the recently available observational capabilities in collecting the much needed simultaneous X-ray and TeV data on these intriguing sources. The data will be essential for addressing a number of unresolved issues in the study of TeV blazars, such as spectral variability, X-ray/TeV correlation and associated time lags, spectral hysteresis, etc. The results will likely provide insights into the properties of the emitting particles, as well as those of the emitting regions, emission mechanism, composition of the jets, and acceleration energetics. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | WEI CUI | USA | 3 | AO3 | COORDINATED X-RAY/TEV OBSERVATIONS OF TEV BLAZARS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703046010/ | Quick Look | ![]() |
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324 | TAU SCO | 248.9722 | -28.2177 | 248.192662 | -28.11602 | 251.449604 | -6.120068 | 351.53437371 | 12.80599439 | 271.5181 | 54696.3145833333 | 2008-08-18 07:33:00 | 54696.6675810185 | 2008-08-18 16:01:19 | 403034050 | 16.3136 | 10 | 16.3504 | 16.3136 | 0 | 16.3584 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.967 | 13.967 | 30.472 | 0 | PROCESSED | 57543.3225694444 | 2016-06-04 07:44:30 | 55084 | 2009-09-10 00:00:00 | 54713.1924189815 | 2008-09-04 04:37:05 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031121 | We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars. | GALACTIC POINT SOURCES | 4 | A | RICHARD IGNACE | USA | 3 | AO3 | X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403034050/ | Quick Look | ![]() |
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325 | CENTAURUS X-3 | 170.3244 | -60.5721 | 169.768632 | -60.297812 | 209.195093 | -56.294338 | 292.07802241 | 0.38603209 | 97.3521 | 54808.2886111111 | 2008-12-08 06:55:36 | 54810.2085532407 | 2008-12-10 05:00:19 | 403046010 | 97.5871 | 90 | 97.5871 | 97.5871 | 0 | 97.5871 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79.6562 | 79.6562 | 165.8537 | 0 | PROCESSED | 57544.7036805556 | 2016-06-05 16:53:18 | 55188 | 2009-12-23 00:00:00 | 54822.6243634259 | 2008-12-22 14:59:05 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031154 | We ask for a 90 ks observation (which will be performed within typically 180 ks taking Suzaku's duty cycle into account) of the accreting HMXB Centaurus X-3 to conduct the most sensitive study to date of the wide range of changes of its broad band spectrum over one 2.1 binary orbit and with pulse phase. Especially we will determine the evolution of the hydrogen absorption column over the orbit and test whether signatures of the tidal wake observed with RXTE can be confirmed. The variable Fe line complex will be studied. The cyclotron resonance scattering feature of Cen X-3 at ~30 keV is especially well suited to test new physical models describing phase-resolved line profiles, since it is very variable over the pulse, with the line centroid spanning an energy range from 28 to 39 keV. | GALACTIC POINT SOURCES | 4 | A | KATJA POTTSCHMIDT | USA | 3 | AO3 | THE BROAD BAND SPECTRUM OF CEN X-3 OVER ORBIT AND PULSE PHASE | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403046010/ | Quick Look | ![]() |
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326 | SS CYG | 325.6842 | 43.5739 | 325.1931 | 43.344666 | 350.456739 | 52.648094 | 90.55430501 | -7.12254626 | 256.8767 | 53692.6066203704 | 2005-11-18 14:33:32 | 53693.8646759259 | 2005-11-19 20:45:08 | 400007010 | 56.043 | 60 | 56.059 | 56.179 | 56.043 | 56.059 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 54.3572 | 54.3572 | 108.6658 | 2 | PROCESSED | 57528.0435763889 | 2016-05-20 01:02:45 | 54247 | 2007-05-27 00:00:00 | 54037.9128472222 | 2006-10-29 21:54:30 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001044 | Although the boundary layer that is formed between the rapidly rotating inner accretion disk and the white dwarf surface has been known as a hard-X-ray emitter, its geometry and structure has not been well understood yet. We aim to investigate the boundary layer structure with SS Cyg, the brightest dwarf nova, by means of a soft X-ray component with the BI CCD, a fluorescent Fe K-alpha line with the FI CCDs, and a continuum reflection by the white dwarf surface with the HXD PIN. It is of great use to observe states of a different mass accretion rate, and hence we propose to observe both in quiescence and in outburst. | GALACTIC POINT SOURCES | 4 | A | MANABU ISHIDA | JAP | 0 | SWG-TOO | SS CYG OBSERVATION IN OUTBURST | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400007010/ | Quick Look | ![]() |
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327 | 73P/SW3 | 17.9545 | -9.1915 | 17.327695 | -9.456837 | 12.929266 | -15.523337 | 138.90931762 | -71.42827213 | 59.4015 | 53893.8691666667 | 2006-06-07 20:51:36 | 53893.9356365741 | 2006-06-07 22:27:19 | 500014040 | 3.236 | 35 | 3.236 | 3.236 | 3.236 | 3.236 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.4909 | 2.4909 | 5.7359 | 0 | PROCESSED | 57534.5832407407 | 2016-05-26 13:59:52 | 54267 | 2007-06-16 00:00:00 | 54052.5308912037 | 2006-11-13 12:44:29 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014040/ | Quick Look | ![]() |
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328 | CYG X-2 | 326.1609 | 38.3293 | 325.643028 | 38.098792 | 346.688554 | 47.972011 | 87.3271497 | -11.30495752 | 51.1203 | 54648.0669097222 | 2008-07-01 01:36:21 | 54650.6154398148 | 2008-07-03 14:46:14 | 403063010 | 72.4308 | 100 | 102.6922 | 72.4308 | 0 | 89.8144 | 1 | 1 | 0 | 2 | 1 | 0 | 0 | 88.1331 | 88.1331 | 220.1678 | 0 | PROCESSED | 57527.0641319444 | 2016-05-19 01:32:21 | 55031 | 2009-07-19 00:00:00 | 54665.3170601852 | 2008-07-18 07:36:34 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031165 | The nature of ultra-dense matter in neutron stars remains enigmatic. To probe this requires accurate neutron star radii and masses. We recently showed that broad iron lines in neutron star low-mass X-ray binaries (LMXBs) constrain the neutron star radius. LMXBs also provide us with another tool, kHz quasi-periodic oscillations (QPOs). Combining the inner disk velocity (from modeling the iron line) and the frequency of the kHz QPOs gives a method to measure the neutron star mass. We propose a 100 ks observation of Cyg X-2 with Suzaku to provide a detailed iron line profile. Combined with simultaneous observations with RXTE to determine the kHz QPO frequency, we will measure the neutron star mass. Cyg X-2 is the perfect test case as it already has a known mass from optical observations. | GALACTIC POINT SOURCES | 4 | B | EDWARD CACKETT | USA | 3 | AO3 | MEASURING NEUTRON STAR MASSES USING BROAD IRON LINES AND KHZ QPOS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403063010/ | Quick Look | ![]() |
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329 | JUPITER | 226.6157 | -16.1957 | 225.916913 | -16.003222 | 228.709072 | 1.245307 | 344.00356707 | 35.68981432 | 118.4907 | 53792.7940856482 | 2006-02-26 19:03:29 | 53793.8599421296 | 2006-02-27 20:38:19 | 401001030 | 40.7912 | 36 | 40.7992 | 40.7912 | 40.7992 | 40.7992 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35.5363 | 35.5363 | 92.0739 | 0 | PROCESSED | 57533.1063078704 | 2016-05-25 02:33:05 | 54401 | 2007-10-28 00:00:00 | 53905.5868055556 | 2006-06-19 14:05:00 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011003 | We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure. | GALACTIC POINT SOURCES | 4 | C | RONALD ELSNER | USA | 1 | AO1 | JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401001030/ | Quick Look | ![]() |
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330 | 4U 1608-52 | 243.1805 | -52.3646 | 242.219607 | -52.236867 | 251.312675 | -30.647361 | 330.96698106 | -0.80844416 | 94.0316 | 55270.6937615741 | 2010-03-15 16:39:01 | 55271.6668287037 | 2010-03-16 16:00:14 | 404044020 | 32.7181 | 30 | 32.7181 | 32.7261 | 0 | 32.7181 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 26.988 | 26.988 | 84.0558 | 1 | PROCESSED | 57550.9065277778 | 2016-06-11 21:45:24 | 55651 | 2011-03-31 00:00:00 | 55285.1175462963 | 2010-03-30 02:49:16 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041223 | The true nature of X-ray emission from neutron star X-ray binaries (NSXRBs) has not been clear for sometime and there are many possibilities for the spectral model. Recent progress has been made, but relies on RXTE data which lacks the low energy sensitivity where disk emission is most prominent. Using Suzaku we propose four 30 ksec observations of the transient 4U 1608-52 throughout an outburst. We will test how spectral parameters change with luminosity, allowing us to untangle the correct model. An essential part of this proposal is the unique ability of Suzaku to detect asymmetric broad iron emission lines in NSXRBs. We will study how the iron line varies throughout the outburst, which combined with the spectral fits will test the interaction between the accretion disk and corona. | GALACTIC POINT SOURCES | 4 | A | EDWARD CACKETT | USA | 4 | AO4-TOO | ACCRETION DISK EVOLUTION THROUGHOUT A NEUTRON STAR LMXB OUTBURST | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404044020/ | Quick Look | ![]() |
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331 | BETA LYR | 282.5094 | 33.3738 | 282.047614 | 33.314587 | 288.857821 | 55.998718 | 63.19462876 | 14.79594569 | 59.4704 | 53862.545474537 | 2006-05-07 13:05:29 | 53862.9952083333 | 2006-05-07 23:53:06 | 401036010 | 20.2515 | 20 | 20.2675 | 20.2515 | 20.2675 | 20.2675 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 9.8947 | 9.8947 | 38.8519 | 1 | PROCESSED | 57533.7394212963 | 2016-05-25 17:44:46 | 54401 | 2007-10-28 00:00:00 | 53913.8191550926 | 2006-06-27 19:39:35 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011031 | The goal of our project is to determine the location and properties of the hard X-ray emitting gas in the massive B7II+B0V interacting binary Beta Lyr. Our experiment is designed to distinguish between X-rays originating in the mass transfer stream and those originating in the extended circumbinary envelope. Modeling of XIS spectra will allow us to constrain the plasma temperature and emission measure, while the light curve with three exposures and high count rates will probe variability at around the 1% level over both the orbital timescale (13 days) and dynamical flow timescales (hours). Our request is for 20 ksec exposures at 3 different orbital phases to catch the system in and out of eclipse. | GALACTIC POINT SOURCES | 4 | A | RICHARD IGNACE | USA | 1 | AO1 | AN X-RAY STUDY OF HOT PLASMA IN THE INTERACTING BINARY BETA LYRAE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401036010/ | Quick Look | ![]() |
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332 | BETA LYR | 282.5093 | 33.3719 | 282.047501 | 33.312687 | 288.85715 | 55.996853 | 63.19278609 | 14.79528012 | 53.4973 | 53871.4311226852 | 2006-05-16 10:20:49 | 53871.8571875 | 2006-05-16 20:34:21 | 401036030 | 18.1954 | 20 | 18.1954 | 18.1954 | 18.1954 | 18.1954 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 19.8421 | 19.8421 | 36.8079 | 0 | PROCESSED | 57534.3160532407 | 2016-05-26 07:35:07 | 54401 | 2007-10-28 00:00:00 | 53920.4164351852 | 2006-07-04 09:59:40 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011031 | The goal of our project is to determine the location and properties of the hard X-ray emitting gas in the massive B7II+B0V interacting binary Beta Lyr. Our experiment is designed to distinguish between X-rays originating in the mass transfer stream and those originating in the extended circumbinary envelope. Modeling of XIS spectra will allow us to constrain the plasma temperature and emission measure, while the light curve with three exposures and high count rates will probe variability at around the 1% level over both the orbital timescale (13 days) and dynamical flow timescales (hours). Our request is for 20 ksec exposures at 3 different orbital phases to catch the system in and out of eclipse. | GALACTIC POINT SOURCES | 4 | A | RICHARD IGNACE | USA | 1 | AO1 | AN X-RAY STUDY OF HOT PLASMA IN THE INTERACTING BINARY BETA LYRAE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401036030/ | Quick Look | ![]() |
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333 | SKY_50.0_-62.4 | 50.0507 | -62.4328 | 49.819854 | -62.612067 | 354.772614 | -72.643934 | 278.67600391 | -47.08169247 | 281.591 | 53795.7055671296 | 2006-03-01 16:56:01 | 53796.9369675926 | 2006-03-02 22:29:14 | 501001010 | 80.145 | 80 | 80.153 | 80.145 | 80.153 | 80.145 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 74.0122 | 74.0122 | 106.376 | 0 | PROCESSED | 57533.1282638889 | 2016-05-25 03:04:42 | 54401 | 2007-10-28 00:00:00 | 53905.6164930556 | 2006-06-19 14:47:45 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011252 | We propose Suzaku XIS observations of the hot gas in the Galactic halo and Local Bubble. The spectra's bright emission lines and complexes will reveal the plasma's ionization history and thus its origins. The Local Bubble's spectrum will be garnered from an observation of a nearby opaque cloud. The halo's spectrum will be found by subtracting the Local Bubble spectrum from that of an adjacent off-cloud observation. In order to better constrain the models, we will also draw upon existing FUSE O VI emission data for these directions. With the combined O VI and soft X-ray data, we will be able to constrain the plasma's conditions and ionization history and, thus, constrain detailed models of the hot gas in the halo and Local Bubble. | GALACTIC DIFFUSE EMISSION | 5 | A | ROBIN SHELTON | USA | 1 | AO1 | SUZAKU XIS OBSERVATIONS OF THE GALACTIC HALO AND LOCAL BUBBLE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501001010/ | Quick Look | ![]() |
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334 | PSR B1259-63 | 195.6931 | -63.8349 | 194.903784 | -63.566278 | 227.685916 | -50.892951 | 304.18120501 | -0.9906484 | 99.8696 | 55566.8369212963 | 2011-01-05 20:05:10 | 55569.3959722222 | 2011-01-08 09:30:12 | 405037010 | 90.0407 | 80 | 90.0407 | 90.0407 | 0 | 90.0407 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74.4506 | 74.4506 | 221.0618 | 1 | PROCESSED | 57600.639375 | 2016-07-31 15:20:42 | 55961 | 2012-02-04 00:00:00 | 55595.2642939815 | 2011-02-03 06:20:35 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051221 | We propose to observe a gamma-ray binary PSR B1259-63 during the pulsar's second disk crossing after periastron passage. PSR B1259-63 is a young radio pulsar orbiting around a B2e star with a highly eccentric 3.4 yr orbit. Suzaku XIS+HXD measurements of the hard continuum emission from the binary system allow us to investigate particle acceleration in a highly variable environment as a result of interactions between the relativistic wind of the pulsar and the circumstellar disk of the Be star. With the advent of the Fermi Gamma-ray Space Telescope, we will be able to simultaneously observe X-rays and GeV gamma-rays during the disk transit for the first time. The observations of PSR B1259-63 will give us a unique opportunity to study the physics of pulsar winds on AU-scale. | GALACTIC POINT SOURCES | 4 | A | YASUNOBU UCHIYAMA | USA | 5 | AO5 | SUZAKU BROADBAND OBSERVATIONS OF A GAMMA-RAY BINARY PSRB1259-63 DURING THE POST-PERIASTRON FLARE IN 2011 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405037010/ | Quick Look | ![]() |
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335 | 4U 1728-34 | 262.9799 | -33.9051 | 262.153704 | -33.869072 | 264.067005 | -10.60817 | 354.23908298 | -0.18221646 | 278.0266 | 55473.517349537 | 2010-10-04 12:24:59 | 55475.6876967593 | 2010-10-06 16:30:17 | 405048010 | 50.5472 | 100 | 50.6522 | 50.5472 | 0 | 50.6522 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95.3606 | 95.3606 | 187.4678 | 3 | PROCESSED | 57553.6884490741 | 2016-06-14 16:31:22 | 55867 | 2011-11-02 00:00:00 | 55487.4662615741 | 2010-10-18 11:11:25 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051244 | Fe K-alpha lines have been detected in ten NS-LMXBs. Under the commonly accepted interpretation, they can be used to set tight constrains on the accretion disk geometry. 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 kHz QPOs. We have recently shown that simultaneous measurements of Fe lines and kHz QPOs in a NS-LMXB appear to contradict this picture. We propose to observe 4U 1728-34 with Suzaku five times for 20 ks, simultaneously with RXTE and ATCA. This program will allow us to study and compare the dynamics of the inner edge of the disk as inferred from the Fe line and the kHz QPOs, as well as the relation of both observables with the jet radio emission. | GALACTIC POINT SOURCES | 4 | A | MANUEL LINARES | USA | 5 | AO5 | ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405048010/ | Quick Look | ![]() |
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336 | 4U 1636-536 | 250.2272 | -53.754 | 249.230789 | -53.657507 | 256.461332 | -31.236669 | 332.91133194 | -4.81789372 | 91.2454 | 54160.0424421296 | 2007-03-01 01:01:07 | 54160.8931597222 | 2007-03-01 21:26:09 | 401050030 | 38.7193 | 38 | 38.7274 | 38.7193 | 0 | 38.7194 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 48.1459 | 48.1459 | 73.498 | 1 | PROCESSED | 57537.5161111111 | 2016-05-29 12:23:12 | 54695 | 2008-08-17 00:00:00 | 54167.6400462963 | 2007-03-08 15:21:40 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011117 | Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. | GALACTIC POINT SOURCES | 4 | A | JEROEN HOMAN | USA | 1 | AO1 | THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401050030/ | Quick Look | ![]() |
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337 | SWIFTJ2000.6+3210 | 300.1137 | 32.1218 | 299.624092 | 31.983158 | 312.678705 | 51.196511 | 68.93835501 | 1.08211502 | 255.6072 | 54039.0205671296 | 2006-10-31 00:29:37 | 54039.3029976852 | 2006-10-31 07:16:19 | 401053020 | 12.7484 | 10 | 12.7564 | 12.7484 | 12.7564 | 12.7564 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 11.727 | 11.727 | 24.3939 | 0 | PROCESSED | 57535.9859490741 | 2016-05-27 23:39:46 | 54775 | 2008-11-05 00:00:00 | 54056.1959953704 | 2006-11-17 04:42:14 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011132 | INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. | GALACTIC POINT SOURCES | 4 | A | RANDALL SMITH | USA | 1 | AO1 | HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401053020/ | Quick Look | ![]() |
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338 | HD162020 | 267.6661 | -40.3245 | 266.789333 | -40.311026 | 268.130752 | -16.898333 | 350.73610578 | -6.73339029 | 259.9986 | 55833.0255208333 | 2011-09-29 00:36:45 | 55833.4279513889 | 2011-09-29 10:16:15 | 406037040 | 16.7297 | 15 | 16.7377 | 16.7377 | 0 | 16.7297 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15.7286 | 15.7286 | 34.7499 | 0 | PROCESSED | 57603.2728356482 | 2016-08-03 06:32:53 | 56225 | 2012-10-25 00:00:00 | 55858.1397453704 | 2011-10-24 03:21:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061202 | Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. | GALACTIC POINT SOURCES | 4 | A | IGNAZIO PILLITTERI | USA | 6 | AO6 | STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406037040/ | Quick Look | ![]() |
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339 | CH CYG | 291.1621 | 50.2424 | 290.833167 | 50.142645 | 313.7082 | 70.490137 | 81.86550652 | 15.56609243 | 185.7481 | 53739.5736458333 | 2006-01-04 13:46:03 | 53740.2919560185 | 2006-01-05 07:00:25 | 400016020 | 33.3058 | 25 | 33.3075 | 33.3378 | 33.3155 | 33.3058 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 28.4615 | 28.4615 | 62.056 | 1 | PROCESSED | 57532.6355902778 | 2016-05-24 15:15:15 | 54247 | 2007-05-27 00:00:00 | 54039.6712268518 | 2006-10-31 16:06:34 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001082 | CH Cygni is a symbiotic star in which a white dwarf is believed to be accreting the wind of the red giant. ASCA observation revealed a complex X-ray spectrum consisting of a heavily absorbed hard component and a relatively unabsorbed soft component. We propose to obtain the spectrum of CH Cyg above 10 keV for the first time using Suzaku HXD (PIN), while simultaneously obtaining high quality spectrum below 10 keV with the XIS. | GALACTIC POINT SOURCES | 4 | A | KOJI MUKAI | JAP | 0 | SWG | SUZAKU OBSERVATION OF THE SYMBIOTIC SYSTEM CH CYGNI | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400016020/ | Quick Look | ![]() |
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340 | ETA CARINAE | 161.2181 | -59.7282 | 160.732192 | -59.464935 | 202.181916 | -58.969104 | 287.59637986 | -0.67920855 | 289.0006 | 54274.2459259259 | 2007-06-23 05:54:08 | 54275.9015509259 | 2007-06-24 21:38:14 | 402039010 | 58.3961 | 50 | 58.4041 | 58.3961 | 0 | 58.4041 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.552 | 51.552 | 143.0099 | 1 | PROCESSED | 57539.0368981482 | 2016-05-31 00:53:08 | 54695 | 2008-08-17 00:00:00 | 54322.5140856482 | 2007-08-10 12:20:17 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021026 | XMM-Newton observations in 2003 suggest that X-ray emission from Eta Carinae has a hard X-ray component above 10 keV in addition to the thermal emission with kT ~3-5 keV. The excess is apparently strongest near the 2-10 keV X-ray maximum, and possibly produced by very hot plasma or 1st-order Fermi acceleration of particles which then inverse Compton-upscatter UV seed photons from the stellar photospheres. We propose a 50 ksec observation of Eta Carinae with the Suzaku telescope during AO2, compare the X-ray spectrum with earlier observations and determine the level of emission at E >9 keV. | GALACTIC POINT SOURCES | 4 | B | KENJI HAMAGUCHI | USA | 2 | AO2 | HARD X-RAY EMISSION FROM ETA CARINAE | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402039010/ | Quick Look | ![]() |
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341 | SNR G93.3+6.9 S2 | 312.6887 | 55.4958 | 312.345372 | 55.307685 | 351.959804 | 67.182569 | 93.24230604 | 7.18061007 | 40.0056 | 53905.9701736111 | 2006-06-19 23:17:03 | 53906.4293865741 | 2006-06-20 10:18:19 | 501081010 | 16.0092 | 15 | 16.0352 | 16.0272 | 16.0092 | 16.0352 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 18.3757 | 18.3757 | 39.6679 | 1 | PROCESSED | 57534.7256134259 | 2016-05-26 17:24:53 | 54401 | 2007-10-28 00:00:00 | 53927.314537037 | 2006-07-11 07:32:56 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011242 | The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. | GALACTIC DIFFUSE EMISSION | 5 | B | Q. DANIEL WANG | USA | 1 | AO1 | G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501081010/ | Quick Look | ![]() |
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342 | GX17+2 | 274.0087 | -14.1006 | 273.298097 | -14.118345 | 273.929719 | 9.285377 | 16.37694194 | 1.24456043 | 269.7113 | 54362.2773032407 | 2007-09-19 06:39:19 | 54362.8543402778 | 2007-09-19 20:30:15 | 402050010 | 19.0959 | 20 | 19.0959 | 19.1044 | 0 | 19.0959 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 16.0445 | 16.0445 | 49.8499 | 0 | PROCESSED | 57540.0136458333 | 2016-06-01 00:19:39 | 54751 | 2008-10-12 00:00:00 | 54384.4487037037 | 2007-10-11 10:46:08 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021111 | Z sources are bright low-mass X-ray binaries with variable spectra that describe a characteristic "Z" shape in an X-ray color-color plot. The forces driving the spectral shape and variability of the Z sources are not well understood, as there are few detectors with the necessary capabilities. GX17+2 is a Sco-type Z sources with an unusual time-varying hard X-ray tail whose origin is uncertain. Bright X-ray sources also illuminate the interstellar medium. Highly absorbed X-ray sources show halos due to dust scattering as well as absorption features. These will allow us to place constraints on interstellar dust and gas models. Suzaku can address all of these issues with simultaneous observations of the hard X-ray continuum and the dust-scattered X-ray halo. | GALACTIC POINT SOURCES | 4 | A | RANDALL SMITH | USA | 2 | AO2 | OBSERVING THE SPECTRUM AND HALO OF GX17+2 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402050010/ | Quick Look | ![]() |
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343 | A 0535+26 | 84.7195 | 26.3786 | 83.941618 | 26.351102 | 85.26575 | 3.024576 | 181.38803208 | -2.61609461 | 86.1856 | 55067.9626273148 | 2009-08-24 23:06:11 | 55069.1599421296 | 2009-08-26 03:50:19 | 404054010 | 51.8668 | 45 | 51.8706 | 51.8706 | 0 | 51.8668 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.078 | 42.078 | 103.4298 | 1 | PROCESSED | 57548.3667708333 | 2016-06-09 08:48:09 | 55448 | 2010-09-09 00:00:00 | 55078.219837963 | 2009-09-04 05:16:34 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041232 | We propose to perform Target of Opportunity Observations of one accreting neutron star in outburst during Suzaku's AO-4. The aim of the observations is to observe the source at a level of 40 and 200mCrab, to determine the properties of the cyclotron line(s) in this system and to constrain its broad band spectrum. | GALACTIC POINT SOURCES | 4 | A | KATJA POTTSCHMIDT | USA | 4 | AO4-TOO | CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404054010/ | Quick Look | ![]() |
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344 | PUP A : SE | 126.0128 | -43.1802 | 125.58355 | -43.01733 | 147.904142 | -59.590498 | 260.74447692 | -3.25911558 | 277.1832 | 53843.3098842593 | 2006-04-18 07:26:14 | 53843.8328009259 | 2006-04-18 19:59:14 | 501089010 | 29.7493 | 30 | 29.7493 | 29.8172 | 29.7652 | 29.7612 | 4 | 2 | 4 | 4 | 1 | 0 | 0 | 22.8867 | 22.8867 | 45.174 | 0 | PROCESSED | 57533.5119675926 | 2016-05-25 12:17:14 | 54401 | 2007-10-28 00:00:00 | 53907.001412037 | 2006-06-21 00:02:02 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011246 | We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present. | GALACTIC DIFFUSE EMISSION | 5 | A | UNA HWANG | USA | 1 | AO1 | MAPPING OXYGEN IN PUPPIS A | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501089010/ | Quick Look | ![]() |
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345 | AQL X-1 | 287.816 | 0.5784 | 287.177723 | 0.494688 | 289.376856 | 22.828471 | 35.71219982 | -4.14539755 | 284.0925 | 54371.6493402778 | 2007-09-28 15:35:03 | 54372.062662037 | 2007-09-29 01:30:14 | 402053010 | 13.8252 | 15 | 13.8252 | 13.8252 | 0 | 13.8252 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 13.745 | 13.745 | 35.704 | 0 | PROCESSED | 57540.1327199074 | 2016-06-01 03:11:07 | 54769 | 2008-10-30 00:00:00 | 54402.3541550926 | 2007-10-29 08:29:59 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021114 | We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. | GALACTIC POINT SOURCES | 4 | A | RONALD REMILLARD | USA | 2 | AO2-TOO | X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402053010/ | Quick Look | ![]() |
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346 | 4U 0115+63 | 19.6139 | 63.7554 | 18.78861 | 63.492562 | 49.805717 | 49.807631 | 125.91367385 | 1.04017806 | 82.1235 | 55750.053587963 | 2011-07-08 01:17:10 | 55751.0210763889 | 2011-07-09 00:30:21 | 406049010 | 42.2748 | 45 | 42.2748 | 42.3548 | 0 | 42.3548 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.1432 | 42.1432 | 83.5779 | 1 | PROCESSED | 57602.5577662037 | 2016-08-02 13:23:11 | 56163 | 2012-08-24 00:00:00 | 55778.4311226852 | 2011-08-05 10:20:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061234 | We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | KATJA POTTSCHMIDT | USA | 6 | AO6-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406049010/ | Quick Look | ![]() |
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347 | 2S 0921-630 | 140.6632 | -63.3 | 140.373022 | -63.085068 | 195.142403 | -68.892754 | 281.84517925 | -9.33739383 | 20.5636 | 54340.7614351852 | 2007-08-28 18:16:28 | 54341.8335532407 | 2007-08-29 20:00:19 | 402057010 | 43.2131 | 40 | 43.2131 | 43.2211 | 0 | 43.2211 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.8568 | 15.8568 | 92.6158 | 0 | PROCESSED | 57539.9304976852 | 2016-05-31 22:19:55 | 54721 | 2008-09-12 00:00:00 | 54353.4365625 | 2007-09-10 10:28:39 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021118 | 2S 0921-630 is a bright, long-period LMXB that is thought to contain an accretion disk corona. Observations with both the Chandra HETGS and XMM-Newton spectrometers revealed line emission from a photoionized plasma. The spectral features are consistent with the predictions for emission from an accretion disk corona. However, with the present data it is impossible to determine whether the emission originates in the corona or in a localized region of the disk. We propose to observer 2S 0921-630 with Suzaku at four orbital phases in order to localize and identify the emitting plasma. The simultaneous HXD coverage will also allow us to constrain the underlying continuum and allow more sensitive study of the high energy region of the spectrum. | GALACTIC POINT SOURCES | 4 | A | JEAN COTTAM | USA | 2 | AO2 | PHASE-RESOLVED SPECTROSCOPY OF 2S 0921-630 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402057010/ | Quick Look | ![]() |
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348 | HEN 3-1591 | 271.8863 | -25.8981 | 271.110376 | -25.90538 | 271.688765 | -2.468309 | 5.07192211 | -2.68044312 | 269.6421 | 56203.7249537037 | 2012-10-03 17:23:56 | 56204.7793981482 | 2012-10-04 18:42:20 | 407042010 | 51.3876 | 50 | 51.3877 | 51.3876 | 0 | 51.4036 | 4 | 3 | 0 | 3 | 1 | 0 | 0 | 52.3681 | 52.3681 | 91.0959 | 1 | PROCESSED | 57607.2899884259 | 2016-08-07 06:57:35 | 56592 | 2013-10-27 00:00:00 | 56226.5545601852 | 2012-10-26 13:18:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071211 | The number of symbiotic stars known to be medium energy (2-10 keV) X-ray emitters has increased markedly in the last several years. These are white dwarfs accreting from a giant mass donor, unlike the less common class of symbiotic X-ray binaries in which the accretor is a neutron star. The X-ray spectra of the white dwarf symbiotics can be used to constrain the white dwarf mass and accretion rate. Here we focus on one object, Hen 3-1591, which belongs to a rare subclass of d'-type yellow symbiotic, commonly thought to harbor a young white dwarf. Hen 3-1591 is the first of this subclass to show medium energy X-ray emission, and hence we propose a moderately deep Suzaku observation to characterize its white dwarf and the circum-binary environment. | GALACTIC POINT SOURCES | 4 | B | KOJI MUKAI | USA | 7 | AO7 | THE X-RAY EMISSION OF THE YELLOW SYMBIOTIC STAR, HEN 3-1591 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407042010/ | Quick Look | ![]() |
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349 | NGC 5506 | 213.3121 | -3.2119 | 212.6632 | -2.97838 | 212.190756 | 9.596557 | 339.14659218 | 53.80640928 | 287.3747 | 53958.1015972222 | 2006-08-11 02:26:18 | 53959.4488425926 | 2006-08-12 10:46:20 | 701030020 | 53.2962 | 63 | 53.3042 | 53.2962 | 53.3042 | 53.3042 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 47.9832 | 47.9832 | 116.386 | 1 | PROCESSED | 57535.2817476852 | 2016-05-27 06:45:43 | 54695 | 2008-08-17 00:00:00 | 54116.3307291667 | 2007-01-16 07:56:15 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011312 | NGC 5506 is one of the brightest Seyferts in the X-ray sky, the second brightest in the PIN bandpass. Obscuring gas has kept the true nature of this AGN secret until recent optical and infrared studies have unmasked the narrow-line-seyfert 1 nucleus. With this knowledge, NGC 5506 is the perfect candidate for confirming the generality of a new result based on a recent XMM observation of Mkn 766, ie that the ionized component of Fe K emission originates from the inner accretion disk and closely tracks the hard X-ray continuum flux. This immediately gives us the ionization-state and size-scale of the inner disk. We request a 150 ks Suzaku observation to see whether a similar result holds for NGC 5506 and, by extension, may be a property of NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TRACEY TURNER | USA | 1 | AO1 | SUZAKU STUDY OF THE BRIGHTEST NARROW LINE SEYFERT 1: NGC 5506 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701030020/ | Quick Look | ![]() |
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350 | MBM12 OFF-CLOUD | 41.3205 | 18.3346 | 40.61976 | 18.124407 | 44.482795 | 2.251416 | 157.33933963 | -36.81758445 | 247.4802 | 53772.648599537 | 2006-02-06 15:33:59 | 53774.618275463 | 2006-02-08 14:50:19 | 501104010 | 75.3292 | 70 | 75.3372 | 75.3292 | 75.3372 | 75.3372 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 67.769 | 67.769 | 170.1159 | 1 | PROCESSED | 57532.9691550926 | 2016-05-24 23:15:35 | 54401 | 2007-10-28 00:00:00 | 53905.9757523148 | 2006-06-19 23:25:05 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011262 | Suzaku will observe MBM 12, a nearby molecular cloud which shadows all but the most local soft X-ray emission. The goal of that observation is to measure the O VII and O VIII emission from the Local Hot Bubble, taking advantage of Suzaku's low energy sensitivity and low background. In light of this, we propose to observe the diffuse background near the MBM 12 position. This will: (1) Measure the O VII and O VIII emission from the Galactic disk and halo, after subtracting the local emission, and (2) confirm that this background emission does not contaminate the initial observation. The absolute measure of the strength of the O VII line, as well as the O VIII/O VII ratio, is essential to understanding the origin of the Galactic component to the 3/4 keV diffuse emission. | GALACTIC DIFFUSE EMISSION | 5 | B | RANDALL SMITH | USA | 1 | AO1 | THE ORIGIN OF THE GALACTIC DIFFUSE 3/4 KEV X-RAY BACKGROUND | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501104010/ | Quick Look | ![]() |
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351 | CYGNUS X-1 | 299.5969 | 35.1891 | 299.126785 | 35.052601 | 313.664382 | 54.235906 | 71.32710759 | 3.05572664 | 254.8701 | 56231.3416782407 | 2012-10-31 08:12:01 | 56232.109212963 | 2012-11-01 02:37:16 | 407072010 | 0.3726 | 30 | 1.9394 | 1.9908 | 0 | 0.3726 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 30.0857 | 30.0857 | 66.3059 | 0 | PROCESSED | 57607.9427430556 | 2016-08-07 22:37:33 | 56611 | 2013-11-15 00:00:00 | 56245.5107407407 | 2012-11-14 12:15:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071241 | We propose for a single 30 ks observation of the accreting black hole Cygnus X-1. NuSTAR is an upcoming (to be launched in Spring 2012) hard X-ray (5-80 keV) mission that will plan its schedule to obtain simultaneous coverage of Cyg X-1 with Suzaku. The observations will be used for both science and cross-calibration. The combination of Suzaku and NuSTAR will provide the best measurement of the reflection component, including a relativistically broadened iron line and a hard X-ray excess, and the information will be used to test emission models and constrain the Cyg X-1 accretion geometry. The XIS capabilities to measure the iron line are essential for the science, and the HXD coverage is essential for the cross-calibration. | GALACTIC POINT SOURCES | 4 | A | JOHN TOMSICK | USA | 7 | AO7 | CYGNUS X-1 WITH SUZAKU AND NUSTAR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407072010/ | Quick Look | ![]() |
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352 | MRK 766 | 184.6147 | 29.8197 | 183.986078 | 30.097268 | 171.204802 | 28.944359 | 190.62410896 | 82.27145087 | 134.9989 | 54421.893287037 | 2007-11-17 21:26:20 | 54423.2363310185 | 2007-11-19 05:40:19 | 701035020 | 59.3635 | 50 | 59.3635 | 59.3635 | 0 | 59.3635 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 51.1517 | 51.1517 | 116.0238 | 1 | PROCESSED | 57540.5762384259 | 2016-06-01 13:49:47 | 54800 | 2008-11-30 00:00:00 | 54433.2716666667 | 2007-11-29 06:31:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011328 | X-ray spectroscopy of Mkn 766 has revealed ionised Fe emission that varies with the continuum on 10 ks timescales: direct evidence for ionised reflection from the accretion disk. This bright NLSy1 also shows extreme spectral variability, with the low state being dominated by a hard, constant reflection component, probably from cool distant material. We propose to measure the spectrum above 10 keV; the hot component should vary with the continuum, the cold distant component should be constant, and we can measure their relative contributions to test the predictions of the lower-energy analysis. This source is complex and needs the high-energy spectrum from Suzaku: it seems likely that previous complex behavior of several Seyferts can be described by these components | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TRACEY TURNER | USA | 1 | AO1 | DECOMPOSITION OF SEYFERT SPECTRA: TRACKING THE INNER DISK IN MKN 766 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701035020/ | Quick Look | ![]() |
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353 | TAU SCO | 248.9729 | -28.218 | 248.19336 | -28.116323 | 251.450261 | -6.120276 | 351.53455344 | 12.80533126 | 274.2608 | 54703.1981597222 | 2008-08-25 04:45:21 | 54703.5447222222 | 2008-08-25 13:04:24 | 403034060 | 15.0183 | 10 | 15.0263 | 15.0343 | 0 | 15.0183 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.9049 | 12.9049 | 29.9119 | 0 | PROCESSED | 57543.3841898148 | 2016-06-04 09:13:14 | 55084 | 2009-09-10 00:00:00 | 54713.2754976852 | 2008-09-04 06:36:43 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031121 | We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars. | GALACTIC POINT SOURCES | 4 | A | RICHARD IGNACE | USA | 3 | AO3 | X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403034060/ | Quick Look | ![]() |
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354 | COMET_8P_TUTTLE-P2_01 | 39.6412 | -35.6843 | 39.127956 | -35.899537 | 21.259605 | -47.847912 | 240.18300744 | -65.68930545 | 257.5577 | 54490.0082291667 | 2008-01-25 00:11:51 | 54490.1627083333 | 2008-01-25 03:54:18 | 502063010 | 4.3468 | 5 | 4.3468 | 4.3468 | 0 | 4.3468 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 4.4029 | 4.4029 | 13.3279 | 1 | PROCESSED | 57541.3739236111 | 2016-06-02 08:58:27 | 54912 | 2009-03-22 00:00:00 | 54546.0974189815 | 2008-03-21 02:20:17 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063010/ | Quick Look | ![]() |
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355 | GX 301-2 | 186.5611 | -62.8021 | 185.862176 | -62.525248 | 221.491572 | -52.675278 | 300.05773343 | -0.07103063 | 326.712 | 54703.5522800926 | 2008-08-25 13:15:17 | 54704.0036689815 | 2008-08-26 00:05:17 | 403044010 | 11.4275 | 60 | 11.4292 | 11.4306 | 0 | 11.4275 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.7148 | 10.7148 | 38.9939 | 0 | PROCESSED | 57543.3977546296 | 2016-06-04 09:32:46 | 55218 | 2010-01-22 00:00:00 | 54720.435462963 | 2008-09-11 10:27:04 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031152 | We propose the first observation of the bright neutron star GX 301-2 with Suzaku. The aim of the proposed 60 ks observation is a study of the broadband spectrum of the source in unprecedented detail and quality. This will allow us to analyze the structure (including density and clumpiness) of the intense wind of the optical companion and the gas stream flowing from Wray 977 to the neutron star. Spectral data will be used to study the evolution of nH and the iron line with very high time resolution. Furthermore, we will perform phase resolved spectroscopy to study the spectral variation of the cyclotron line with pulse phase. | GALACTIC POINT SOURCES | 4 | A | RICHARD ROTHSCHILD | USA | 3 | AO3 | BROAD-BAND STUDY OF GX 301-2 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403044010/ | Quick Look | ![]() |
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356 | COMET_8P_TUTTLE-P2_06 | 39.9457 | -36.3936 | 39.436659 | -36.607889 | 21.099638 | -48.591179 | 241.70384829 | -65.28238509 | 258.0349 | 54490.6963773148 | 2008-01-25 16:42:47 | 54490.8293287037 | 2008-01-25 19:54:14 | 502063060 | 6.6904 | 6.7 | 6.6906 | 6.6906 | 0 | 6.6904 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 4.338 | 4.338 | 11.4799 | 0 | PROCESSED | 57541.3927893518 | 2016-06-02 09:25:37 | 54912 | 2009-03-22 00:00:00 | 54546.1201736111 | 2008-03-21 02:53:03 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063060/ | Quick Look | ![]() |
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357 | ETA CARINAE | 161.2819 | -59.6866 | 160.795238 | -59.423234 | 202.165647 | -58.917186 | 287.60543966 | -0.62739972 | 356.4874 | 56894.0150810185 | 2014-08-25 00:21:43 | 56894.6884375 | 2014-08-25 16:31:21 | 409027010 | 34.5098 | 30 | 34.5098 | 34.5256 | 0 | 34.5258 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5156712963 | 2016-08-16 12:22:34 | 57285 | 2015-09-20 00:00:00 | 56910.6449884259 | 2014-09-10 15:28:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091202 | Eta Carinae is an extremely massive binary system whose strong winds produce a variety of high-energy X-ray and possibly gamma-ray emission. Earlier XMM-Newton, Suzaku and INTEGRAL observations found interesting features in the extremely hard X-ray band: i) a flat spectral component above 9 keV toward the flux maximum; ii) strong 15-20 keV emission during an occultation of the wind-wind colliding plasma; iii) stable power-law emission above 25 keV. These features are signs of the highest energy processes yet detected in any colliding wind binary. Broad band X-ray observations around periastron are essential to understanding those features. We therefore propose Suzaku observations at 5 key phases around the next periastron passage of eta Carinae in 2014.6. | GALACTIC POINT SOURCES | 4 | A | KENJI HAMAGUCHI | USA | 9 | AO9 | PROBING THE HIGHEST ENERGY PHENOMENA OF ETA CARINAE AROUND PERIASTRON IN 2014 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409027010/ | Quick Look | ![]() |
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358 | G332.5-5.6 NE | 251.0925 | -54.3783 | 250.085838 | -54.28574 | 257.162856 | -31.775018 | 332.77088512 | -5.61037777 | 77.916 | 54504.4521296296 | 2008-02-08 10:51:04 | 54505.6669444444 | 2008-02-09 16:00:24 | 502067010 | 71.1926 | 80 | 71.2006 | 71.2086 | 0 | 71.1926 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 65.2508 | 65.2508 | 104.9418 | 0 | PROCESSED | 57541.5340277778 | 2016-06-02 12:49:00 | 54883 | 2009-02-21 00:00:00 | 54515.6965509259 | 2008-02-19 16:43:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021216 | We propose to observe G332.5-5.6, a puzzling supernova remnant with several unusual features: high radio polarization, central emission with bilaterally symmetric limbs, and evidence for enhanced nitrogen suggesting interaction with processed circumstellar material. Very little is known about G332.5-5.6, so our observations will provide information on the remnant shock speed, age, and evolutionary state; on the possible presence of nonthermal emission, either due to a pulsar in the center or to shock-accelerated electrons in the limbs; and on abundances, which might identify ejecta emission and allow the classification of the supernova. | GALACTIC DIFFUSE EMISSION | 5 | B | STEPHEN REYNOLDS | USA | 2 | AO2 | G332.5-5.6: AN UNUSUAL SUPERNOVA REMNANT WITH CIRCUMSTELLAR INTERACTION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502067010/ | Quick Look | ![]() |
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359 | HD6903 | 17.4507 | 19.662 | 16.780979 | 19.395948 | 23.622213 | 11.325445 | 128.84764567 | -42.9987034 | 70.0004 | 55031.3824305556 | 2009-07-19 09:10:42 | 55032.3578703704 | 2009-07-20 08:35:20 | 404034010 | 36.8135 | 35 | 36.8295 | 36.8135 | 0 | 36.8215 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29.6727 | 29.6727 | 84.2639 | 0 | PROCESSED | 57547.8823958333 | 2016-06-08 21:10:39 | 55419 | 2010-08-11 00:00:00 | 55048.3029976852 | 2009-08-05 07:16:19 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041201 | Suzaku XIS spectra of two G0 III Hertzsprung gap giants will complete a multi-observatory survey of the anomalous coronal behavior of this "X-ray deficient" class. The abrupt rise in coronal luminosities from the warmer giants to their cooler cousins, only slightly further advanced in evolution, might signal disruption of a "fossil" magnetosphere by a newly born solar-like dynamo. Key discriminators are the coronal energy distribution, composition (FIP bias), and sporadic hard emission associated with flaring. The proposed targets are the brightest not previously observed in X-rays at CCD resolution, and both have supporting HST UV spectra. Expanding the high energy sample of this key class of objects is essential for probing their contrary, but perhaps deeply significant, behavior. | GALACTIC POINT SOURCES | 4 | B | THOMAS AYRES | USA | 4 | AO4 | ANOMALOUS CORONAE IN THE MIDST OF THE HERTZSPRUNG GAP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404034010/ | Quick Look | ![]() |
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360 | GS 2023+338 | 306.0444 | 33.8015 | 305.554336 | 33.638661 | 321.046576 | 51.052001 | 73.0785131 | -2.14854563 | 252.4521 | 55142.9636805556 | 2009-11-07 23:07:42 | 55144.0550810185 | 2009-11-09 01:19:19 | 404059010 | 42.3246 | 40 | 42.3486 | 42.3246 | 0 | 42.3566 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29.1404 | 29.1404 | 94.2839 | 1 | PROCESSED | 57549.1887384259 | 2016-06-10 04:31:47 | 55531 | 2010-12-01 00:00:00 | 55155.1065625 | 2009-11-20 02:33:27 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041243 | The quiescent state is the dominant accretion mode for black holes on all mass scales. Our knowledge of the X-ray spectrum is limited due to the characteristic low luminosity in this state. Here, we propose a 40 ks observation of the most luminous quiescent stellar mass black hole GS 2023+338 (V404 Cyg). These observations will allow us to detect hard X-ray emission from a quiescent stellar mass black hole for the first time, providing unique contraints on the nature of the accretion flow in this low luminosity state. | GALACTIC POINT SOURCES | 4 | B | MARK REYNOLDS | USA | 4 | AO4 | CONSTRAINING THE QUIESCENT ACCRETION FLOW AROUND A BLACK HOLE WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404059010/ | Quick Look | ![]() |
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361 | ETA CARINAE | 161.2814 | -59.6826 | 160.794718 | -59.419235 | 202.159659 | -58.914636 | 287.60335194 | -0.62397837 | 335.8837 | 56875.8359259259 | 2014-08-06 20:03:44 | 56876.6961111111 | 2014-08-07 16:42:24 | 409028010 | 21.5455 | 30 | 21.5455 | 21.5455 | 0 | 21.5455 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9.9582 | 9.9582 | 22.028 | 0 | PROCESSED | 57616.4668518518 | 2016-08-16 11:12:16 | 57264 | 2015-08-30 00:00:00 | 56898.441875 | 2014-08-29 10:36:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091202 | Eta Carinae is an extremely massive binary system whose strong winds produce a variety of high-energy X-ray and possibly gamma-ray emission. Earlier XMM-Newton, Suzaku and INTEGRAL observations found interesting features in the extremely hard X-ray band: i) a flat spectral component above 9 keV toward the flux maximum; ii) strong 15-20 keV emission during an occultation of the wind-wind colliding plasma; iii) stable power-law emission above 25 keV. These features are signs of the highest energy processes yet detected in any colliding wind binary. Broad band X-ray observations around periastron are essential to understanding those features. We therefore propose Suzaku observations at 5 key phases around the next periastron passage of eta Carinae in 2014.6. | GALACTIC POINT SOURCES | 4 | A | KENJI HAMAGUCHI | USA | 9 | AO9 | PROBING THE HIGHEST ENERGY PHENOMENA OF ETA CARINAE AROUND PERIASTRON IN 2014 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409028010/ | Quick Look | ![]() |
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362 | IGR J14536-5522 | 223.4257 | -55.3573 | 222.511349 | -55.15352 | 238.942519 | -36.822348 | 319.76650903 | 3.46705373 | 279.1547 | 56870.9840277778 | 2014-08-01 23:37:00 | 56872.0398263889 | 2014-08-03 00:57:21 | 409031010 | 38.8825 | 40 | 38.8825 | 38.8905 | 0 | 38.8905 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.4455902778 | 2016-08-16 10:41:39 | 57270 | 2015-09-05 00:00:00 | 56902.7225231482 | 2014-09-02 17:20:26 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091211 | Cataclysmic variables (CVs) detected in the INTEGRAL and Swift BAT hard X-ray surveys are predominantly magnetic systems of the intermediate polar subtype. However, as the survey sensitivity improves, an increasing number of polars are also detected as hard X-ray sources, even though the majority of polars are soft X-ray bright and hard X-ray faint. Over the long term, we hope to understand why most polars are soft X-ray dominated, and why a subset is hard X-ray bright. Here we propose Suzaku observations of four poorly studied BAT-detected polars, 1RXS J032540.0-081442, Swift J2319.4+2619, IW Eri, and IGR J14536-5522, supported by ground-based observations including optical polarimetry, to determine their system parameters. | GALACTIC POINT SOURCES | 4 | A | KOJI MUKAI | USA | 9 | AO9 | HARD X-RAY BRIGHT POLARS: WHY ARE THEY DIFFERENT? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409031010/ | Quick Look | ![]() |
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363 | CEP X-4 | 324.858 | 56.9961 | 324.464066 | 56.769041 | 5.88583 | 63.403956 | 99.01064753 | 3.3270936 | 51.1039 | 56826.8679282407 | 2014-06-18 20:49:49 | 56828.0363541667 | 2014-06-20 00:52:21 | 409037010 | 29.7647 | 50 | 29.7647 | 50.4597 | 0 | 30.9332 | 2 | 3 | 0 | 2 | 1 | 0 | 0 | 53.3133 | 53.3133 | 100.9358 | 1 | PROCESSED | 57615.3130671296 | 2016-08-15 07:30:49 | 57206 | 2015-07-03 00:00:00 | 56839.8053240741 | 2014-07-01 19:19:40 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091232 | We propose to perform Target of Opportunity observations of two accreting neutron stars that are known cyclotron line sources, out of a sample of five, in outburst. The aim is to observe the sources for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | FELIX FUERST | USA | 9 | AO9-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409037010/ | Quick Look | ![]() |
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364 | 4U 1608-52 | 243.1735 | -52.4241 | 242.21194 | -52.296335 | 251.322253 | -30.70644 | 330.92310685 | -0.84886634 | 127.9983 | 55277.989849537 | 2010-03-22 23:45:23 | 55278.9140393518 | 2010-03-23 21:56:13 | 404044040 | 16.0728 | 30 | 16.0728 | 16.0728 | 0 | 16.0728 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 15.6557 | 15.6557 | 79.8439 | 2 | PROCESSED | 57550.9805439815 | 2016-06-11 23:31:59 | 55665 | 2011-04-14 00:00:00 | 55299.4128819444 | 2010-04-13 09:54:33 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041223 | The true nature of X-ray emission from neutron star X-ray binaries (NSXRBs) has not been clear for sometime and there are many possibilities for the spectral model. Recent progress has been made, but relies on RXTE data which lacks the low energy sensitivity where disk emission is most prominent. Using Suzaku we propose four 30 ksec observations of the transient 4U 1608-52 throughout an outburst. We will test how spectral parameters change with luminosity, allowing us to untangle the correct model. An essential part of this proposal is the unique ability of Suzaku to detect asymmetric broad iron emission lines in NSXRBs. We will study how the iron line varies throughout the outburst, which combined with the spectral fits will test the interaction between the accretion disk and corona. | GALACTIC POINT SOURCES | 4 | A | EDWARD CACKETT | USA | 4 | AO4-TOO | ACCRETION DISK EVOLUTION THROUGHOUT A NEUTRON STAR LMXB OUTBURST | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404044040/ | Quick Look | ![]() |
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365 | HESS J1804-216 | 271.1693 | -21.6722 | 270.417896 | -21.676057 | 271.077547 | 1.764239 | 8.44223916 | -0.04647489 | 89.0483 | 53831.6120138889 | 2006-04-06 14:41:18 | 53832.4919328704 | 2006-04-07 11:48:23 | 500007010 | 37.5222 | 50 | 37.5222 | 37.5222 | 37.5222 | 37.5222 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 28.9336 | 28.9336 | 75.9901 | 0 | PROCESSED | 57533.4045138889 | 2016-05-25 09:42:30 | 54247 | 2007-05-27 00:00:00 | 54042.288900463 | 2006-11-03 06:56:01 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001029 | HESS found several new TeV sources in the Galactic Plane Survey. Possible origin would be PWN or synchrotron X-ray SNR shell. However many of these new TeV sources (their sizes are ~10 arcmin) have no counterpart in any other wavelength. They can be main contributors to the Galactic Cosmic rays. In order to reveal the nature of these fantastic objects, we propose to observe the extended sources. HESS~J1616-508 is already observed and we found this source has quite low surface brightness in X-rays compared with TeV gamma-rays, indicating this is a dark particle accelerator Here, we point out HESS~J1804-216 which has possible counterparts in other wavelengths, then it might be the missing link between known Galactic accelerators and dark particle accelerators. | GALACTIC DIFFUSE EMISSION | 5 | A | AYA BAMBA | JAP | 0 | SWG | SEARCH FOR X-RAY COUNTERPARTS OF ``DARK PARTICLE ACCELERATORS'' | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500007010/ | Quick Look | ![]() |
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366 | HESS J1804-216 BGD | 270.9564 | -22.0176 | 270.203045 | -22.020418 | 270.877317 | 1.420312 | 8.04431311 | -0.04388906 | 89.2004 | 53832.4925462963 | 2006-04-07 11:49:16 | 53833.454375 | 2006-04-08 10:54:18 | 500008010 | 40.7171 | 50 | 40.7171 | 40.7171 | 40.7171 | 40.7171 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 30.6429 | 30.6429 | 83.0879 | 1 | PROCESSED | 57533.4349537037 | 2016-05-25 10:26:20 | 54247 | 2007-05-27 00:00:00 | 54056.4266666667 | 2006-11-17 10:14:24 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001029 | HESS found several new TeV sources in the Galactic Plane Survey. Possible origin would be PWN or synchrotron X-ray SNR shell. However many of these new TeV sources (their sizes are ~10 arcmin) have no counterpart in any other wavelength. They can be main contributors to the Galactic Cosmic rays. In order to reveal the nature of these fantastic objects, we propose to observe the extended sources. HESS~J1616-508 is already observed and we found this source has quite low surface brightness in X-rays compared with TeV gamma-rays, indicating this is a dark particle accelerator Here, we point out HESS~J1804-216 which has possible counterparts in other wavelengths, then it might be the missing link between known Galactic accelerators and dark particle accelerators. | GALACTIC DIFFUSE EMISSION | 5 | A | AYA BAMBA | JAP | 0 | SWG | SEARCH FOR X-RAY COUNTERPARTS OF ``DARK PARTICLE ACCELERATORS'' | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500008010/ | Quick Look | ![]() |
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367 | RXJ_0852-4622_NW | 132.2926 | -45.6157 | 131.862494 | -45.429101 | 157.976747 | -59.482382 | 265.39238743 | -1.14402175 | 137.763 | 53723.4478240741 | 2005-12-19 10:44:52 | 53727.3016666667 | 2005-12-23 07:14:24 | 500010010 | 175.453 | 150 | 175.453 | 175.525 | 175.4608 | 175.461 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 230.0025 | 230.0025 | 332.9437 | 7 | PROCESSED | 57532.5654513889 | 2016-05-24 13:34:15 | 54247 | 2007-05-27 00:00:00 | 54059.902662037 | 2006-11-20 21:39:50 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001048 | We propose to observe two lobes of X-ray and gamma-ray emission from the shell remnant RXJ 0852-4622 (Vela Jr) with HXD. The 1-10 keV spectrum of this remnant is essentially a featureless continuum attributed to synchrotron emission from accelerated electrons, with the X-ray and gamma-ray morphologies being very well matched. Observations at energies above 10 keV with HXD will probe the cut-off energy of the synchrotron spectrum, shedding light on the electron acceleration efficiency. The large size of the remnant makes it possible to observe different portions of the limb with separate HXD PIN observations. | GALACTIC DIFFUSE EMISSION | 5 | A | UNA HWANG | JAP | 0 | SWG | HXD OBSERVATION OF NONTHERMAL EMISSION FROM RXJ 0852-4622 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500010010/ | Quick Look | ![]() |
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368 | SMC DIFFUSE 1 | 13.0188 | -72.8206 | 12.579325 | -73.092182 | 312.037754 | -64.558836 | 302.86615918 | -44.30756989 | 221.6864 | 53687.4452893518 | 2005-11-13 10:41:13 | 53688.2231944445 | 2005-11-14 05:21:24 | 500011010 | 46.7789 | 50 | 46.7789 | 46.7869 | 46.7869 | 46.7869 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 47.8684 | 47.8684 | 67.1999 | 0 | PROCESSED | 57527.967337963 | 2016-05-19 23:12:58 | 54247 | 2007-05-27 00:00:00 | 54038.3531712963 | 2006-10-30 08:28:34 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001049 | We propose to use Suzaku XIS to observe regions of diffuse emission in the Magellanic Clouds. The diffuse component was identified by ROSAT PSPC observations, but has never been studied with a true spectroscopic instrument. Suzaku is well-matched to the angular size and expected temperature of the regions of diffuse emission in the LMC. Not only will such observations give a clear view of the temperature structure of this gas, they will provide a direct measurement of ambient abundances in the Clouds. | GALACTIC DIFFUSE EMISSION | 5 | A | UNA HWANG | JAP | 0 | SWG | DIFFUSE EMISSION IN THE MAGELLANIC CLOUDS | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500011010/ | Quick Look | ![]() |
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369 | 73P/SW3 | 18.4857 | -9.3839 | 17.859598 | -9.648443 | 13.351737 | -15.906108 | 140.65827116 | -71.47693301 | 59.4008 | 53893.6903703704 | 2006-06-07 16:34:08 | 53893.7356365741 | 2006-06-07 17:39:19 | 500014010 | 3.228 | 35 | 3.228 | 3.228 | 3.228 | 3.228 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3.312 | 3.312 | 3.9039 | 0 | PROCESSED | 57534.5195486111 | 2016-05-26 12:28:09 | 54267 | 2007-06-16 00:00:00 | 54052.5070949074 | 2006-11-13 12:10:13 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014010/ | Quick Look | ![]() |
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370 | 73P/SW3 | 18.2949 | -9.3163 | 17.668546 | -9.581131 | 13.199293 | -15.770045 | 140.03044964 | -71.46265703 | 59.3979 | 53894.3358101852 | 2006-06-08 08:03:34 | 53894.4022800926 | 2006-06-08 09:39:17 | 500014110 | 1.4249 | 35 | 1.4249 | 1.4249 | 1.4249 | 1.4249 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1.433 | 1.433 | 5.742 | 0 | PROCESSED | 57534.5994444445 | 2016-05-26 14:23:12 | 54267 | 2007-06-16 00:00:00 | 54052.5225694444 | 2006-11-13 12:32:30 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014110/ | Quick Look | ![]() |
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371 | 73P/SW3 | 18.4874 | -9.3902 | 17.861309 | -9.65474 | 13.350771 | -15.912562 | 140.66879726 | -71.4825298 | 59.4036 | 53894.6018055556 | 2006-06-08 14:26:36 | 53894.680775463 | 2006-06-08 16:20:19 | 500014150 | 3.232 | 35 | 3.232 | 3.232 | 3.232 | 3.232 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3.293 | 3.293 | 6.8159 | 0 | PROCESSED | 57534.6057638889 | 2016-05-26 14:32:18 | 54267 | 2007-06-16 00:00:00 | 54052.5265509259 | 2006-11-13 12:38:14 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014150/ | Quick Look | ![]() |
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372 | CYGNUS LOOP NE3 | 313.7583 | 32.1826 | 313.244151 | 31.990973 | 329.188805 | 47.043725 | 75.71932756 | -8.27611719 | 222.9011 | 53703.7415162037 | 2005-11-29 17:47:47 | 53704.2355208333 | 2005-11-30 05:39:09 | 500022010 | 21.1338 | 20 | 21.1916 | 21.7199 | 21.1338 | 21.3599 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20.2445 | 20.2445 | 42.6799 | 1 | PROCESSED | 57528.1127893518 | 2016-05-20 02:42:25 | 54247 | 2007-05-27 00:00:00 | 54038.7522106482 | 2006-10-30 18:03:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001093 | We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 0 | SWG | CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500022010/ | Quick Look | ![]() |
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373 | PSR B1259-63 | 195.6913 | -63.8356 | 194.901997 | -63.566976 | 227.68559 | -50.893989 | 304.18038114 | -0.9913128 | 117.5773 | 55594.1927662037 | 2011-02-02 04:37:35 | 55594.4487731482 | 2011-02-02 10:46:14 | 405038010 | 21.4781 | 20 | 21.4941 | 21.4781 | 0 | 21.4941 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15.6774 | 15.6774 | 22.1119 | 0 | PROCESSED | 57600.7966435185 | 2016-07-31 19:07:10 | 55974 | 2012-02-17 00:00:00 | 55607.1295601852 | 2011-02-15 03:06:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051221 | We propose to observe a gamma-ray binary PSR B1259-63 during the pulsar's second disk crossing after periastron passage. PSR B1259-63 is a young radio pulsar orbiting around a B2e star with a highly eccentric 3.4 yr orbit. Suzaku XIS+HXD measurements of the hard continuum emission from the binary system allow us to investigate particle acceleration in a highly variable environment as a result of interactions between the relativistic wind of the pulsar and the circumstellar disk of the Be star. With the advent of the Fermi Gamma-ray Space Telescope, we will be able to simultaneously observe X-rays and GeV gamma-rays during the disk transit for the first time. The observations of PSR B1259-63 will give us a unique opportunity to study the physics of pulsar winds on AU-scale. | GALACTIC POINT SOURCES | 4 | A | YASUNOBU UCHIYAMA | USA | 5 | AO5 | SUZAKU BROADBAND OBSERVATIONS OF A GAMMA-RAY BINARY PSRB1259-63 DURING THE POST-PERIASTRON FLARE IN 2011 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405038010/ | Quick Look | ![]() |
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374 | 3C 111 | 64.5741 | 38.0889 | 63.737568 | 37.967565 | 69.370671 | 16.452489 | 161.62276278 | -8.7838332 | 81.5451 | 54700.4141898148 | 2008-08-22 09:56:26 | 54703.1836111111 | 2008-08-25 04:24:24 | 703034010 | 122.378 | 120 | 122.386 | 122.378 | 0 | 122.378 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 109.7067 | 109.7067 | 239.2517 | 1 | PROCESSED | 57543.4018287037 | 2016-06-04 09:38:38 | 55084 | 2009-09-10 00:00:00 | 54713.6361226852 | 2008-09-04 15:16:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031332 | The origin of the high-energy emission from Broad-Line Radio Galaxies is still an open issue. A plausible scenario is reprocessed emission from a cold medium (disk) diluted by variable, non-thermal jet flux. To test this scenario we propose Suzaku observations of the BLRG 3C 111, which exhibits flux variability above 10 keV from available data, suggesting a jet contribution. Moreover, 3C 111 was previously detected with EGRET at GeV energies, and synergy with GLAST will thus be exploited in the proposed program. The coupled timing and spectral information provided by Suzaku are key to disentangle the disk and jet contributions, and determine their respective role for the source energy budget. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RITA SAMBRUNA | USA | 3 | AO3 | SUZAKU OBSERVATIONS OF 3C 111: UNCOVERING THE JET WITHIN | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703034010/ | Quick Look | ![]() |
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375 | SKY_53.3_-63.4 | 53.24 | -63.4549 | 53.047022 | -63.62196 | 354.144887 | -74.40934 | 278.62179386 | -45.30780651 | 286.1724 | 53797.8694444444 | 2006-03-03 20:52:00 | 53800.3342476852 | 2006-03-06 08:01:19 | 501002010 | 101.4752 | 100 | 101.4752 | 101.4752 | 101.4752 | 101.4752 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 145.4318 | 145.4318 | 212.8539 | 4 | PROCESSED | 57533.1863425926 | 2016-05-25 04:28:20 | 54401 | 2007-10-28 00:00:00 | 53906.7729282407 | 2006-06-20 18:33:01 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011252 | We propose Suzaku XIS observations of the hot gas in the Galactic halo and Local Bubble. The spectra's bright emission lines and complexes will reveal the plasma's ionization history and thus its origins. The Local Bubble's spectrum will be garnered from an observation of a nearby opaque cloud. The halo's spectrum will be found by subtracting the Local Bubble spectrum from that of an adjacent off-cloud observation. In order to better constrain the models, we will also draw upon existing FUSE O VI emission data for these directions. With the combined O VI and soft X-ray data, we will be able to constrain the plasma's conditions and ionization history and, thus, constrain detailed models of the hot gas in the halo and Local Bubble. | GALACTIC DIFFUSE EMISSION | 5 | A | ROBIN SHELTON | USA | 1 | AO1 | SUZAKU XIS OBSERVATIONS OF THE GALACTIC HALO AND LOCAL BUBBLE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501002010/ | Quick Look | ![]() |
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376 | 4U 1630-47 | 248.5034 | -47.402 | 247.582302 | -47.297867 | 254.088861 | -25.13983 | 336.90313759 | 0.24577164 | 279.8256 | 55432.911724537 | 2010-08-24 21:52:53 | 55435.6134259259 | 2010-08-27 14:43:20 | 405051010 | 99.9373 | 100 | 99.9373 | 99.9373 | 0 | 99.9373 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 90.4512 | 90.4512 | 233.3976 | 2 | PROCESSED | 57553.2849652778 | 2016-06-14 06:50:21 | 55815 | 2011-09-11 00:00:00 | 55449.4369560185 | 2010-09-10 10:29:13 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051252 | Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions. | GALACTIC POINT SOURCES | 4 | A | JOHN TOMSICK | USA | 5 | AO5-TOO | CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405051010/ | Quick Look | ![]() |
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377 | ABELL 2667 | 357.9715 | -25.9262 | 357.325218 | -26.204419 | 347.258509 | -22.861194 | 34.71945037 | -76.63317585 | 64.8859 | 55721.5923611111 | 2011-06-09 14:13:00 | 55722.9050925926 | 2011-06-10 21:43:20 | 806029010 | 51.2214 | 50 | 51.2294 | 51.2294 | 0 | 51.2214 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.4843 | 40.4843 | 113.4098 | 1 | PROCESSED | 57602.2712962963 | 2016-08-02 06:30:40 | 55652 | 2011-04-01 00:00:00 | 55757.6995486111 | 2011-07-15 16:47:21 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061116 | We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 6 | AO6-LP | THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806029010/ | Quick Look | ![]() |
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378 | V1082 SGR | 286.8363 | -20.7721 | 286.094048 | -20.85102 | 285.710494 | 1.754645 | 15.88147607 | -12.67535412 | 81.3818 | 56009.1848148148 | 2012-03-23 04:26:08 | 56010.4459375 | 2012-03-24 10:42:09 | 406042010 | 39.4605 | 40 | 39.4605 | 39.4605 | 0 | 39.4605 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36.0171 | 36.0171 | 108.924 | 2 | PROCESSED | 57605.0088541667 | 2016-08-05 00:12:45 | 56399 | 2013-04-17 00:00:00 | 56023.1564236111 | 2012-04-06 03:45:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061217 | V1082 Sgr is a BAT-detected cataclysmic variable with a 20 hr orbital period that exhibits high and low states. The high X-ray luminosity and the presence of the HeII 4686 lines in its optical spectrum have led to the suggestion that this is an intermediate polar (IP). We propose an exploratory 40 ks Suzaku observation with the aim of establishing if it is indeed an IP. If it is, then this system may provide a unique opportunity to study an IP in a low state, which has not been possible with other IPs. | GALACTIC POINT SOURCES | 4 | C | KOJI MUKAI | USA | 6 | AO6 | AN UNUSUAL BAT-DETECTED CATACLYSMIC VARIABLE, V1082 SGR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406042010/ | Quick Look | ![]() |
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379 | G156.2+5.7E | 75.8128 | 51.6405 | 74.832405 | 51.569986 | 80.017374 | 28.69124 | 156.70319129 | 6.10796494 | 274.6638 | 54149.9177893518 | 2007-02-18 22:01:37 | 54151.1750231482 | 2007-02-20 04:12:02 | 501074010 | 53.3331 | 50 | 53.3494 | 53.3491 | 0 | 53.3331 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50.8218 | 50.8218 | 108.6199 | 2 | PROCESSED | 57537.4302893518 | 2016-05-29 10:19:37 | 54773 | 2008-11-03 00:00:00 | 54158.2839583333 | 2007-02-27 06:48:54 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011235 | G156.2+5.7 (RX J04591+5147) is thought to be a 26,000 yr old Type Ia remnant expanding in a low density medium. Ginga and ASCA observations reveal a hard emission component, interpreted as arising from shock-accelerated electrons, making this the oldest SNR in which shock acceleration has been found. Recent reanalysis of the ASCA data leaves ambiguity about the existence of this component. The importance of understanding the evolution of shock acceleration in SNRs makes vital confirming the existence of the hard component and localizing it. We propose 50 ks XIS observations of 3 locations to localize the hard component. Given its angular size, lack of small high contrast features, 0.4 keV thermal component with strong lines, and hard component, G156.2+5.7 is an ideal Suzaku target. | GALACTIC DIFFUSE EMISSION | 5 | C | ROBERT PETRE | USA | 1 | AO1 | A SEARCH FOR HARD X-RAY EMISSION FROM THE EVOLVED SNR G156.2+5.7 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501074010/ | Quick Look | ![]() |
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380 | SNR G93.3+6.9 S3 | 313.171 | 55.2801 | 312.823004 | 55.090273 | 352.082126 | 66.837166 | 93.24775568 | 6.83197363 | 40.0152 | 53906.4300462963 | 2006-06-20 10:19:16 | 53906.7266087963 | 2006-06-20 17:26:19 | 501082010 | 16.3347 | 15 | 16.3347 | 16.3587 | 16.3507 | 16.3427 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 13.9186 | 13.9186 | 25.6159 | 0 | PROCESSED | 57534.7339814815 | 2016-05-26 17:36:56 | 54401 | 2007-10-28 00:00:00 | 53926.2481365741 | 2006-07-10 05:57:19 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011242 | The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. | GALACTIC DIFFUSE EMISSION | 5 | B | Q. DANIEL WANG | USA | 1 | AO1 | G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501082010/ | Quick Look | ![]() |
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381 | PUP A : NE | 125.7583 | -42.7117 | 125.326284 | -42.549841 | 147.156331 | -59.259606 | 260.25284038 | -3.14403225 | 277.1213 | 53842.913287037 | 2006-04-17 21:55:08 | 53843.3091319445 | 2006-04-18 07:25:09 | 501087010 | 20.7109 | 20 | 20.7336 | 20.7349 | 20.7189 | 20.7109 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 19.7443 | 19.7443 | 34.1899 | 1 | PROCESSED | 57533.5127083333 | 2016-05-25 12:18:18 | 54401 | 2007-10-28 00:00:00 | 53906.9450231482 | 2006-06-20 22:40:50 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011246 | We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present. | GALACTIC DIFFUSE EMISSION | 5 | A | UNA HWANG | USA | 1 | AO1 | MAPPING OXYGEN IN PUPPIS A | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501087010/ | Quick Look | ![]() |
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382 | TYCHO SNR | 6.3139 | 64.1469 | 5.613879 | 63.870082 | 42.846574 | 53.765969 | 120.08177164 | 1.42013769 | 53.7834 | 54682.0646759259 | 2008-08-04 01:33:08 | 54686.9529398148 | 2008-08-08 22:52:14 | 503085010 | 312.892 | 400 | 312.916 | 312.892 | 0 | 312.908 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 289.9494 | 289.9494 | 307.8699 | 3 | PROCESSED | 57543.3766782407 | 2016-06-04 09:02:25 | 54557 | 2008-04-01 00:00:00 | 54707.038287037 | 2008-08-29 00:55:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031003 | Recent Suzaku studies of the Type Ia supernova remnant, Tycho, have revealed tantalizing evidence for secondary Fe-peak elements (specifically Cr and Mn) in the integrated X-ray spectrum. Here we propose to confirm and extend these detections by measuring the spatial variation of Cr/Fe line fluxes across the remnant, paying particular attention to the composition of a previously known Fe-rich region along the eastern limb. The unique capabilities of the XIS onboard Suzaku (high spectral resolution and large effective area) are crucial to the proposed study and no other operating instrument can detect the weak lines from these trace species within reasonable exposure times. | GALACTIC DIFFUSE EMISSION | 5 | A | JOHN HUGHES | USA | 3 | AO3 | SECONDARY FE-PEAK ELEMENTS AS A PROBE OF SN IA EXPLOSION PHYSICS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503085010/ | Quick Look | ![]() |
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383 | N11 SB | 74.1823 | -66.412 | 74.156384 | -66.487992 | 354.048784 | -83.709745 | 277.1886014 | -36.07081942 | 146.432 | 54046.4407291667 | 2006-11-07 10:34:39 | 54047.232037037 | 2006-11-08 05:34:08 | 501091010 | 30.452 | 30 | 30.452 | 30.452 | 30.452 | 30.452 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 26.405 | 26.405 | 68.3659 | 0 | PROCESSED | 57536.0384953704 | 2016-05-28 00:55:26 | 54455 | 2007-12-21 00:00:00 | 54088.5643287037 | 2006-12-19 13:32:38 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011251 | Clusters of massive stars, through their stellar winds and supernovae, form large diffuse structures known as superbubbles (SBs), which play an essential role in shaping the local interstellar medium. Most SB models indicate that these objects should be dominated by thermal plasma processes. However, observations of 2 SBs have detected significant nonthermal contributions to their X-ray emission, which raises many questions. Is it generated by synchrotron, inverse-Compton, or nonthermal Bremsstrahlung processes? Are colliding stellar winds or internal supernova remnants responsible? We therefore propose to examine the X-ray emission from 4 X-ray bright SBs, to search for nonthermal X-ray emission, and if possible place strong constraints on the source of this emission. | GALACTIC DIFFUSE EMISSION | 5 | C | ROSA WILLIAMS | USA | 1 | AO1 | A SEARCH FOR NONTHERMAL X-RAY EMISSION FROM SUPERBUBBLES | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501091010/ | Quick Look | ![]() |
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384 | GAMMA CASSIOPEIAE | 14.1598 | 60.7356 | 13.401441 | 60.465287 | 43.939726 | 48.837698 | 123.56796459 | -2.12972511 | 72.5084 | 55755.0038888889 | 2011-07-13 00:05:36 | 55756.333587963 | 2011-07-14 08:00:22 | 406040010 | 55.394 | 50 | 55.394 | 55.394 | 0 | 55.394 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 56.2164 | 56.2164 | 114.8778 | 0 | PROCESSED | 57602.6019791667 | 2016-08-02 14:26:51 | 56183 | 2012-09-13 00:00:00 | 55816.6655208333 | 2011-09-12 15:58:21 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061207 | We propose a 50 ks Suzaku observation to obtain for the first time the hard X-ray spectrum of the classical Be star Gamma Cas. This star is a prototype of the "Gamma Cas stars" class, whose nature is not yet understood. Earlier XMM-Newton and Swift BAT observations gave a hint of the presence of the hard X-ray emission above 10 keV. The broadband Suzaku spectrum will allow to establish its X-ray emission mechanism - non-thermal emission or reflection of thermal emission from a neutral surface. On this basis, we will be able to discriminate the mechanisms between the magnetic disk dynamo and the accretion on a compact star. These new data will be pivotal in solving the enigma of Gamma Cas and revealing the true nature of this astrophysically important object. | GALACTIC POINT SOURCES | 4 | C | KENJI HAMAGUCHI | USA | 6 | AO6 | SUZAKU'S HARD LOOK AT GAMMA CASSIOPEIAE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406040010/ | Quick Look | ![]() |
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385 | SDSS J1723+5553 | 260.8912 | 55.8942 | 260.65651 | 55.938805 | 243.54174 | 78.493359 | 83.89291292 | 34.34970174 | 8.0654 | 54986.3677777778 | 2009-06-04 08:49:36 | 54986.8148032407 | 2009-06-04 19:33:19 | 704051010 | 35.9368 | 30 | 35.9448 | 35.9368 | 0 | 35.9528 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 29.0393 | 29.0393 | 38.6159 | 0 | PROCESSED | 57547.4618865741 | 2016-06-08 11:05:07 | 55364 | 2010-06-17 00:00:00 | 54998.1759722222 | 2009-06-16 04:13:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041422 | BALQSOs can be used to probe geometric and evolutionary models of quasars and AGN feedback. Recent studies have found larger (~2X) BALQSO fractions in NIR selected samples compared to those in optical samples and have suggested that the NIR samples of BALQSOs better represent the general population of BALQSOs. We propose to observe three bright, red 2MASS selected BALQSOs with Suzaku, to complement archival X-ray observations of BALQSOs that may have been biased by their selection on optical properties only. Combined with the archival sample, we will measure the average X-ray properties of BALQSOs. By comparing the hard X-ray to K_s band flux ratios at a range of optical to infrared colors, we will test the robustness of NIR selection and the origin of the large NIR BALQSO fraction. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | XINYU DAI | USA | 4 | AO4 | X-RAY PROPERTIES OF 2MASS SELECTED BALQSOS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704051010/ | Quick Look | ![]() |
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386 | E0102-72 | 16.0206 | -72.0231 | 15.615717 | -72.291056 | 314.640431 | -65.037838 | 301.55102123 | -45.07123322 | 281.396 | 53752.9742708333 | 2006-01-17 23:22:57 | 53755.3752199074 | 2006-01-20 09:00:19 | 100044020 | 41.2605 | 20 | 41.268 | 41.8524 | 41.2605 | 41.361 | 3 | 4 | 3 | 4 | 1 | 0 | 0 | 99.7935 | 99.7935 | 207.4298 | 3 | PROCESSED | 57532.7555555556 | 2016-05-24 18:08:00 | 54247 | 2007-05-27 00:00:00 | 54040.6979513889 | 2006-11-01 16:45:03 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001097 | We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip | CALIBRATION | 1 | A | HIRONORI MATSUMOTO | JAP | 0 | SWG | XIS FLIGHT CAIBRATION PLAN | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100044020/ | Quick Look | ![]() |
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387 | B1920+10(2) | 292.8971 | 10.8605 | 292.305399 | 10.753499 | 296.831046 | 32.19317 | 47.18977478 | -3.80874006 | 248.6642 | 54783.7420833333 | 2008-11-13 17:48:36 | 54785.8981365741 | 2008-11-15 21:33:19 | 503091010 | 100.4577 | 100 | 100.4577 | 100.4577 | 0 | 100.4577 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93.8731 | 93.8731 | 186.248 | 0 | PROCESSED | 57544.4390972222 | 2016-06-05 10:32:18 | 55167 | 2009-12-02 00:00:00 | 54797.1537731482 | 2008-11-27 03:41:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031204 | A bow-shock pulsar wind nebula with an exceptionally long tail has been detected in X-ray observations of the pulsar PSR B1929+10. Recent observations suggest that such long structures may be associated with many other pulsars. Being the longest extended structures observed around Galactic compact objects. The physical processes responsible for the formation of such tails are not well understood, and the existing numerical models may only be valid at small distances from the pulsar. To determine the major factors governing the post-shock wind, we propose to observe the tail of PSR B1929+10, measure its full extent, map the surface brightness distribution, and perform spatially resolved spectroscopy. We will also measure the pulsar spectrum to study the properties of its polar caps. | GALACTIC DIFFUSE EMISSION | 5 | C | ZDENKA MISANOVIC | USA | 3 | AO3 | STUDYING THE LONG PULSAR TAIL OF THE PSR B1929+10 WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503091010/ | Quick Look | ![]() |
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388 | GCL4 | 265.3437 | -29.192 | 264.548064 | -29.167468 | 265.905576 | -5.816983 | 359.29532739 | 0.65531706 | 106.9407 | 54907.3257986111 | 2009-03-17 07:49:09 | 54908.0711111111 | 2009-03-18 01:42:24 | 503102010 | 33.6554 | 25 | 33.6794 | 33.6558 | 0 | 33.6554 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.0521 | 30.0521 | 64.3899 | 0 | PROCESSED | 57545.8492939815 | 2016-06-06 20:22:59 | 55329 | 2010-05-13 00:00:00 | 54920.054837963 | 2009-03-30 01:18:58 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031234 | We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity. | GALACTIC DIFFUSE EMISSION | 5 | B | FARHAD YUSEF-ZADEH | USA | 3 | AO3 | A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503102010/ | Quick Look | ![]() |
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389 | COMET_8P_TUTTLE-P1-6 | 28.2017 | 6.7525 | 27.54593 | 6.506397 | 28.607042 | -4.520684 | 148.82276905 | -53.00641332 | 248.5018 | 54470.8491666667 | 2008-01-05 20:22:48 | 54470.9154050926 | 2008-01-05 21:58:11 | 502062060 | 2.0266 | 2 | 2.0266 | 2.0266 | 0 | 2.0266 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2.044 | 2.044 | 5.664 | 0 | PROCESSED | 57541.0007986111 | 2016-06-02 00:01:09 | 54908 | 2009-03-18 00:00:00 | 54542.2318634259 | 2008-03-17 05:33:53 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062060/ | Quick Look | ![]() |
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390 | COMET_8P_TUTTLE-P2_02 | 39.704 | -35.8295 | 39.191609 | -36.044542 | 21.228259 | -48.000366 | 240.49763907 | -65.60654763 | 257.6692 | 54490.1630902778 | 2008-01-25 03:54:51 | 54490.2960069444 | 2008-01-25 07:06:15 | 502063020 | 5.2049 | 5 | 5.2049 | 5.2049 | 0 | 5.2049 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 5.5919 | 5.5919 | 11.4499 | 0 | PROCESSED | 57541.3791898148 | 2016-06-02 09:06:02 | 54912 | 2009-03-22 00:00:00 | 54546.1091666667 | 2008-03-21 02:37:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063020/ | Quick Look | ![]() |
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391 | COMET_8P_TUTTLE-P2_07 | 40.0041 | -36.5319 | 39.495887 | -36.746007 | 21.066088 | -48.735556 | 241.99586619 | -65.20252382 | 258.1285 | 54490.8297106482 | 2008-01-25 19:54:47 | 54490.962662037 | 2008-01-25 23:06:14 | 502063070 | 5.2676 | 5 | 5.2916 | 5.2676 | 0 | 5.2994 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2.753 | 2.753 | 11.4799 | 0 | PROCESSED | 57541.3952777778 | 2016-06-02 09:29:12 | 54912 | 2009-03-22 00:00:00 | 54546.130462963 | 2008-03-21 03:07:52 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063070/ | Quick Look | ![]() |
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392 | COMET_8P_TUTTLE-P2_BGD-2 | 40.4817 | -37.5941 | 39.980067 | -37.806706 | 20.824934 | -49.853115 | 244.17118034 | -64.55380496 | 254.4101 | 54492.5631365741 | 2008-01-27 13:30:55 | 54492.7293287037 | 2008-01-27 17:30:14 | 502064020 | 6.9797 | 5 | 6.9797 | 7.0037 | 0 | 6.9877 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 5.5471 | 5.5471 | 14.3519 | 0 | PROCESSED | 57554.5355671296 | 2016-06-15 12:51:13 | 54912 | 2009-03-22 00:00:00 | 54546.2537847222 | 2008-03-21 06:05:27 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502064020/ | Quick Look | ![]() |
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393 | G21.5-0.9 | 278.4035 | -10.5067 | 277.711514 | -10.545731 | 278.460081 | 12.687392 | 21.56184596 | -0.8687642 | 103.5554 | 54188.7945023148 | 2007-03-29 19:04:05 | 54189.6252199074 | 2007-03-30 15:00:19 | 502065010 | 25.1416 | 100 | 25.156 | 25.1416 | 0 | 25.156 | 1 | 2 | 0 | 1 | 1 | 0 | 0 | 22.889 | 22.889 | 71.7699 | 1 | PROCESSED | 57538.0286921296 | 2016-05-30 00:41:19 | 54695 | 2008-08-17 00:00:00 | 54209.5181018518 | 2007-04-19 12:26:04 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021211 | We propose an observation of the supernova remnant (SNR) G21.5--0.9. This SNR has a centrally peaked X-ray morphology which coupled with its non-thermal emission, suggested that the SNR's central engine was an undetected pulsar. Last year, a radio pulsar associated with the remnant was discovered (Gupta et al. 2005; Camilo et al. 2006). These announcements concur on the period of the pulsar and its period derivative making it the second highest spin-down luminosity pulsar. Deep Chandra imaging uncovered the missing shell (Matheson & Safi-Harb, 2005). Recent INTEGRAL and SWIFT/BAT slew observations detected G21.5--0.9 at more than 10 and 8 sigma respectively. The proposed observation will be the first self-consistent broad-band timing and spectral analysis from soft to very hard X-ray. | GALACTIC DIFFUSE EMISSION | 5 | B | ILANA HARRUS | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF THE SUPERNOVA REMNANT G21.5-0.9 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502065010/ | Quick Look | ![]() |
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394 | G296.1-0.5N | 177.8287 | -62.3875 | 177.210977 | -62.109277 | 215.982021 | -55.076396 | 296.02814016 | -0.3243747 | 322.3815 | 54321.2538541667 | 2007-08-09 06:05:33 | 54323.4522453704 | 2007-08-11 10:51:14 | 502068010 | 77.1759 | 67 | 77.1759 | 77.1759 | 0 | 77.1759 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 68.4846 | 68.4846 | 189.9237 | 1 | PROCESSED | 57539.4859953704 | 2016-05-31 11:39:50 | 54716 | 2008-09-07 00:00:00 | 54347.5137268518 | 2007-09-04 12:19:46 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021218 | Supernova (SN) explosions within wind-blown bubbles are common among core-collapse (CC) SNe, and are expected to occur for some Type Ia SNe. We propose observations of an X-ray bright supernova remnant (SNR), G296.1-0.5, with very strong evidence for an explosion within a bubble. Spectroscopy with Suzaku will provide us with temperatures, abundances, and ionization ages of the X-ray emitting gas. If we detect SN ejecta, we will distinguish between a CC or a Type Ia progenitor. Gas temperatures will provide us with the shock speeds, while ionization ages will tell us when this gas was shocked. We will infer how progenitor winds affected the ambient medium prior to the explosion. The proposed observations will advance our knowledge of poorly understood SNR evolution in wind-blown bubbles. | GALACTIC DIFFUSE EMISSION | 5 | B | KAZIMIERZ BORKOWSKI | USA | 2 | AO2 | G296.1-0.5: A SUPERNOVA EXPLOSION WITHIN A BUBBLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502068010/ | Quick Look | ![]() |
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395 | GC CENTER #2 | 266.7693 | -28.6295 | 265.976908 | -28.611884 | 267.143281 | -5.22043 | 0.42794484 | -0.11339991 | 74.7707 | 53821.958587963 | 2006-03-27 23:00:22 | 53823.7585069444 | 2006-03-29 18:12:15 | 500005010 | 88.4247 | 100 | 88.4327 | 88.4247 | 88.4327 | 88.4327 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 64.5911 | 64.5911 | 155.5019 | 2 | PROCESSED | 57533.3630324074 | 2016-05-25 08:42:46 | 54247 | 2007-05-27 00:00:00 | 54133.0079861111 | 2007-02-02 00:11:30 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001020 | We propose to obtain high quality spectrum near the GC. The objective is to resolve 6.4, 6.7, and 6.9 keV line and determine the high energy tail and sub-structures, which may be X-ray reflection from Sgr A* (6.4 keV line + 7.1 keV edge + high energy tail), thermal plasma (6.7 + 6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 0 | SWG | SUZAKU GALACTIC CENTER OBSERVATION PROJECT: #2 SGR B1 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500005010/ | Quick Look | ![]() |
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396 | 4U1626-67 | 248.0601 | -67.4675 | 246.801189 | -67.3606 | 258.324109 | -44.911512 | 321.78071552 | -13.09322804 | 103.0359 | 53803.0543518518 | 2006-03-09 01:18:16 | 53805.818275463 | 2006-03-11 19:38:19 | 400015010 | 102.6392 | 100 | 102.654 | 102.6392 | 102.6472 | 102.654 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 93.3932 | 93.3932 | 238.7819 | 3 | PROCESSED | 57533.2349652778 | 2016-05-25 05:38:21 | 54247 | 2007-05-27 00:00:00 | 54042.4663657407 | 2006-11-03 11:11:34 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001081 | The X-ray spectrum of the 7 second LMXRB pulsar 4U1626-67 is dominated by low energy line emission with little evedence of iron K line in the pulse phase resolved spectra. It showd also cyclotron line at 37 keV that departs from the correlation of energy cutoff cyclotron energy observed in many other X-ray pulsars. This Suzaku observation allow to characterize the overall continuum, the low energy, the iron K alpha and cyclotron lines as function of the pulse phase, | GALACTIC POINT SOURCES | 4 | A | LORELLA ANGELINI | JAP | 0 | SWG | 4U1626-67: PHASE RESOLVED SPECTRA AND CYCLOTRON LINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400015010/ | Quick Look | ![]() |
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397 | 1FGL J1018.6-5856 | 154.7369 | -58.9465 | 154.294298 | -58.695121 | 196.565847 | -60.86994 | 284.35429996 | -1.68890631 | 297.8367 | 56093.0246875 | 2012-06-15 00:35:33 | 56093.5348032407 | 2012-06-15 12:50:07 | 407071010 | 20.8203 | 20 | 20.8203 | 20.8203 | 0 | 20.8203 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.813 | 16.813 | 44.0639 | 0 | PROCESSED | 57605.6779282407 | 2016-08-05 16:16:13 | 56542 | 2013-09-07 00:00:00 | 56176.237025463 | 2012-09-06 05:41:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071234 | We propose Suzaku observations of a newly discovered gamma-ray binary 1FGL J1018.6-5856. Recent observations by the Fermi Gamma-ray Space Telescope and follow-up observations in other wavelengths revealed that the gamma-ray source is a new member of the rare gamma-ray binary class with an orbital period of 16 days. We propose two types of observations with Suzaku. One is a continuous observation of a sharp X-ray peak found in the lightcurve by the Swift XRT. Another is a series of snap shot observations in orbital phase between the peaks. We aim to perform phase-resolved spectral analysis which is not possible with the Swift XRT data. We also compare the Swift XRT lightcurve with new lightcurves taken by Suzaku in order to test the repeatability of the X-ray orbital modulation. | GALACTIC POINT SOURCES | 4 | B | TAKAAKI TANAKA | USA | 7 | AO7 | SUZAKU OBSERVATIONS OF A NEWLY DISCOVERED GAMMA-RAY BINARY: 1FGL J1018.6-5856 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407071010/ | Quick Look | ![]() |
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398 | SNR 0049-73.6 | 12.7817 | -73.3677 | 12.345533 | -73.639533 | 310.812589 | -64.728588 | 302.96274339 | -43.76053264 | 62.7682 | 54629.4818518518 | 2008-06-12 11:33:52 | 54632.7605787037 | 2008-06-15 18:15:14 | 503094010 | 120.478 | 120 | 120.486 | 120.478 | 0 | 120.486 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 107.7079 | 107.7079 | 283.2419 | 3 | PROCESSED | 57542.894525463 | 2016-06-03 21:28:07 | 55008 | 2009-06-26 00:00:00 | 54642.6050694444 | 2008-06-25 14:31:18 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031211 | We propose to observe the O-rich supernova remnant (SNR) 0049-73.6 in the Small Magellanic Cloud (SMC). SNR 0049-73.6 shares some similarities and differences with another O-rich SNR 0103-72.6 in the SMC. High resolution X-ray spectroscopy of these SNRs with Suzaku/XIS observations should provide a useful insight for the details of thermal evolution of a core-collapse SNR. We began this program with an AO1 Suzaku/XIS observation of SNR 0103-72.6. We here propose to continue this program with our AO3 Suzaku observation of 0049-73.6. We request for a 120 ks Suzaku/XIS observation of 0049-73.6. | GALACTIC DIFFUSE EMISSION | 5 | B | SANGWOOK PARK | USA | 3 | AO3 | OXYGEN-RICH SUPERNOVA REMNANT 0049-73.6 IN THE SMC | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503094010/ | Quick Look | ![]() |
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399 | CD -28 3719 | 105.2866 | -29.1168 | 104.795571 | -29.044554 | 111.677742 | -51.412828 | 240.20191687 | -10.89157366 | 97.0723 | 56577.3593634259 | 2013-10-12 08:37:29 | 56579.416099537 | 2013-10-14 09:59:11 | 408032010 | 14.3679 | 90 | 14.3679 | 90.0777 | 0 | 90.0777 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 78.3569 | 78.3569 | 177.6659 | 1 | PROCESSED | 57645.4999652778 | 2016-09-14 11:59:57 | 57009 | 2014-12-18 00:00:00 | 56642.7667476852 | 2013-12-16 18:24:07 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081214 | Since they were discovered, it has been almost impossible to directly observe the accretion region in most symbiotic stars, in which a white dwarf (WD) accretes from the wind of a red giant. With the discovery that hard X-ray emission (E > 2 keV) is a common feature of WD symbiotics, that situation has finally changed. We propose to use Suzaku observations of 3 typical symbiotics with hard X-ray emission to test the hypothesis that such emission emanates from an accretion-disk boundary layer. With the proposed observations, we will determine whether the WD's magnetic field is high enough to disrupt the accretion flow, and estimate the WD mass and accretion rate. This work has implications for the study of accretion in wide binaries and symbiotics stars as progenitors of SNIa. | GALACTIC POINT SOURCES | 4 | B | JENNIFER SOKOLOSKI | USA | 8 | AO8 | X-RAYS FROM THE ACCRETION FLOWS IN SYMBIOTIC STARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408032010/ | Quick Look | ![]() |
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400 | TYCHO SNR | 6.3115 | 64.1447 | 5.611508 | 63.867881 | 42.842768 | 53.765034 | 120.08050675 | 1.41805528 | 43.1557 | 54689.3425578704 | 2008-08-11 08:13:17 | 54690.918275463 | 2008-08-12 22:02:19 | 503085020 | 102.8556 | 100 | 102.8556 | 102.8556 | 0 | 102.8556 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91.9078 | 91.9078 | 136.1039 | 1 | PROCESSED | 57543.2895717593 | 2016-06-04 06:56:59 | 54557 | 2008-04-01 00:00:00 | 54706.7896412037 | 2008-08-28 18:57:05 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031003 | Recent Suzaku studies of the Type Ia supernova remnant, Tycho, have revealed tantalizing evidence for secondary Fe-peak elements (specifically Cr and Mn) in the integrated X-ray spectrum. Here we propose to confirm and extend these detections by measuring the spatial variation of Cr/Fe line fluxes across the remnant, paying particular attention to the composition of a previously known Fe-rich region along the eastern limb. The unique capabilities of the XIS onboard Suzaku (high spectral resolution and large effective area) are crucial to the proposed study and no other operating instrument can detect the weak lines from these trace species within reasonable exposure times. | GALACTIC DIFFUSE EMISSION | 5 | A | JOHN HUGHES | USA | 3 | AO3 | SECONDARY FE-PEAK ELEMENTS AS A PROBE OF SN IA EXPLOSION PHYSICS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503085020/ | Quick Look | ![]() |
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401 | GCL1 | 265.1726 | -28.5274 | 264.381201 | -28.50205 | 265.733071 | -5.157711 | 359.7799359 | 1.13423351 | 69.7267 | 54900.8188425926 | 2009-03-10 19:39:08 | 54901.4557175926 | 2009-03-11 10:56:14 | 503099010 | 29.706 | 25 | 29.7241 | 29.722 | 0 | 29.706 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.5649 | 30.5649 | 55.02 | 1 | PROCESSED | 57545.7841782407 | 2016-06-06 18:49:13 | 55329 | 2010-05-13 00:00:00 | 54916.3706828704 | 2009-03-26 08:53:47 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031234 | We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity. | GALACTIC DIFFUSE EMISSION | 5 | B | FARHAD YUSEF-ZADEH | USA | 3 | AO3 | A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503099010/ | Quick Look | ![]() |
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402 | SLX 1737-282 | 265.2352 | -28.3094 | 264.445148 | -28.284356 | 265.781005 | -4.938001 | 359.99405573 | 1.20298654 | 69.9745 | 54901.4562384259 | 2009-03-11 10:56:59 | 54901.8035648148 | 2009-03-11 19:17:08 | 503103010 | 18.316 | 10 | 18.3324 | 18.332 | 0 | 18.316 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.3659 | 16.3659 | 30.0019 | 0 | PROCESSED | 57545.7980208333 | 2016-06-06 19:09:09 | 55329 | 2010-05-13 00:00:00 | 54916.9907638889 | 2009-03-26 23:46:42 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031234 | We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity. | GALACTIC DIFFUSE EMISSION | 5 | C | FARHAD YUSEF-ZADEH | USA | 3 | AO3 | A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503103010/ | Quick Look | ![]() |
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403 | TYCHO SNR | 6.3244 | 64.1507 | 5.624265 | 63.873888 | 42.856632 | 53.765731 | 120.08671326 | 1.42345384 | 81.1044 | 53913.439224537 | 2006-06-27 10:32:29 | 53915.6530555556 | 2006-06-29 15:40:24 | 500024010 | 101.1274 | 100 | 101.1434 | 101.1274 | 101.1434 | 101.1434 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 94.5123 | 94.5123 | 191.2068 | 3 | PROCESSED | 57534.8252199074 | 2016-05-26 19:48:19 | 54289 | 2007-07-08 00:00:00 | 54052.7199884259 | 2006-11-13 17:16:47 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001099 | We propose to observe Tycho's Supernova Remnant with Suzaku. The proposal has two main goals: (1) to measure the energy spectrum of the entire remnant above 10 keV with the HXD, and (2) to study the 0.5-10 keV band spectrum as a function of position with the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | JOHN HUGHES | JAP | 0 | SWG | SUZAKU STUDY OF TYCHO'S SUPERNOVA REMNANT | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500024010/ | Quick Look | ![]() |
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404 | NEP #3 | 270.0483 | 66.5696 | 270.04982 | 66.569341 | 34.92017 | 89.983512 | 96.39421541 | 29.79223028 | 188.0738 | 55180.9320949074 | 2009-12-15 22:22:13 | 55182.0557638889 | 2009-12-17 01:20:18 | 504074010 | 50.1769 | 50 | 50.1769 | 50.1769 | 0 | 50.1769 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33.3374 | 33.3374 | 97.0499 | 1 | PROCESSED | 57549.895162037 | 2016-06-10 21:29:02 | 54922 | 2009-04-01 00:00:00 | 55200.4707291667 | 2010-01-04 11:17:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | STEVEN SNOWDEN | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504074010/ | Quick Look | ![]() |
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405 | HESS J1809-193E | 272.0013 | -19.5033 | 271.261943 | -19.51123 | 271.881238 | 3.92439 | 10.71539243 | 0.332309 | 270.1011 | 55085.7498148148 | 2009-09-11 17:59:44 | 55087.1564351852 | 2009-09-13 03:45:16 | 504079010 | 51.0289 | 50 | 51.0289 | 51.0289 | 0 | 51.0289 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.8753 | 41.8753 | 121.5198 | 2 | PROCESSED | 57548.5914699074 | 2016-06-09 14:11:43 | 55465 | 2010-09-26 00:00:00 | 55098.3372337963 | 2009-09-24 08:05:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041303 | We propose a detailed study of the extended VHE source HESS J1809-193 neighboring young PSR J1809-1917 with a known X-ray pulsar-wind nebula (PWN). As the chance coincidence is very unlikely, there should be a connection between the two. Furthermore, previous short Chandra observations of this field have revealed a large-scale asymmetric PWN extending toward the center of the TeV source. Thus, this is an excellent case for testing whether the unidentified TeV sources near young pulsars are, in fact, relic PWNe crushed by the asymmetric SNR reverse shock. We will probe the nature of the X-ray emission by measuring the surface brightness and spatially-resolved spectra across the large extent of the TeV source. Suzaku XIS is ideally suited for this purpose because of its low background. | GALACTIC DIFFUSE EMISSION | 5 | A | OLEG KARGALTSEV | USA | 4 | AO4 | CRUSHED PLERION HESS J1809-193: TEV TO X-RAY CONNECTION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504079010/ | Quick Look | ![]() |
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406 | G156.2+5.7 (NW2) | 74.4322 | 52.0607 | 73.448956 | 51.983713 | 79.105505 | 29.208158 | 155.84514532 | 5.68920631 | 266.0115 | 55258.7553587963 | 2010-03-03 18:07:43 | 55259.9821643518 | 2010-03-04 23:34:19 | 504081010 | 52.8646 | 50 | 52.8678 | 52.8678 | 0 | 52.8646 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.3866 | 49.3866 | 105.991 | 1 | PROCESSED | 57550.7899189815 | 2016-06-11 18:57:29 | 55689 | 2011-05-08 00:00:00 | 55322.3173842593 | 2010-05-06 07:37:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041311 | The large Galactic (R=50') supernova remnant (SNR) G156.2+5.7 is one of the few evolved SNRs with possible X-ray non-thermal (hard-tail) emission. Based on our recent observations with the Suzaku XIS, we found an indication of correlation between the X-ray hard-tail emission and radio emission. In addition, we confirmed the existence of metal-rich ejecta in the central portion, but found no evidence of ejecta in the rim regions. To investigate the correlation between the X-ray hard-tail emission and the radio emission, and the distributions of the X-ray emitting ejecta in this SNR, we propose to extend our observations with the Suzaku XIS. We request three pointings with a total exposure time of 150 ks. | GALACTIC DIFFUSE EMISSION | 5 | C | SATORU KATSUDA | USA | 4 | AO4 | REVEALING X-RAY HARD-TAIL AND EJECTA STRUCTURES IN THE EVOLVED SNR G156.2+5.7 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504081010/ | Quick Look | ![]() |
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407 | XB1916-053 | 289.7015 | -5.2503 | 289.036388 | -5.342643 | 290.518339 | 16.797779 | 31.34764946 | -8.47089453 | 261.8034 | 56948.5140856482 | 2014-10-18 12:20:17 | 56952.1112152778 | 2014-10-22 02:40:09 | 409032020 | 140.4495 | 300 | 140.4575 | 140.4655 | 0 | 140.4495 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 6.8873 | 6.8873 | 14.636 | 0 | PROCESSED | 57616.6738773148 | 2016-08-16 16:10:23 | 56748 | 2014-04-01 00:00:00 | 57000.2058680556 | 2014-12-09 04:56:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091221 | XB1916-053 is a prototypical dipping low mass X-ray binary (LMXB) with a dip recurrence period of 3000.6+-0.2s. However, extensive optical observations also show a longer stable period of 3027s. The former is most likely the orbital period, and the latter the superhump period caused by the precession of an elliptical accretion disk at a period of 3.9 days, representing the beat period between optical and X-ray periods. The morphology of the X-ray dips does indeed change dramatically over several days, but existing data suggest a somewhat longer period for the dip morphology cycle of 4.7 days. Here we propose a 300ks Suzaku observation of XB1916-053 with as few interruptions as possible, to conduct a definitive timing and spectroscopic study of its disk emission and dipping activity. | GALACTIC POINT SOURCES | 4 | B | ALAN SMALE | USA | 9 | AO9 | THE PRECESSING DISK IN THE DIPPING X-RAY BINARY XB1916-053 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409032020/ | Quick Look | ![]() |
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408 | 330.2+1.0 | 240.2338 | -51.588 | 239.290439 | -51.447752 | 249.06097 | -30.286548 | 330.14009051 | 0.98414205 | 285.0002 | 55078.1480671296 | 2009-09-04 03:33:13 | 55080.8126736111 | 2009-09-06 19:30:15 | 504083010 | 127.7746 | 150 | 127.7826 | 127.7746 | 0 | 127.7746 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 112.8484 | 112.8484 | 230.1578 | 1 | PROCESSED | 57548.4938657407 | 2016-06-09 11:51:10 | 55455 | 2010-09-16 00:00:00 | 55089.3295949074 | 2009-09-15 07:54:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041312 | Observations of G330.2+1.0 have revealed that it is a rare supernova remnant whose X-ray emission is dominated by synchrotron radiation. The available X-ray data provides rather poor constraints on the physical properties of the remnant. We propose to perform a deep Suzaku observation to obtain good spectral data. Joint spectral analyses of Suzaku and radio data will enable us to accurately and precisely measure the synchrotron spectral index and cutoff frequency, the electron temperature, the emission measure, and, perhaps, the relative elemental abundances. As a result, it will be possible to compute accurate and precise values for the spectral index and maximum energy of the nonthermal electrons, the strength of the magnetic field, and the ambient density, age, and shock velocity. | GALACTIC DIFFUSE EMISSION | 5 | B | GLENN ALLEN | USA | 4 | AO4 | MULTIWAVELENGTH SPECTROSCOPY OF 330.2 1.0 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504083010/ | Quick Look | ![]() |
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409 | LMC X-4 | 83.1804 | -66.3624 | 83.172059 | -66.39551 | 0.975905 | -87.276392 | 276.32693529 | -32.54034863 | 209.1491 | 54480.3607175926 | 2008-01-15 08:39:26 | 54480.7919560185 | 2008-01-15 19:00:25 | 702038010 | 21.6579 | 20 | 21.6726 | 21.6579 | 0 | 21.6726 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.8837 | 22.8837 | 37.252 | 0 | PROCESSED | 57541.3108796296 | 2016-06-02 07:27:40 | 54860 | 2009-01-29 00:00:00 | 54490.3089236111 | 2008-01-25 07:24:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021127 | We propose for a series of three 20ks observations of the binary X-ray pulsar LMC X-4. This source shows 13.5 s pulsations, a 1.4 d orbital period, and a long-period (~30 d) variability due to a warped, precessing accretion disk. The proposed analysis will use pulse-phase spectroscopy with XIS to explore changes in the X-ray pulses and spectra at three different phases in the disk precession. This work will give us a detailed picture of the accretion flow, particularly for the inner regions of the accretion disk that are illuminated by the X-rays from the neutron star. This project takes advantage of the strengths of the XIS, particularly its excellent spectral resolution, sufficient (1s) time resolution in Window mode, and wide PSF that limits pile-up effects. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RYAN HICKOX | USA | 2 | AO2 | SUPERORBITAL VARIATION OF LMC X-4: EXPLORING THE ACCRETION FLOW | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702038010/ | Quick Look | ![]() |
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410 | 73P/SW3 | 18.0599 | -9.2267 | 17.433228 | -9.491881 | 13.014248 | -15.596574 | 139.25333623 | -71.43625621 | 59.4006 | 53894.0025 | 2006-06-08 00:03:36 | 53894.0689699074 | 2006-06-08 01:39:19 | 500014060 | 3.235 | 35 | 3.235 | 3.235 | 3.235 | 3.235 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.49 | 2.49 | 5.7359 | 0 | PROCESSED | 57534.5883796296 | 2016-05-26 14:07:16 | 54267 | 2007-06-16 00:00:00 | 54052.5346759259 | 2006-11-13 12:49:56 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014060/ | Quick Look | ![]() |
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411 | NGC5548 | 214.4969 | 25.1266 | 213.929993 | 25.356783 | 201.998856 | 36.406453 | 31.93001973 | 70.4949274 | 285.8791 | 54310.1810648148 | 2007-07-29 04:20:44 | 54311.0209953704 | 2007-07-30 00:30:14 | 702042070 | 31.8099 | 30 | 31.8099 | 31.8099 | 0 | 31.8099 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 29.503 | 29.503 | 72.5279 | 1 | PROCESSED | 57539.3547569444 | 2016-05-31 08:30:51 | 54706 | 2008-08-28 00:00:00 | 54339.4245486111 | 2007-08-27 10:11:21 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021307 | We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARTIN ELVIS | USA | 2 | AO2 | NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702042070/ | Quick Look | ![]() |
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412 | 73P/SW3 | 18.338 | -9.3332 | 17.711705 | -9.597966 | 13.233056 | -15.802283 | 140.17356876 | -71.46762322 | 59.3974 | 53894.4024768518 | 2006-06-08 09:39:34 | 53894.4682986111 | 2006-06-08 11:14:21 | 500014120 | 1.5551 | 35 | 1.5551 | 1.5551 | 1.5551 | 1.5551 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1.566 | 1.566 | 5.682 | 0 | PROCESSED | 57534.5988773148 | 2016-05-26 14:22:23 | 54267 | 2007-06-16 00:00:00 | 54052.5441782407 | 2006-11-13 13:03:37 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014120/ | Quick Look | ![]() |
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413 | NGC 1365 | 53.3968 | -36.1347 | 52.919388 | -36.301683 | 36.801187 | -53.032832 | 237.94662462 | -54.6022242 | 221.6565 | 54486.2300578704 | 2008-01-21 05:31:17 | 54490.0002083333 | 2008-01-25 00:00:18 | 702047010 | 160.5057 | 150 | 160.5057 | 160.5137 | 0 | 160.5137 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 146.8139 | 146.8139 | 325.6768 | 4 | PROCESSED | 57541.4786342593 | 2016-06-02 11:29:14 | 54883 | 2009-02-21 00:00:00 | 54515.5847800926 | 2008-02-19 14:02:05 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021314 | We propose a 150 ksec observation of the Seyfert Galaxy NGC 1365. This galaxy have a unique set of properties: FeXXV and FeXXVI Kalpha and Kbeta absorption lines (the highest S/N detection so far among AGNs), rapidly varying cold absorber (nH variations of ~10^23/cm^2 in a few hours, changes from Compton-thick to Compton-thin in two days), a relativistic iron emission line. This new long observation will use at best the unique capabilities of Suzaku to constrain the dimensions of the absorbers, and, for the first time, will investigate the dynamics and physical conditions of the hot absorber responsible of the iron absorption lines. It is likely that an occultation will occur during the observation. This occultation would directly set the dimension of the X-ray source. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | GUIDO RISALITI | USA | 2 | AO2 | BLACK HOLE OCCULTATION AND OUTFLOW VARIABILITY IN NGC 1365 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702047010/ | Quick Look | ![]() |
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414 | SN1006 SE | 225.8656 | -42.0517 | 225.046486 | -41.856364 | 235.600187 | -23.734349 | 327.61589547 | 14.40537 | 115.0022 | 53765.3759259259 | 2006-01-30 09:01:20 | 53766.487662037 | 2006-01-31 11:42:14 | 500016010 | 51.6076 | 50 | 51.6132 | 51.6212 | 51.6212 | 51.6076 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 55.6704 | 55.6704 | 96.0399 | 2 | PROCESSED | 57532.8333564815 | 2016-05-24 20:00:02 | 54247 | 2007-05-27 00:00:00 | 54040.6484259259 | 2006-11-01 15:33:44 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001062 | We propose two Suzaku pointings of the Galactic supernova remnant (SNR) that exploded as a supernova in 1006. The main goal of the project is to use the XIS measure the abundances of low-Z elements in the ejecta. | GALACTIC DIFFUSE EMISSION | 5 | A | JOHN HUGHES | JAP | 0 | SWG | THE EJECTA IN SN1006 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500016010/ | Quick Look | ![]() |
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415 | SGR C | 266.1523 | -29.4673 | 265.354719 | -29.446679 | 266.622211 | -6.071258 | 359.43182832 | -0.08906822 | 82.0001 | 53786.5315393518 | 2006-02-20 12:45:25 | 53789.4515509259 | 2006-02-23 10:50:14 | 500018010 | 106.9219 | 100 | 106.9219 | 106.9219 | 106.9219 | 106.9219 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 46.6069 | 46.6069 | 252.2778 | 2 | PROCESSED | 57533.0732175926 | 2016-05-25 01:45:26 | 54247 | 2007-05-27 00:00:00 | 54041.6109375 | 2006-11-02 14:39:45 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001079 | We propose 100 ksec observation of the Sgr C cloud in the Galactic center region. The cloud emits strong 6.4-keV line, and is a candidate of X-ray reflection nebula; the molecular cloud which emits fluorescence and scattered X-rays irradiated by an external X-ray source. The past activity of Sgr~A$^*$, the Galactic nucleus, may be the origin of 6.4-keV line. We will study 6.4-keV line and verify the X-ray reflection scenario. The second objective is to study the distribution of high ionized and neutral iron lines in the GC region. Chandra observation indicates that H-like iron line is very strong in this region. With the higher energy resolution of XIS, we can confirm the Chandra results. High energy diffuse emission above 10 keV is also a important target by HXD. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI MURAKAMI | JAP | 0 | SWG | FOSSILS OF THE GALACTIC CENTER ACTIVITY | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500018010/ | Quick Look | ![]() |
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416 | NGC 6300 | 259.2549 | -62.8185 | 258.083078 | -62.76377 | 263.641528 | -39.613132 | 328.49505458 | -14.05378352 | 296.7285 | 54390.5141087963 | 2007-10-17 12:20:19 | 54392.375162037 | 2007-10-19 09:00:14 | 702049010 | 82.577 | 80 | 82.577 | 82.577 | 0 | 82.577 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 105.5127 | 105.5127 | 160.7798 | 1 | PROCESSED | 57540.3276041667 | 2016-06-01 07:51:45 | 54770 | 2008-10-31 00:00:00 | 54403.3802083333 | 2007-10-30 09:07:30 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021331 | Recent X-ray observations of Seyfert 2 galaxies have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by AGN Unified Schemes. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (60 ksec each) of four local bright Compton-thin Seyfert2s, selected from the Swift/BAT survey with a hard X-ray flux exceeding 1e-10 cgs to form a flux-limited sample. The unprecedented broad bandpass of Suzaku offers a unique tool to investigate the X-ray emission, placing strong constraints on the geometry and location of the reprocessing matter. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | JAMES REEVES | USA | 2 | AO2 | REVEALING THE REPROCESSING MATTER IN SEYFERT 2 GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702049010/ | Quick Look | ![]() |
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417 | SEP #3 | 89.9578 | -66.5683 | 89.959755 | -66.568521 | 317.285609 | -89.984917 | 276.39273536 | -29.82821774 | 172.4885 | 55179.5059259259 | 2009-12-14 12:08:32 | 55180.9169444444 | 2009-12-15 22:00:24 | 504073010 | 44.408 | 50 | 44.408 | 44.416 | 0 | 44.416 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23.8784 | 23.8784 | 121.9018 | 1 | PROCESSED | 57549.8504282407 | 2016-06-10 20:24:37 | 54922 | 2009-04-01 00:00:00 | 55200.462337963 | 2010-01-04 11:05:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | STEVEN SNOWDEN | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504073010/ | Quick Look | ![]() |
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418 | G156.2+5.7 (E2) | 75.2673 | 51.6789 | 74.287315 | 51.605827 | 79.638917 | 28.767744 | 156.46612231 | 5.86221802 | 271.6298 | 55248.7736574074 | 2010-02-21 18:34:04 | 55250.0369675926 | 2010-02-23 00:53:14 | 504082010 | 50.3308 | 50 | 50.3468 | 50.3308 | 0 | 50.3468 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 46.1424 | 46.1424 | 109.1379 | 0 | PROCESSED | 57550.6943865741 | 2016-06-11 16:39:55 | 55632 | 2011-03-12 00:00:00 | 55266.2981597222 | 2010-03-11 07:09:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041311 | The large Galactic (R=50') supernova remnant (SNR) G156.2+5.7 is one of the few evolved SNRs with possible X-ray non-thermal (hard-tail) emission. Based on our recent observations with the Suzaku XIS, we found an indication of correlation between the X-ray hard-tail emission and radio emission. In addition, we confirmed the existence of metal-rich ejecta in the central portion, but found no evidence of ejecta in the rim regions. To investigate the correlation between the X-ray hard-tail emission and the radio emission, and the distributions of the X-ray emitting ejecta in this SNR, we propose to extend our observations with the Suzaku XIS. We request three pointings with a total exposure time of 150 ks. | GALACTIC DIFFUSE EMISSION | 5 | C | SATORU KATSUDA | USA | 4 | AO4 | REVEALING X-RAY HARD-TAIL AND EJECTA STRUCTURES IN THE EVOLVED SNR G156.2+5.7 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504082010/ | Quick Look | ![]() |
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419 | PUP A : S | 125.6829 | -43.1445 | 125.254263 | -42.982932 | 147.449231 | -59.669734 | 260.57740663 | -3.43620983 | 277.8865 | 53843.8334606482 | 2006-04-18 20:00:11 | 53844.4397569444 | 2006-04-19 10:33:15 | 501090010 | 31.1445 | 30 | 31.1605 | 31.1525 | 31.1445 | 31.1685 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 26.5856 | 26.5856 | 52.3719 | 1 | PROCESSED | 57533.5191550926 | 2016-05-25 12:27:35 | 54401 | 2007-10-28 00:00:00 | 53907.0902199074 | 2006-06-21 02:09:55 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011246 | We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present. | GALACTIC DIFFUSE EMISSION | 5 | A | UNA HWANG | USA | 1 | AO1 | MAPPING OXYGEN IN PUPPIS A | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501090010/ | Quick Look | ![]() |
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420 | ESO 506-G027 | 189.6943 | -27.3584 | 189.030338 | -27.083667 | 200.074921 | -21.229266 | 299.48164005 | 35.42851647 | 302.0467 | 54314.0460300926 | 2007-08-02 01:06:17 | 54315.2572222222 | 2007-08-03 06:10:24 | 702080010 | 41.7453 | 40 | 41.7533 | 41.7613 | 0 | 41.7453 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 38.2828 | 38.2828 | 104.6399 | 2 | PROCESSED | 57539.3906134259 | 2016-05-31 09:22:29 | 54710 | 2008-09-01 00:00:00 | 54340.5553125 | 2007-08-28 13:19:39 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021374 | Though Compton thick AGN are expected to constitute a sizable fraction of the Seyfert population (Maiolino et al 1998 and Risaliti et al 1999), the fraction and the signatures of Compton thick AGN is unknown. The SWIFT BAT all-sky AGN survey has detected a complete sample of AGN with flux > 1-3e-11 erg/cm^2/s in the 15-200 keV band. At this energy range, the effects of heavy obscuration are minimal and thus BAT will allow us to determine the true fraction of Compton-thick sources. However, the BAT spectra are not simultaneous with XRT and XRT does not have the spectral resolution (with 10 ks) necessary to characterize a heavily absorbed 0.3-10 keV spectrum. We propose HXD nominal Suzaku observations of 4 possible Compton thick sources for which we recently obtained XMM 10 ks follow-ups. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RICHARD MUSHOTZKY | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF POSSIBLY COMPTON THICK AGN FROM THE SWIFT BAT SURVEY | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702080010/ | Quick Look | ![]() |
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421 | DEM L238 | 83.8177 | -70.5927 | 83.963728 | -70.62236 | 296.31824 | -85.384034 | 281.24911245 | -31.77318091 | 307.401 | 55308.023125 | 2010-04-22 00:33:18 | 55312.9730902778 | 2010-04-26 23:21:15 | 505063010 | 199.7795 | 200 | 199.7795 | 199.7795 | 0 | 199.7795 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 167.8355 | 167.8355 | 427.6297 | 5 | PROCESSED | 57551.4910069444 | 2016-06-12 11:47:03 | 55287 | 2010-04-01 00:00:00 | 55326.6889699074 | 2010-05-10 16:32:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051102 | Type Ia SNe play a central role in modern astrophysics, and yet we know little about their progenitors. Some of these progenitors are expected to significantly modify ambient medium around them prior to SN explosions. A standard Type Ia SNR model, a white dwarf explosion in a uniform ambient medium, fails to account for bright Fe-rich ejecta and faint blast waves seen in majority of Type Ia SNRs in the Magellanic Clouds. A promising explanation involves presence of dense circumstellar medium (CSM) around their progenitors. We propose a Suzaku study of 4 mature Type Ia SNRs in the LMC, with the goal of determining chemical abundances, temperatures and ionization ages within their ejecta. This will allow us to construct dynamical SNR models, and learn about their CSM and progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | KAZIMIERZ BORKOWSKI | USA | 5 | AO5 | TYPE IA REMNANTS IN THE LARGE MAGELLANIC CLOUD: WHAT PROGENITORS? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505063010/ | Quick Look | ![]() |
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422 | VELA FRAGMENT B | 135.5139 | -43.4767 | 135.058427 | -43.278826 | 159.573758 | -56.461444 | 265.2464603 | 1.98991007 | 89.0012 | 54044.6051388889 | 2006-11-05 14:31:24 | 54046.4341898148 | 2006-11-07 10:25:14 | 501085010 | 57.8804 | 60 | 57.8964 | 57.8804 | 57.8964 | 57.8964 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 56.9652 | 56.9652 | 158.0219 | 2 | PROCESSED | 57536.0751157407 | 2016-05-28 01:48:10 | 54695 | 2008-08-17 00:00:00 | 54091.4107175926 | 2006-12-22 09:51:26 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011245 | Ejecta fragments from the nearby Vela supernova remnant provide a unique opportunity to examine supernova ejecta as they shock and finally merge into the interstellar medium (ISM). Fragments "A" and "D", observed with Chandra and XMM-Newton, show strongly enhanced but very different abundances. These fragments are indeed ejecta, but originating in different layers of the precursor. We propose to observe another fragment, "B". The abundances and distribution will provide further evidence about the origin and evolution of these ejecta clumps, In combination with the existing observations of fragments A and D, these data will provide a much more complete picture of the variation in ejecta fragment abundances and their interaction with the remnant shell and the surrounding ISM. | GALACTIC DIFFUSE EMISSION | 5 | C | TERRANCE GAETZ | USA | 1 | AO1 | SEARCHING FOR EJECTA IN VELA SNR FRAGMENT B | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501085010/ | Quick Look | ![]() |
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423 | VELA PWN E3 | 129.9962 | -45.3672 | 129.571682 | -45.189023 | 154.98711 | -60.107857 | 264.19786494 | -2.25193357 | 304.5033 | 55712.1335069444 | 2011-05-31 03:12:15 | 55712.4099305556 | 2011-05-31 09:50:18 | 506046010 | 14.1787 | 15 | 14.2027 | 14.1947 | 0 | 14.1787 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.6599 | 12.6599 | 23.8759 | 0 | PROCESSED | 57602.1638078704 | 2016-08-02 03:55:53 | 56093 | 2012-06-15 00:00:00 | 55725.9978240741 | 2011-06-13 23:56:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | B | SATORU KATSUDA | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506046010/ | Quick Look | ![]() |
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424 | SNR HB3 SE-B | 35.7593 | 62.192 | 34.815236 | 61.964819 | 57.837975 | 44.676486 | 133.39304715 | 1.19520932 | 247.4986 | 56323.4084259259 | 2013-01-31 09:48:08 | 56323.7710532407 | 2013-01-31 18:30:19 | 507057010 | 25.8366 | 20 | 25.8446 | 25.8366 | 0 | 25.8526 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19.3092 | 19.3092 | 31.3279 | 1 | PROCESSED | 57608.6657638889 | 2016-08-08 15:58:42 | 56711 | 2014-02-23 00:00:00 | 56345.4750462963 | 2013-02-22 11:24:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071316 | We propose to study the large SNR HB3, which is classified as the mixed-morphology SNRs. The Fermi LAT revealed recently bright gamma-ray emissions adjacent to the southeastern shell of HB3, indicating the gamma rays originate in shocked molecular clouds associated with the nearby HII region W3/W4. However it is difficult to determine the gamma-ray origins since the HII regions are dominant in all energy bands except for X-ray. Our aim is to obtain the spatial structure and the temperature of thermal X-ray emissions at this site. These information will help us to understand whether HB3 interacts with molecular clouds. For this purpose, we require high sensitivities and the wide field of view to cover the southeastern shell. Suzaku is an ideal X-ray observatory to achieve this objective. | GALACTIC DIFFUSE EMISSION | 5 | C | JUNICHIRO KATSUTA | USA | 7 | AO7 | SUZAKU OBSERVATION OF A GAMMA-RAY EMISSION SNR, HB3 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507057010/ | Quick Look | ![]() |
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425 | SNR HB3 SE-C | 36.0358 | 62.4578 | 35.086232 | 62.23139 | 58.169094 | 44.855041 | 133.42083063 | 1.4890972 | 247.4994 | 56323.7716666667 | 2013-01-31 18:31:12 | 56324.1585532407 | 2013-02-01 03:48:19 | 507058010 | 24.142 | 20 | 24.1616 | 24.142 | 0 | 24.1696 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23.4547 | 23.4547 | 33.4239 | 0 | PROCESSED | 57608.6786342593 | 2016-08-08 16:17:14 | 56711 | 2014-02-23 00:00:00 | 56345.4779976852 | 2013-02-22 11:28:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071316 | We propose to study the large SNR HB3, which is classified as the mixed-morphology SNRs. The Fermi LAT revealed recently bright gamma-ray emissions adjacent to the southeastern shell of HB3, indicating the gamma rays originate in shocked molecular clouds associated with the nearby HII region W3/W4. However it is difficult to determine the gamma-ray origins since the HII regions are dominant in all energy bands except for X-ray. Our aim is to obtain the spatial structure and the temperature of thermal X-ray emissions at this site. These information will help us to understand whether HB3 interacts with molecular clouds. For this purpose, we require high sensitivities and the wide field of view to cover the southeastern shell. Suzaku is an ideal X-ray observatory to achieve this objective. | GALACTIC DIFFUSE EMISSION | 5 | C | JUNICHIRO KATSUTA | USA | 7 | AO7 | SUZAKU OBSERVATION OF A GAMMA-RAY EMISSION SNR, HB3 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507058010/ | Quick Look | ![]() |
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426 | COMET_8P_TUTTLE-P1-10 | 28.408 | 5.7525 | 27.75444 | 5.506869 | 28.446793 | -5.529035 | 149.8061723 | -53.84230192 | 248.5015 | 54471.1158333333 | 2008-01-06 02:46:48 | 54471.1820717593 | 2008-01-06 04:22:11 | 502062100 | 3.2196 | 3.2 | 3.2196 | 3.2196 | 0 | 3.2196 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2.166 | 2.166 | 5.6799 | 0 | PROCESSED | 57541.2676967593 | 2016-06-02 06:25:29 | 54908 | 2009-03-18 00:00:00 | 54542.2429513889 | 2008-03-17 05:49:51 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062100/ | Quick Look | ![]() |
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427 | COMET_8P_TUTTLE-P2_09 | 40.126 | -36.804 | 39.619449 | -37.017725 | 21.006365 | -49.022029 | 242.56232387 | -65.03879756 | 253.3121 | 54491.0963773148 | 2008-01-26 02:18:47 | 54491.2292824074 | 2008-01-26 05:30:10 | 502063090 | 4.3979 | 4 | 4.3979 | 4.3979 | 0 | 4.3979 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 4.752 | 4.752 | 11.4439 | 0 | PROCESSED | 57541.402662037 | 2016-06-02 09:39:50 | 54912 | 2009-03-22 00:00:00 | 54546.2142592593 | 2008-03-21 05:08:32 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063090/ | Quick Look | ![]() |
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428 | COMA SW1 | 194.4352 | 27.7266 | 193.830461 | 27.996528 | 181.158138 | 30.970186 | 56.45564066 | 88.47880121 | 314.5924 | 55735.5408796296 | 2011-06-23 12:58:52 | 55735.8654166667 | 2011-06-23 20:46:12 | 806047010 | 8.9948 | 10 | 9.0028 | 8.9948 | 0 | 9.0108 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 8.5423 | 8.5423 | 28.0339 | 1 | PROCESSED | 57602.3938773148 | 2016-08-02 09:27:11 | 55652 | 2011-04-01 00:00:00 | 55794.9989583333 | 2011-08-21 23:58:30 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806047010/ | Quick Look | ![]() |
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429 | COMA SW6 | 193.5264 | 26.9952 | 192.918358 | 27.266175 | 180.700954 | 29.954854 | 20.45636346 | 89.39137704 | 314.5991 | 55736.3040393518 | 2011-06-24 07:17:49 | 55736.5884259259 | 2011-06-24 14:07:20 | 806049010 | 15.6938 | 15 | 15.6938 | 15.7258 | 0 | 15.7098 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.0934 | 13.0934 | 24.5599 | 0 | PROCESSED | 57602.3988657407 | 2016-08-02 09:34:22 | 55652 | 2011-04-01 00:00:00 | 55795.0033333333 | 2011-08-22 00:04:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806049010/ | Quick Look | ![]() |
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430 | COMA SW6.5 | 193.4098 | 26.8733 | 192.801305 | 27.144404 | 180.65639 | 29.799393 | 5.58469416 | 89.44734556 | 314.5984 | 55736.5887615741 | 2011-06-24 14:07:49 | 55737.1238773148 | 2011-06-25 02:58:23 | 806050010 | 16.5376 | 15 | 16.5616 | 16.5536 | 0 | 16.5376 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.6623 | 16.6623 | 46.208 | 2 | PROCESSED | 57602.4126157407 | 2016-08-02 09:54:10 | 55652 | 2011-04-01 00:00:00 | 55795.0480324074 | 2011-08-22 01:09:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806050010/ | Quick Look | ![]() |
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431 | G21.5-0.9 | 278.4038 | -10.5066 | 277.711815 | -10.545632 | 278.460388 | 12.687474 | 21.56207071 | -0.86897985 | 103.5553 | 54190.0674074074 | 2007-03-31 01:37:04 | 54191.7405671296 | 2007-04-01 17:46:25 | 502065020 | 53.5261 | 100 | 53.5261 | 53.551 | 0 | 53.5661 | 1 | 2 | 0 | 1 | 1 | 0 | 0 | 48.618 | 48.618 | 144.5418 | 0 | PROCESSED | 57538.0817013889 | 2016-05-30 01:57:39 | 54695 | 2008-08-17 00:00:00 | 54200.5054861111 | 2007-04-10 12:07:54 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021211 | We propose an observation of the supernova remnant (SNR) G21.5--0.9. This SNR has a centrally peaked X-ray morphology which coupled with its non-thermal emission, suggested that the SNR's central engine was an undetected pulsar. Last year, a radio pulsar associated with the remnant was discovered (Gupta et al. 2005; Camilo et al. 2006). These announcements concur on the period of the pulsar and its period derivative making it the second highest spin-down luminosity pulsar. Deep Chandra imaging uncovered the missing shell (Matheson & Safi-Harb, 2005). Recent INTEGRAL and SWIFT/BAT slew observations detected G21.5--0.9 at more than 10 and 8 sigma respectively. The proposed observation will be the first self-consistent broad-band timing and spectral analysis from soft to very hard X-ray. | GALACTIC DIFFUSE EMISSION | 5 | B | ILANA HARRUS | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF THE SUPERNOVA REMNANT G21.5-0.9 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502065020/ | Quick Look | ![]() |
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432 | NGC 788 | 30.262 | -6.7593 | 29.638132 | -7.000547 | 25.672425 | -17.884233 | 165.15039638 | -63.76864601 | 77.358 | 54660.0353819444 | 2008-07-13 00:50:57 | 54661.0516666667 | 2008-07-14 01:14:24 | 703032010 | 45.9073 | 40 | 45.9153 | 45.9073 | 0 | 45.9153 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 39.594 | 39.594 | 87.7999 | 0 | PROCESSED | 57543.0405902778 | 2016-06-04 00:58:27 | 55048 | 2009-08-05 00:00:00 | 54682.1458564815 | 2008-08-04 03:30:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031323 | The classical unified model predicts only one type of Seyfert II (Sy2). Recent observations of SWIFT BAT-detected AGN found at least 4 classes of Sy2s: (1) objects with high column density and scattered soft x-rays, (2) Compton thick objects, (3) `hidden' AGN (Ueda et al. 2007), and (4) the `changing look' objects (Risaliti et al. 2006). The nature of these sources can only be revealed with high quality broad-band X-ray spectra from Suzaku. Thus, we are proposing 40ks observations for 2 of the brightest BAT AGN without high quality data, NGC 788, a type (3) object showing polarized optical broad lines, and NGC 3281, a classified (2) object. Such observations are necessary to build a reasonably large sample of high-quality, broad-band Sy2 spectra covering the range of X-ray/optical types. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RICHARD MUSHOTZKY | USA | 3 | AO3 | SUZAKU OBSERVATIONS OF X-RAY BRIGHT TYPE II AGN | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703032010/ | Quick Look | ![]() |
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433 | Q0122-380 | 21.0759 | -37.7461 | 20.512127 | -38.006435 | 1.342949 | -42.439189 | 271.91657466 | -77.33125236 | 48.7944 | 54615.4511921296 | 2008-05-29 10:49:43 | 54616.2009722222 | 2008-05-30 04:49:24 | 703035010 | 28.481 | 25 | 28.481 | 28.489 | 0 | 28.497 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.8107 | 26.8107 | 64.7699 | 1 | PROCESSED | 57542.6524421296 | 2016-06-03 15:39:31 | 54999 | 2009-06-17 00:00:00 | 54633.6971759259 | 2008-06-16 16:43:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031334 | Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GEORGE CHARTAS | USA | 3 | AO3 | A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703035010/ | Quick Look | ![]() |
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434 | Q0551-3637 | 88.2026 | -36.6158 | 87.768837 | -36.625605 | 87.11791 | -60.039805 | 242.36930247 | -26.91846995 | 296.4731 | 54575.4385763889 | 2008-04-19 10:31:33 | 54575.6251041667 | 2008-04-19 15:00:09 | 703036010 | 3.8954 | 22 | 3.8954 | 3.8954 | 0 | 3.8954 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3.773 | 3.773 | 16.0959 | 0 | PROCESSED | 57542.3345601852 | 2016-06-03 08:01:46 | 54979 | 2009-05-28 00:00:00 | 54588.1227314815 | 2008-05-02 02:56:44 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031334 | Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GEORGE CHARTAS | USA | 3 | AO3 | A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703036010/ | Quick Look | ![]() |
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435 | 0509-67.5 | 77.4191 | -67.5347 | 77.43679 | -67.59534 | 342.967322 | -85.012032 | 278.15520093 | -34.57404921 | 36.9172 | 56491.0670601852 | 2013-07-18 01:36:34 | 56495.4689583333 | 2013-07-22 11:15:18 | 508072020 | 152.6517 | 150 | 152.6997 | 152.6517 | 0 | 152.6997 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 139.7536 | 139.7536 | 380.2994 | 7 | PROCESSED | 57612.009537037 | 2016-08-12 00:13:44 | 56383 | 2013-04-01 00:00:00 | 56509.8769097222 | 2013-08-05 21:02:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081315 | We propose deep observations of the LMC SNRs N63A and 0509-67.5. The Chandra observation of N63A showed possible signatures of He-like Fe emission and radiative recombination continua of Si and S. With the new observation by Suzaku, we will determine the plasma state of this SNR. The remarkable characteristic of 0509-67.5 is its extremely-low ionization age. This SNR, therefore, provides us a unique opportunity to explore detailed emission features of lowly-ionized atoms. The immediate objective of this observation is to accurately measure the Fe K-beta to K-alpha flux ratio to constrain the dominant charge state of the Fe ejecta. Both observations will provide us crucial datasets useful to improve our knowledge of SNR plasma and atomic physics. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROYA YAMAGUCHI | USA | 8 | AO8 | LEAVING A LEGACY OF SUZAKU: HIGH-QUALITY SPECTRAL DATASET ON IMPORTANT SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508072020/ | Quick Look | ![]() |
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436 | Q0109-3518 | 17.9376 | -35.0527 | 17.356449 | -35.318066 | 0.204002 | -38.849268 | 275.45528409 | -80.96443984 | 40.3411 | 54606.0677199074 | 2008-05-20 01:37:31 | 54606.6772453704 | 2008-05-20 16:15:14 | 703037010 | 29.9585 | 18 | 29.9665 | 29.9585 | 0 | 29.9665 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22.8339 | 22.8339 | 52.6559 | 1 | PROCESSED | 57542.5808101852 | 2016-06-03 13:56:22 | 54982 | 2009-05-31 00:00:00 | 54616.3810300926 | 2008-05-30 09:08:41 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031334 | Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GEORGE CHARTAS | USA | 3 | AO3 | A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703037010/ | Quick Look | ![]() |
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437 | G189 EAST | 95.4705 | 22.4826 | 94.715097 | 22.507311 | 95.056054 | -0.862354 | 189.63783855 | 3.93426331 | 258.2106 | 57096.5099652778 | 2015-03-15 12:14:21 | 57098.6780324074 | 2015-03-17 16:16:22 | 509036010 | 66.0529 | 85 | 66.0529 | 86.2237 | 0 | 86.2397 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8236226852 | 2016-08-17 19:46:01 | 57524 | 2016-05-16 00:00:00 | 57157.5685416667 | 2015-05-15 13:38:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091314 | We propose observations of G189.6+3.3, a large candidate supernova remnant (SNR) that overlaps with the much better studied remnant IC 443. Little is known about G189; ROSAT images show a shell-like structure about 1.5$^{circ}$ in diameter, but it has never been observed with modern X-ray telescopes. Its association, or lack thereof, with IC 443 is unknown. It may not be a supernova remnant at all; a superbubble origin for the X-ray emission also provides an intriguing possibility. Spatially-resolved spectroscopy with Suzaku will allow the detailed measurement of the plasma properties, illuminating the nature of this object. Determining the nature of G189 will help to probe the evolution of the ISM driven by the deaths of massive stars. | GALACTIC DIFFUSE EMISSION | 5 | B | BRIAN WILLIAMS | USA | 9 | AO9 | OBSERVATIONS OF G189.6+3.3: AN SNR COMPANION TO IC 443? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509036010/ | Quick Look | ![]() |
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438 | KES 69 | 278.2575 | -10.136 | 277.567341 | -10.174332 | 278.335469 | 13.065931 | 21.8245316 | -0.57033928 | 267.6495 | 56927.2830902778 | 2014-09-27 06:47:39 | 56929.1391435185 | 2014-09-29 03:20:22 | 509037010 | 77.3795 | 80 | 77.3795 | 77.9708 | 0 | 77.9953 | 2 | 2 | 0 | 3 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5892361111 | 2016-08-16 14:08:30 | 57345 | 2015-11-19 00:00:00 | 56979.4056944444 | 2014-11-18 09:44:12 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091315 | We propose to conduct Suzaku observations of the Galactic supernova remnants (SNRs) Kes 69 (G21.8-0.6) and 3C 396 (G39.2-0.3). These SNRs were detected in the infrared by Spitzer and their infrared colors suggest that shocked molecules produce the observed emission. Published analyses of the X-ray emission from these SNRs (along with our own analysis of archival XMM-Newton and Chandra observations of these sources) reveals that the emission from both Kes 69 and 3C 396 is thermal and that they may both be mixed-morphology SNRs (MMSNRs) but deeper observations are needed to clarify their X-ray spectral properties. In particular, we will investigate whether these X-ray emitting plasmas are overionized, which is observed for other MMSNRs. | GALACTIC DIFFUSE EMISSION | 5 | A | THOMAS PANNUTI | USA | 9 | AO9 | SUZAKU OBSERVATIONS OF THE SPITZER-DETECTED GALACTIC SUPERNOVA REMNANTS KES 69 (G21.8-0.6) AND 3C 396 (G39.2-0.3) | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509037010/ | Quick Look | ![]() |
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439 | FERMI_JET_COCOON_2 | 320.2279 | -29.504 | 319.485138 | -29.716859 | 313.416673 | -13.31861 | 17.00065384 | -44.00205209 | 255.063 | 56981.4053356482 | 2014-11-20 09:43:41 | 56981.8683217593 | 2014-11-20 20:50:23 | 509048010 | 19.9032 | 20 | 19.9032 | 19.9032 | 0 | 19.9032 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7951736111 | 2016-08-16 19:05:03 | 57362 | 2015-12-06 00:00:00 | 56995.5937268518 | 2014-12-04 14:14:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091322 | The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way. | GALACTIC DIFFUSE EMISSION | 5 | C | MATTHEW MILLER | USA | 9 | AO9 | OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509048010/ | Quick Look | ![]() |
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440 | DIFFUSE1E | 200.6072 | 7.3824 | 199.979251 | 7.643505 | 196.163547 | 14.87503 | 324.76377809 | 68.9302329 | 123.5311 | 57011.0086458333 | 2014-12-20 00:12:27 | 57011.5252083333 | 2014-12-20 12:36:18 | 509062010 | 23.9762 | 20 | 23.9762 | 24.5362 | 0 | 24.5362 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5495023148 | 2016-08-17 13:11:17 | 57475 | 2016-03-28 00:00:00 | 57107.4289583333 | 2015-03-26 10:17:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091324 | In the course of a program to fit spatial models to the Galactic hot gas content, we discovered a few fields that were highly discrepant in the strength of their O VII and/or O VIII line strengths. These are rare emission regions, occurring in fewer than 1% of the fields and they are not due to known extended emission regions (SNR, galaxy clusters, etc.). These emission anomalies probably signify locations of unusual physics, such as shocks, conductive heating, or local heat injection. We propose observations to determine the angular extent of these unusual regions and to better define the intensities of the O VII and O VIII lines. These observations will help identify the relevant physical process and the nature of the phenomenon causing them. | GALACTIC DIFFUSE EMISSION | 5 | C | JOEL BREGMAN | USA | 9 | AO9 | UNIDENTIFIED BRIGHT X-RAY BACKGROUND REGIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509062010/ | Quick Look | ![]() |
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441 | VELA FRAGMENT C | 136.2696 | -44.691 | 135.819541 | -44.490549 | 161.57955 | -57.213344 | 266.51473212 | 1.58715492 | 269.3614 | 54580.6978703704 | 2008-04-24 16:44:56 | 54582.3056481482 | 2008-04-26 07:20:08 | 503095010 | 84.1167 | 70 | 84.1167 | 84.1167 | 0 | 84.1167 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91.3547 | 91.3547 | 138.9018 | 2 | PROCESSED | 57542.4305439815 | 2016-06-03 10:19:59 | 54960 | 2009-05-09 00:00:00 | 54594.2480324074 | 2008-05-08 05:57:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031212 | Ejecta fragments projecting from the nearby Vela supernova remnant provide a unique opportunity to examine supernova ejecta as they shock and finally merge into the interstellar medium (ISM). Fragments "A" and "D", observed with Chandra and XMM, and Fragment "B", observed with Suzaku, show strongly enhanced (but very different) abundances. These fragments are indeed ejecta, but originating in different layers of the precursor. We propose to observe two of the remaining ejecta fragments. In combination with the existing observations of Fragments A, B, and D, these data will provide a much more complete picture of the variation in ejecta fragment abundances and their interactions with the remnant shell and the surrounding ISM. | GALACTIC DIFFUSE EMISSION | 5 | B | TERRANCE GAETZ | USA | 3 | AO3 | SEARCHING FOR EJECTA IN THE VELA SUPERNOVA REMNANT FRAGMENTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503095010/ | Quick Look | ![]() |
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442 | 3C120 | 68.2984 | 5.3555 | 67.633855 | 5.251051 | 67.433469 | -16.402094 | 190.37315865 | -27.39441526 | 237.4585 | 53775.1527199074 | 2006-02-09 03:39:55 | 53776.2433217593 | 2006-02-10 05:50:23 | 700001010 | 41.9321 | 160 | 41.9321 | 41.9321 | 41.9321 | 41.9321 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 34.0941 | 34.0941 | 94.2219 | 1 | PROCESSED | 57532.9769791667 | 2016-05-24 23:26:51 | 54247 | 2007-05-27 00:00:00 | 53906.2470601852 | 2006-06-20 05:55:46 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001003 | Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 0 | SWG | BROAD-BAND MONITORING OF 3C120 IN VARIOUS ACCRETING STATES | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700001010/ | Quick Look | ![]() |
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443 | PKS2155-304 | 329.7191 | -30.2247 | 328.99529 | -30.464273 | 321.189186 | -16.770975 | 17.73226544 | -52.24760927 | 254.1358 | 53704.7749884259 | 2005-11-30 18:35:59 | 53706.3613888889 | 2005-12-02 08:40:24 | 700012010 | 63.9114 | 80 | 63.9194 | 63.9114 | 63.9194 | 63.9166 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 58.0114 | 58.0114 | 137.0498 | 3 | PROCESSED | 57532.3797685185 | 2016-05-24 09:06:52 | 54247 | 2007-05-27 00:00:00 | 54038.8920138889 | 2006-10-30 21:24:30 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001100 | Jets in blazars are believed to be a powerful site of particle acceleration. TeV emitting blazars are very important, because we can study very end of electron distribution near the maximum energy by using X-ray spectrum, because X-ray emission is believed to be due to synchrotron emission from the higher energy electron. Comparison of spectral index between X-ray and TeV gives us a crucial information on these source, because this is very sensitive to the particle injection and rapid cooling. In order to maximize the capability of sensitive hard X-ray observations of Suzaku, we propose reserved TOO observations for the next six months of PV phase from the TeV emitting blazars established by HESS, selected from five candidates. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TADAYUKI TAKAHASHI | JAP | 0 | SWG-TOO | RESERVED TOO OBSERVATIONS OF SELECTED TEV-BRIGHT BLAZARS | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700012010/ | Quick Look | ![]() |
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444 | ANTLIA E1 | 157.8782 | -35.3295 | 157.312453 | -35.072071 | 176.074864 | -40.746998 | 273.21530285 | 19.3432713 | 277.4995 | 56091.5629398148 | 2012-06-13 13:30:38 | 56092.2633912037 | 2012-06-14 06:19:17 | 807066010 | 25.747 | 23 | 25.755 | 25.747 | 0 | 25.755 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.9291 | 22.9291 | 60.5139 | 1 | PROCESSED | 57605.6597106482 | 2016-08-05 15:49:59 | 56473 | 2013-06-30 00:00:00 | 56107.272650463 | 2012-06-29 06:32:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071521 | We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KA-WAH WONG | USA | 7 | AO7 | MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807066010/ | Quick Look | ![]() |
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445 | HESS J1809-193B | 272.6789 | -19.1585 | 271.941455 | -19.169725 | 272.527802 | 4.258732 | 11.32661741 | -0.06027609 | 269.0544 | 55084.4838773148 | 2009-09-10 11:36:47 | 55085.7488310185 | 2009-09-11 17:58:19 | 504078010 | 52.4748 | 50 | 52.4748 | 52.4748 | 0 | 52.4748 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.3733 | 43.3733 | 109.2758 | 1 | PROCESSED | 57548.5486226852 | 2016-06-09 13:10:01 | 55475 | 2010-10-06 00:00:00 | 55109.4280555556 | 2009-10-05 10:16:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041303 | We propose a detailed study of the extended VHE source HESS J1809-193 neighboring young PSR J1809-1917 with a known X-ray pulsar-wind nebula (PWN). As the chance coincidence is very unlikely, there should be a connection between the two. Furthermore, previous short Chandra observations of this field have revealed a large-scale asymmetric PWN extending toward the center of the TeV source. Thus, this is an excellent case for testing whether the unidentified TeV sources near young pulsars are, in fact, relic PWNe crushed by the asymmetric SNR reverse shock. We will probe the nature of the X-ray emission by measuring the surface brightness and spatially-resolved spectra across the large extent of the TeV source. Suzaku XIS is ideally suited for this purpose because of its low background. | GALACTIC DIFFUSE EMISSION | 5 | A | OLEG KARGALTSEV | USA | 4 | AO4 | CRUSHED PLERION HESS J1809-193: TEV TO X-RAY CONNECTION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504078010/ | Quick Look | ![]() |
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446 | 330.2+1.0 | 240.2384 | -51.525 | 239.295706 | -51.384773 | 249.047523 | -30.224565 | 330.18352169 | 1.02987491 | 98.9027 | 55239.832025463 | 2010-02-12 19:58:07 | 55242.125150463 | 2010-02-15 03:00:13 | 504083030 | 92.505 | 30 | 92.513 | 92.505 | 0 | 92.521 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86.0965 | 86.0965 | 198.0897 | 4 | PROCESSED | 57550.6564699074 | 2016-06-11 15:45:19 | 55622 | 2011-03-02 00:00:00 | 55253.5397685185 | 2010-02-26 12:57:16 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041312 | Observations of G330.2+1.0 have revealed that it is a rare supernova remnant whose X-ray emission is dominated by synchrotron radiation. The available X-ray data provides rather poor constraints on the physical properties of the remnant. We propose to perform a deep Suzaku observation to obtain good spectral data. Joint spectral analyses of Suzaku and radio data will enable us to accurately and precisely measure the synchrotron spectral index and cutoff frequency, the electron temperature, the emission measure, and, perhaps, the relative elemental abundances. As a result, it will be possible to compute accurate and precise values for the spectral index and maximum energy of the nonthermal electrons, the strength of the magnetic field, and the ambient density, age, and shock velocity. | GALACTIC DIFFUSE EMISSION | 5 | B | GLENN ALLEN | USA | 4 | AO4 | MULTIWAVELENGTH SPECTROSCOPY OF 330.2 1.0 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504083030/ | Quick Look | ![]() |
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447 | NGC 526A | 20.9794 | -35.0729 | 20.408158 | -35.333404 | 3.010528 | -40.076485 | 263.77547728 | -79.45131683 | 257.0195 | 55578.7592939815 | 2011-01-17 18:13:23 | 55580.6404050926 | 2011-01-19 15:22:11 | 705044010 | 72.9346 | 70 | 72.9346 | 72.9346 | 0 | 72.9346 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 63.1372 | 63.1372 | 162.4977 | 2 | PROCESSED | 57600.6980324074 | 2016-07-31 16:45:10 | 55961 | 2012-02-04 00:00:00 | 55595.4905671296 | 2011-02-03 11:46:25 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051434 | The Compton-thin NELG NGC 526a has large hard X-ray variability and likely an abnormally flat photon index, Gamma near 1.6. We request two observations of 70 ks each, spaced six months apart, to accurately constrain Compton reflection and obtain geometrical constraints on the accreting material to test Seyfert unification schemes, as well as constrain coronal power law parameters. Importantly, we will track long-term spectral variability to constrain the location and nature of the reflecting material. We also will resolve the moderately broad Fe K alpha line, which may indicate the presence of a truncated accretion disk, and thus constrain the amount of reflection off an accretion disk versus that from a torus. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | ALEX MARKOWITZ | USA | 5 | AO5 | COMPTON REFLECTION AND LONG-TERM SPECTRAL VARIABILITY IN THE SEYFERT AGN NGC 526A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705044010/ | Quick Look | ![]() |
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448 | MARKARIAN 335 | 1.5539 | 20.2624 | 0.911019 | 19.984083 | 9.744165 | 17.917566 | 108.74842011 | -41.36053721 | 68.4831 | 53907.0624537037 | 2006-06-21 01:29:56 | 53910.7585532407 | 2006-06-24 18:12:19 | 701031010 | 151.2884 | 150 | 151.2964 | 151.2884 | 151.2964 | 151.2964 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 140.9812 | 140.9812 | 319.3028 | 4 | PROCESSED | 57534.8340046296 | 2016-05-26 20:00:58 | 54401 | 2007-10-28 00:00:00 | 53928.5392361111 | 2006-07-12 12:56:30 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011323 | We propose to observe the two Seyfert 1 galaxies Mrk 335 and ESO198-G024 for a total exposure of 150 ks each with the high sensitivity and broad band coverage of the Suzaku satellite. Both sources show a broad Fe K line and a strong soft excess. One appealing explanation for the nature of the soft excess is reflection. Fundamental to this hypothesis is the assumption that the same self-consistent reflection spectrum explains the Fe K line (including its shape), the soft excess, and also the Compton reflection hump above 20 keV. Suzaku's ability to measure all three reflection components simultaneously enables the different spectral models to be disentangled and reflection to be strongly tested. Understanding black hole accretion is fundamental to NASA's "SEU" theme. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | JON MILLER | USA | 1 | AO1 | REVEALING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701031010/ | Quick Look | ![]() |
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449 | NGC 1068 | 40.6928 | -0.0667 | 40.052721 | -0.278811 | 38.248989 | -15.097296 | 172.18986515 | -51.95763403 | 248.588 | 54141.0038078704 | 2007-02-10 00:05:29 | 54141.9168287037 | 2007-02-10 22:00:14 | 701039010 | 41.6229 | 35 | 41.6309 | 41.6309 | 0 | 41.6229 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.8024 | 41.8024 | 78.8839 | 0 | PROCESSED | 57537.346875 | 2016-05-29 08:19:30 | 54525 | 2008-02-29 00:00:00 | 54151.5012962963 | 2007-02-20 12:01:52 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011333 | The majority of accretion onto supermassive black holes in the local Universe occurs in obscured Seyferts. At moderate redshifts, the optical narrow emission-lines used to identify Seyfert 2s become difficult to isolate from the host galaxy's emission, resulting in an underestimate of the numbers of Seyfert 2s. Seyfert 2s are a critical component of AGN synthesis models of the Cosmic X-ray Background (CXB), as these sources are likely responsible for the unresolved component of the 2-8 keV background and may also contribute significantly to the 30 keV background. We propose to use Suzaku observations of ten local Seyfert 2s to measure their ultrahard (>10 keV) emission and examine how Seyfert 2s at moderate redshifts contribute to the CXB. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | AARON STEFFEN | USA | 1 | AO1 | MEASURING THE ULTRAHARD X-RAY EMISSION OF A LOCAL POPULATION OF SEYFERT 2S | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701039010/ | Quick Look | ![]() |
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450 | VELA SNR CB-LBG | 130.6266 | -44.6167 | 130.194556 | -44.436193 | 154.988854 | -59.23497 | 263.87788945 | -1.43970243 | 293.482 | 55319.3460648148 | 2010-05-03 08:18:20 | 55319.7940046296 | 2010-05-03 19:03:22 | 505071010 | 27.1799 | 20 | 27.1799 | 27.1799 | 0 | 27.1799 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.0945 | 25.0945 | 38.6939 | 1 | PROCESSED | 57551.3691203704 | 2016-06-12 08:51:32 | 55696 | 2011-05-15 00:00:00 | 55330.1543981482 | 2010-05-14 03:42:20 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051304 | The Vela SNR is known to have ejecta bullets outside the main shell. In addition to these bullets, signatures of ejecta inside the main shell have been uncovered in recent X-ray studies. Mostly, these are rich in light metals such as O, Ne, or Mg, whereas no Fe-rich ejecta had yet been detected. Based on archival XMM-Newton data, we found a possible Fe-rich ejecta bullet headed roughly in the opposite direction of Vela pulsar's motion. This would provide us with a window into the core-collapse SN explosion of the Vela SNR. Since its electron temperature is very low (~0.1 keV), the good Suzaku XIS response below 0.5 keV is suitable to study this object. We propose to observe it in four pointings. The requested exposure time is 20 ks each, resulting in a total exposure time of 80 ks. | GALACTIC DIFFUSE EMISSION | 5 | B | SATORU KATSUDA | USA | 5 | AO5 | IRON-RICH EJECTA BULLET IN THE VELA SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505071010/ | Quick Look | ![]() |
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451 | NGC 4593 | 189.9131 | -5.3426 | 189.268208 | -5.068085 | 191.201579 | -0.987759 | 297.48049807 | 57.40434975 | 112.24 | 54449.1962384259 | 2007-12-15 04:42:35 | 54451.972349537 | 2007-12-17 23:20:11 | 702040010 | 118.8415 | 107 | 118.8415 | 118.8415 | 0 | 118.8415 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 108.976 | 108.976 | 239.7899 | 6 | PROCESSED | 57540.92 | 2016-06-01 22:04:48 | 54829 | 2008-12-29 00:00:00 | 54462.4425462963 | 2007-12-28 10:37:16 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021302 | We propose a 80 ksec observation of the bright Seyfert 1 NGC 4593 to resolve the moderately relativistic Fe K line, and test for a truncated or ionized accretion disk. To achieve accurate modeling of the broad Fe line, Suzaku's broad bandpass is required to deconvolve the broadband emitting component and accurately constrain the continuum. NGC 4593 is one of the few Seyferts to also show evidence for Fe XXVI emission at 6.9 keV; we will use the XIS to confirm the line and constrain its origin. If the thin accretion disk is truncated or transitions to an ADAF, it would reveal NGC 4593 to be an analogue of low/hard-state X-ray Binaries. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | ALEX MARKOWITZ | USA | 2 | AO2 | DOES THE SEYFERT AGN NGC 4593 HAVE A TRUNCATED OR IONIZED ACCRETION DISK? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702040010/ | Quick Look | ![]() |
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452 | NGC7582 | 349.5472 | -42.3304 | 348.858747 | -42.603943 | 331.723267 | -34.368393 | 348.20905034 | -65.68466064 | 49.5845 | 54221.7937384259 | 2007-05-01 19:02:59 | 54222.3176273148 | 2007-05-02 07:37:23 | 702052010 | 23.9412 | 25 | 23.9572 | 23.9412 | 0 | 23.9572 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.5816 | 21.5816 | 45.256 | 0 | PROCESSED | 57538.5368402778 | 2016-05-30 12:53:03 | 54695 | 2008-08-17 00:00:00 | 54228.073275463 | 2007-05-08 01:45:31 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021332 | We propose to perform 4 Suzaku observations of 25 ks each (for a total of 100 ks) of the bright Seyfert 2 galaxy,NGC 7582.The aim of this proposal is to measure the distance of the gas that absorbs the nuclear radiation, by analyzing the pattern of variability of its column density.NGC7582 is the ideal target for this kind of analysis, because it already showed large variations of the column density of the absorber between X-ray observations taken a few years apart.With the present proposal, we intend to probe a wider range of timescales, from a week to about six months, in order to measure the distance of the absorber from the nucleus. This measure is crucial to understand the nature of the absorber in type 2 objects and the validity of the torus paradigm. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARCO CHIABERGE | USA | 2 | AO2 | MEASURING THE DISTANCE OF THE ABSORBER IN NGC 7582 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702052010/ | Quick Look | ![]() |
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453 | NGC7582 | 349.6446 | -42.4137 | 348.956435 | -42.687331 | 331.752163 | -34.475865 | 347.94526846 | -65.70277041 | 233.1822 | 54413.9093981482 | 2007-11-09 21:49:32 | 54414.6459490741 | 2007-11-10 15:30:10 | 702052030 | 29.3538 | 25 | 29.3538 | 29.3538 | 0 | 29.3538 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24.4331 | 24.4331 | 63.6319 | 1 | PROCESSED | 57540.4723842593 | 2016-06-01 11:20:14 | 54790 | 2008-11-20 00:00:00 | 54423.1929398148 | 2007-11-19 04:37:50 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021332 | We propose to perform 4 Suzaku observations of 25 ks each (for a total of 100 ks) of the bright Seyfert 2 galaxy,NGC 7582.The aim of this proposal is to measure the distance of the gas that absorbs the nuclear radiation, by analyzing the pattern of variability of its column density.NGC7582 is the ideal target for this kind of analysis, because it already showed large variations of the column density of the absorber between X-ray observations taken a few years apart.With the present proposal, we intend to probe a wider range of timescales, from a week to about six months, in order to measure the distance of the absorber from the nucleus. This measure is crucial to understand the nature of the absorber in type 2 objects and the validity of the torus paradigm. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARCO CHIABERGE | USA | 2 | AO2 | MEASURING THE DISTANCE OF THE ABSORBER IN NGC 7582 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702052030/ | Quick Look | ![]() |
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454 | NGC7582 | 349.6411 | -42.4153 | 348.952917 | -42.688928 | 331.748482 | -34.476047 | 347.94523476 | -65.69973119 | 236.7954 | 54420.0722337963 | 2007-11-16 01:44:01 | 54420.8960532407 | 2007-11-16 21:30:19 | 702052040 | 31.8955 | 25 | 31.8955 | 31.8955 | 0 | 31.8955 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.7806 | 25.7806 | 71.1719 | 0 | PROCESSED | 57540.5407060185 | 2016-06-01 12:58:37 | 54797 | 2008-11-27 00:00:00 | 54430.3041203704 | 2007-11-26 07:17:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021332 | We propose to perform 4 Suzaku observations of 25 ks each (for a total of 100 ks) of the bright Seyfert 2 galaxy,NGC 7582.The aim of this proposal is to measure the distance of the gas that absorbs the nuclear radiation, by analyzing the pattern of variability of its column density.NGC7582 is the ideal target for this kind of analysis, because it already showed large variations of the column density of the absorber between X-ray observations taken a few years apart.With the present proposal, we intend to probe a wider range of timescales, from a week to about six months, in order to measure the distance of the absorber from the nucleus. This measure is crucial to understand the nature of the absorber in type 2 objects and the validity of the torus paradigm. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARCO CHIABERGE | USA | 2 | AO2 | MEASURING THE DISTANCE OF THE ABSORBER IN NGC 7582 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702052040/ | Quick Look | ![]() |
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455 | 3C 33 | 17.2445 | 13.2796 | 16.584921 | 13.013252 | 20.958615 | 5.507742 | 129.4936436 | -49.368548 | 249.2604 | 54460.3029282407 | 2007-12-26 07:16:13 | 54463.6390509259 | 2007-12-29 15:20:14 | 702059010 | 127.3677 | 100 | 127.3757 | 127.3757 | 0 | 127.3677 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 106.5885 | 106.5885 | 288.2036 | 7 | PROCESSED | 57541.0545833333 | 2016-06-02 01:18:36 | 54854 | 2009-01-23 00:00:00 | 54483.4886458333 | 2008-01-18 11:43:39 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021356 | We propose a 100 ks Suzaku observation of the nucleus of the nearby (z=0.0597) FRII radio galaxy 3C 33, to constrain the nature of its Compton reflection component, and make an accurate measurement of its Fe Ka emission line. 3C 33 (awarded category-C time in Suzaku AO-1, not observed) is the only radio-loud AGN with evidence of Compton reflection in its low-energy (< 10 keV) spectrum, and so offers a unique opportunity to study both the soft- and hard-band properties of reflection. The HXD will allow us, for the first time, to constrain the nature of the Compton reflection component in 3C 33 and, when combined with the superb sensitivity of the XIS, will enable us to determine the line-of-sight geometry and structure of the reflecting region. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | DANIEL EVANS | USA | 2 | AO2 | CONSTRAINING THE REFLECTION PROPERTIES OF THE NARROW-LINE RADIO GALAXY 3C 33 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702059010/ | Quick Look | ![]() |
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456 | Q1017+1055 | 155.041 | 10.671 | 154.377707 | 10.922699 | 152.99156 | 0.282434 | 230.36219873 | 50.83483368 | 121.1263 | 54431.9135185185 | 2007-11-27 21:55:28 | 54432.4376851852 | 2007-11-28 10:30:16 | 702064010 | 18.0486 | 20 | 18.0486 | 18.0486 | 0 | 18.0486 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.0316 | 15.0316 | 45.2819 | 0 | PROCESSED | 57540.6059606482 | 2016-06-01 14:32:35 | 54805 | 2008-12-05 00:00:00 | 54438.285150463 | 2007-12-04 06:50:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021361 | The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | GEORGE CHARTAS | USA | 2 | AO2 | AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702064010/ | Quick Look | ![]() |
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457 | 3C 273 | 187.2559 | 1.9961 | 186.616492 | 2.272457 | 185.868054 | 4.712799 | 289.92713501 | 64.30042167 | 293.1671 | 54281.0022569444 | 2007-06-30 00:03:15 | 54282.2661342593 | 2007-07-01 06:23:14 | 702070010 | 54.8927 | 67 | 54.8927 | 54.8927 | 0 | 54.8927 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.2592 | 51.2592 | 109.1439 | 1 | PROCESSED | 57539.0801388889 | 2016-05-31 01:55:24 | 54695 | 2008-08-17 00:00:00 | 54322.4904166667 | 2007-08-10 11:46:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021364 | We propose a Suzaku campaign on the bright z=0.158 quasar 3C 273. The source exhibits a Seyfert-like X-ray spectrum when the luminosity is low but is dominated by emission from the jet in a high state. Suzaku will be able to measure the broadband spectrum, especially X-ray reprocessed features, with greater sensitivity than ever before. Decoupling and monitoring of the disk and jet components will enable detailed spectroscopy to help understand the disk-jet connection and the wider implications for AGN physics in general. The target is bright and well-suited because for most AGN either the disk or jet component dominates. For this pilot study we propose two 50 ks observations, one in each visibility window. The science goals cannot be achieved with existing data or other missions. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TAHIR YAQOOB | USA | 2 | AO2 | EXPLORING THE ACCRETION DISK AND JET CONNECTION IN 3C 273 WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702070010/ | Quick Look | ![]() |
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458 | SWIFT J0318.7+6828 | 49.4315 | 68.5395 | 48.26024 | 68.35635 | 69.167768 | 48.016071 | 135.6962435 | 9.37350025 | 42.3301 | 54365.4488078704 | 2007-09-22 10:46:17 | 54367.125162037 | 2007-09-24 03:00:14 | 702075010 | 77.1156 | 53 | 77.1396 | 77.1156 | 0 | 77.1396 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.6855 | 70.6855 | 144.7978 | 1 | PROCESSED | 57540.0779513889 | 2016-06-01 01:52:15 | 54770 | 2008-10-31 00:00:00 | 54403.1984490741 | 2007-10-30 04:45:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021372 | The nature and even the existence of type II quasars is highly controversial. Due to their highly obscured nature, very hard (> 15 keV) observations are needed to probe their properties. With the 9-month SWIFT BAT all-sky AGN survey, detection of heavily obscured sources is now possible. Indeed, 6 type II quasars have been identified. Their properties, however, are a challenge to standard AGN models e.g., all but one of these sources are strong radio sources and several have optical spectra indicative of an un-absorbed source. We propose Suzaku observations of the 5 without broadband high signal to noise x-ray data to perform a detailed analysis of their x-ray properties and to understand their relationship to the lower luminosity well studied Seyfert IIs. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RICHARD MUSHOTZKY | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF SWIFT BAT TYPE II QUASARS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702075010/ | Quick Look | ![]() |
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459 | VELA PWN E6 | 131.2685 | -45.4809 | 130.840764 | -45.298021 | 156.629635 | -59.743456 | 264.83769354 | -1.61837696 | 304.5065 | 55712.9576273148 | 2011-05-31 22:58:59 | 55713.2292939815 | 2011-06-01 05:30:11 | 506049010 | 18.1968 | 15 | 18.2048 | 18.1968 | 0 | 18.2128 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.209 | 14.209 | 23.4699 | 0 | PROCESSED | 57602.1814699074 | 2016-08-02 04:21:19 | 56103 | 2012-06-25 00:00:00 | 55735.9387268518 | 2011-06-23 22:31:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | B | SATORU KATSUDA | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506049010/ | Quick Look | ![]() |
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460 | NGC 4051 | 180.7952 | 44.5393 | 180.156844 | 44.817625 | 159.255387 | 40.346248 | 148.86124636 | 70.08047443 | 126.4079 | 54793.7 | 2008-11-23 16:48:00 | 54795.572025463 | 2008-11-25 13:43:43 | 703023020 | 78.3855 | 70 | 78.3935 | 78.3855 | 0 | 78.3939 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 62.7604 | 62.7604 | 161.7358 | 0 | PROCESSED | 57544.5729513889 | 2016-06-05 13:45:03 | 54557 | 2008-04-01 00:00:00 | 54811.74875 | 2008-12-11 17:58:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031014 | The powerful combination of Principal Components Analysis with time-resolved X-ray spectroscopy of Seyfert AGN has shown strong evidence that changes in a complex absorber are the origin of much of observed AGN spectral and flux variability. Large column, high ionization layers of gas may arise in a disk wind, representing a significant new, and possibly dominant, component, responsible for shaping the X-ray spectrum of AGN. The broad bandpass of Suzaku gives us a unique opportunity to model primary and reflected continua and the effects of variable absorbing zones, and test wind and other models. We propose a long 340 ks exposure on the NLSy1 NGC 4051 whose large amplitude of variability and well-studied complex absorption will test those models to the limit | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TRACEY TURNER | USA | 3 | AO3 | DECONSTRUCTING SEYFERT SPECTRA - TIME FOR A PARADIGM SHIFT? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703023020/ | Quick Look | ![]() |
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461 | SMC X-1 | 19.2829 | -73.4465 | 18.951639 | -73.709645 | 312.337269 | -66.476032 | 300.41108523 | -43.55576838 | 356.8796 | 55658.8646759259 | 2011-04-07 20:45:08 | 55659.2447106482 | 2011-04-08 05:52:23 | 706030010 | 18.4662 | 18 | 18.4662 | 18.55 | 0 | 18.5448 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15.5577 | 15.5577 | 32.8239 | 0 | PROCESSED | 57601.4235185185 | 2016-08-01 10:09:52 | 56040 | 2012-04-23 00:00:00 | 55673.2343055556 | 2011-04-22 05:37:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JOSEPH NEILSEN | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030010/ | Quick Look | ![]() |
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462 | SMC X-1 | 19.2476 | -73.446 | 18.915775 | -73.709202 | 312.329896 | -66.466401 | 300.42473809 | -43.55764171 | 6.4299 | 55669.2561805556 | 2011-04-18 06:08:54 | 55669.705775463 | 2011-04-18 16:56:19 | 706030020 | 17.2769 | 18 | 17.2769 | 17.2849 | 0 | 17.4844 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 17.6646 | 17.6646 | 38.8159 | 0 | PROCESSED | 57601.5313657407 | 2016-08-01 12:45:10 | 56058 | 2012-05-11 00:00:00 | 55691.1543171296 | 2011-05-10 03:42:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JOSEPH NEILSEN | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030020/ | Quick Look | ![]() |
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463 | NGC 7172 | 330.5062 | -31.8708 | 329.778877 | -32.112297 | 321.223494 | -18.549637 | 15.12698367 | -53.06449716 | 59.7356 | 54611.0658680556 | 2008-05-25 01:34:51 | 54612.8558217593 | 2008-05-26 20:32:23 | 703030010 | 82.2797 | 80 | 82.2797 | 82.2877 | 0 | 82.2877 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71.7465 | 71.7465 | 154.6338 | 0 | PROCESSED | 57542.6661805556 | 2016-06-03 15:59:18 | 54999 | 2009-06-17 00:00:00 | 54633.7016203704 | 2008-06-16 16:50:20 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031322 | X-ray observations of Seyfert 2 have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by the AGN Unification Scheme. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (80 ksec each) of three bright Compton-thin Seyfert 2 galaxies, selected from the Swift/BAT survey, with a hard X-ray flux exceeding 9e-11cgs, to form a flux-limited sample. The unprecedented bandpass of Suzaku offers a unique tool to investigate the X-ray emission of these sources, allowing us to put strong constraints on the reprocessing matter in Seyfert 2s. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | VALENTINA BRAITO | USA | 3 | AO3 | THE NATURE OF THE X-RAY ABSORBER IN SEYFERT 2 GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703030010/ | Quick Look | ![]() |
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464 | NGC 3281 | 157.9591 | -34.9074 | 157.391937 | -34.649823 | 175.881528 | -40.345828 | 273.03211125 | 19.73409342 | 278.2413 | 54607.8508449074 | 2008-05-21 20:25:13 | 54609.2287615741 | 2008-05-23 05:29:25 | 703033010 | 46.234 | 40 | 46.242 | 46.25 | 0 | 46.234 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.4549 | 41.4549 | 119.038 | 0 | PROCESSED | 57542.6257175926 | 2016-06-03 15:01:02 | 54988 | 2009-06-06 00:00:00 | 54620.2890162037 | 2008-06-03 06:56:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031323 | The classical unified model predicts only one type of Seyfert II (Sy2). Recent observations of SWIFT BAT-detected AGN found at least 4 classes of Sy2s: (1) objects with high column density and scattered soft x-rays, (2) Compton thick objects, (3) `hidden' AGN (Ueda et al. 2007), and (4) the `changing look' objects (Risaliti et al. 2006). The nature of these sources can only be revealed with high quality broad-band X-ray spectra from Suzaku. Thus, we are proposing 40ks observations for 2 of the brightest BAT AGN without high quality data, NGC 788, a type (3) object showing polarized optical broad lines, and NGC 3281, a classified (2) object. Such observations are necessary to build a reasonably large sample of high-quality, broad-band Sy2 spectra covering the range of X-ray/optical types. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RICHARD MUSHOTZKY | USA | 3 | AO3 | SUZAKU OBSERVATIONS OF X-RAY BRIGHT TYPE II AGN | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703033010/ | Quick Look | ![]() |
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465 | 3C279 | 194.0699 | -5.7328 | 193.422743 | -5.462367 | 195.164566 | 0.26232 | 305.15066173 | 57.11808922 | 113.6425 | 54854.8772222222 | 2009-01-23 21:03:12 | 54856.125162037 | 2009-01-25 03:00:14 | 703049020 | 56.937 | 200 | 56.937 | 56.937 | 0 | 56.937 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.6263 | 12.6263 | 107.7799 | 2 | PROCESSED | 57545.3327777778 | 2016-06-06 07:59:12 | 55328 | 2010-05-12 00:00:00 | 54880.5584259259 | 2009-02-18 13:24:08 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031346 | We propose a 200 ks observation of 3C279, the archetypal EGRET blazar to be conducted simultaneously with GLAST as well as many other facilities, with the goal of obtaining broadband spectra and light-curves. The flux in all observable bands is known to be rapidly variable, but the information regarding the correlation between the time history of flux in various bands is limited, and the proposed observations are designed to remedy this shortcoming. Such detailed spectral and variability studies are crucial to discriminate between different radiation scenarios responsible for production of X-rays and gamma-rays, and to constrain the matter content and by extension, the formation process of the jet, dissipation of the jet energy, and energization of the radiating particles. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GRZEGORZ MADEJSKI | USA | 3 | AO3 | SUZAKU AND GLAST OBSERVATIONS OF 3C279 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703049020/ | Quick Look | ![]() |
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466 | NGC985 | 38.6279 | -8.738 | 38.014145 | -8.956444 | 33.218289 | -22.635173 | 180.72422437 | -59.4803664 | 62.3866 | 55027.6174884259 | 2009-07-15 14:49:11 | 55028.5925231482 | 2009-07-16 14:13:14 | 704042010 | 31.9969 | 30 | 31.9969 | 32.0063 | 0 | 32.0063 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.7241 | 25.7241 | 84.2379 | 1 | PROCESSED | 57547.8515856482 | 2016-06-08 20:26:17 | 55406 | 2010-07-29 00:00:00 | 55040.2752430556 | 2009-07-28 06:36:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041414 | We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | EZEQUIEL TREISTER | USA | 4 | AO4 | THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704042010/ | Quick Look | ![]() |
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467 | COMA NW6.5 | 194.0774 | 29.5523 | 193.474522 | 29.822643 | 179.856398 | 32.45513 | 99.36309014 | 87.34957637 | 319.9974 | 55734.7422685185 | 2011-06-22 17:48:52 | 55735.2522569444 | 2011-06-23 06:03:15 | 806045010 | 15.5013 | 15 | 15.5013 | 15.5151 | 0 | 15.5093 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.3764 | 17.3764 | 44.0599 | 0 | PROCESSED | 57602.3928587963 | 2016-08-02 09:25:43 | 55652 | 2011-04-01 00:00:00 | 55768.3250231482 | 2011-07-26 07:48:02 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806045010/ | Quick Look | ![]() |
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468 | ABELL 1795 | 207.2241 | 26.601 | 206.646901 | 26.849155 | 193.922602 | 34.994161 | 33.84733119 | 77.1817764 | 130.8638 | 53714.5034259259 | 2005-12-10 12:04:56 | 53714.7752199074 | 2005-12-10 18:36:19 | 800012010 | 13.0982 | 120 | 13.1062 | 13.0982 | 13.1062 | 13.1062 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 10.3759 | 10.3759 | 23.4639 | 1 | PROCESSED | 57532.3922453704 | 2016-05-24 09:24:50 | 54247 | 2007-05-27 00:00:00 | 54038.7903703704 | 2006-10-30 18:58:08 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001056 | We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MARK BAUTZ | JAP | 0 | SWG | TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800012010/ | Quick Look | ![]() |
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469 | CEN A S LOBE NO. 4 | 196.751 | -45.1436 | 196.031726 | -44.876448 | 214.740849 | -34.712794 | 305.81117883 | 17.64110832 | 288.0039 | 55421.3479282407 | 2010-08-13 08:21:01 | 55421.67375 | 2010-08-13 16:10:12 | 705035010 | 20.642 | 20 | 20.642 | 20.65 | 0 | 20.658 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.9643 | 18.9643 | 28.1439 | 0 | PROCESSED | 57552.9465277778 | 2016-06-13 22:43:00 | 55803 | 2011-08-30 00:00:00 | 55435.1577314815 | 2010-08-27 03:47:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051401 | We propose a set of four pointings (200 ks), to study the X-ray emission from the Southern giant lobe of the radio galaxy Cen A. Those lobes clearly separated from the central source, have been detected as a source of diffuse gamma-ray emission by the Fermi Telescope. The goal of the Suzaku observations is two-fold: first, to measure the diffuse component of the non-thermal X-ray emission with both the XIS and the HXD in order to determine the details of the distribution of the radiating relativistic particles (and B field), and second, to measure the thermal emission from the lobes (using primarily the XIS), to determine temperature and density of the X-ray emitting plasma, which, via consideration of pressure balance, will determine the content of energetic protons (cosmic rays). | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GRZEGORZ MADEJSKI | USA | 5 | AO5 | SUZAKU OBSERVATIONS OF THE SOUTHERN LOBE OF CEN A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705035010/ | Quick Look | ![]() |
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470 | IRAS 00397-1312 | 10.5707 | -12.9503 | 9.941553 | -13.224287 | 4.464578 | -16.066781 | 113.89016485 | -75.66108211 | 246.4295 | 55558.1361342593 | 2010-12-28 03:16:02 | 55560.2501388889 | 2010-12-30 06:00:12 | 705046010 | 83.7928 | 90 | 83.7928 | 83.7928 | 0 | 83.7928 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71.9314 | 71.9314 | 182.6317 | 1 | PROCESSED | 57632.5965856482 | 2016-09-01 14:19:05 | 56040 | 2012-04-23 00:00:00 | 55670.3615046296 | 2011-04-19 08:40:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051441 | We propose two Suzaku-HXD observations of two ULIRGs hosting a deeply buried AGN. These two objects are expected to host a powerful AGN in the luminosity range of quasars, based on solid evidence from mid-IR Spitzer spectroscopy. However, these sources are completely buried behind a screen of dust with column density in excess of 10^24 cm^-2, so not only the primary emission below 10 keV is obscured, but the reflected emission, usually ascribed to a circumnuclear "torus", is also absent. This suggests a complete spherical coverage of the X-ray source along all directions. The unique capabilities of Suzaku at high energies will allow to confirm the existence of these objects, representing the most extreme examples of buried AGNs, both in terms of obscuration and of intrinsic luminosity. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | GUIDO RISALITI | USA | 5 | AO5 | BURIED QUASAR 2S INSIDE ULIRGS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705046010/ | Quick Look | ![]() |
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471 | NGC 4945 | 196.3415 | -49.5274 | 195.611435 | -49.259681 | 217.040288 | -38.699914 | 305.25336122 | 13.28155854 | 286.7821 | 55386.9936226852 | 2010-07-09 23:50:49 | 55388.2626388889 | 2010-07-11 06:18:12 | 705047020 | 44.1517 | 40 | 44.1517 | 44.1597 | 0 | 44.1517 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.1612 | 40.1612 | 109.434 | 0 | PROCESSED | 57552.6167824074 | 2016-06-13 14:48:10 | 55777 | 2011-08-04 00:00:00 | 55411.4916898148 | 2010-08-03 11:48:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051442 | We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GUIDO RISALITI | USA | 5 | AO5 | HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705047020/ | Quick Look | ![]() |
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472 | NGC 4945 | 196.2918 | -49.5144 | 195.562046 | -49.246615 | 216.996084 | -38.704359 | 305.2209968 | 13.29631795 | 319.7988 | 55438.8990277778 | 2010-08-30 21:34:36 | 55439.9896990741 | 2010-08-31 23:45:10 | 705047040 | 39.3859 | 40 | 39.3859 | 39.3859 | 0 | 39.3859 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.7823 | 35.7823 | 94.2239 | 0 | PROCESSED | 57553.267962963 | 2016-06-14 06:25:52 | 55815 | 2011-09-11 00:00:00 | 55449.2596296296 | 2010-09-10 06:13:52 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051442 | We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GUIDO RISALITI | USA | 5 | AO5 | HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705047040/ | Quick Look | ![]() |
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473 | ESP 39607 | 11.5922 | -40.0968 | 10.997666 | -40.369881 | 351.254657 | -40.701682 | 307.24150307 | -76.98900447 | 243.1952 | 55549.7680208333 | 2010-12-19 18:25:57 | 55551.3175810185 | 2010-12-21 07:37:19 | 705048010 | 60.6687 | 60 | 60.6927 | 60.6687 | 0 | 60.6847 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.9555 | 48.9555 | 133.8399 | 3 | PROCESSED | 57554.5018402778 | 2016-06-15 12:02:39 | 55960 | 2012-02-03 00:00:00 | 55593.2278472222 | 2011-02-01 05:28:06 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051443 | We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195 keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log(L_x) > 45.5 erg/sec) absorbed type II QSOs in the local universe and the most ripe for study with Suzaku. The newly discovered source SWIFT J2344.6-4233 at a redshift of z=0.6 is the most luminous object in the BAT sample with log(L_x) = 46.5 erg/sec. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | WAYNE BAUMGARTNER | USA | 5 | AO5 | SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705048010/ | Quick Look | ![]() |
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474 | 3C 433 | 320.9422 | 25.055 | 320.383545 | 24.83969 | 333.197862 | 37.998992 | 74.46917661 | -17.70913692 | 252.1178 | 55506.5663310185 | 2010-11-06 13:35:31 | 55508.0953472222 | 2010-11-08 02:17:18 | 705050010 | 62.5009 | 60 | 62.54 | 62.5009 | 0 | 62.54 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.4271 | 44.4271 | 132.0698 | 0 | PROCESSED | 57554.0198958333 | 2016-06-15 00:28:39 | 55890 | 2011-11-25 00:00:00 | 55524.1485416667 | 2010-11-24 03:33:54 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051443 | We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195 keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log(L_x) > 45.5 erg/sec) absorbed type II QSOs in the local universe and the most ripe for study with Suzaku. The newly discovered source SWIFT J2344.6-4233 at a redshift of z=0.6 is the most luminous object in the BAT sample with log(L_x) = 46.5 erg/sec. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | WAYNE BAUMGARTNER | USA | 5 | AO5 | SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705050010/ | Quick Look | ![]() |
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475 | 0509-67.5 | 77.4163 | -67.5163 | 77.433384 | -67.576954 | 343.17919 | -85.012675 | 278.13367069 | -34.57909379 | 302.8449 | 56393.0595949074 | 2013-04-11 01:25:49 | 56397.1258912037 | 2013-04-15 03:01:17 | 508072010 | 175.9192 | 320 | 175.9352 | 175.9192 | 0 | 175.9432 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 166.6668 | 166.6668 | 351.2916 | 3 | PROCESSED | 57611.1504513889 | 2016-08-11 03:36:39 | 56383 | 2013-04-01 00:00:00 | 56425.6930439815 | 2013-05-13 16:37:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081315 | We propose deep observations of the LMC SNRs N63A and 0509-67.5. The Chandra observation of N63A showed possible signatures of He-like Fe emission and radiative recombination continua of Si and S. With the new observation by Suzaku, we will determine the plasma state of this SNR. The remarkable characteristic of 0509-67.5 is its extremely-low ionization age. This SNR, therefore, provides us a unique opportunity to explore detailed emission features of lowly-ionized atoms. The immediate objective of this observation is to accurately measure the Fe K-beta to K-alpha flux ratio to constrain the dominant charge state of the Fe ejecta. Both observations will provide us crucial datasets useful to improve our knowledge of SNR plasma and atomic physics. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROYA YAMAGUCHI | USA | 8 | AO8 | LEAVING A LEGACY OF SUZAKU: HIGH-QUALITY SPECTRAL DATASET ON IMPORTANT SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508072010/ | Quick Look | ![]() |
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476 | MBM16-OFF | 46.1075 | 13.1563 | 45.420617 | 12.96209 | 47.406639 | -4.032974 | 165.8625544 | -38.38773927 | 69.5985 | 56513.919849537 | 2013-08-09 22:04:35 | 56515.9119791667 | 2013-08-11 21:53:15 | 508073010 | 83.0565 | 80 | 83.0565 | 83.0565 | 0 | 83.0565 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81.1386 | 81.1386 | 172.0979 | 2 | PROCESSED | 57612.2143981482 | 2016-08-12 05:08:44 | 56953 | 2014-10-23 00:00:00 | 56587.5588541667 | 2013-10-22 13:24:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081322 | We propose the observation of three off-cloud targets near the targets of the Solar Wind Charge Exchange (SWCX) Key Project to study the properties of the Diffuse X-ray Background below 1 keV, with particular focus on the characterization of the Galactic Halo. The Key Project targets are at a distance of a few hundreds pc from the Sun and their high density portions shields about 90% of X-rays at the O VII energy, our proposed targets, instead, shield only about 50% of the Galactic Halo emission. The contrast between on- and off-cloud allows us to disentangle the foreground and background emissions. In particular we will focus on the properties of the galactic halo, which dominates the oxygen background emission. | GALACTIC DIFFUSE EMISSION | 5 | A | EUGENIO URSINO | USA | 8 | AO8 | PROPERTIES OF THE GALACTIC HALO THROUGH SHADOW OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508073010/ | Quick Look | ![]() |
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477 | Z8852 | 347.6318 | 7.5789 | 346.999079 | 7.307292 | 351.631711 | 11.858062 | 84.17423864 | -47.55525942 | 260.3346 | 54065.5867013889 | 2006-11-26 14:04:51 | 54066.1543287037 | 2006-11-27 03:42:14 | 801074010 | 14.8526 | 15 | 14.8526 | 14.8526 | 0 | 14.8526 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.9834 | 13.9834 | 49.0379 | 0 | PROCESSED | 57536.1918402778 | 2016-05-28 04:36:15 | 54695 | 2008-08-17 00:00:00 | 54088.6000694444 | 2006-12-19 14:24:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801074010/ | Quick Look | ![]() |
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478 | WISE J1819+4532 | 274.9137 | 45.5584 | 274.555701 | 45.535406 | 279.54226 | 68.836144 | 73.38480627 | 24.31157427 | 77.6532 | 56020.3333333333 | 2012-04-03 08:00:00 | 56021.0070833333 | 2012-04-04 00:10:12 | 707038010 | 30.8819 | 30 | 30.8819 | 30.8819 | 0 | 30.8819 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.564 | 27.564 | 58.2039 | 0 | PROCESSED | 57605.0974537037 | 2016-08-05 02:20:20 | 56399 | 2013-04-17 00:00:00 | 56033.2380787037 | 2012-04-16 05:42:50 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071443 | We request a 30-ks observation of WISE J1819+4532, an extreme WISE-selected AGN at z=2.031. This source stands out even amongst the rare WISE-selected sources we have been targeting: at mid-IR wavelengths, WISE J1819+4532 is ~10x brighter than similarly selected WISE sources, and more than 50x brighter than extreme Spitzer-selected sources. Assuming the local mid-IR to hard X-ray correlations, the implied intrinsic hard X-ray luminosity is L(2-10)~3e46 erg/s. WISE J1819+4532 is optically faint and the optical spectrum shows a typical obscured AGN with narrow emission lines. However, the object is infrared bright and the near-IR spectrum shows broad H-alpha emission. This implies that WISE J1819+4532 is a rare example of a an extremely luminous, semi-obscured AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | DANIEL STERN | USA | 7 | AO7 | WISE J1819+4532: AN OBSCURED, HYPERLUMINOUS ULIRG/AGN AT Z~2 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707038010/ | Quick Look | ![]() |
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479 | ZW229-15 | 286.3333 | 42.4706 | 285.936982 | 42.393229 | 298.560222 | 64.301193 | 73.09172558 | 15.5517204 | 34.6696 | 55715.0128356482 | 2011-06-03 00:18:29 | 55719.6251736111 | 2011-06-07 15:00:15 | 706035010 | 167.0838 | 165 | 168.6766 | 167.0838 | 0 | 168.6846 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 218.1832 | 218.1832 | 398.4357 | 2 | PROCESSED | 57602.3250694445 | 2016-08-02 07:48:06 | 56127 | 2012-07-19 00:00:00 | 55757.7055671296 | 2011-07-15 16:56:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061414 | The optical emission from AGN is though to be a combination of direct radiation from an accretion disk and reprocessed x-ray emission. Separating these components requires simultaneous high-precision x-ray/optical monitoring, which has heretofore not been achieved. We propose to gather this necessary data via simultaneous optical and x-ray monitoring of the Sy 1 galaxy Zw 229-15. Kepler is monitoring Zw 229-15 every 30 minutes with unprecedented 99% duty cycle and 0.1% repeatability. The key missing data is an appropriate x-ray campaign. We propose a 64-orbit (165 ks) Suzaku long-look combined with a series of 48 Swift visits to probe lags of 0.1-10 days. This will be the first experiment sensitive to such short lags and thus will critically test the present disc/reprocessing paradigm | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RICHARD MUSHOTZKY | USA | 6 | AO6 | SIMULTANEOUS SUZAKU/SWIFT/ KEPLER MONITORING OF ZW 229-15 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706035010/ | Quick Look | ![]() |
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480 | A2495 | 342.5662 | 10.9218 | 341.941655 | 10.656649 | 348.262816 | 16.910805 | 81.19678392 | -41.92445268 | 65.1354 | 54260.5857523148 | 2007-06-09 14:03:29 | 54261.1668287037 | 2007-06-10 04:00:14 | 801080020 | 25.7806 | 18 | 25.7806 | 25.7806 | 0 | 25.7806 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.9762 | 20.9762 | 50.1959 | 2 | PROCESSED | 57538.8757291667 | 2016-05-30 21:01:03 | 54695 | 2008-08-17 00:00:00 | 54270.430625 | 2007-06-19 10:20:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801080020/ | Quick Look | ![]() |
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481 | 0528+134 | 82.7323 | 13.541 | 82.025359 | 13.504077 | 82.83368 | -9.719507 | 191.35839601 | -11.00951452 | 89.1633 | 55832.6802314815 | 2011-09-28 16:19:32 | 55833.0119444444 | 2011-09-29 00:17:12 | 706043010 | 14.7892 | 10 | 14.7892 | 14.7892 | 0 | 14.7892 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.8659 | 15.8659 | 28.6359 | 0 | PROCESSED | 57603.2623032407 | 2016-08-03 06:17:43 | 56225 | 2012-10-25 00:00:00 | 55875.6223958333 | 2011-11-10 14:56:15 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061601 | We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | SVETLANA JORSTAD | USA | 6 | AO6 | EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706043010/ | Quick Look | ![]() |
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482 | G93.3+6.9 NW RIM | 312.9527 | 55.5354 | 312.608547 | 55.346344 | 352.30712 | 67.106977 | 93.368132 | 7.08938459 | 52.0991 | 56814.8070023148 | 2014-06-06 19:22:05 | 56817.24125 | 2014-06-09 05:47:24 | 509040010 | 107.8986 | 100 | 107.9066 | 107.9066 | 0 | 107.8986 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.2100115741 | 2016-08-15 05:02:25 | 57236 | 2015-08-02 00:00:00 | 56869.6106481482 | 2014-07-31 14:39:20 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091316 | We propose three relatively long observations (totaling 280 ksec) of the high Galactic latitude supernova remnant G093.3+6.9, previously observed in AO-1 with a series of short exposures. This remnant is of particular interest because it is expanding in a low-density medium, appears sub-energetic, and has mixed-morphology, with central thermal X-ray emission surrounded by a radio synchrotron shell. Fits to the spectrum suggest a Type Ia SNR, but the possible presence of a pulsar wind nebula challenges that interpretation. The new pointings will significantly improve the statistics for key regions (rims and background), allowing us to type the remnant, determine its age, study its energetics, place limits on nonthermal X-ray emission, and better characterize the PWN. | GALACTIC DIFFUSE EMISSION | 5 | C | MICHAEL STAGE | USA | 9 | AO9 | G093.3+6.9: SUPERNOVA PHYSICS IN A LOW-DENSITY MEDIUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509040010/ | Quick Look | ![]() |
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483 | OFF-FIELD4 | 173.7625 | -36.8508 | 173.145535 | -36.574162 | 191.286304 | -35.787139 | 286.33839516 | 23.54732297 | 109.4045 | 57008.1600925926 | 2014-12-17 03:50:32 | 57009.6814699074 | 2014-12-18 16:21:19 | 509045010 | 81.321 | 80 | 81.321 | 81.321 | 0 | 81.321 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5308680556 | 2016-08-17 12:44:27 | 56748 | 2014-04-01 00:00:00 | 57112.4059490741 | 2015-03-31 09:44:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091321 | Our special vantage point in our Galaxy allows us to study the Galactic warm-hot halo along several sightlines and determine its physical properties. The combination of absorption and emission measurements provides a powerful tool in this regard. Instead of average emission and absorption measures used in previous studies, one immediate step forward would be to use emission measures close to absorption sightlines. With proposed observations we will determine emission measures close to five sightlines in which we have the most accurate absorption measurements with Chandra. This will break the degeneracy between density and path-length and robustly measure the extent and mass of the warm-hot halo, placing strongest constraints yet on the fraction of missing baryons in the warm-hot plasma. | GALACTIC DIFFUSE EMISSION | 5 | C | ANJALI GUPTA | USA | 9 | AO9 | CIRCUM-GALACTIC MEDIUM OF THE MILKY WAY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509045010/ | Quick Look | ![]() |
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484 | MCG-03-34-64 | 200.5996 | -16.727 | 199.930176 | -16.465808 | 205.288367 | -7.470033 | 313.53711237 | 45.50625694 | 110.133 | 56296.8837384259 | 2013-01-04 21:12:35 | 56301.1737384259 | 2013-01-09 04:10:11 | 707027010 | 155.7127 | 150 | 155.7367 | 155.7127 | 0 | 155.7287 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 135.0516 | 135.0516 | 370.6038 | 4 | PROCESSED | 57608.5292824074 | 2016-08-08 12:42:10 | 56018 | 2012-04-01 00:00:00 | 56336.6958680556 | 2013-02-13 16:42:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071423 | Analysis of Suzaku observations selected from the BAT 58-month catalog has shown extreme hard X-ray excesses to exist in ~70% of type 1 AGN, and these can be modeled by partial-covering of Compton-thick gas. This new result shows the importance of broad X-ray coverage, currently available only with Suzaku. The most extreme of the sample sources, MCG-03-34-64 and NGC 1194, show significant spectral and flux variability above 10 keV, likely attributable to changes in the Compton-thick absorber. We request new observations of MCG-03-34-64 (150 ks) and NGC 1194 (200 ks) to study the X-ray reprocessor in these extreme systems, confirm the high-energy spectral variability and constrain the nature and location of the Compton-thick absorber. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TRACEY TURNER | USA | 7 | AO7 | THE CASE FOR VARIATIONS IN COMPTON-THICK ABSORPTION: MCG-03-34-64 AND NGC 1194 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707027010/ | Quick Look | ![]() |
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485 | FERMI_JET_COCOON_5 | 306.4609 | -33.261 | 305.672059 | -33.424933 | 300.742491 | -13.631284 | 9.28791468 | -33.23258901 | 260.3818 | 56968.8506481482 | 2014-11-07 20:24:56 | 56969.3612847222 | 2014-11-08 08:40:15 | 509051010 | 22.0438 | 20 | 22.0518 | 22.0438 | 0 | 22.0573 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7478125 | 2016-08-16 17:56:51 | 57358 | 2015-12-02 00:00:00 | 56982.4350694445 | 2014-11-21 10:26:30 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091322 | The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way. | GALACTIC DIFFUSE EMISSION | 5 | C | MATTHEW MILLER | USA | 9 | AO9 | OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509051010/ | Quick Look | ![]() |
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486 | H1821+643 | 275.4669 | 64.3595 | 275.403094 | 64.333117 | 318.334051 | 86.844268 | 94.01942058 | 27.4280098 | 65.0004 | 56402.5419444444 | 2013-04-20 13:00:24 | 56404.6925462963 | 2013-04-22 16:37:16 | 708037020 | 128.2485 | 400 | 128.2703 | 128.2485 | 0 | 128.2485 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 132.8215 | 132.8215 | 185.8058 | 2 | PROCESSED | 57611.1374884259 | 2016-08-11 03:17:59 | 56383 | 2013-04-01 00:00:00 | 56425.6256712963 | 2013-05-13 15:00:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081436 | H1821+643 (z=0.297) is not "just another quasar". This luminous active galactic nucleus (AGN) is an extremely rare example of a powerful quasar at the center of a rich, cooling-core cluster of galaxies. As such, it may represent a key evolutionary stage in the complex interplay between AGN and the core regions of the intracluster medium (ICM). Our analysis of archival XMM-Newton data has found evidence for a relativistically broad iron line. Here, we build on this request deep (400ks) Suzaku spectroscopy of H1821+643 to (1) measure the spin of this supermassive black hole and (2) search for powerful highly ionized outflows. In addition to measuring spin in the most luminous and distant object yet, this will enable us to test key predictions of recent models for AGN feedback. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | CHRISTOPHER REYNOLDS | USA | 8 | AO8 | THE BLACK HOLE SPIN AND IONIZED OUTFLOWS IN THE COOLING-FLOW QUASAR H1821+643 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708037020/ | Quick Look | ![]() |
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487 | IRAS F11119+3257 | 168.6582 | 32.6829 | 167.981225 | 32.955487 | 156.042952 | 25.438757 | 192.21056175 | 68.35212615 | 301.5808 | 56425.1110185185 | 2013-05-13 02:39:52 | 56431.3329050926 | 2013-05-19 07:59:23 | 708038010 | 252.2992 | 250 | 252.3232 | 252.2992 | 0 | 252.3232 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 220.3036 | 220.3036 | 400.8599 | 10 | PROCESSED | 57611.4720717593 | 2016-08-11 11:19:47 | 56858 | 2014-07-20 00:00:00 | 56491.9181828704 | 2013-07-18 22:02:11 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081441 | Recent Herschel observations provided a breakthrough in identifying powerful, large-scale molecular outflows in ULIRGs, indicating that AGN feedback can indeed have a strong impact on star formation and galaxy evolution, in accordance with theoretical models. However, observational evidence for the connection between the putative fast nuclear AGN winds required for the formation of these large-scale outflows is missing. X-ray observations of blue-shifted Fe K absorption lines directly probe ultra-fast outflows (UFOs) ejected from the AGN accretion disk with v>10,000km/s. A 250ks Suzaku exposure of the ULIRG F11119+3257 with observed extreme molecular/neutral/ionized outflows would allow to characterize the expected UFO, providing the "smoking gun" evidence for feedback driven by AGN winds. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | FRANCESCO TOMBESI | USA | 8 | AO8 | IRAS F11119+3257: THE "SMOKING GUN" EVIDENCE FOR AGN FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708038010/ | Quick Look | ![]() |
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488 | UGC 03142 | 70.9469 | 28.9681 | 70.161272 | 28.87543 | 73.291585 | 6.626144 | 172.09277202 | -10.99747628 | 264.8107 | 56335.692349537 | 2013-02-12 16:36:59 | 56336.9946296296 | 2013-02-13 23:52:16 | 707032010 | 51.2847 | 50 | 51.2847 | 51.2927 | 0 | 51.3007 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.5632 | 47.5632 | 112.51 | 1 | PROCESSED | 57610.6216898148 | 2016-08-10 14:55:14 | 56721 | 2014-03-05 00:00:00 | 56349.5963541667 | 2013-02-26 14:18:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071424 | A hard X-ray-selected (BAT) AGN sample shows a remarkable 70% of the local population of type 1 AGN to have extreme hard excesses above 20 keV, likely caused by Compton-thick gas in the line-of-sight, covering at least 50% of the source. We request six snapshot observations to complete a Suzaku survey of a BAT-flux-limited sample and make a complete and unbiased measurement of the incidence. Analysis of the new sources will be performed in conjunction with existing exposures, providing exciting new insight into the previously unknown structures in hard X-ray selected AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TRACEY TURNER | USA | 7 | AO7 | INVESTIGATING COMPTON-THICK ABSORBERS IN TYPE 1 AGN: OVERHAULING THE AGN PARADIGM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707032010/ | Quick Look | ![]() |
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489 | MCG -5-23-16 | 146.9445 | -30.9023 | 146.395049 | -30.669659 | 162.619875 | -41.096298 | 262.72964912 | 17.28396386 | 118.3849 | 53711.9526388889 | 2005-12-07 22:51:48 | 53714.4939699074 | 2005-12-10 11:51:19 | 700002010 | 95.6774 | 100 | 95.6774 | 95.7174 | 95.7174 | 95.6854 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 85.5647 | 85.5647 | 219.5251 | 3 | PROCESSED | 57532.4508680556 | 2016-05-24 10:49:15 | 54247 | 2007-05-27 00:00:00 | 54039.1988310185 | 2006-10-31 04:46:19 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001006 | We request a 100ks Suzaku observation of the bright Seyfert galaxy, MCG -5-23-16 simultaneously with approved XMM-Newton and Chandra HETG observations in December 2005. MCG -5-23-16 has one of the best known examples of a relativistically broadened iron K line. With a Swift-BAT flux of 1.6e-10 cgs (15-100 keV), it is one of the brightest AGN above 10 keV. The simultaneous observations will allow us to determine the shape of the broad relativistic Fe line after subtracting the narrow line components measured by HETG. Importantly, Suzaku's wide bandpass will accurately measure the broad-band continuum and reflection component of MCG -5-23-16, essential for constraining the broad iron line. These observations will also allow us to determine the temperature of the high energy cut-off. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JAMES REEVES | JAP | 0 | SWG | PROBING THE BROAD IRON LINE AND HIGH ENERGY CONTINUUM OF MCG -5-23-16 SIMULTANEOUSLY WITH SUZAKU, XMM-NEWTON AND CHANDRA | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700002010/ | Quick Look | ![]() |
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490 | IRAS 12127-1412 | 183.8305 | -14.4966 | 183.185484 | -14.2187 | 189.338442 | -11.765951 | 289.94461652 | 47.46236248 | 294.8513 | 56113.7580671296 | 2012-07-05 18:11:37 | 56115.2862615741 | 2012-07-07 06:52:13 | 707037010 | 63.6095 | 60 | 63.6095 | 63.6095 | 0 | 63.6095 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57.584 | 57.584 | 132.012 | 2 | PROCESSED | 57606.6111342593 | 2016-08-06 14:40:02 | 56508 | 2013-08-04 00:00:00 | 56142.1406018518 | 2012-08-03 03:22:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071441 | We propose to observe with the Hard X-ray Detector onboard Suzaku the two Ultraluminous Infrared Galaxies IRAS 00182-7112 and IRAS 12127-1412, both of which are known to harbour very luminous and highly obscured active galactic nuclei (AGN). An AGN reflection component arising from ionized gas is clearly identified at 2 10 keV: the detection of the direct AGN emission above 10 keV and the measure of the reflection efficiency would provide fundamental information on both the physical structure of Compton-thick AGN embedded in a nuclear starburst and their feedback on the surrounding environment. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | EMANUELE NARDINI | USA | 7 | AO7 | THE PHYSICAL STRUCTURE OF COMPTON-THICK AGN/ULIRGS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707037010/ | Quick Look | ![]() |
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491 | PG 1211+143 | 183.6045 | 14.1097 | 182.967898 | 14.387617 | 177.569786 | 14.352789 | 267.53559231 | 74.37841457 | 120.7913 | 53698.7348263889 | 2005-11-24 17:38:09 | 53701.3397453704 | 2005-11-27 08:09:14 | 700009010 | 96.3241 | 100 | 96.59 | 97.5802 | 96.3241 | 96.3241 | 3 | 2 | 3 | 3 | 1 | 0 | 0 | 84.0087 | 84.0087 | 225.0438 | 2 | PROCESSED | 57528.1616203704 | 2016-05-20 03:52:44 | 54247 | 2007-05-27 00:00:00 | 54038.7422106482 | 2006-10-30 17:48:47 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001041 | A 100ks Suzaku observation of the NLS1, PG 1211+143 is proposed. Previous XMM-Newton and Chandra observation claimed both blue-shifted (0.1c) and redshifted (0.26c-0.40c) iron Kalpha absorption lines. The redshifted iron K lines may originate from matter falling onto the supermassive black hole. The high effective area and low background of Suzaku XIS above 5 keV will enable us to measure these relativistically shifted iron lines in PG 1211+143 with great accuracy. Constraining the time variability of the lines will allow us to determine the physical origins of the absorption, e.g. failed jet/outflow or gravitational redshift from a Kerr black hole. The excellent broadband capabilities of Suzaku will accurately determine the continuum, essential for modeling the iron K band. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JAMES REEVES | JAP | 0 | SWG | EXPLORING THE RELATIVISTICALLY SHIFTED IRON LINES IN PG 1211+143 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700009010/ | Quick Look | ![]() |
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492 | 3C345 | 250.7487 | 39.7945 | 250.326948 | 39.887223 | 238.332578 | 61.133151 | 63.43440525 | 40.94504508 | 267.732 | 56181.2697453704 | 2012-09-11 06:28:26 | 56181.4772337963 | 2012-09-11 11:27:13 | 707043010 | 12.7008 | 10 | 12.7088 | 12.7168 | 0 | 12.7008 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.7314 | 10.7314 | 17.9199 | 0 | PROCESSED | 57606.986412037 | 2016-08-06 23:40:26 | 56582 | 2013-10-17 00:00:00 | 56212.7656712963 | 2012-10-12 18:22:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071601 | We propose to perform two 2-week multi-frequency campaigns of observations of a sample of gamma-ray blazars during Fermi Cycle 5. The campaigns will involve: (1) gamma-ray monitoring with the Fermi LAT, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B, V, R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku and Swift; (6) mid-IR measurements with IRTF; and (7) near-IR photometric J, H, and K observations. The research aims i) to search for correlated variability on short timescales; ii) to compile SEDs at different states of gamma-ray and radio jet activitiy; and iii) to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | SVETLANA JORSTAD | USA | 7 | AO7 | MULTI-FREQUENCY CAMPAIGNS TO STUDY RAPID VARIABILITY IN GAMMA_RAY BLAZARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707043010/ | Quick Look | ![]() |
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493 | HOLMBERG II X-1 | 124.8874 | 70.7162 | 123.586257 | 70.872801 | 106.845907 | 49.308193 | 144.27230635 | 32.72696637 | 127.9069 | 56552.1954398148 | 2013-09-17 04:41:26 | 56553.2994212963 | 2013-09-18 07:11:10 | 708015010 | 52.19 | 50 | 52.19 | 52.19 | 0 | 52.19 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.9852 | 48.9852 | 95.376 | 0 | PROCESSED | 57612.6731481482 | 2016-08-12 16:09:20 | 56954 | 2014-10-24 00:00:00 | 56588.6670717593 | 2013-10-23 16:00:35 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081251 | Recent X-ray observations have produced evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in an unusual super-Eddington state. Current data are unable to deliver a clear answer, as attempts to model the 0.5-10keV spectra have been plagued by degeneracies resulting from the limited bandpass, owing to the previous lack of focusing hard X-ray telescopes. Combined, Suzaku and NuSTAR will obtain high-quality spectra covering 0.5-30keV, providing powerful probes for understanding the accretion modes and nature of the central BHs. A definitive statement on the existence of either 100-1000Msun black holes or extreme accretion states will be an important legacy of both missions. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | DOMINIC WALTON | USA | 8 | AO8 | COORDINATED SUZAKU AND NUSTAR OBSERVATIONS OF HOLMBERG II X-1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708015010/ | Quick Look | ![]() |
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494 | MKN 335 | 1.5763 | 20.2091 | 0.933386 | 19.930785 | 9.740827 | 17.860354 | 108.75916207 | -41.41726175 | 71.5255 | 56457.9792939815 | 2013-06-14 23:30:11 | 56461.868287037 | 2013-06-18 20:50:20 | 708016020 | 154.8168 | 300 | 154.8648 | 154.8168 | 0 | 154.8568 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 141.5908 | 141.5908 | 335.8944 | 3 | PROCESSED | 57611.6590162037 | 2016-08-11 15:48:59 | 56383 | 2013-04-01 00:00:00 | 56512.7189467593 | 2013-08-08 17:15:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081411 | The idea of this proposal is trigger a 300ks observation with Suzaku of the Narrow Line Seyfert 1 Galaxy Mkn 335 during one of its low X-ray flux states. The goal here is to measure its underlying broad-band continuum with Suzaku during a low state and compare it with the 2006 high-state observations. Mkn 335 is one of the best examples of an AGN that went into a deep minimum X-ray flux state. Two competing models can explain these extreme low states: reflection models and partial covering absorber models. Both models still require a variable underlying intrinsic continuum. The science driver is to find out what is causing these low X-ray flux states that have been observed in several NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | DIRK GRUPE | USA | 8 | AO8-TOO | INTRINSIC LOW-STATE X-RAY LUMINOSITY OF THE NLS1 MKN 335 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708016020/ | Quick Look | ![]() |
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495 | CENTAURUS CLUSTER | 192.2012 | -41.3132 | 191.510497 | -41.040677 | 209.072585 | -32.853902 | 302.40029759 | 21.55583076 | 106.2442 | 53731.2579050926 | 2005-12-27 06:11:23 | 53732.1808333333 | 2005-12-28 04:20:24 | 800014010 | 36.5192 | 30 | 36.5192 | 36.5464 | 36.5464 | 36.5224 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 32.1498 | 32.1498 | 79.7399 | 0 | PROCESSED | 57532.5349652778 | 2016-05-24 12:50:21 | 54247 | 2007-05-27 00:00:00 | 54039.373900463 | 2006-10-31 08:58:25 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001070 | A dramatic central concentration of iron and silicon is present in the Centaurus cluster. Apart from this well-recognized contribution from Type Ia supernova, enrichment process due to Type II supernova is poorly understood. Centaurus cluster is most suited for the study of large-scale oxygen distribution, for which XIS is most sensitive. The XIS data will give us a key knowledge about how past Type II supernova have affected the enrichment process. The data would also confirm that the central gas is a mixture of hot and cool components with much better sensitivity than before. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YASUSHI FUKAZAWA | JAP | 0 | SWG | OXYGEN DISTRIBUTION AND MIXTURE OF HOT AND COOL GAS IN THE CENTAURUS CLUSTER | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800014010/ | Quick Look | ![]() |
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496 | NGC5929 | 231.5229 | 41.6989 | 231.07632 | 41.872918 | 210.309469 | 57.436696 | 67.89643134 | 55.30533508 | 120.4869 | 56651.8033217593 | 2013-12-25 19:16:47 | 56652.6042824074 | 2013-12-26 14:30:10 | 708022010 | 24.649 | 30 | 24.649 | 24.6689 | 0 | 24.6565 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.1767 | 25.1767 | 69.1919 | 0 | PROCESSED | 57613.6825925926 | 2016-08-13 16:22:56 | 56383 | 2013-04-01 00:00:00 | 56700.6301388889 | 2014-02-12 15:07:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081418 | Using Suzaku's sensitivity in the 2-50keV range, we propose to obtain broad-band spectral fits to the X-ray emission from five Seyfert galaxies which have nuclei that are likely to be Compton-thick. We will thereby derive estimates of their absorbing column densities (hitherto unknown), Fe line widths and equivalent widths, absorption-corrected nuclear X-ray emission and the reprocessed components. With these new estimates we will have complete measurements for a rigorously selected sample of 20 Seyferts that are matched in orientation-independent parameters. The sample selection enables us to account for orientation effects which dominate in them, and investigate the AGN evolution, AGN-star burst connection, and host galaxy evolution. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | PRAJVAL SHASTRI | USA | 8 | AO8 | COMPTON-THICK SEYFERT NUCLEI AND SEYFERT UNIFICATION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708022010/ | Quick Look | ![]() |
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497 | MRK533 | 351.9889 | 8.7759 | 351.354325 | 8.500435 | 356.155514 | 11.232339 | 90.62800693 | -48.78900326 | 248.1747 | 56634.8830671296 | 2013-12-08 21:11:37 | 56636.0847569444 | 2013-12-10 02:02:03 | 708023010 | 52.194 | 50 | 52.194 | 52.194 | 0 | 52.194 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.5617 | 48.5617 | 103.8059 | 0 | PROCESSED | 57613.5724421296 | 2016-08-13 13:44:19 | 56383 | 2013-04-01 00:00:00 | 56646.7358449074 | 2013-12-20 17:39:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081418 | Using Suzaku's sensitivity in the 2-50keV range, we propose to obtain broad-band spectral fits to the X-ray emission from five Seyfert galaxies which have nuclei that are likely to be Compton-thick. We will thereby derive estimates of their absorbing column densities (hitherto unknown), Fe line widths and equivalent widths, absorption-corrected nuclear X-ray emission and the reprocessed components. With these new estimates we will have complete measurements for a rigorously selected sample of 20 Seyferts that are matched in orientation-independent parameters. The sample selection enables us to account for orientation effects which dominate in them, and investigate the AGN evolution, AGN-star burst connection, and host galaxy evolution. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | PRAJVAL SHASTRI | USA | 8 | AO8 | COMPTON-THICK SEYFERT NUCLEI AND SEYFERT UNIFICATION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708023010/ | Quick Look | ![]() |
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498 | NGC 4552 | 188.9456 | 12.612 | 188.314388 | 12.887225 | 183.105993 | 15.109639 | 287.9907408 | 75.02773792 | 120.0696 | 54072.312974537 | 2006-12-03 07:30:41 | 54072.8405092593 | 2006-12-03 20:10:20 | 701037010 | 20.4398 | 20 | 20.4398 | 20.4398 | 0 | 20.4398 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.553 | 16.553 | 45.5439 | 0 | PROCESSED | 57536.226875 | 2016-05-28 05:26:42 | 54455 | 2007-12-21 00:00:00 | 54088.5410069444 | 2006-12-19 12:59:03 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011333 | The majority of accretion onto supermassive black holes in the local Universe occurs in obscured Seyferts. At moderate redshifts, the optical narrow emission-lines used to identify Seyfert 2s become difficult to isolate from the host galaxy's emission, resulting in an underestimate of the numbers of Seyfert 2s. Seyfert 2s are a critical component of AGN synthesis models of the Cosmic X-ray Background (CXB), as these sources are likely responsible for the unresolved component of the 2-8 keV background and may also contribute significantly to the 30 keV background. We propose to use Suzaku observations of ten local Seyfert 2s to measure their ultrahard (>10 keV) emission and examine how Seyfert 2s at moderate redshifts contribute to the CXB. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | AARON STEFFEN | USA | 1 | AO1 | MEASURING THE ULTRAHARD X-RAY EMISSION OF A LOCAL POPULATION OF SEYFERT 2S | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701037010/ | Quick Look | ![]() |
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499 | PDS 456 | 262.0807 | -14.2604 | 261.370018 | -14.220332 | 262.221238 | 8.96686 | 10.39565911 | 11.16772638 | 98.239 | 54155.7486574074 | 2007-02-24 17:58:04 | 54160.0355787037 | 2007-03-01 00:51:14 | 701056010 | 190.6002 | 188 | 190.6082 | 190.6002 | 0 | 190.6142 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 176.4708 | 176.4708 | 370.3428 | 4 | PROCESSED | 57537.5850578704 | 2016-05-29 14:02:29 | 54757 | 2008-10-18 00:00:00 | 54168.6244560185 | 2007-03-09 14:59:13 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011351 | A long 150ks Suzaku observation of the most luminous nearby quasar, PDS 456, is proposed. In the X-ray band, PDS 456 shows a deep iron K absorption trough. One possibility is that the absorption arises from a massive 0.1c outflow, of column density 10^24 cm^-2. Such an outflow would represent a significant fraction of the quasar energy budget. A deep Suzaku observation is proposed to test this outflow model, in particular the high energy bandpass of Suzaku is essential for measuring the profile of the absorption feature and determining the kinematics of the outflow. It is also possible to differentiate between competing models for the iron K feature, most notably between an outflow and a strong reflection component from the innermost radii around a Kerr black hole. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JAMES REEVES | USA | 1 | AO1 | SOLVING THE ORIGIN OF THE DEEP IRON K ABSORPTION IN PDS 456 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701056010/ | Quick Look | ![]() |
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500 | ABELL 1005 | 156.925 | 68.2013 | 156.004708 | 68.456472 | 124.194907 | 52.556114 | 140.47803773 | 43.70739533 | 119.4313 | 56609.4953819444 | 2013-11-13 11:53:21 | 56610.8334490741 | 2013-11-14 20:00:10 | 708042010 | 61.3496 | 60 | 61.3496 | 61.3496 | 0 | 61.3496 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 58.9645 | 58.9645 | 115.5998 | 2 | PROCESSED | 57613.3284722222 | 2016-08-13 07:53:00 | 56994 | 2014-12-03 00:00:00 | 56625.7198611111 | 2013-11-29 17:16:36 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081533 | We propose to map out the core of the A981 supercluster with three Suzaku observations. The A981 supercluster contains four Abell richness class 2 clusters within a redshift range of 2,000 km/s. All four clusters also overlap within their virial radii, at least in projection. The low and steady background of the Suzaku telescope is ideal for studying the low surface brightness X-ray emission between the clusters. Such observations will determine if the clusters are interacting via the detection of merger-induced shocks or perturbed features in the outskirts of the individual clusters. Our proposed Suzaku observations will help elucidate the fundamental astrophysics that occurs during the formation of very massive clusters. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | LAURENCE DAVID | USA | 8 | AO8 | MAPPING THE ABELL 981 SUPER CLUSTER WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708042010/ | Quick Look | ![]() |
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501 | BL LACERTAE | 330.6466 | 42.3471 | 330.130697 | 42.105096 | 354.282545 | 49.658149 | 92.61224541 | -10.37092111 | 71.9797 | 53882.2303703704 | 2006-05-27 05:31:44 | 53883.305775463 | 2006-05-28 07:20:19 | 701073010 | 48.5294 | 50 | 48.5454 | 48.5454 | 48.5294 | 48.5374 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35.5443 | 35.5443 | 92.902 | 1 | PROCESSED | 57534.4514236111 | 2016-05-26 10:50:03 | 54401 | 2007-10-28 00:00:00 | 53926.2373032407 | 2006-07-10 05:41:43 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011377 | We propose two 50 ks Suzaku observations, one for each of gamma-ray bright blazars PKS 1510-089 and BL Lacertae, to be coordinated with optical and radio observations. The goal is to obtain broadband spectra and light-curves. The X-ray fluxes are known to be rapidly variable, but there is no information about the correlation between the spectral shape and flux, which is necessary to establish the origin of previously detected prominent soft X-ray excesses. They are crucial to discriminate between different radiation scenarios responsible for production of hard X-rays and gamma-rays, and to constrain the content and by extension, the acceleration process of the jet. These observations will be ingredients of a "pilot" campaigns for the future joint Suzaku-GLAST investigations. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GRZEGORZ MADEJSKI | USA | 1 | AO1 | SUZAKU OBSERVATIONS OF GAMMA-RAY BRIGHT BLAZARS BL LACERTAE AND PKS 1510-089 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701073010/ | Quick Look | ![]() |
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502 | BEYOND VIRGO 4 | 187.7154 | 16.9006 | 187.085728 | 17.176651 | 180.130581 | 18.529302 | 276.92044319 | 78.71921322 | 118.472 | 55915.331099537 | 2011-12-20 07:56:47 | 55916.0466666667 | 2011-12-21 01:07:12 | 806063010 | 30.1361 | 30 | 30.1361 | 30.1361 | 0 | 30.1361 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.7334 | 22.7334 | 61.818 | 0 | PROCESSED | 57604.1732407407 | 2016-08-04 04:09:28 | 56299 | 2013-01-07 00:00:00 | 55932.1295949074 | 2012-01-06 03:06:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061523 | To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NORBERT WERNER | USA | 6 | AO6 | LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806063010/ | Quick Look | ![]() |
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503 | LMC X-4 | 83.221 | -66.3591 | 83.212611 | -66.392014 | 1.088478 | -87.292124 | 276.32094979 | -32.52452295 | 284.2438 | 54561.5523842593 | 2008-04-05 13:15:26 | 54562.3058333333 | 2008-04-06 07:20:24 | 702036020 | 25.3397 | 20 | 25.3425 | 25.3425 | 0 | 25.3397 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24.502 | 24.502 | 65.07 | 0 | PROCESSED | 57542.2490046296 | 2016-06-03 05:58:34 | 54943 | 2009-04-22 00:00:00 | 54574.4237152778 | 2008-04-18 10:10:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021127 | We propose for a series of three 20ks observations of the binary X-ray pulsar LMC X-4. This source shows 13.5 s pulsations, a 1.4 d orbital period, and a long-period (~30 d) variability due to a warped, precessing accretion disk. The proposed analysis will use pulse-phase spectroscopy with XIS to explore changes in the X-ray pulses and spectra at three different phases in the disk precession. This work will give us a detailed picture of the accretion flow, particularly for the inner regions of the accretion disk that are illuminated by the X-rays from the neutron star. This project takes advantage of the strengths of the XIS, particularly its excellent spectral resolution, sufficient (1s) time resolution in Window mode, and wide PSF that limits pile-up effects. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RYAN HICKOX | USA | 2 | AO2 | SUPERORBITAL VARIATION OF LMC X-4: EXPLORING THE ACCRETION FLOW | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702036020/ | Quick Look | ![]() |
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504 | NGC5548 | 214.4955 | 25.1272 | 213.928592 | 25.357387 | 201.997114 | 36.406484 | 31.93108614 | 70.4962838 | 289.7815 | 54303.4447337963 | 2007-07-22 10:40:25 | 54304.2711111111 | 2007-07-23 06:30:24 | 702042060 | 28.9178 | 30 | 28.9258 | 28.9258 | 0 | 28.9178 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24.8181 | 24.8181 | 71.3839 | 1 | PROCESSED | 57539.29125 | 2016-05-31 06:59:24 | 54706 | 2008-08-28 00:00:00 | 54339.5363310185 | 2007-08-27 12:52:19 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021307 | We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARTIN ELVIS | USA | 2 | AO2 | NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702042060/ | Quick Look | ![]() |
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505 | NGC 4507 | 188.8987 | -39.9119 | 188.223538 | -39.636542 | 205.656728 | -32.779926 | 299.63576127 | 22.85843053 | 109.5879 | 54454.5145717593 | 2007-12-20 12:20:59 | 54456.5835532407 | 2007-12-22 14:00:19 | 702048010 | 103.626 | 80 | 103.634 | 103.626 | 0 | 103.634 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 110.9021 | 110.9021 | 178.7279 | 0 | PROCESSED | 57540.963900463 | 2016-06-01 23:08:01 | 54829 | 2008-12-29 00:00:00 | 54462.288287037 | 2007-12-28 06:55:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021331 | Recent X-ray observations of Seyfert 2 galaxies have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by AGN Unified Schemes. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (60 ksec each) of four local bright Compton-thin Seyfert2s, selected from the Swift/BAT survey with a hard X-ray flux exceeding 1e-10 cgs to form a flux-limited sample. The unprecedented broad bandpass of Suzaku offers a unique tool to investigate the X-ray emission, placing strong constraints on the geometry and location of the reprocessing matter. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | JAMES REEVES | USA | 2 | AO2 | REVEALING THE REPROCESSING MATTER IN SEYFERT 2 GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702048010/ | Quick Look | ![]() |
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506 | RCS215222-0503.9 | 328.0881 | -5.0633 | 327.433899 | -5.298799 | 328.489701 | 7.382957 | 52.1030598 | -42.03624594 | 70.7002 | 55696.1248842593 | 2011-05-15 02:59:50 | 55696.8398263889 | 2011-05-15 20:09:21 | 806081010 | 30.6482 | 30 | 30.6482 | 30.6482 | 0 | 30.6482 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 25.3728 | 25.3728 | 61.744 | 0 | PROCESSED | 57602.0507986111 | 2016-08-02 01:13:09 | 56072 | 2012-05-25 00:00:00 | 55705.2063310185 | 2011-05-24 04:57:07 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061533 | Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 19 optically-selected clusters of galaxies, half at z~0.3 and half at z~0.8. Here we propose 6 additional observations in order to uniformly span a total redshift range of 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | AMALIA HICKS | USA | 6 | AO6 | AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806081010/ | Quick Look | ![]() |
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507 | HOLMBERG IX X-1 | 149.4756 | 69.0751 | 148.45738 | 69.31359 | 119.76782 | 51.701026 | 141.91985765 | 41.06519535 | 104.8942 | 56976.7425347222 | 2014-11-15 17:49:15 | 56977.5230787037 | 2014-11-16 12:33:14 | 709015020 | 34.1281 | 30 | 34.1281 | 34.1281 | 0 | 34.1281 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7878240741 | 2016-08-16 18:54:28 | 57359 | 2015-12-03 00:00:00 | 56993.4304513889 | 2014-12-02 10:19:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091251 | Broadband X-ray spectroscopy of ultraluminous X-ray sources (ULXs) with NuSTAR and Suzaku has begun to provide important information regarding the nature of these enigmatic sources. Recent NuSTAR observations of the extreme ULX Holmberg IX X-1 revealed unusual spectral variability, and different competing evolutionary scenarios can explain the available data. Resolving this degeneracy is critical to determining the nature of the accretion onto this source, and requires multi-epoch broadband spectroscopy probing a more diverse range of fluxes. We propose to undertake 4x30 ks coordinated Suzaku+NuSTAR observations of Holmberg IX X-1 to provide the additional spectra needed to robustly determine the nature of the observed evolution, providing a vital step in our understanding of extreme ULXs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | DOMINIC WALTON | USA | 9 | AO9 | MULTI-EPOCH BROADBAND X-RAY SPECTROSCOPY OF HOLMBERG IX X-1 WITH SUZAKU AND NUSTAR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709015020/ | Quick Look | ![]() |
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508 | I ZW 18 | 143.5064 | 55.23 | 142.623877 | 55.452479 | 125.705805 | 38.222173 | 160.54065348 | 44.84408453 | 279.2158 | 56792.4911111111 | 2014-05-15 11:47:12 | 56792.8568402778 | 2014-05-15 20:33:51 | 709021010 | 17.2612 | 100 | 17.2612 | 17.2612 | 0 | 17.2612 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.549 | 16.549 | 31.1279 | 0 | PROCESSED | 57615.102650463 | 2016-08-15 02:27:49 | 57358 | 2015-12-02 00:00:00 | 56818.6775347222 | 2014-06-10 16:15:39 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091441 | The source of energetic photons that reionized and heated the early universe remains uncertain. Early galaxies had low metallicity and the best local analogs are blue compact dwarf galaxies (BCDs) with low metallicity. We propose to observe two such galaxies known to be luminous in X-rays and accurately measure their spectrum with the Suzaku XIS. These observations are important to our understanding of the heating of the universe during the epoch of reionization. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | PHILIP KAARET | USA | 9 | AO9 | X-RAYS FROM LOW-METALLICITY BLUE COMPACT DWARF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709021010/ | Quick Look | ![]() |
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509 | XBONGBLUE1 | 217.1061 | 32.8569 | 216.573655 | 33.079659 | 200.393656 | 44.372245 | 54.10325006 | 68.28811801 | 132.8525 | 54453.8528587963 | 2007-12-19 20:28:07 | 54454.166875 | 2007-12-20 04:00:18 | 702082010 | 15.1725 | 13 | 15.1725 | 15.1725 | 0 | 15.1725 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.6996 | 15.6996 | 27.1259 | 0 | PROCESSED | 57540.9008217593 | 2016-06-01 21:37:11 | 54828 | 2008-12-28 00:00:00 | 54461.0450231482 | 2007-12-27 01:04:50 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021376 | We propose to use Suzaku's large collecting area and excellent energy response to measure accurate X-ray spectra for 9 XBONGs and 8 luminous Type 2 AGN selected from very large samples of identified XBONGs and Type 2 AGN found in our Chandra XBootes survey. We have obtained optical spectra for 258 XBONGs and identified ~700 X-ray luminous Type 2 AGN at z>0.7. With known source positions and X-ray fluxes, we select sources that are relatively bright with little or no contamination from other X-ray sources. Thus we will measure individual spectra for these bright sources. We propose eight 15 ksec Suzaku XIS observations to measure the absorption in 8 luminous z > 0.8 Type 2 AGN and eight 10 ksec observations to measure the absorption and iron emission for nine XBONGs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | CHRISTINE JONES | USA | 2 | AO2 | OBSCURED AGN AND XBONGS IN BOOTES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702082010/ | Quick Look | ![]() |
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510 | A1060 | 159.1744 | -27.531 | 158.58579 | -27.271265 | 172.752913 | -33.32931 | 269.60056717 | 26.48279097 | 103.6438 | 53696.6258796296 | 2005-11-22 15:01:16 | 53697.7211111111 | 2005-11-23 17:18:24 | 800003010 | 39.139 | 40 | 39.139 | 39.147 | 39.155 | 39.155 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 34.6024 | 34.6024 | 94.6259 | 1 | PROCESSED | 57528.0675462963 | 2016-05-20 01:37:16 | 54247 | 2007-05-27 00:00:00 | 54037.8583449074 | 2006-10-29 20:36:01 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001021 | A1060 is a bright non cD cluster and gives us a unique opportunity to study injection process of metals in the intracluster space. Reliable measurement of oxygen distribution with XIS will tell us whether the metals produced by Type-II supernova (mainly oxygen) ditributes over a different scale compared with the SN-Ia product (Fe). A1060 is the best cluster where we can directly observe distribution of metals produced by general cluster galaxies. Also, central increase of temperature by 20%, probably connected with motions of bright central galaxies, suggests that non-thermal X-rays may be produced. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | TAKAYA OHASHI | JAP | 0 | SWG | OXYGEN DISTRIBUTION AND CENTRAL GAS FEATURES OF A1060 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800003010/ | Quick Look | ![]() |
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511 | NGC720 | 28.2529 | -13.7362 | 27.644452 | -13.982164 | 20.9363 | -23.62893 | 173.01572713 | -70.35499124 | 242.5294 | 53734.3673611111 | 2005-12-30 08:49:00 | 53739.5627546296 | 2006-01-04 13:30:22 | 800009010 | 177.1929 | 100 | 177.1929 | 177.1929 | 177.1929 | 177.1929 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 9.6621 | 9.6621 | 47.5408 | 0 | PROCESSED | 57532.602962963 | 2016-05-24 14:28:16 | 54247 | 2007-05-27 00:00:00 | 54039.6651736111 | 2006-10-31 15:57:51 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001031 | We propose to observe an isolated elliptical galaxy NGC720 with Suzaku. Isolated elliptical galaxies are important to probe the ISM metal abundance, since their hot gas is not affected by the amibient bright intracluster medium which often exists around X-ray bright elliptical galaxies. Suzaku is expected to measure the Oxygen abundance in the ISM bettern than XMM-Newton and constrain the origin of metals in the ISM and also ICM. Dark matter content around elliptical galaxies can also be constrained better than XMM-Newton. Such a measurement is difficult for X-ray bright galaxies due to the superposition of the cluster potential. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YASUSHI FUKAZAWA | JAP | 0 | SWG | OXYGEN ABUNDANCE AND DARK MATTER CONTENT AROUDN AN ISOLATED ELLIPTICAL GALAXY NGC720 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800009010/ | Quick Look | ![]() |
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512 | NGC3227 | 155.8772 | 19.8684 | 155.194638 | 20.121777 | 150.38806 | 9.142968 | 216.98573476 | 55.44624837 | 110.6974 | 54797.8953703704 | 2008-11-27 21:29:20 | 54799.750162037 | 2008-11-29 18:00:14 | 703022050 | 79.4298 | 50 | 79.4298 | 79.4339 | 0 | 79.4378 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.8439 | 39.8439 | 160.2418 | 1 | PROCESSED | 57544.6203819444 | 2016-06-05 14:53:21 | 54557 | 2008-04-01 00:00:00 | 54809.8059490741 | 2008-12-09 19:20:34 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031013 | We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARTIN ELVIS | USA | 3 | AO3 | NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703022050/ | Quick Look | ![]() |
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513 | MKN 279 | 208.2253 | 69.3021 | 207.933654 | 69.547649 | 144.919228 | 67.626916 | 115.05735618 | 46.87522986 | 345.4595 | 54965.2632407407 | 2009-05-14 06:19:04 | 54968.6668287037 | 2009-05-17 16:00:14 | 704031010 | 160.3514 | 150 | 160.3594 | 160.3514 | 0 | 160.3594 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 150.386 | 150.386 | 293.9979 | 3 | PROCESSED | 57546.636099537 | 2016-06-07 15:15:59 | 55345 | 2010-05-29 00:00:00 | 54978.3987152778 | 2009-05-27 09:34:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041403 | We aim to test if the high-luminosity Seyfert 1.5 Mkn 279 contains an ionized inner accretion disk by using Suzaku to spectroscopically separate the ionized and neutral reflectors. This source is relatively unobscured, allowing clear modeling of the shape of the strong soft excess; we will also test for a Fe K diskline component, which may be missing if the disk is ionized or truncated. Only a broadband X-ray spectrum, including simultaneous > 10 keV coverage to constrain Compton reflection, will allow us to thoroughly test blurred, ionized disk reflection models and constrain the nature of the reflector(s). | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ALEX MARKOWITZ | USA | 4 | AO4 | DOES THE LOW-OBSCURATION, LOW-REFLECTION, HIGH-LUMINOSITY SEYFERT MKN279 CONTAIN AN IONIZED OR TRUNCATED ACCRETION DISK? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704031010/ | Quick Look | ![]() |
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514 | NGC1194 | 45.9522 | -1.1044 | 45.31576 | -1.299082 | 43.150403 | -17.672733 | 179.17914291 | -48.96176874 | 76.9913 | 55044.6911689815 | 2009-08-01 16:35:17 | 55045.8141087963 | 2009-08-02 19:32:19 | 704046010 | 50.3161 | 50 | 50.3161 | 50.5961 | 0 | 50.5961 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.4268 | 48.4268 | 97.0038 | 1 | PROCESSED | 57548.0499074074 | 2016-06-09 01:11:52 | 55427 | 2010-08-19 00:00:00 | 55061.5275115741 | 2009-08-18 12:39:37 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041414 | We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | EZEQUIEL TREISTER | USA | 4 | AO4 | THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704046010/ | Quick Look | ![]() |
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515 | NGC 4472 | 187.4441 | 8.005 | 186.80838 | 8.281234 | 183.627851 | 10.299036 | 286.9163593 | 70.20028227 | 117.8054 | 54072.8427893518 | 2006-12-03 20:13:37 | 54075.7014699074 | 2006-12-06 16:50:07 | 801064010 | 121.0358 | 120 | 121.0358 | 121.0358 | 0 | 121.0358 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 103.4464 | 103.4464 | 246.9548 | 6 | PROCESSED | 57536.3089467593 | 2016-05-28 07:24:53 | 54702 | 2008-08-24 00:00:00 | 54089.1857523148 | 2006-12-20 04:27:29 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011403 | We propose Suzaku observations of a sample of bright elliptical galaxies, with a preference toward galaxies that have (or potentially have) high quality XMM-Newton RGS data, as part of a program to investigate their star formation history and chemical evolution via abundance studies of the hot interstellar medium. Joint XIS/RGS analysis enables one to directly account for the effects of resonance scattering and thermal structure in order to minimize degeneracies in the abundance estimates. At the same time, the incidence of resonance scattering serves as an indicator of the prevalence and causes of ISM turbulence. The unprecedented opportunity to measure and map oxygen abundances afforded by the XIS is key to constraining nucleosynthetic origins and enrichment mechanisms. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MICHAEL LOEWENSTEIN | USA | 1 | AO1 | INVESTIGATING THE CHEMICAL EVOLUTION OF ELLIPTICAL GALAXIES WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801064010/ | Quick Look | ![]() |
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516 | NGC 4649 | 190.9148 | 11.557 | 190.284732 | 11.830628 | 185.371113 | 14.926523 | 295.86493189 | 74.32191724 | 113.3108 | 54098.4203703704 | 2006-12-29 10:05:20 | 54104.1473263889 | 2007-01-04 03:32:09 | 801065010 | 224.0304 | 120 | 224.0304 | 224.0304 | 0 | 224.0304 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.3042 | 26.3042 | 69.2898 | 1 | PROCESSED | 57536.4300578704 | 2016-05-28 10:19:17 | 54743 | 2008-10-04 00:00:00 | 54132.9809027778 | 2007-02-01 23:32:30 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011403 | We propose Suzaku observations of a sample of bright elliptical galaxies, with a preference toward galaxies that have (or potentially have) high quality XMM-Newton RGS data, as part of a program to investigate their star formation history and chemical evolution via abundance studies of the hot interstellar medium. Joint XIS/RGS analysis enables one to directly account for the effects of resonance scattering and thermal structure in order to minimize degeneracies in the abundance estimates. At the same time, the incidence of resonance scattering serves as an indicator of the prevalence and causes of ISM turbulence. The unprecedented opportunity to measure and map oxygen abundances afforded by the XIS is key to constraining nucleosynthetic origins and enrichment mechanisms. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MICHAEL LOEWENSTEIN | USA | 1 | AO1 | INVESTIGATING THE CHEMICAL EVOLUTION OF ELLIPTICAL GALAXIES WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801065010/ | Quick Look | ![]() |
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517 | UGC03957 | 115.2433 | 55.429 | 114.235063 | 55.545488 | 106.863653 | 33.455815 | 162.22286538 | 28.93195726 | 271.243 | 53841.9927314815 | 2006-04-16 23:49:32 | 53842.2828587963 | 2006-04-17 06:47:19 | 801072010 | 10.7714 | 12 | 10.7794 | 10.7794 | 10.7874 | 10.7714 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 9.642 | 9.642 | 25.0079 | 0 | PROCESSED | 57533.4729166667 | 2016-05-25 11:21:00 | 54401 | 2007-10-28 00:00:00 | 53906.7753240741 | 2006-06-20 18:36:28 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801072010/ | Quick Look | ![]() |
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518 | IC 2497 | 145.222 | 34.6799 | 144.47003 | 34.907483 | 135.80747 | 19.598067 | 190.267728 | 48.8163504 | 306.2341 | 54939.6906365741 | 2009-04-18 16:34:31 | 54941.5550810185 | 2009-04-20 13:19:19 | 704053010 | 76.4837 | 75 | 76.4837 | 76.4837 | 0 | 76.4837 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 63.948 | 63.948 | 161.0478 | 2 | PROCESSED | 57546.2140046296 | 2016-06-07 05:08:10 | 55318 | 2010-05-02 00:00:00 | 54952.1320717593 | 2009-05-01 03:10:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041432 | The discovery of `Hanny's Voorwerp' near IC 2497 opens an unprecedented window into the time evolution of a single AGN on timescales up to 100,000 years. Based on its properties, the Voorwerp was illuminated by a luminous AGN ~100,000 years ago, but the AGN host galaxy - IC 2497 - does not seem to host a sufficiently luminous AGN. Thus, IC 2497 either hosts a highly obscured AGN only detectable in hard X-rays, or it has dropped in luminosity by a factor of 10-1000. We propose to observe IC 2497 with Suzaku for 75 ksec to determine the hard X-ray luminosity and spectrum to measure the amount of obscuration and the current intrinsic luminosity of its AGN. Only with hard X-ray observations can we break the degeneracy between obscuration and decrease in luminosity. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KEVIN SCHAWINSKI | USA | 4 | AO4 | HOW FAST CAN AN AGN SHUT DOWN? - SUZAKU OBSERVATION OF IC 2497 AND `HANNY'S VOORWERP' | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704053010/ | Quick Look | ![]() |
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519 | A272 | 28.7603 | 33.9026 | 28.031098 | 33.657734 | 38.955118 | 20.665911 | 137.73606223 | -27.1341127 | 64.9465 | 53943.0449537037 | 2006-07-27 01:04:44 | 53943.6842476852 | 2006-07-27 16:25:19 | 801084010 | 22.2455 | 21 | 22.2535 | 22.2535 | 22.2455 | 22.2535 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 24.6035 | 24.6035 | 55.2319 | 0 | PROCESSED | 57535.0602430556 | 2016-05-27 01:26:45 | 54401 | 2007-10-28 00:00:00 | 53955.6516782407 | 2006-08-08 15:38:25 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801084010/ | Quick Look | ![]() |
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520 | A566 | 106.0915 | 63.2647 | 104.91759 | 63.339113 | 99.420321 | 40.34898 | 152.76309519 | 25.45548296 | 285.637 | 54178.3128587963 | 2007-03-19 07:30:31 | 54178.8029976852 | 2007-03-19 19:16:19 | 801085010 | 22.2711 | 20 | 22.2711 | 22.2711 | 0 | 22.2711 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.1523 | 22.1523 | 42.3399 | 0 | PROCESSED | 57537.7151157407 | 2016-05-29 17:09:46 | 54695 | 2008-08-17 00:00:00 | 54185.9799305556 | 2007-03-26 23:31:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801085010/ | Quick Look | ![]() |
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521 | RXJ 0658 | 104.704 | -55.933 | 104.461428 | -55.862903 | 130.333928 | -77.302143 | 266.02429497 | -21.20357002 | 164.9362 | 54095.6181597222 | 2006-12-26 14:50:09 | 54098.4099421296 | 2006-12-29 09:50:19 | 801089010 | 101.3845 | 100 | 101.3845 | 101.3845 | 0 | 101.3845 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 84.3679 | 84.3679 | 241.1547 | 2 | PROCESSED | 57637.5971180556 | 2016-09-06 14:19:51 | 54702 | 2008-08-24 00:00:00 | 54111.5842013889 | 2007-01-11 14:01:15 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011448 | We propose SUZAKU X-ray observations of an intriguing cluster of galaxies, RXJ0658, to determine and characterize the nature of the hard X-ray spectral emission and other nonthermal activity. It also has many other interesting features, such as a cold front, evidence for merger, a shock, and regions of unusually high temperature, all of which are related to the hard X-ray emission and the nonthermal activity. The more accurate measure of the spectral characteristics of the hard component, when combined with the radio and other past X-ray data, can reveal the nature of the emission process and the acceleration mechanism of the relativistic electrons, provide a means of measuring the magnetic field strength, and aid in understanding the process of formation of clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | VAHE PETROSIAN | USA | 1 | AO1 | HARD X-RAY EMISSION FROM CLUSTER RXJ0658 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801089010/ | Quick Look | ![]() |
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522 | CEN A S LOBE NO. 1 | 200.8664 | -45.1602 | 200.128121 | -44.89936 | 217.870253 | -33.408756 | 308.83796576 | 17.34395301 | 288.0039 | 55418.6612962963 | 2010-08-10 15:52:16 | 55419.7758101852 | 2010-08-11 18:37:10 | 705032010 | 75.1654 | 80 | 75.1654 | 75.1654 | 0 | 75.1654 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64.2728 | 64.2728 | 96.2818 | 0 | PROCESSED | 57552.9742476852 | 2016-06-13 23:22:55 | 55803 | 2011-08-30 00:00:00 | 55428.1537152778 | 2010-08-20 03:41:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051401 | We propose a set of four pointings (200 ks), to study the X-ray emission from the Southern giant lobe of the radio galaxy Cen A. Those lobes clearly separated from the central source, have been detected as a source of diffuse gamma-ray emission by the Fermi Telescope. The goal of the Suzaku observations is two-fold: first, to measure the diffuse component of the non-thermal X-ray emission with both the XIS and the HXD in order to determine the details of the distribution of the radiating relativistic particles (and B field), and second, to measure the thermal emission from the lobes (using primarily the XIS), to determine temperature and density of the X-ray emitting plasma, which, via consideration of pressure balance, will determine the content of energetic protons (cosmic rays). | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GRZEGORZ MADEJSKI | USA | 5 | AO5 | SUZAKU OBSERVATIONS OF THE SOUTHERN LOBE OF CEN A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705032010/ | Quick Look | ![]() |
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523 | SEGUE 1 | 151.7658 | 16.0862 | 151.086487 | 16.330668 | 148.083031 | 4.208593 | 220.47149585 | 50.42674703 | 110.8027 | 56248.0740625 | 2012-11-17 01:46:39 | 56250.3182291667 | 2012-11-19 07:38:15 | 807046010 | 85.4391 | 85 | 85.4622 | 85.4431 | 0 | 85.4391 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 77.5645 | 77.5645 | 193.8419 | 4 | PROCESSED | 57608.0603240741 | 2016-08-08 01:26:52 | 56641 | 2013-12-15 00:00:00 | 56275.5584490741 | 2012-12-14 13:24:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071502 | Our ongoing dedicated X-ray search for dark matter targeting dwarf spheroidal galaxies set new constraints on the mass and mixing angle of the sterile neutrino -- a plausible dark matter candidate that emits an X-ray via radiative decay. We have proposed a new well-motivated candidate -- moduli dark matter, that also produces a detectable X-ray line. We propose Suzaku observations of the Segue 1 dwarf spheroidal -- the most dark matter dominated galaxy known. Its extreme nature implies that it provides the tightest constraints on sterile neutrino and moduli parameters in the event of a detection, and best limits in the absence of one. The resulting spectrum is optimal for exploring new physics, such as string theory compactification or supersymmetry breaking, and as a legacy for Astro-H. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MICHAEL LOEWENSTEIN | USA | 7 | AO7 | SEARCH FOR DARK MATTER WITH SUZAKU OBSERVATIONS OF THE MOST DARK MATTER DOMINATED GALAXY IN THE UNIVERSE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807046010/ | Quick Look | ![]() |
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524 | CEN A S LOBE NO. 3 | 205.7514 | -45.1409 | 204.991343 | -44.889287 | 221.546575 | -31.897052 | 312.39292182 | 16.78143613 | 279.0007 | 55420.9668981482 | 2010-08-12 23:12:20 | 55421.3452777778 | 2010-08-13 08:17:12 | 705034010 | 20.0575 | 20 | 20.0815 | 20.0735 | 0 | 20.0575 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 18.9436 | 18.9436 | 32.6879 | 1 | PROCESSED | 57552.9389467593 | 2016-06-13 22:32:05 | 55803 | 2011-08-30 00:00:00 | 55435.169537037 | 2010-08-27 04:04:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051401 | We propose a set of four pointings (200 ks), to study the X-ray emission from the Southern giant lobe of the radio galaxy Cen A. Those lobes clearly separated from the central source, have been detected as a source of diffuse gamma-ray emission by the Fermi Telescope. The goal of the Suzaku observations is two-fold: first, to measure the diffuse component of the non-thermal X-ray emission with both the XIS and the HXD in order to determine the details of the distribution of the radiating relativistic particles (and B field), and second, to measure the thermal emission from the lobes (using primarily the XIS), to determine temperature and density of the X-ray emitting plasma, which, via consideration of pressure balance, will determine the content of energetic protons (cosmic rays). | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GRZEGORZ MADEJSKI | USA | 5 | AO5 | SUZAKU OBSERVATIONS OF THE SOUTHERN LOBE OF CEN A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705034010/ | Quick Look | ![]() |
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525 | DRACO | 260.0265 | 57.929 | 259.823545 | 57.97767 | 237.171171 | 80.222303 | 86.38548758 | 34.73420948 | 52.1224 | 54196.7611458333 | 2007-04-06 18:16:03 | 54198.2216898148 | 2007-04-08 05:19:14 | 802051010 | 63.3232 | 67 | 63.3232 | 63.3232 | 0 | 63.3232 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64.9572 | 64.9572 | 126.1818 | 2 | PROCESSED | 57538.1232291667 | 2016-05-30 02:57:27 | 54829 | 2008-12-29 00:00:00 | 54203.3603703704 | 2007-04-13 08:38:56 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021405 | We propose 50 ksec Suzaku observations of the Ursa Minor and Draco dwarf spheroidal galaxies. These dense, dark-matter-dominated systems are carefully selected as the strongest potential sources of line emission from radiatively decaying keV dark matter of any astrophysical object. The low-level, stable Suzaku background makes it the most sensitive instrument to-date for this purpose. At the very least, constraints that enter a significant new regime are derived: non-detections are still of great importance. In the best case, the long sought-after identity of dark matter will be discovered, pointing the way to physics beyond the Standard Model. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MICHAEL LOEWENSTEIN | USA | 2 | AO2 | SEARCH FOR WARM DARK MATTER WITH SUZAKU OBSERVATIONS OF DWARF SPHEROIDAL GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802051010/ | Quick Look | ![]() |
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526 | SDSS J0854+3524 | 133.7386 | 35.4192 | 132.953536 | 35.610263 | 126.168595 | 17.306871 | 188.0033984 | 39.53150085 | 111.2842 | 56214.3546527778 | 2012-10-14 08:30:42 | 56214.8244560185 | 2012-10-14 19:47:13 | 807063010 | 20.6148 | 20 | 20.6148 | 20.6148 | 0 | 20.6148 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.084 | 18.084 | 40.56 | 0 | PROCESSED | 57607.7601157407 | 2016-08-07 18:14:34 | 56598 | 2013-11-02 00:00:00 | 56232.4365856482 | 2012-11-01 10:28:41 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071512 | Fossil groups (FGs) are systems dominated by a single large galaxy with a cluster-scale X-ray halo. They are thought to be old, isolated galaxy groups in which the large galaxies have coalesced through dynamical friction, but recent studies reveal a more complicated picture. We propose Suzaku observations of 5 optically selected FG candidates. These targets will extend our previous survey, which identified 12 FGs; when combined with 5 FG candidates approved for the current Chandra cycle, this will create the largest uniformly-selected sample of real FGs. The L_X and T_X measured will be used with optical spectroscopy to extend FG scaling relations to low mass, and to plan deeper X-ray spectroscopic follow-up to constrain the formation epoch and evolution of these puzzling systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ERIC MILLER | USA | 7 | AO7 | FINDING FOSSIL GROUPS WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807063010/ | Quick Look | ![]() |
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527 | BOOTES GROUP 30 | 219.4427 | 33.5107 | 218.918921 | 33.726455 | 202.46828 | 45.823682 | 55.01212205 | 66.25629851 | 308.903 | 54276.6949189815 | 2007-06-25 16:40:41 | 54277.5271875 | 2007-06-26 12:39:09 | 802056010 | 38.5045 | 38 | 38.5045 | 38.5045 | 0 | 38.5045 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.7473 | 35.7473 | 71.8979 | 1 | PROCESSED | 57539.0466782407 | 2016-05-31 01:07:13 | 54702 | 2008-08-24 00:00:00 | 54333.4389583333 | 2007-08-21 10:32:06 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021424 | We propose four 30 ksec Suzaku pointings (120 ksec total) to obtain Lx and Tx for 4 distant (0.15 < z < 0.35) galaxy groups discovered in a contiguous, 9.3 sq. deg Chandra survey in Bootes. Our targets are spatially resolved by Chandra and are chosen to minimize point-source contamination of the Suzaku group spectra. The XIS data will significantly expand the sample of groups with known temperature in this redshift range, and so will improve constraints on group evolution mechanisms. We will use the existing, deep multicolor imaging and 20,000-object spectroscopic catalog for Bootes to study the effect of local environment on group properties, as well as the relationship between optically-selected and X-ray selected groups, for the first time in this redshift range. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MARSHALL BAUTZ | USA | 2 | AO2 | SUZAKU SPECTROSCOPY OF DISTANT GALAXY GROUPS IN BOOTES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802056010/ | Quick Look | ![]() |
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528 | SMC X-1 | 19.2337 | -73.4445 | 18.901627 | -73.707724 | 312.330059 | -66.462167 | 300.42986971 | -43.55966827 | 9.1005 | 55673.6490625 | 2011-04-22 15:34:39 | 55674.1112037037 | 2011-04-23 02:40:08 | 706030030 | 15.6526 | 18 | 15.6526 | 15.6526 | 0 | 15.871 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 21.2614 | 21.2614 | 39.9199 | 1 | PROCESSED | 57601.5606597222 | 2016-08-01 13:27:21 | 56067 | 2012-05-20 00:00:00 | 55692.2968634259 | 2011-05-11 07:07:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JOSEPH NEILSEN | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030030/ | Quick Look | ![]() |
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529 | RXJ1159+5531 | 179.9637 | 55.4123 | 179.320531 | 55.690619 | 149.995673 | 49.037125 | 137.70641489 | 60.21165624 | 302.8269 | 56074.0600694445 | 2012-05-27 01:26:30 | 56075.6800578704 | 2012-05-28 16:19:17 | 807064010 | 82.2339 | 100 | 82.2419 | 82.2419 | 0 | 82.2339 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 98.6011 | 98.6011 | 139.964 | 1 | PROCESSED | 57605.5596875 | 2016-08-05 13:25:57 | 56657 | 2013-12-31 00:00:00 | 56086.0194328704 | 2012-06-08 00:27:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071513 | With Chandra and Suzaku we recently constrained the hot gas and dark matter out to the virial radius (rvir=R108) in the fossil group/cluster RXJ1159+5531. Unlike some recent observations of cluster outskirts, the gas fraction is consistent with the cosmic value, and the entropy profile at rvir is consistent with gravity-only structure formation simulations. As a fossil group, RXJ1159+5531 may be unusually relaxed at large scales. If so, the gas properties should not vary much azimuthally. We propose a complementary Suzaku observation to explore this by measuring the gas in a different azimuthal region, more than doubling the current (~27%) azimuthal coverage. Our results will help determine if gas clumping, invoked to explain the outskirts of some clusters, is ubiquitous. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | PHILIP HUMPHREY | USA | 7 | AO7 | RELAXED GAS AT THE VIRIAL RADIUS IN A FOSSIL GROUP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807064010/ | Quick Look | ![]() |
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530 | PKS 0745-191 | 116.7966 | -19.5079 | 116.243978 | -19.383587 | 123.623714 | -39.870751 | 236.58636127 | 2.85363493 | 294.0004 | 54234.0374884259 | 2007-05-14 00:53:59 | 54234.8446643518 | 2007-05-14 20:16:19 | 802062050 | 33.4146 | 30 | 33.4146 | 33.4226 | 0 | 33.4226 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31.3065 | 31.3065 | 69.7239 | 1 | PROCESSED | 57538.6567708333 | 2016-05-30 15:45:45 | 54695 | 2008-08-17 00:00:00 | 54245.5456712963 | 2007-05-25 13:05:46 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021440 | PKS 0745-191 is the X-ray brightest galaxy cluster beyond a redshift of 0.1. It has a smooth surface brightness profile and appears relaxed. Using the low background of Suzaku we will measure the temperature of the intracluster medium to the virial radius of the cluster. Its high temperature means that we will be unaffected by any loss of effective area at low energies. In addition the cluster is bright enough so that the bremsstrahlung emission will be easily detected using the PIN detector. This will allow us to search for any nonthermal component as well as accurately determining the high temperature components in the cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ANDREW YOUNG | USA | 2 | AO2 | PKS 0745-191: THE BRIGHTEST CLUSTER BEYOND Z=0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802062050/ | Quick Look | ![]() |
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531 | MRK 841 | 226.0091 | 10.4587 | 225.405512 | 10.653095 | 220.178836 | 26.612533 | 11.24319757 | 54.63999984 | 112.9994 | 55931.8646180556 | 2012-01-05 20:45:03 | 55937.1896990741 | 2012-01-11 04:33:10 | 706029010 | 244.3518 | 350 | 244.3518 | 244.3518 | 0 | 244.3598 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 229.726 | 229.726 | 419.686 | 4 | PROCESSED | 57604.4310648148 | 2016-08-04 10:20:44 | 55652 | 2011-04-01 00:00:00 | 55946.5082407407 | 2012-01-20 12:11:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061119 | We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | CHRISTOPHER REYNOLDS | USA | 6 | AO6-LP | A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706029010/ | Quick Look | ![]() |
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532 | ABELL 665 | 127.3329 | 65.7462 | 126.195484 | 65.912794 | 110.615683 | 44.954956 | 149.92967896 | 34.55444535 | 289.9972 | 56027.8062847222 | 2012-04-10 19:21:03 | 56028.5592476852 | 2012-04-11 13:25:19 | 807072030 | 50.3486 | 50 | 50.3526 | 50.3486 | 0 | 50.3561 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.3856 | 47.3856 | 65.049 | 0 | PROCESSED | 57605.1517939815 | 2016-08-05 03:38:35 | 56018 | 2012-04-01 00:00:00 | 56044.1669791667 | 2012-04-27 04:00:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071522 | We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 7 | AO7 | COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807072030/ | Quick Look | ![]() |
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533 | NGC 3079 | 150.444 | 55.6163 | 149.59923 | 55.857396 | 130.078493 | 40.265138 | 157.91350273 | 48.36319014 | 294.1052 | 54590.7432407407 | 2008-05-04 17:50:16 | 54591.1147800926 | 2008-05-05 02:45:17 | 803039010 | 14.4083 | 100 | 14.4083 | 14.4083 | 0 | 14.4083 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.9538 | 12.9538 | 32.0799 | 0 | PROCESSED | 57542.4484027778 | 2016-06-03 10:45:42 | 54999 | 2009-06-17 00:00:00 | 54602.2023958333 | 2008-05-16 04:51:27 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031303 | We will determine whether AGN can drive galactic-scale winds by observing NGC 3079, the best nearby candidate for such a wind. The edge-on spiral NGC 3079 hosts a Compton-thick AGN and is surrounded by a 40 kpc-scale soft X-ray nebula, the largest manifestation of outflow activity also seen in the optical and radio. Proving the outflow is AGN-driven requires Suzaku's unique abilities. We will measure the AGN luminosity using the HXD in the 15-40 keV range and the 2-10 keV band reflection spectrum to assess whether the AGN can radiatively-or-mechanically power the observed superwind. We will determine the origin of the soft X-ray nebula using the relative elemental abundances in the plasma. We can also detect any significant starburst through the 6.7 keV line emission it would create. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | DAVID STRICKLAND | USA | 3 | AO3 | NGC 3079'S 40 KPC-SCALE OUTFLOW: AGN OR STARBURST-DRIVEN? | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803039010/ | Quick Look | ![]() |
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534 | CYGNUS A CLUSTER | 299.7609 | 40.7885 | 299.328588 | 40.65123 | 317.589132 | 59.411403 | 76.19456446 | 5.8531495 | 241.849 | 54785.9049537037 | 2008-11-15 21:43:08 | 54786.9154976852 | 2008-11-16 21:58:19 | 803050010 | 44.6587 | 45 | 44.6587 | 44.6587 | 0 | 44.6587 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 42.966 | 42.966 | 87.28 | 0 | PROCESSED | 57544.3868055556 | 2016-06-05 09:17:00 | 55167 | 2009-12-02 00:00:00 | 54796.9718981482 | 2008-11-26 23:19:32 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031426 | The radio galaxy Cygnus A lies in a cooling core cluster which is currently undergoing a cluster merger with a particularly simple geometry. We propose XIS spectra of the radio source/cooling core interaction region, merger shock region, and second subcluster. The Fe K emission line will be used to measure gas velocities in these 3 regions to determine the dynamics of the merger, and to constrain hydro/N-body simulations of the merger. Collisionless merger shocks may produce detectable non-equilibrium effects. We will also determine an upper limit for the rate of expansion of the X-ray bubble around the radio source, studying the interaction of the radio galaxy and X-ray gas in the only FR-II radio galaxy in a nearby cluster. HXD data will constrain inverse Compton from the radio source. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | DANIEL WIK | USA | 3 | AO3 | PROPERTIES OF THE MERGER AND RADIO SOURCE INTERACTION IN THE CYGNUS A CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803050010/ | Quick Look | ![]() |
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535 | ABELL 2597 | 351.1561 | -12.0446 | 350.50582 | -12.319475 | 347.114403 | -7.564991 | 65.23010074 | -64.66820365 | 250.0003 | 56262.3308680556 | 2012-12-01 07:56:27 | 56263.5369212963 | 2012-12-02 12:53:10 | 807073020 | 50.0345 | 50 | 50.0585 | 50.0425 | 0 | 50.0345 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 44.785 | 44.785 | 104.1919 | 0 | PROCESSED | 57608.1666319444 | 2016-08-08 03:59:57 | 56018 | 2012-04-01 00:00:00 | 56336.4705902778 | 2013-02-13 11:17:39 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071522 | We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 7 | AO7 | COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807073020/ | Quick Look | ![]() |
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536 | NGC 2110 | 88.0457 | -7.4586 | 87.441571 | -7.469572 | 87.744639 | -30.884812 | 212.92775975 | -16.54787795 | 79.201 | 56170.1053009259 | 2012-08-31 02:31:38 | 56172.5412268518 | 2012-09-02 12:59:22 | 707034010 | 103.2595 | 100 | 103.2595 | 103.2595 | 0 | 103.2595 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102.8063 | 102.8063 | 210.4361 | 1 | PROCESSED | 57607.0102199074 | 2016-08-07 00:14:43 | 56667 | 2014-01-10 00:00:00 | 56301.6411458333 | 2013-01-09 15:23:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071426 | We request two 100 ks | EXTRAGALACTIC COMPACT SOURCES | 7 | B | ELIZABETH RIVERS | USA | 7 | AO7 | TRACKING THE PARTIAL COVERING ABSORBERS IN NGC 2110: CONSTRAINTS FOR CLUMPY ABSORBER MODELS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707034010/ | Quick Look | ![]() |
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537 | NGC 4125 | 182.0568 | 65.1777 | 181.434624 | 65.455888 | 140.391429 | 57.000336 | 130.16762444 | 51.33919783 | 175.9017 | 55103.512037037 | 2009-09-29 12:17:20 | 55105.4578009259 | 2009-10-01 10:59:14 | 804047010 | 104.0801 | 100 | 104.0801 | 104.0881 | 0 | 104.0961 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93.7257 | 93.7257 | 168.0857 | 0 | PROCESSED | 57548.726712963 | 2016-06-09 17:26:28 | 55491 | 2010-10-22 00:00:00 | 55125.5744212963 | 2009-10-21 13:47:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041502 | Recent observations of relaxed galaxy groups have revealed ubiquitous abundance gradients, indicating large-scale mixing of the gas, possibly driven by AGN feedback. Exploiting the low background and good sensitivity of Suzaku, we have found similar gradients in two lower mass, galaxy-scale systems, which has important implications for models of feedback and chemical enrichment. We propose to observe two more isolated elliptical galaxies, thus starting to building a sample for determining the frequency and properties of such abundance gradients in early-type galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | PHILIP HUMPHREY | USA | 4 | AO4 | ABUNDANCE GRADIENTS IN EARLY-TYPE GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804047010/ | Quick Look | ![]() |
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538 | NGC6482 | 267.957 | 23.086 | 267.434837 | 23.097176 | 267.256842 | 46.506557 | 48.10607859 | 22.91404378 | 109.6205 | 55238.2645949074 | 2010-02-11 06:21:01 | 55239.2919444444 | 2010-02-12 07:00:24 | 804050010 | 46.5467 | 45 | 46.5467 | 46.5467 | 0 | 46.5467 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.5166 | 28.5166 | 88.7438 | 0 | PROCESSED | 57550.5834143518 | 2016-06-11 14:00:07 | 55622 | 2011-03-02 00:00:00 | 55251.3186458333 | 2010-02-24 07:38:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041513 | Fossil groups present a puzzle to current theories of structure formation. Despite the low number of bright galaxies, their high velocity dispersions and gas temperatures indicate potential wells deeper than that of normal groups. Their measured c200 are high indicating very early formation epochs, which is in contradiction with the lack of cooling cores observed. We can constrain their ages by looking at the distribution of the SN Ia and II ejecta near their core. If they are formed more recently than normal groups by galaxy merging near the core, the central gas should have a reduction of SN Ia dominance, differently from what is observed in normal groups. We propose to test this with the most optimal and nearest fossil group, NGC6482, matching very well the capabilities of Suzaku. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | RENATO DUPKE | USA | 4 | AO4 | DISCRIMINATING COMPETING MODELS FOR THE ORIGIN OF FOSSIL GROUPS OF GALAXIES WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804050010/ | Quick Look | ![]() |
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539 | NGC741MOSAICE_P4 | 29.8808 | 5.7741 | 29.226568 | 5.531917 | 29.834623 | -6.020542 | 152.02832852 | -53.20754513 | 71.8261 | 55054.5770138889 | 2009-08-11 13:50:54 | 55054.8084953704 | 2009-08-11 19:24:14 | 804052040 | 11.0257 | 10 | 11.0257 | 11.3217 | 0 | 11.3057 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 11.3902 | 11.3902 | 19.9959 | 0 | PROCESSED | 57548.1244328704 | 2016-06-09 02:59:11 | 55448 | 2010-09-09 00:00:00 | 55081.2593055556 | 2009-09-07 06:13:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JOEL BREGMAN | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804052040/ | Quick Look | ![]() |
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540 | 1730-130 | 263.2641 | -13.0933 | 262.559168 | -13.058946 | 263.324851 | 10.191548 | 12.02258907 | 10.80244107 | 271.1606 | 55829.6599537037 | 2011-09-25 15:50:20 | 55830.0946643518 | 2011-09-26 02:16:19 | 706046010 | 11.0858 | 10 | 11.0938 | 11.0938 | 0 | 11.0858 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.8811 | 9.8811 | 37.5359 | 1 | PROCESSED | 57603.2457407407 | 2016-08-03 05:53:52 | 56225 | 2012-10-25 00:00:00 | 55875.6203703704 | 2011-11-10 14:53:20 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061601 | We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | SVETLANA JORSTAD | USA | 6 | AO6 | EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706046010/ | Quick Look | ![]() |
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541 | ABELL 426 E2 | 50.6767 | 41.5228 | 49.847142 | 41.344864 | 59.17553 | 22.199581 | 151.03351832 | -12.94989772 | 90.0008 | 55041.7150115741 | 2009-07-29 17:09:37 | 55041.9654976852 | 2009-07-29 23:10:19 | 804057010 | 12.9048 | 10 | 12.9048 | 12.9048 | 0 | 12.9048 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.962 | 12.962 | 21.6399 | 1 | PROCESSED | 57547.969849537 | 2016-06-08 23:16:35 | 55419 | 2010-08-11 00:00:00 | 55050.2440277778 | 2009-08-07 05:51:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804057010/ | Quick Look | ![]() |
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542 | ABELL 426 N6 | 48.8242 | 42.9264 | 47.990569 | 42.741631 | 58.170143 | 23.930613 | 149.06870737 | -12.52705179 | 59.999 | 55063.8243055556 | 2009-08-20 19:47:00 | 55064.6334837963 | 2009-08-21 15:12:13 | 804068010 | 36.5265 | 30 | 36.5345 | 36.5265 | 0 | 36.5425 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.8843 | 30.8843 | 69.9119 | 0 | PROCESSED | 57548.3037731482 | 2016-06-09 07:17:26 | 55441 | 2010-09-02 00:00:00 | 55075.1362037037 | 2009-09-01 03:16:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804068010/ | Quick Look | ![]() |
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543 | ESO 511-G030 | 214.8452 | -26.646 | 214.125789 | -26.416487 | 221.403618 | -12.022581 | 326.22952078 | 32.2164843 | 286.9689 | 56130.0282407407 | 2012-07-22 00:40:40 | 56136.3340856482 | 2012-07-28 08:01:05 | 707023020 | 224.0255 | 270 | 224.0255 | 224.0255 | 0 | 224.0335 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 195.6334 | 195.6334 | 410.8958 | 3 | PROCESSED | 57606.8434606482 | 2016-08-06 20:14:35 | 56646 | 2013-12-20 00:00:00 | 56279.0046064815 | 2012-12-18 00:06:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071413 | The study of "bare" Seyfert 1 AGN is essential to measure the true properties of the inner regions of the accretion disk. The nearby Seyfert ESO 511-G30 is a prime candidate for fulfilling this role due to its broad Fe K component and lack of any intrinsic warm absorption. It is also one of the X-ray brightest bare Seyferts featured in the Swift 58 month BAT catalogue as yet unobserved with Suzaku. We propose a 270 ks Suzaku observation of ESO 511-G30 to unambiguously constrain the properties of the accretion disk and subsequently the black hole spin. In addition, the HXD data will allow us to measure the Compton reflection hump, while the excellent soft X-ray spectral resolution of XIS will allow the origin of the soft excess to be determined. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JAMES REEVES | USA | 7 | AO7 | MEASURING THE ACCRETION DISK AND BLACK HOLE PROPERTIES OF ESO 511-G30 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707023020/ | Quick Look | ![]() |
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544 | SNR 1987A | 83.833 | -69.2775 | 83.924877 | -69.307216 | 307.543742 | -86.433259 | 279.71430694 | -31.94790633 | 135.9732 | 56233.5143981482 | 2012-11-02 12:20:44 | 56234.854375 | 2012-11-03 20:30:18 | 707020010 | 81.2764 | 80 | 81.2764 | 81.2844 | 0 | 81.2924 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 78.5842 | 78.5842 | 115.7599 | 0 | PROCESSED | 57607.9555439815 | 2016-08-07 22:55:59 | 56611 | 2013-11-15 00:00:00 | 56245.4956365741 | 2012-11-14 11:53:43 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071331 | Despite extensive observations of supernova remnant (SNR) 1987A with Chandra and XMM-Newton, the origin of the hard band (3-10 keV) X-ray emission is elusive (thermal vs nonthermal). A straightforward way to discriminate the thermal and nonthermal origins of the hard X-rays is to detect Fe K lines. The Suzaku XIS provides a uniquely efficient opportunity for a sensitive search for the Fe K lines, which is an excellent complement to the existing Chandra and XMM-Newton studies of SNR 1987A. Thus, we propose an 80 ks Suzaku observation of SNR 1987A. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | SANGWOOK PARK | USA | 7 | AO7 | X-RAY EMISSION FROM SUPERNOVA REMNANT 1987A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707020010/ | Quick Look | ![]() |
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545 | A1413_FIELD_3 | 179.0207 | 23.4251 | 178.377297 | 23.70339 | 169.347727 | 21.006295 | 226.37028623 | 76.95859752 | 302.9994 | 55347.1862037037 | 2010-05-31 04:28:08 | 55348.2079050926 | 2010-06-01 04:59:23 | 805061010 | 40.9225 | 40 | 40.9225 | 40.9385 | 0 | 40.9305 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.9944 | 32.9944 | 88.2578 | 0 | PROCESSED | 57553.3965856482 | 2016-06-14 09:31:05 | 55287 | 2010-04-01 00:00:00 | 55393.4280208333 | 2010-07-16 10:16:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805061010/ | Quick Look | ![]() |
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546 | A383_FIELD_2 | 41.9447 | -3.4083 | 41.315431 | -3.616408 | 38.400744 | -18.662791 | 177.53047769 | -53.46482162 | 60.9996 | 55389.1380208333 | 2010-07-12 03:18:45 | 55390.062662037 | 2010-07-13 01:30:14 | 805063010 | 43.3415 | 40 | 43.3575 | 43.3415 | 0 | 43.3575 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.2589 | 39.2589 | 79.8749 | 0 | PROCESSED | 57552.6168055556 | 2016-06-13 14:48:12 | 55287 | 2010-04-01 00:00:00 | 55411.2445601852 | 2010-08-03 05:52:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805063010/ | Quick Look | ![]() |
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547 | CTA102 | 338.1458 | 11.7401 | 337.526658 | 11.482274 | 344.409824 | 19.371456 | 77.43997335 | -38.57166798 | 72.4263 | 56431.345462963 | 2013-05-19 08:17:28 | 56431.6134606482 | 2013-05-19 14:43:23 | 707045010 | 9.5626 | 10 | 9.5706 | 9.5626 | 0 | 9.5706 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.283 | 7.283 | 23.1439 | 0 | PROCESSED | 57611.3187847222 | 2016-08-11 07:39:03 | 56809 | 2014-06-01 00:00:00 | 56443.5010069444 | 2013-05-31 12:01:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071601 | We propose to perform two 2-week multi-frequency campaigns of observations of a sample of gamma-ray blazars during Fermi Cycle 5. The campaigns will involve: (1) gamma-ray monitoring with the Fermi LAT, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B, V, R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku and Swift; (6) mid-IR measurements with IRTF; and (7) near-IR photometric J, H, and K observations. The research aims i) to search for correlated variability on short timescales; ii) to compile SEDs at different states of gamma-ray and radio jet activitiy; and iii) to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | SVETLANA JORSTAD | USA | 7 | AO7 | MULTI-FREQUENCY CAMPAIGNS TO STUDY RAPID VARIABILITY IN GAMMA_RAY BLAZARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707045010/ | Quick Look | ![]() |
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548 | LEDA 168563 | 73.0158 | 49.5506 | 72.064208 | 49.467096 | 77.740518 | 26.831198 | 157.24701812 | 3.42018054 | 86.3166 | 56536.8773611111 | 2013-09-01 21:03:24 | 56539.0592708333 | 2013-09-04 01:25:21 | 708017010 | 100.011 | 100 | 100.035 | 100.011 | 0 | 100.035 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 92.947 | 92.947 | 188.5018 | 1 | PROCESSED | 57612.530162037 | 2016-08-12 12:43:26 | 56383 | 2013-04-01 00:00:00 | 56608.7327893518 | 2013-11-12 17:35:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081413 | We propose to carry out Suzaku observations, a 100 ks each, of three Seyfert I nuclei hard X-ray selected by Swift. Our goal is to distinguish between various competing models proposed for the X-ray spectra of Seyfert I nuclei. Especially we will test, by observing these targets, the ionized relativistic reflection (hereafter IRR). We will take advantage of Suzaku s unique capability of detecting hard X-rays beyond 10 keV by its HXD-PIN, simultaneously with X-rays in lower to medium energy bands by its XIS on board. With our proposed studies we will gain deeper understanding of accretion-powered AGN in general. Since the IRR takes place close to the black hole we will test the effects of strong gravity, such as the black hole spin. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | SACHIKO TSURUTA | USA | 8 | AO8 | SPECTRAL STUDIES OF SOME HARD X-RAY SELECTED SEYFERT NUCLEI | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708017010/ | Quick Look | ![]() |
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549 | MKW 4-OFFSET1 | 181.1304 | 2.2289 | 180.489911 | 2.507266 | 180.147119 | 2.494288 | 276.66004128 | 62.68282085 | 114.5816 | 55528.2862847222 | 2010-11-28 06:52:15 | 55530.2501967593 | 2010-11-30 06:00:17 | 805081010 | 79.4261 | 80 | 79.4261 | 79.4261 | 0 | 79.4261 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 68.2112 | 68.2112 | 169.6679 | 2 | PROCESSED | 57554.312025463 | 2016-06-15 07:29:19 | 55909 | 2011-12-14 00:00:00 | 55543.4043402778 | 2010-12-13 09:42:15 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051525 | We propose a set of two 19 arcmin offset observations for the galaxy groups MKW 4 to measure spatially resolved density, temperature and iron abundance out to r_{500}. These measurements are crucial for an accurate determination of the gas mass profile and gas fraction, for probing the entropy profile near the region where the accretion shocks start to be important, and for exploring the chemical enrichment at a spatial scale which retains information of early SNII and SNIa enrichment. Due to its brightness, regularity and low temperature, the object is an ideal candidate for an offset observation of its peripheral gas by Suzaku, making an excellent use of its low background and soft X-ray sensitivity. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | FABIO GASTALDELLO | USA | 5 | AO5 | THE OUTSKIRTS OF MKW 4 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805081010/ | Quick Look | ![]() |
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550 | PKS 0745-191 | 116.3632 | -19.0871 | 115.808852 | -18.964679 | 122.979801 | -39.556071 | 236.01662317 | 2.71025988 | 294.0001 | 55316.6424189815 | 2010-04-30 15:25:05 | 55317.3675231482 | 2010-05-01 08:49:14 | 805085010 | 34.9999 | 35 | 34.9999 | 34.9999 | 0 | 34.9999 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.7804 | 32.7804 | 62.6419 | 2 | PROCESSED | 57551.3324074074 | 2016-06-12 07:58:40 | 55696 | 2011-05-15 00:00:00 | 55330.1114236111 | 2010-05-14 02:40:27 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051526 | Suzaku has enabled us to make the first measurement of the temperature profile beyond the virial radius of any cluster. The gas in the outskirts of galaxy clusters presents information of astrophysical and cosmological importance. Measurements at the virial radius, where the dominant gas behavior switches from infall to equilibrium, can improve cluster mass estimates. Temperature and entropy profiles in the outskirts describe the accretion history and energy balance of clusters, near where they must match the background properties of the Universe. But these observations are just beginning. How do clusters grow? Are there large scale accretion shocks? To what extent are clusters relaxed? Here we propose to continue our study of PKS 0745-191 using Suzaku's unique capability to map this area. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATTHEW GEORGE | USA | 5 | AO5 | BEYOND THE VIRIAL RADIUS OF PKS 0745-191, THE BRIGHTEST CLUSTER PAST Z=0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805085010/ | Quick Look | ![]() |
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551 | IGR J09026-4812 | 135.6468 | -48.2323 | 135.224236 | -48.033912 | 164.675258 | -60.400706 | 268.86967218 | -1.09239209 | 115.8572 | 56622.3203356482 | 2013-11-26 07:41:17 | 56622.9521990741 | 2013-11-26 22:51:10 | 708031010 | 37.7924 | 35 | 37.8244 | 37.8164 | 0 | 37.7924 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.2029 | 35.2029 | 54.5859 | 1 | PROCESSED | 57613.429212963 | 2016-08-13 10:18:04 | 56383 | 2013-04-01 00:00:00 | 56632.5852777778 | 2013-12-06 14:02:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081419 | The BAT AGN sample constitutes an unprecedented all-sky hard X-ray survey of the local AGN population. However, to properly model the X-ray absorption & reflection, coverage below 10 keV is needed with CCD spectral resolution and adequate signal-to-noise. We propose to observe 11 AGN with Suzaku, which will increase the completeness of a flux-limited sample with such coverage from 85 to 158 sources. The 11 AGN only have severely underexposed Swift XRT coverage below 10 keV whereas the remaining sources have either Suzaku or XMM coverage. The Suzaku data have the additional advantage of sensitivity above 10 keV that helps to mitigate the long time-baseline of the BAT spectra. The new observations will create a significantly enhanced legacy data set that will provide value for years to come. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TAHIR YAQOOB | USA | 8 | AO8 | ROBUST CHARACTERIZATION OF ABSORPTION AND REFLECTION IN A LOCAL FLUX-LIMITED AGN POPULATION FROM THE SWIFT BAT SURVEY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708031010/ | Quick Look | ![]() |
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552 | ABELL 981 | 156.0884 | 68.0988 | 155.16023 | 68.352315 | 123.8863 | 52.287736 | 140.87577234 | 43.55064218 | 119.4308 | 56601.2179398148 | 2013-11-05 05:13:50 | 56601.7917708333 | 2013-11-05 19:00:09 | 708040010 | 27.5945 | 30 | 27.6025 | 27.5945 | 0 | 27.5945 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.286 | 25.286 | 49.574 | 1 | PROCESSED | 57613.2182060185 | 2016-08-13 05:14:13 | 56980 | 2014-11-19 00:00:00 | 56614.6564583333 | 2013-11-18 15:45:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081533 | We propose to map out the core of the A981 supercluster with three Suzaku observations. The A981 supercluster contains four Abell richness class 2 clusters within a redshift range of 2,000 km/s. All four clusters also overlap within their virial radii, at least in projection. The low and steady background of the Suzaku telescope is ideal for studying the low surface brightness X-ray emission between the clusters. Such observations will determine if the clusters are interacting via the detection of merger-induced shocks or perturbed features in the outskirts of the individual clusters. Our proposed Suzaku observations will help elucidate the fundamental astrophysics that occurs during the formation of very massive clusters. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | LAURENCE DAVID | USA | 8 | AO8 | MAPPING THE ABELL 981 SUPER CLUSTER WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708040010/ | Quick Look | ![]() |
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553 | HOLMBERG IX X-1 | 149.4572 | 69.0544 | 148.43919 | 69.292844 | 119.777434 | 51.680142 | 141.94722641 | 41.07197433 | 311.5038 | 57118.9110416667 | 2015-04-06 21:51:54 | 57119.5667708333 | 2015-04-07 13:36:09 | 709015030 | 31.5263 | 30 | 31.5263 | 31.5263 | 0 | 31.5263 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.9243402778 | 2016-08-17 22:11:03 | 57513 | 2016-05-05 00:00:00 | 57129.4193171296 | 2015-04-17 10:03:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091251 | Broadband X-ray spectroscopy of ultraluminous X-ray sources (ULXs) with NuSTAR and Suzaku has begun to provide important information regarding the nature of these enigmatic sources. Recent NuSTAR observations of the extreme ULX Holmberg IX X-1 revealed unusual spectral variability, and different competing evolutionary scenarios can explain the available data. Resolving this degeneracy is critical to determining the nature of the accretion onto this source, and requires multi-epoch broadband spectroscopy probing a more diverse range of fluxes. We propose to undertake 4x30 ks coordinated Suzaku+NuSTAR observations of Holmberg IX X-1 to provide the additional spectra needed to robustly determine the nature of the observed evolution, providing a vital step in our understanding of extreme ULXs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | DOMINIC WALTON | USA | 9 | AO9 | MULTI-EPOCH BROADBAND X-RAY SPECTROSCOPY OF HOLMBERG IX X-1 WITH SUZAKU AND NUSTAR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709015030/ | Quick Look | ![]() |
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554 | ABELL 1795 Far South | 207.2227 | 26.2001 | 206.644395 | 26.44826 | 194.131601 | 34.631873 | 32.0541753 | 77.13779505 | 129.4115 | 53716.5361921296 | 2005-12-12 12:52:07 | 53717.4168865741 | 2005-12-13 10:00:19 | 800012050 | 40.1206 | 30 | 40.1366 | 40.1526 | 40.1206 | 40.1366 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39.4373 | 39.4373 | 76.0819 | 1 | PROCESSED | 57532.4477314815 | 2016-05-24 10:44:44 | 54247 | 2007-05-27 00:00:00 | 54039.1460069445 | 2006-10-31 03:30:15 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001056 | We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MARK BAUTZ | JAP | 0 | SWG | TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800012050/ | Quick Look | ![]() |
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555 | ABELL 3112 | 49.4982 | -44.2507 | 49.063827 | -44.432376 | 25.5219 | -58.972557 | 252.95298598 | -56.06981795 | 43.5004 | 56466.5743634259 | 2013-06-23 13:47:05 | 56468.5418055556 | 2013-06-25 13:00:12 | 808068010 | 119.1247 | 200 | 119.1247 | 119.1247 | 0 | 119.1247 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 114.5618 | 114.5618 | 169.9418 | 0 | PROCESSED | 57611.6340856482 | 2016-08-11 15:13:05 | 56848 | 2014-07-10 00:00:00 | 56481.8003356482 | 2013-07-08 19:12:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081522 | The hot X-ray emitting gas in clusters of galaxies is a very large repository of metals produced by stars and galaxies. These metals enter the intra-cluster medium (ICM) via strong galactic winds, supernovae explosions, and ram-pressure stripping. However, the details of the mechanisms that transport metals to the ICM and the origin of these metals remain still unclear. We aim to accurately measure the temperature and abundance patterns of a bright nearby galaxy cluster A3112 out to the virial radius and compare these data with metal abundance yields produced by supernovae. Our proposed observation will provide information about how these metals are created, as well as how and when the metals were transported to the ICM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ESRA BULBUL | USA | 8 | AO8 | CHEMICAL EVOLUTION HISTORY OF A COOL CORE CLUSTER A3112 OUT TO THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808068010/ | Quick Look | ![]() |
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556 | OJ 287 | 133.705 | 20.1043 | 132.989927 | 20.295379 | 130.505973 | 2.596868 | 206.81753743 | 35.82068078 | 285.8744 | 57148.4467708333 | 2015-05-06 10:43:21 | 57151.4189351852 | 2015-05-09 10:03:16 | 710011020 | 110.2819 | 323 | 110.2819 | 112.3099 | 0 | 112.3099 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.1271643518 | 2016-08-18 03:03:07 | 57113 | 2015-04-01 00:00:00 | 57164.5272337963 | 2015-05-22 12:39:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 101431 | Kepler will observe OJ 287 with 1 min sampling and >90% duty cycle for ~75 days in 2015, providing an unprecedented opportunity to quantitatively compare optical and X-ray variations in one of the brightest and most active blazars in the sky. We request continuous Suzaku coverage for 128 orbits (323 ks) in a simultaneous campaign including XMM, Swift, radio and multi-color optical monitoring. Suzaku samples key intermediate timescales of hours-days, allowing measurement of CCFs and PSDs spanning a wide range of temporal frequencies. These will be used to test models and determine source parameters e.g. if the X-rays are due to synchrotron-self Compton the optical should lead the X-rays by ~1 day, but if they are "synchrotron flashes" the bands should vary nearly simultaneously. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RICK EDELSON | USA | 10 | AO10 | SIMULTANEOUS SUZAKU/KEPLER/MULTIWAVELENGTH MONITORING OF OJ 287 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710011020/ | Quick Look | ![]() |
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557 | OJ 287 | 133.7049 | 20.1044 | 132.989827 | 20.295479 | 130.505855 | 2.596938 | 206.81738245 | 35.82062575 | 285.8744 | 57151.4189467593 | 2015-05-09 10:03:17 | 57154.3266666667 | 2015-05-12 07:50:24 | 710011030 | 107.7143 | 323 | 107.7143 | 107.7143 | 0 | 107.7143 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.6879166667 | 2016-08-18 16:30:36 | 57113 | 2015-04-01 00:00:00 | 57164.5596527778 | 2015-05-22 13:25:54 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 101431 | Kepler will observe OJ 287 with 1 min sampling and >90% duty cycle for ~75 days in 2015, providing an unprecedented opportunity to quantitatively compare optical and X-ray variations in one of the brightest and most active blazars in the sky. We request continuous Suzaku coverage for 128 orbits (323 ks) in a simultaneous campaign including XMM, Swift, radio and multi-color optical monitoring. Suzaku samples key intermediate timescales of hours-days, allowing measurement of CCFs and PSDs spanning a wide range of temporal frequencies. These will be used to test models and determine source parameters e.g. if the X-rays are due to synchrotron-self Compton the optical should lead the X-rays by ~1 day, but if they are "synchrotron flashes" the bands should vary nearly simultaneously. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RICK EDELSON | USA | 10 | AO10 | SIMULTANEOUS SUZAKU/KEPLER/MULTIWAVELENGTH MONITORING OF OJ 287 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710011030/ | Quick Look | ![]() |
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558 | ABELL2811 | 10.4703 | -28.5552 | 9.856516 | -28.82929 | 357.097887 | -30.138768 | 358.34166022 | -87.45073592 | 232.1065 | 53702.1678240741 | 2005-11-28 04:01:40 | 53702.8814699074 | 2005-11-28 21:09:19 | 800005010 | 30.6546 | 25 | 30.6626 | 30.6826 | 30.6546 | 30.6659 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 28.3254 | 28.3254 | 61.656 | 0 | PROCESSED | 57528.0937268518 | 2016-05-20 02:14:58 | 54247 | 2007-05-27 00:00:00 | 54038.5109722222 | 2006-10-30 12:15:48 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001025 | We propose to observe the central region of the Sculptor supercluster at z=0.11, in a search for the theoretically predicted Warm/Hot Intergalactic Medium (WHIM). The WHIM has been 'missing' observationally, until recent detection of the X-ray absorption due to the ionized light elements in the background quasar spectra. Still there is no confident detection of the expected soft X-ray emission. This is mainly because that the X-ray brightness is very low, compared to the Galactic diffuse emission in the soft X-ray band and/or the spectral sensitivity of previous experiments are limited. To separate the expected X-ray lines of the WHIM (mainly O VII) from the Galactic emission, we select an unique supercluster at z>0.1. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | TAKAYUKI TAMURA | JAP | 0 | SWG | THE SCULPTOR SUPERCLUSTER: SEARCH FOR THE WARM/HOT INTERGALACTIC MEDIUM | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800005010/ | Quick Look | ![]() |
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559 | A426 | 49.9554 | 41.5039 | 49.127963 | 41.323287 | 58.608686 | 22.329679 | 150.58326426 | -13.26576669 | 260.2176 | 53767.568900463 | 2006-02-01 13:39:13 | 53768.5294560185 | 2006-02-02 12:42:25 | 800010010 | 50.3986 | 50 | 50.4066 | 50.4066 | 50.3986 | 50.4066 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 54.4364 | 54.4364 | 82.9758 | 0 | PROCESSED | 57532.8781365741 | 2016-05-24 21:04:31 | 54247 | 2007-05-27 00:00:00 | 54041.0862152778 | 2006-11-02 02:04:09 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001036 | A426 is the X-ray brightest cluster in the Sky. The core is X-ray peaked, has a short radiative cooling time, a temperature drop and a central radio source which is blowing bubbles in the intracluster medium. A radio minihalo extends over the central 6 arcmin. A coincident power-law component is seen in deep Chandra data. This is likely to be inverse Compton emission from the electron population responsible for the radio emission. The region is expected to be a luminous, extended, hard X-ray source easily detectable by the Suzaku HXD. Confirmation of this hard X-ray component will enable the magnetic field to be securely determined in the intracluster gas. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ANDREW FABIAN | JAP | 0 | SWG | THE HARD X-RAY FLUX FROM THE CORE OF THE PERSEUS CLUSTER | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800010010/ | Quick Look | ![]() |
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560 | ABELL 773 | 139.6415 | 51.5835 | 138.770726 | 51.794221 | 124.818527 | 33.970374 | 166.25628799 | 43.50358503 | 276.9979 | 55683.2110185185 | 2011-05-02 05:03:52 | 55684.0730208333 | 2011-05-03 01:45:09 | 806027020 | 47.2223 | 50 | 47.2303 | 47.2223 | 0 | 47.2383 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.5115 | 46.5115 | 74.4719 | 0 | PROCESSED | 57601.9085185185 | 2016-08-01 21:48:16 | 55652 | 2011-04-01 00:00:00 | 55697.3168981482 | 2011-05-16 07:36:20 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061116 | We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 6 | AO6-LP | THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806027020/ | Quick Look | ![]() |
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561 | CENCL OFFSET2 | 192.2009 | -41.1804 | 191.510431 | -40.907877 | 208.999282 | -32.736275 | 302.39848339 | 21.68862024 | 106.52 | 53733.2507407407 | 2005-12-29 06:01:04 | 53734.3543865741 | 2005-12-30 08:30:19 | 800016010 | 43.2773 | 40 | 43.2853 | 43.2853 | 43.2773 | 43.2933 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35.2531 | 35.2531 | 95.332 | 1 | PROCESSED | 57532.5900578704 | 2016-05-24 14:09:41 | 54247 | 2007-05-27 00:00:00 | 54039.6041203704 | 2006-10-31 14:29:56 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001070 | A dramatic central concentration of iron and silicon is present in the Centaurus cluster. Apart from this well-recognized contribution from Type Ia supernova, enrichment process due to Type II supernova is poorly understood. Centaurus cluster is most suited for the study of large-scale oxygen distribution, for which XIS is most sensitive. The XIS data will give us a key knowledge about how past Type II supernova have affected the enrichment process. The data would also confirm that the central gas is a mixture of hot and cool components with much better sensitivity than before. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YASUSHI FUKAZAWA | JAP | 0 | SWG | OXYGEN DISTRIBUTION AND MIXTURE OF HOT AND COOL GAS IN THE CENTAURUS CLUSTER | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800016010/ | Quick Look | ![]() |
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562 | NGC 4636 | 190.7243 | 2.7556 | 190.086173 | 3.029415 | 188.766391 | 6.778722 | 297.77503713 | 65.54179663 | 112.2967 | 53710.1073726852 | 2005-12-06 02:34:37 | 53711.9446643518 | 2005-12-07 22:40:19 | 800018010 | 79.201 | 80 | 79.201 | 79.201 | 79.201 | 79.201 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 75.7771 | 75.7771 | 158.7278 | 2 | PROCESSED | 57532.4099421296 | 2016-05-24 09:50:19 | 54247 | 2007-05-27 00:00:00 | 54038.9551388889 | 2006-10-30 22:55:24 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001083 | We propose to observe NGC 4636 for 50~ksec in a single pointing, to determine the chemical evolution of elliptical galaxies via the determination of the spatially resolved abundance of Oxygen and other elements. Being one of the most X-ray luminous ellipticals, and having been observed by both Chandra and XMM, this is also an important target to compare the capabilities of the three observatories and interpret the results of the Suzaku XIS in light of the source spectrum provided by the XMM RGS. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ENECTALI FIGUEROA-FELICIANO | JAP | 0 | SWG | OBSERVATION OF THE X-RAY LUMINOUS EXTENDED EARLY-TYPE GALAXY NGC 4636 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800018010/ | Quick Look | ![]() |
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563 | ABELL 2667 | 357.7341 | -26.0226 | 357.087227 | -26.30077 | 347.004408 | -22.85609 | 34.17814736 | -76.43580815 | 64.8804 | 55722.9055208333 | 2011-06-10 21:43:57 | 55724.4196990741 | 2011-06-12 10:04:22 | 806029020 | 51.6577 | 50 | 51.6657 | 51.6577 | 0 | 51.6721 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.656 | 45.656 | 130.802 | 1 | PROCESSED | 57602.2808333333 | 2016-08-02 06:44:24 | 55652 | 2011-04-01 00:00:00 | 55757.7009027778 | 2011-07-15 16:49:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061116 | We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 6 | AO6-LP | THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806029020/ | Quick Look | ![]() |
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564 | COMA E6.5 | 196.9526 | 27.8857 | 196.354379 | 28.152377 | 183.408228 | 32.112773 | 45.6576416 | 86.29162208 | 279.9993 | 55731.5902199074 | 2011-06-19 14:09:55 | 55732.0578935185 | 2011-06-20 01:23:22 | 806037010 | 14.9596 | 15 | 14.9676 | 14.9596 | 0 | 14.9676 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.6142 | 13.6142 | 40.3999 | 0 | PROCESSED | 57602.3577314815 | 2016-08-02 08:35:08 | 55652 | 2011-04-01 00:00:00 | 55770.17125 | 2011-07-28 04:06:36 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806037010/ | Quick Look | ![]() |
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565 | COMA SW7 | 193.2936 | 26.7739 | 192.684688 | 27.045132 | 180.600519 | 29.664204 | 350.54999025 | 89.47529971 | 314.5993 | 55737.124212963 | 2011-06-25 02:58:52 | 55737.4447106482 | 2011-06-25 10:40:23 | 806051010 | 15.4152 | 15 | 15.4152 | 15.4232 | 0 | 15.4232 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15.0368 | 15.0368 | 27.6719 | 0 | PROCESSED | 57602.4087847222 | 2016-08-02 09:48:39 | 55652 | 2011-04-01 00:00:00 | 55795.0185763889 | 2011-08-22 00:26:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806051010/ | Quick Look | ![]() |
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566 | 30 DORADUS | 84.6512 | -69.1008 | 84.737262 | -69.126573 | 305.902613 | -86.759222 | 279.46621821 | -31.68092384 | 162.7542 | 55895.6278472222 | 2011-11-30 15:04:06 | 55897.0640162037 | 2011-12-02 01:32:11 | 806052010 | 101.6448 | 100 | 101.6528 | 101.6528 | 0 | 101.6448 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89.0823 | 89.0823 | 124.076 | 0 | PROCESSED | 57604.044837963 | 2016-08-04 01:04:34 | 56281 | 2012-12-20 00:00:00 | 55907.9795486111 | 2011-12-12 23:30:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061322 | We propose a deep Suzaku observation of 30 Doradus to provide a direct X-ray measurement of the chemical enrichment in the enclosed hot gas. The soft X-ray sensitivity and spectral resolution of this observation will allow us to measure key elemental abundances and thus to test models for metal yields of massive stars. We will determine the spatial variation in the thermal and chemical properties of the hot gas and the effect on the global estimation of the chemical enrichment from an integrated spectrum, as would be obtained for a distant starburst region. We will also estimate the mass-loading from the general interstellar medium --- a key parameter for determining the evolution of the hot gas. The results will serve as an observational benchmark for understanding massive star feedback. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | Q. DANIEL WANG | USA | 6 | AO6 | X-RAY SPECTROSCOPIC MAPPING OF 30 DORADUS: CHEMICAL ENRICHMENT BY MASSIVE STARS IN A CLOSED BOX | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806052010/ | Quick Look | ![]() |
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567 | RCS131723-0201.3 | 199.3422 | -2.034 | 198.698505 | -1.770799 | 198.620431 | 5.687336 | 316.04491283 | 60.17589221 | 291.8811 | 55756.3454513889 | 2011-07-14 08:17:27 | 55756.9585532407 | 2011-07-14 23:00:19 | 806078010 | 24.921 | 25 | 24.921 | 24.921 | 0 | 24.921 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23.1205 | 23.1205 | 52.9619 | 1 | PROCESSED | 57602.5803009259 | 2016-08-02 13:55:38 | 56163 | 2012-08-24 00:00:00 | 55783.6867939815 | 2011-08-10 16:28:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061533 | Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 19 optically-selected clusters of galaxies, half at z~0.3 and half at z~0.8. Here we propose 6 additional observations in order to uniformly span a total redshift range of 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | AMALIA HICKS | USA | 6 | AO6 | AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806078010/ | Quick Look | ![]() |
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568 | PKS 0745-191 | 116.9737 | -19.0727 | 116.418821 | -18.947622 | 123.702706 | -39.408553 | 236.29361594 | 3.21678926 | 294.0001 | 54232.5006712963 | 2007-05-12 12:00:58 | 54233.2258564815 | 2007-05-13 05:25:14 | 802062030 | 30.7942 | 30 | 30.8022 | 30.7942 | 0 | 30.8022 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.6388 | 26.6388 | 62.6301 | 0 | PROCESSED | 57538.6331134259 | 2016-05-30 15:11:41 | 54695 | 2008-08-17 00:00:00 | 54245.5042592593 | 2007-05-25 12:06:08 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021440 | PKS 0745-191 is the X-ray brightest galaxy cluster beyond a redshift of 0.1. It has a smooth surface brightness profile and appears relaxed. Using the low background of Suzaku we will measure the temperature of the intracluster medium to the virial radius of the cluster. Its high temperature means that we will be unaffected by any loss of effective area at low energies. In addition the cluster is bright enough so that the bremsstrahlung emission will be easily detected using the PIN detector. This will allow us to search for any nonthermal component as well as accurately determining the high temperature components in the cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ANDREW YOUNG | USA | 2 | AO2 | PKS 0745-191: THE BRIGHTEST CLUSTER BEYOND Z=0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802062030/ | Quick Look | ![]() |
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569 | SDSS J1302+4729 | 195.5068 | 47.4831 | 194.946247 | 47.751657 | 168.926268 | 48.423966 | 117.80880843 | 69.53967787 | 316.2365 | 56076.2710648148 | 2012-05-29 06:30:20 | 56076.7058217593 | 2012-05-29 16:56:23 | 807060010 | 20.427 | 20 | 20.427 | 20.427 | 0 | 20.427 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24.66 | 24.66 | 37.5599 | 1 | PROCESSED | 57605.5578240741 | 2016-08-05 13:23:16 | 56500 | 2013-07-27 00:00:00 | 56134.0735300926 | 2012-07-26 01:45:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071512 | Fossil groups (FGs) are systems dominated by a single large galaxy with a cluster-scale X-ray halo. They are thought to be old, isolated galaxy groups in which the large galaxies have coalesced through dynamical friction, but recent studies reveal a more complicated picture. We propose Suzaku observations of 5 optically selected FG candidates. These targets will extend our previous survey, which identified 12 FGs; when combined with 5 FG candidates approved for the current Chandra cycle, this will create the largest uniformly-selected sample of real FGs. The L_X and T_X measured will be used with optical spectroscopy to extend FG scaling relations to low mass, and to plan deeper X-ray spectroscopic follow-up to constrain the formation epoch and evolution of these puzzling systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ERIC MILLER | USA | 7 | AO7 | FINDING FOSSIL GROUPS WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807060010/ | Quick Look | ![]() |
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570 | ANTLIA E5 | 159.3469 | -35.3315 | 158.776481 | -35.071439 | 177.451568 | -40.165459 | 274.29394045 | 19.97884062 | 279.4997 | 56095.3697337963 | 2012-06-17 08:52:25 | 56096.5972916667 | 2012-06-18 14:20:06 | 807070010 | 46.7814 | 45 | 46.7894 | 46.7814 | 0 | 46.7974 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.0617 | 41.0617 | 106.0579 | 2 | PROCESSED | 57605.7158333333 | 2016-08-05 17:10:48 | 56590 | 2013-10-25 00:00:00 | 56219.6892361111 | 2012-10-19 16:32:30 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071521 | We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KA-WAH WONG | USA | 7 | AO7 | MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807070010/ | Quick Look | ![]() |
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571 | RCS0442-2815 | 70.5602 | -28.2499 | 70.060746 | -28.343732 | 62.940418 | -49.88298 | 228.44078987 | -39.40072076 | 273.8381 | 54903.705462963 | 2009-03-13 16:55:52 | 54905.2669444444 | 2009-03-15 06:24:24 | 803060010 | 52.3573 | 40 | 52.3573 | 52.3573 | 0 | 52.3573 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.4137 | 47.4137 | 134.8779 | 1 | PROCESSED | 57545.8322222222 | 2016-06-06 19:58:24 | 55329 | 2010-05-13 00:00:00 | 54917.4174652778 | 2009-03-27 10:01:09 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031441 | Comparisons between moderate-z X-ray and high-z optically selected clusters indicate that the latter have lower Lx than expected for a given Tx, however it is hard to tell if such discrepancies are due to cluster evolution or selection effects. In an attempt to isolate these two variables, we propose the first detailed comparison of X-ray and optically selected clusters that are well-matched in both velocity dispersion (a quantity independent of both methods) and redshift. Our X-ray analysis of X-ray selected CNOC clusters is complete. Here we propose to determine Lx, Tx, and gas distribution/morphology for an optically selected sample, most of which already have velocity dispersion data in hand, enabling rigorous quantitative comparisons between physical characteristics of the two groups. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 3 | AO3 | COSMOLOGY WITH CLUSTERS: CONSTRAINING PHYSICAL DIFFERENCES BETWEEN X-RAY AND OPTICALLY SELECTED SAMPLES AT MODERATE-Z | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803060010/ | Quick Look | ![]() |
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572 | ABELL 665 | 128.154 | 65.9045 | 127.018266 | 66.074275 | 110.985423 | 45.219486 | 149.6634974 | 34.85484411 | 289.999 | 56026.3998958333 | 2012-04-09 09:35:51 | 56027.1251967593 | 2012-04-10 03:00:17 | 807072010 | 50.431 | 50 | 50.431 | 50.431 | 0 | 50.431 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.0111 | 41.0111 | 62.6599 | 1 | PROCESSED | 57605.1298958333 | 2016-08-05 03:07:03 | 56018 | 2012-04-01 00:00:00 | 56044.1528240741 | 2012-04-27 03:40:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071522 | We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 7 | AO7 | COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807072010/ | Quick Look | ![]() |
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573 | ABELL 665 | 127.5519 | 65.9953 | 126.410061 | 66.162736 | 110.613991 | 45.219649 | 149.61230509 | 34.59661242 | 290.0005 | 56027.1259953704 | 2012-04-10 03:01:26 | 56027.8057638889 | 2012-04-10 19:20:18 | 807072020 | 51.446 | 50 | 51.446 | 51.446 | 0 | 51.446 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.2769 | 43.2769 | 58.728 | 1 | PROCESSED | 57605.1345717593 | 2016-08-05 03:13:47 | 56018 | 2012-04-01 00:00:00 | 56044.1899537037 | 2012-04-27 04:33:32 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071522 | We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 7 | AO7 | COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807072020/ | Quick Look | ![]() |
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574 | RCS110619-0423.6 | 166.5769 | -4.3915 | 165.941193 | -4.121064 | 169.375504 | -9.341083 | 260.07293798 | 49.52807614 | 109.9541 | 56253.8521296296 | 2012-11-22 20:27:04 | 56256.0092476852 | 2012-11-25 00:13:19 | 807075010 | 77.0765 | 75 | 77.0925 | 77.0765 | 0 | 77.1005 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69.3805 | 69.3805 | 186.3458 | 4 | PROCESSED | 57608.1296875 | 2016-08-08 03:06:45 | 56641 | 2013-12-15 00:00:00 | 56275.577025463 | 2012-12-14 13:50:55 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071525 | Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 24 optically-selected clusters of galaxies out to z~1. Here we propose 5 additional observations in order to uniformly span our total mass-redshift space over the range 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 7 | AO7 | AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES II | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807075010/ | Quick Look | ![]() |
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575 | NGC741 E | 29.459 | 5.6113 | 28.805334 | 5.368113 | 29.381945 | -6.027315 | 151.51137993 | -53.53548595 | 71.776 | 55054.8091087963 | 2009-08-11 19:25:07 | 55055.0619675926 | 2009-08-12 01:29:14 | 804053010 | 11.3778 | 10 | 11.3778 | 11.3858 | 0 | 11.3938 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 8.0052 | 8.0052 | 21.838 | 0 | PROCESSED | 57548.1250231482 | 2016-06-09 03:00:02 | 55430 | 2010-08-22 00:00:00 | 55064.1656134259 | 2009-08-21 03:58:29 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JOEL BREGMAN | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804053010/ | Quick Look | ![]() |
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576 | NGC741MOSAICS_P1 | 29.0595 | 4.7357 | 28.408059 | 4.491575 | 28.699079 | -6.708921 | 151.53660126 | -54.49712787 | 71.6617 | 55052.4780671296 | 2009-08-09 11:28:25 | 55052.6946643518 | 2009-08-09 16:40:19 | 804054010 | 9.3222 | 10 | 9.3302 | 9.3222 | 0 | 9.3302 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.003 | 8.003 | 18.6719 | 1 | PROCESSED | 57548.0801967593 | 2016-06-09 01:55:29 | 55451 | 2010-09-12 00:00:00 | 55084.9869212963 | 2009-09-10 23:41:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JOEL BREGMAN | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804054010/ | Quick Look | ![]() |
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577 | ABELL 426 E3 | 51.0503 | 41.5202 | 50.219736 | 41.343661 | 59.4655 | 22.121233 | 151.27232524 | -12.79481746 | 89.0003 | 55041.9666666667 | 2009-07-29 23:12:00 | 55042.2904398148 | 2009-07-30 06:58:14 | 804058010 | 11.2798 | 10 | 11.2798 | 11.5518 | 0 | 11.5518 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 10.7201 | 10.7201 | 27.9661 | 0 | PROCESSED | 57547.981412037 | 2016-06-08 23:33:14 | 55427 | 2010-08-19 00:00:00 | 55060.7814236111 | 2009-08-17 18:45:15 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804058010/ | Quick Look | ![]() |
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578 | RCS1620+3046 | 245.0418 | 30.7908 | 244.551505 | 30.909318 | 234.634805 | 51.209306 | 50.54291734 | 44.60353773 | 131.519 | 55203.6116666667 | 2010-01-07 14:40:48 | 55204.6008564815 | 2010-01-08 14:25:14 | 804081010 | 43.4882 | 38 | 43.4882 | 43.4882 | 0 | 43.4882 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.6324 | 16.6324 | 85.4538 | 0 | PROCESSED | 57550.1212615741 | 2016-06-11 02:54:37 | 55584 | 2011-01-23 00:00:00 | 55218.2018402778 | 2010-01-22 04:50:39 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041525 | Understanding relationships between baryons in galaxy clusters and the underlying dark matter distributions is crucial for using clusters as cosmological probes. Recent work indicates massive low-Lx clusters at all redshifts, in conflict with self-similarity predictions. The only way to quantify these findings is to observe a cluster sample chosen independently of X-ray properties. We propose to study 14 clusters at 0.15<z<0.45, for which robust velocity dispersions are measured. We were awarded Chandra observations of 8 high-dispersion, low-z targets. Suzaku s superior throughput is required to probe the low-dispersion, high-z side of the distribution. We propose XIS observations of the remaining 6 targets, allowing us to rigorously assess baryon content in an unbiased sample of clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | AMALIA HICKS | USA | 4 | AO4 | DECIPHERING CLUSTER OBSERVABLES: TRACING THE BARYONS IN CLUSTERS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804081010/ | Quick Look | ![]() |
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579 | ABELL 85 S1 | 10.6021 | -9.9841 | 9.970303 | -10.258056 | 5.733976 | -13.366048 | 115.42621428 | -72.72412936 | 230 | 56292.2572800926 | 2012-12-31 06:10:29 | 56295.6314583333 | 2013-01-03 15:09:18 | 807135010 | 139.9982 | 50 | 139.9982 | 139.9982 | 0 | 139.9982 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.82 | 11.82 | 25.4779 | 0 | PROCESSED | 57608.4068402778 | 2016-08-08 09:45:51 | 56703 | 2014-02-15 00:00:00 | 56337.496875 | 2013-02-14 11:55:30 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071791 | We propose exposures with CHandra and Suzaku in Abell 85 to trace the impact of a galaxy group merging with a galaxy cluster at multiple scales. Existing observations of Abell 85 reveal an infalling galaxy group ~300 kpc to the south of the main cluster moving supersonically through the ICM. Stripped gas is observed trailing behind this group to distances of 2 Mpc. We will investigate interactions between this group and the main cluster by observing the shocks associated with the group's motion and the properties of stripped gas. We will be able to measure the properties of the stripped gas from the group's current location out to the virial radius by combining the data from both telescopes. These observations will provide key insights into how the largest structures form. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | S | STEVEN ALLEN | USA | 7 | AO7 | TRACING A MERGER FROM START TO FINISH IN ABELL 85 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807135010/ | Quick Look | ![]() |
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580 | NGC3402 BACKGROUND | 161.6656 | -13.5535 | 161.046219 | -13.289693 | 168.522728 | -19.671776 | 262.34680831 | 39.29035073 | 110.091 | 55549.4379282407 | 2010-12-19 10:30:37 | 55549.7563425926 | 2010-12-19 18:09:08 | 805071010 | 12.5184 | 10 | 12.5344 | 12.5184 | 0 | 12.5344 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.8582 | 11.8582 | 27.4799 | 0 | PROCESSED | 57554.4605439815 | 2016-06-15 11:03:11 | 55960 | 2012-02-03 00:00:00 | 55593.0714699074 | 2011-02-01 01:42:55 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051512 | Using the composite data from dwarf galaxies to rich clusters, we find that the baryon fraction is mainly set by the system's potential well depth. The small scatter of baryon fractions as a function of the gravitational potential well depth indicates a universal baryon loss mechanism for these systems. However, the relation is most poorly constrained in the poor galaxy group regime below 1keV, where few individual measurements exists. Since most galaxies reside in these groups, it is also important to test whether the missing baryons from the galaxies are actually in these poor groups. We propose deep, off-center observations of two such groups, doubling the sample, to better delineate and understand the transition of the baryon loss from clusters to galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | XINYU DAI | USA | 5 | AO5 | BARYON LOSS IN POOR GALAXY GROUPS: DISTINGUISHING PRE-HEATING AND FEEDBACK MODELS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805071010/ | Quick Look | ![]() |
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581 | ESO3060170 | 85.0359 | -40.9515 | 84.636079 | -40.976582 | 81.358883 | -64.245092 | 246.54247084 | -30.30516606 | 320.0075 | 55327.721400463 | 2010-05-11 17:18:49 | 55328.2676388889 | 2010-05-12 06:25:24 | 805075010 | 31.3959 | 30 | 31.4039 | 31.3959 | 0 | 31.4119 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.684 | 28.684 | 47.1899 | 2 | PROCESSED | 57551.4609953704 | 2016-06-12 11:03:50 | 55707 | 2011-05-26 00:00:00 | 55341.5181365741 | 2010-05-25 12:26:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051513 | We propose 30 and 80 ksec observations of the X-ray brightest fossil group, ESO 3060170. The target pointings will reach to 75% of the virial radius from the center of the galaxy, in order to determine the temperature and metal abundances of group gas at large radii. This will allow us to determine the radial profiles of the gaseous iron mass to stellar light ratio, the relative distributions of ejecta from SN Ia and SN II, the entropy, the total mass to light ratio, and the dark matter concentration for this fossil group. The energy resolution and low background of the XIS instrument are crucial for this study, which will help constrain the evolutional history of this fossil group and tell us how fossil groups relate to normal groups and clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | YUANYUAN SU | USA | 5 | AO5 | HOW DO FOSSIL GROUPS OF GALAXIES DIFFER FROM NORMAL GROUPS? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805075010/ | Quick Look | ![]() |
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582 | PKS 0745-191 | 116.4685 | -19.4632 | 115.915912 | -19.340315 | 123.218132 | -39.89918 | 236.39245911 | 2.60836561 | 294.0003 | 55317.3681365741 | 2010-05-01 08:50:07 | 55318.1516087963 | 2010-05-02 03:38:19 | 805086010 | 31.7299 | 35 | 31.7299 | 31.7299 | 0 | 31.7299 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.646 | 27.646 | 67.682 | 0 | PROCESSED | 57551.3418981482 | 2016-06-12 08:12:20 | 55696 | 2011-05-15 00:00:00 | 55330.121087963 | 2010-05-14 02:54:22 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051526 | Suzaku has enabled us to make the first measurement of the temperature profile beyond the virial radius of any cluster. The gas in the outskirts of galaxy clusters presents information of astrophysical and cosmological importance. Measurements at the virial radius, where the dominant gas behavior switches from infall to equilibrium, can improve cluster mass estimates. Temperature and entropy profiles in the outskirts describe the accretion history and energy balance of clusters, near where they must match the background properties of the Universe. But these observations are just beginning. How do clusters grow? Are there large scale accretion shocks? To what extent are clusters relaxed? Here we propose to continue our study of PKS 0745-191 using Suzaku's unique capability to map this area. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATTHEW GEORGE | USA | 5 | AO5 | BEYOND THE VIRIAL RADIUS OF PKS 0745-191, THE BRIGHTEST CLUSTER PAST Z=0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805086010/ | Quick Look | ![]() |
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583 | RCS2318-0024 | 349.6301 | -0.4169 | 348.988896 | -0.690483 | 350.299766 | 3.723056 | 79.21894267 | -55.19865221 | 248.0438 | 55526.0185648148 | 2010-11-26 00:26:44 | 55527.293912037 | 2010-11-27 07:03:14 | 805089010 | 50.305 | 73 | 50.329 | 50.305 | 0 | 50.337 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.6346 | 45.6346 | 110.1738 | 0 | PROCESSED | 57554.2552893518 | 2016-06-15 06:07:37 | 55903 | 2011-12-08 00:00:00 | 55537.0791898148 | 2010-12-07 01:54:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051527 | Understanding relationships between baryons in galaxy clusters and underlying dark matter distributions is crucial for using clusters as cosmological probes. Recent work indicates massive low-Lx clusters at all redshifts, in conflict with self-similarity predictions. The only way to quantify these findings is to observe a sample chosen independently of X-ray properties. We propose to study 13 clusters at 0.15<z<0.45, for which robust velocity dispersions are measured. We were awarded Suzaku/Chandra observations of 11 high-dispersion, low-z targets. Suzaku's superior throughput is required to complete the low-dispersion, high-z side of the distribution. We propose XIS observations of the remaining 2 targets, allowing us to rigorously assess baryon content in an unbiased sample of clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 5 | AO5 | DECIPHERING CLUSTER OBSERVABLES: TRACING THE BARYONS IN CLUSTERS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805089010/ | Quick Look | ![]() |
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584 | COMET_8P_TUTTLE-P2_11 | 40.2448 | -37.071 | 39.739892 | -37.284352 | 20.945205 | -49.302594 | 243.11250517 | -64.87732742 | 253.5002 | 54491.3630439815 | 2008-01-26 08:42:47 | 54491.4959953704 | 2008-01-26 11:54:14 | 502063110 | 6.3822 | 6.7 | 6.3902 | 6.3822 | 0 | 6.3902 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6.8385 | 6.8385 | 11.4799 | 0 | PROCESSED | 57541.406712963 | 2016-06-02 09:45:40 | 54912 | 2009-03-22 00:00:00 | 54546.1994097222 | 2008-03-21 04:47:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063110/ | Quick Look | ![]() |
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585 | A133_FIELD_3 | 15.3292 | -22.0955 | 14.718033 | -22.364433 | 4.799478 | -26.269218 | 147.50079252 | -84.48957915 | 231.9998 | 56631.4102314815 | 2013-12-05 09:50:44 | 56632.6168981482 | 2013-12-06 14:48:20 | 808083010 | 51.8568 | 50 | 51.8568 | 51.8568 | 0 | 51.8568 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.9569 | 47.9569 | 104.2418 | 0 | PROCESSED | 57613.5483217593 | 2016-08-13 13:09:35 | 57009 | 2014-12-18 00:00:00 | 56643.7003587963 | 2013-12-17 16:48:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081525 | We propose observations of the outskirts of Abell 133, a relaxed galaxy cluster that is the target of a Chandra X-ray Visionary Project. These modest Suzaku observations will leverage the 2.4 Msec of Chandra time spent deeply imaging the region beyond r_500 to search for ICM clumping. Such clumping has been invoked to explain the flat entropy profiles and excess inferred gas fraction beyond r_500 in several clusters observed recently with Suzaku. The proposed Suzaku observations combined with the unprecedented Chandra depth will create a fiducial dataset to compare to the existing Suzaku cluster outskirts data, and they will definitely determine whether the excess inferred gas fractions seen with Suzaku arise from gas clumping. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 8 | AO8 | A DEFINITIVE STUDY OF GALAXY CLUSTER OUTSKIRTS WITH SUZAKU AND CHANDRA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808083010/ | Quick Look | ![]() |
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586 | A133_FIELD_4 | 16.0019 | -22.0663 | 15.391978 | -22.334366 | 5.44253 | -26.509377 | 153.04375578 | -84.18809016 | 231.9997 | 56632.6176967593 | 2013-12-06 14:49:29 | 56633.8716666667 | 2013-12-07 20:55:12 | 808084010 | 52.5282 | 50 | 52.5282 | 52.5282 | 0 | 52.5282 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.912 | 49.912 | 108.3281 | 0 | PROCESSED | 57613.5467013889 | 2016-08-13 13:07:15 | 57061 | 2015-02-08 00:00:00 | 56695.6415046296 | 2014-02-07 15:23:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081525 | We propose observations of the outskirts of Abell 133, a relaxed galaxy cluster that is the target of a Chandra X-ray Visionary Project. These modest Suzaku observations will leverage the 2.4 Msec of Chandra time spent deeply imaging the region beyond r_500 to search for ICM clumping. Such clumping has been invoked to explain the flat entropy profiles and excess inferred gas fraction beyond r_500 in several clusters observed recently with Suzaku. The proposed Suzaku observations combined with the unprecedented Chandra depth will create a fiducial dataset to compare to the existing Suzaku cluster outskirts data, and they will definitely determine whether the excess inferred gas fractions seen with Suzaku arise from gas clumping. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 8 | AO8 | A DEFINITIVE STUDY OF GALAXY CLUSTER OUTSKIRTS WITH SUZAKU AND CHANDRA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808084010/ | Quick Look | ![]() |
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587 | ABELL 1068 | 160.2123 | 39.7867 | 159.491465 | 40.048011 | 145.700686 | 28.920989 | 179.4205229 | 60.1860041 | 130.0008 | 55863.1263310185 | 2011-10-29 03:01:55 | 55864.5459837963 | 2011-10-30 13:06:13 | 806028030 | 53.3186 | 50 | 53.3186 | 53.335 | 0 | 53.3266 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.0713 | 49.0713 | 122.6438 | 0 | PROCESSED | 57603.6522800926 | 2016-08-03 15:39:17 | 55652 | 2011-04-01 00:00:00 | 55874.122662037 | 2011-11-09 02:56:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061116 | We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 6 | AO6-LP | THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806028030/ | Quick Look | ![]() |
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588 | A426VIR N | 48.9538 | 42.7811 | 48.120761 | 42.596803 | 58.224249 | 23.764199 | 149.23070312 | -12.5987294 | 270.5957 | 56710.5023726852 | 2014-02-22 12:03:25 | 56711.155775463 | 2014-02-23 03:44:19 | 808087010 | 23.3776 | 25 | 23.3856 | 23.3856 | 0 | 23.3776 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.5612 | 20.5612 | 56.4419 | 0 | PROCESSED | 57613.8896296296 | 2016-08-13 21:21:04 | 57089 | 2015-03-08 00:00:00 | 56723.6141898148 | 2014-03-07 14:44:26 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081526 | Our analysis of Suzaku Key Project data of the Perseus Cluster of galaxies has uncovered a significant drop in temperature, density and derived thermodynamic properties of the intra-cluster medium in the NW direction at the cluster's virial radius, suggesting the presence of a strong shock. In order to firmly confirm and further explore this feature we propose to expand upon the observation of this region. Confirmation of a shock at the virial radius will provide the first ever direct observation of the formation of a galaxy cluster and virialization of the in-falling hot gas. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ONDREJ URBAN | USA | 8 | AO8 | SHOCK FRONT AT THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808087010/ | Quick Look | ![]() |
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589 | A426VIR W | 48.7321 | 42.6495 | 47.900602 | 42.4644 | 58.012629 | 23.684677 | 149.16205221 | -12.79713949 | 270.0001 | 56711.1564351852 | 2014-02-23 03:45:16 | 56711.6279976852 | 2014-02-23 15:04:19 | 808088010 | 24.7428 | 25 | 24.7587 | 24.7428 | 0 | 24.7667 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22.0168 | 22.0168 | 40.7359 | 0 | PROCESSED | 57613.8909259259 | 2016-08-13 21:22:56 | 57141 | 2015-04-29 00:00:00 | 56764.7613657407 | 2014-04-17 18:16:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081526 | Our analysis of Suzaku Key Project data of the Perseus Cluster of galaxies has uncovered a significant drop in temperature, density and derived thermodynamic properties of the intra-cluster medium in the NW direction at the cluster's virial radius, suggesting the presence of a strong shock. In order to firmly confirm and further explore this feature we propose to expand upon the observation of this region. Confirmation of a shock at the virial radius will provide the first ever direct observation of the formation of a galaxy cluster and virialization of the in-falling hot gas. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ONDREJ URBAN | USA | 8 | AO8 | SHOCK FRONT AT THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808088010/ | Quick Look | ![]() |
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590 | ABELL 1689 (OFFSET) | 198.1886 | -1.1923 | 197.54634 | -0.927328 | 197.227317 | 6.029723 | 314.05162405 | 61.21838483 | 111.865 | 56657.0769444444 | 2013-12-31 01:50:48 | 56660.6460069445 | 2014-01-03 15:30:15 | 808089030 | 53.2272 | 130 | 53.2272 | 53.2272 | 0 | 53.2272 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 3.3279 | 0 | PROCESSED | 57613.7319791667 | 2016-08-13 17:34:03 | 56383 | 2013-04-01 00:00:00 | 56713.6636342593 | 2014-02-25 15:55:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081528 | Recent Suzaku results suggest that the surface brightness in galaxy cluster outskirts is higher than the predictions by self-similar models, indicating that the gas may be clumpy or may not be in collisional equilibrium near and beyond the virial radius. If this is the case, gas emission near cosmological accretion shocks should readily be detected. We propose to search for emission near the accretion shock radius where it is the only region unexplored in galaxy cluster studies in X-ray. These data can place important constraints on accretion models and large-scale structure formation theory. Physical properties at the true virial radius (R100) will also be measured to the highest precision to date. A very deep exposure and the low Suzaku background allow this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KA-WAH WONG | USA | 8 | AO8 | SEARCH FOR ACCRETION SHOCK IN A MASSIVE GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808089030/ | Quick Look | ![]() |
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591 | ABELL 1689 (OFFSET) | 198.1809 | -1.2604 | 197.538539 | -0.995417 | 197.246177 | 5.963813 | 314.01167358 | 61.15261163 | 111.9001 | 56670.9898148148 | 2014-01-13 23:45:20 | 56672.9376388889 | 2014-01-15 22:30:12 | 808089040 | 37.4667 | 90 | 37.4667 | 37.4667 | 0 | 37.4667 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.7681134259 | 2016-08-13 18:26:05 | 56383 | 2013-04-01 00:00:00 | 56687.7783564815 | 2014-01-30 18:40:50 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081528 | Recent Suzaku results suggest that the surface brightness in galaxy cluster outskirts is higher than the predictions by self-similar models, indicating that the gas may be clumpy or may not be in collisional equilibrium near and beyond the virial radius. If this is the case, gas emission near cosmological accretion shocks should readily be detected. We propose to search for emission near the accretion shock radius where it is the only region unexplored in galaxy cluster studies in X-ray. These data can place important constraints on accretion models and large-scale structure formation theory. Physical properties at the true virial radius (R100) will also be measured to the highest precision to date. A very deep exposure and the low Suzaku background allow this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KA-WAH WONG | USA | 8 | AO8 | SEARCH FOR ACCRETION SHOCK IN A MASSIVE GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808089040/ | Quick Look | ![]() |
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592 | COMA W SHOCK2 | 194.0639 | 28.3374 | 193.459144 | 28.607762 | 180.49458 | 31.367738 | 81.80911298 | 88.38803012 | 275.4001 | 56475.6616782407 | 2013-07-02 15:52:49 | 56476.1674884259 | 2013-07-03 04:01:11 | 808091010 | 15.6934 | 15 | 15.7094 | 15.6934 | 0 | 15.7094 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.6254 | 16.6254 | 43.694 | 0 | PROCESSED | 57611.6755902778 | 2016-08-11 16:12:51 | 56858 | 2014-07-20 00:00:00 | 56492.6168865741 | 2013-07-19 14:48:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081529 | Our analysis of Suzaku data of the Coma Cluster revealed an intriguing correlation between the outer edge of its radio halo and the thermodynamic properties of the gas. This correlation seems to be the most pronounced in the western direction where the temperature drops from about 10keV in the annulus spanning 35'-41' to only 1.7keV in the annulus spanning 50'-60'. The Planck Collaboration found a marked local steepening of the radial gradient of the SZ signal at this location and interpret this feature as a shock with a Mach number of about 2. Unfortunately, we currently lack X-ray coverage towards the W in this critical range of 41'-50'. We therefore propose two additional pointings with a total exposure time of 30ks, that will allow us to resolve the temperature gradient in this region. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | AURORA SIMIONESCU | USA | 8 | AO8 | THE MISSING PUZZLE PIECE IN THE COMA SHOCK FRONT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808091010/ | Quick Look | ![]() |
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593 | COMA NW6 | 194.1545 | 29.4183 | 193.551623 | 29.688554 | 179.999631 | 32.366617 | 96.76135884 | 87.44172405 | 319.9992 | 55734.4158796296 | 2011-06-22 09:58:52 | 55734.7419328704 | 2011-06-22 17:48:23 | 806044010 | 13.52 | 15 | 13.52 | 13.52 | 0 | 13.52 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.5945 | 11.5945 | 28.1679 | 1 | PROCESSED | 57602.3747453704 | 2016-08-02 08:59:38 | 55652 | 2011-04-01 00:00:00 | 55768.2886574074 | 2011-07-26 06:55:40 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806044010/ | Quick Look | ![]() |
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594 | BEYOND VIRGO 3 | 187.7131 | 16.6287 | 187.083239 | 16.904753 | 180.24751 | 18.281087 | 277.46526397 | 78.4695575 | 119.4716 | 55906.3990277778 | 2011-12-11 09:34:36 | 55907.0070717593 | 2011-12-12 00:10:11 | 806062010 | 24.1336 | 30 | 24.1336 | 24.1336 | 0 | 24.1336 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22.399 | 22.399 | 52.5119 | 1 | PROCESSED | 57604.102974537 | 2016-08-04 02:28:17 | 56289 | 2012-12-28 00:00:00 | 55920.9612731482 | 2011-12-25 23:04:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061523 | To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NORBERT WERNER | USA | 6 | AO6 | LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806062010/ | Quick Look | ![]() |
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595 | BEYOND VIRGO 5 | 187.715 | 17.1647 | 187.085509 | 17.440751 | 180.014258 | 18.769278 | 276.35604201 | 78.95966269 | 118.1329 | 55918.8504976852 | 2011-12-23 20:24:43 | 55919.8960300926 | 2011-12-24 21:30:17 | 806064010 | 41.7692 | 40 | 41.7772 | 41.7692 | 0 | 41.7772 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.3124 | 34.3124 | 90.2919 | 1 | PROCESSED | 57604.2418402778 | 2016-08-04 05:48:15 | 56340 | 2013-02-17 00:00:00 | 55972.6886458333 | 2012-02-15 16:31:39 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061523 | To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NORBERT WERNER | USA | 6 | AO6 | LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806064010/ | Quick Look | ![]() |
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596 | BEYOND VIRGO 7 | 187.7158 | 17.6999 | 187.086679 | 17.97595 | 179.778986 | 19.25601 | 275.1422843 | 79.44418151 | 118.4175 | 55920.9292708333 | 2011-12-25 22:18:09 | 55922.3029166667 | 2011-12-27 07:16:12 | 806066010 | 51.5018 | 50 | 51.5258 | 51.5178 | 0 | 51.5018 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.0209 | 45.0209 | 118.6698 | 0 | PROCESSED | 57604.2629861111 | 2016-08-04 06:18:42 | 56340 | 2013-02-17 00:00:00 | 55972.6991203704 | 2012-02-15 16:46:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061523 | To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NORBERT WERNER | USA | 6 | AO6 | LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806066010/ | Quick Look | ![]() |
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597 | RCS211853-6334.5 | 319.7157 | -63.5732 | 318.707212 | -63.784045 | 298.683481 | -45.002818 | 330.73727963 | -40.23433007 | 78.3879 | 55689.9756018518 | 2011-05-08 23:24:52 | 55691.0148148148 | 2011-05-10 00:21:20 | 806079010 | 69.5446 | 70 | 69.5526 | 69.5446 | 0 | 69.5526 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57.3836 | 57.3836 | 89.7739 | 0 | PROCESSED | 57601.9954398148 | 2016-08-01 23:53:26 | 56068 | 2012-05-21 00:00:00 | 55701.1727314815 | 2011-05-20 04:08:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061533 | Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 19 optically-selected clusters of galaxies, half at z~0.3 and half at z~0.8. Here we propose 6 additional observations in order to uniformly span a total redshift range of 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | AMALIA HICKS | USA | 6 | AO6 | AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806079010/ | Quick Look | ![]() |
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598 | OFF-FIELD1 | 154.5616 | 22.312 | 153.870987 | 22.562652 | 148.318203 | 10.965902 | 212.25034337 | 55.01303699 | 298.5999 | 56782.6031712963 | 2014-05-05 14:28:34 | 56783.5417939815 | 2014-05-06 13:00:11 | 809052010 | 41.103 | 40 | 41.103 | 41.103 | 0 | 41.103 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.0283 | 39.0283 | 81.0719 | 1 | PROCESSED | 57615.0526388889 | 2016-08-15 01:15:48 | 57162 | 2015-05-20 00:00:00 | 56793.5659490741 | 2014-05-16 13:34:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091501 | Late-type galaxies in the Local Universe are missing over 70% of their baryonic mass, a large fraction of which is likely embedded in the extended, low density warm-hot gaseous halo. However, searches of hot diffuse halos around massive spiral galaxies found them to be relatively small and not very massive. The UV observations have shown that the baryonic halo mass depends on the specific star formation rate (sSFR) and not on the total mass of the galaxy. We propose to observe the halo emission of NGC3221 with very high sSFR. Detection and characterization of the hot halo around this galaxy will expand our understanding of the dependence of halo properties on galaxy properties, and advance our understanding of galaxy formation, feedback and metal enrichment proposed by theoretical models. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | ANJALI GUPTA | USA | 9 | AO9 | SEARCH FOR THE HOT GASEOUS HALO AROUND THE NEARBY SPIRAL GALAXY NGC3221 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809052010/ | Quick Look | ![]() |
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599 | ABELL 98-SOUTH | 11.6766 | 20.275 | 11.015845 | 20.00206 | 18.757977 | 14.029978 | 121.42486866 | -42.58290308 | 251.4904 | 57011.5401736111 | 2014-12-20 12:57:51 | 57012.9168171296 | 2014-12-21 22:00:13 | 809080010 | 48.2579 | 100 | 48.2579 | 49.0544 | 0 | 49.1104 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5485532407 | 2016-08-17 13:09:55 | 56748 | 2014-04-01 00:00:00 | 57107.4443171296 | 2015-03-26 10:39:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091525 | We propose to observe the outskirts of the strongly merging cluster Abell 98 both along and perpendicular to the large scale structure filament implied by the orientation of its three merging subclusters. This is the only remaining one of the four bright, strongly merging "double" clusters originally identified from Einstein observations that has not been observed with Suzaku. A comparison of the extended atmosphere in the filament and off-filament pointings will allow us to test for the presence of unresolved gas clumps, which should be more abundant along the filament, invoked to explain anomalously high (above cosmic) baryon fractions observed in some other clusters. If this "unresolved clumps" hypothesis is correct, then we should find higher baryon fractions along the filament. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SCOTT RANDALL | USA | 9 | AO9 | EXPLORING THE EXTENDED ATMOSPHERE OF THE STRONGLY MERGING CLUSTER ABELL 98 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809080010/ | Quick Look | ![]() |
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600 | ABELL 3411 OFFSET | 130.7649 | -17.3143 | 130.18997 | -17.133567 | 138.838529 | -34.101685 | 241.9812862 | 15.18552207 | 105.3327 | 56967.309849537 | 2014-11-06 07:26:11 | 56968.1939467593 | 2014-11-07 04:39:17 | 809083010 | 38.952 | 39 | 38.952 | 39.272 | 0 | 39.288 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7398263889 | 2016-08-16 17:45:21 | 57358 | 2015-12-02 00:00:00 | 56982.4550231482 | 2014-11-21 10:55:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091528 | Galaxy cluster mergers trigger Mpc-scale shocks in the ICM, which can accelerate particles to relativistic energies to form arc-shaped radio relics. Last year, we discovered a spectacular radio relic in the Planck cluster A3411. The relic has a complex, fragmentary morphology, at odds with the arc-shaped shocks predicted by hydrodynamical simulations. In light of this unexpected discovery, we propose for a 169-ks Suzaku observation to characterize the ICM properties at the radio relic in A3411. The combination of high-quality X-ray and radio data will provide a unique opportunity to (1) measure the shock properties and relate them to the radio structures; (2) explore the reason for the fragmentation of the relic; (3) model the merger event; and (4) test different shock acceleration models. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | REINOUT VAN WEEREN | USA | 9 | AO9 | ABELL 3411: PARTICLE RE-ACCELERATION AND A COMPLEX SHOCK GEOMETRY? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809083010/ | Quick Look | ![]() |
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601 | SWCL1330+4206 | 202.7007 | 42.1031 | 202.156429 | 42.360378 | 179.6615 | 46.801465 | 97.22165079 | 73.00355707 | 325.866 | 57166.2929166667 | 2015-05-24 07:01:48 | 57167.0793171296 | 2015-05-25 01:54:13 | 809088020 | 34.7796 | 34 | 34.7796 | 34.7876 | 0 | 34.7796 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 21.0686 | 21.0686 | 53.048 | 1 | PROCESSED | 57618.72625 | 2016-08-18 17:25:48 | 57548 | 2016-06-09 00:00:00 | 57178.157025463 | 2015-06-05 03:46:07 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091531 | The evolution of X-ray properties of galaxy clusters with redshift provides important constraints on the self-similar models of cluster evolution. The scaling relations and their deviations from self-similar models due to non-gravitational processes are important for modeling the cluster selection function for cosmology. We propose to observe a uniform sample of z ~ 0.6 galaxy clusters, selected from Swift archival data and confirmed by multi-band optical data, using Suzaku to better characterize their X-ray properties such as the X-ray luminosity and temperature. With this uniformly selected sample from a narrow redshift bin, we are able to independently constrain the self-similar evolution of cluster properties with redshift. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | XINYU DAI | USA | 9 | AO9 | X-RAY PROPERTIES OF A UNIFORMLY SELECTED SAMPLE OF Z ~ 0.6 CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809088020/ | Quick Look | ![]() |
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602 | FG09 | 160.7604 | 0.8965 | 160.118108 | 1.158829 | 161.901438 | -6.701816 | 247.95154277 | 49.5505044 | 288.8833 | 56077.2212731482 | 2012-05-30 05:18:38 | 56077.5397337963 | 2012-05-30 12:57:13 | 807050010 | 12.49 | 10 | 12.4944 | 12.49 | 0 | 12.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.8506 | 10.8506 | 27.5119 | 0 | PROCESSED | 57605.5584722222 | 2016-08-05 13:24:12 | 56462 | 2013-06-19 00:00:00 | 56096.107662037 | 2012-06-18 02:35:02 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071511 | Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ELENA D'ONGHIA | USA | 7 | AO7 | SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807050010/ | Quick Look | ![]() |
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603 | FG03 | 118.182 | 45.9572 | 117.286088 | 46.086737 | 111.16384 | 24.564923 | 173.26592635 | 29.42392711 | 92.9981 | 56228.7772453704 | 2012-10-28 18:39:14 | 56229.1078819444 | 2012-10-29 02:35:21 | 807052010 | 14.3185 | 10 | 14.3265 | 14.3185 | 0 | 14.3345 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15.365 | 15.365 | 28.544 | 0 | PROCESSED | 57607.868125 | 2016-08-07 20:50:06 | 56696 | 2014-02-08 00:00:00 | 56330.5013541667 | 2013-02-07 12:01:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071511 | Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ELENA D'ONGHIA | USA | 7 | AO7 | SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807052010/ | Quick Look | ![]() |
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604 | ANTLIA NW4 | 156.477 | -34.4731 | 155.913183 | -34.218342 | 174.203454 | -40.552676 | 271.69853818 | 19.42589093 | 299.2985 | 57168.4177546296 | 2015-05-26 10:01:34 | 57169.4605902778 | 2015-05-27 11:03:15 | 810066010 | 6.3596 | 40 | 6.3596 | 6.8635 | 0 | 6.8635 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 6.7341 | 6.7341 | 78.0621 | 0 | PROCESSED | 57618.7963657407 | 2016-08-18 19:06:46 | 57626 | 2016-08-26 00:00:00 | 57178.2408101852 | 2015-06-05 05:46:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 101522 | We have measured hot gas properties of the nearest non-cool core cluster, Antlia, in the eastern direction out to R200. Our initial results suggest that its density profile is more consistent with some massive clusters, but significantly steeper than its cool core counterpart with a similar temperature (mass), Virgo. We propose to extend our program to observe two other directions to test azimuthal variation, which is likely to be significant. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KA-WAH WONG | USA | 10 | AO10 | MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/810066010/ | Quick Look | ![]() |
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605 | FG26 | 237.2323 | 8.8441 | 236.628181 | 8.995997 | 232.656986 | 28.135005 | 17.92603672 | 44.32356312 | 282.0742 | 56137.0874305556 | 2012-07-29 02:05:54 | 56137.3307986111 | 2012-07-29 07:56:21 | 807054010 | 11.8912 | 10 | 11.8912 | 11.8912 | 0 | 11.8912 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.5983 | 8.5983 | 20.9999 | 0 | PROCESSED | 57606.6870023148 | 2016-08-06 16:29:17 | 56626 | 2013-11-30 00:00:00 | 56260.480474537 | 2012-11-29 11:31:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071511 | Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ELENA D'ONGHIA | USA | 7 | AO7 | SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807054010/ | Quick Look | ![]() |
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606 | ANTLIA E2 | 158.2496 | -35.3292 | 157.682674 | -35.071089 | 176.423673 | -40.599314 | 273.48585529 | 19.50669913 | 277.9997 | 56092.2642361111 | 2012-06-14 06:20:30 | 56093.0181944444 | 2012-06-15 00:26:12 | 807067010 | 24.1741 | 23 | 24.1821 | 24.1741 | 0 | 24.1901 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.8534 | 22.8534 | 65.1359 | 3 | PROCESSED | 57605.6727546296 | 2016-08-05 16:08:46 | 56476 | 2013-07-03 00:00:00 | 56110.5259027778 | 2012-07-02 12:37:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071521 | We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KA-WAH WONG | USA | 7 | AO7 | MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807067010/ | Quick Look | ![]() |
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607 | ABELL 2597 | 351.2512 | -12.298 | 350.600815 | -12.572949 | 347.099073 | -7.834502 | 64.91051751 | -64.90126459 | 250.0013 | 56264.7750115741 | 2012-12-03 18:36:01 | 56266.2606134259 | 2012-12-05 06:15:17 | 807073040 | 54.7187 | 50 | 54.7187 | 54.7427 | 0 | 54.7267 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.919 | 47.919 | 128.3278 | 1 | PROCESSED | 57608.2146759259 | 2016-08-08 05:09:08 | 56018 | 2012-04-01 00:00:00 | 56279.7033912037 | 2012-12-18 16:52:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071522 | We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 7 | AO7 | COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807073040/ | Quick Look | ![]() |
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608 | COMA NW7 | 194.0035 | 29.6909 | 193.400635 | 29.961328 | 179.713479 | 32.548963 | 101.76403044 | 87.24693436 | 319.9995 | 55735.2525925926 | 2011-06-23 06:03:44 | 55735.5383680556 | 2011-06-23 12:55:15 | 806046010 | 16.1218 | 15 | 16.1514 | 16.1458 | 0 | 16.1218 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14.8517 | 14.8517 | 24.6879 | 0 | PROCESSED | 57602.3868518518 | 2016-08-02 09:17:04 | 55652 | 2011-04-01 00:00:00 | 55768.6489930556 | 2011-07-26 15:34:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806046010/ | Quick Look | ![]() |
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609 | I ZW 18 | 143.5151 | 55.2494 | 142.632451 | 55.471905 | 125.701519 | 38.241912 | 160.51246258 | 44.84288886 | 130.2629 | 56934.0191666667 | 2014-10-04 00:27:36 | 56935.6258680556 | 2014-10-05 15:01:15 | 709021020 | 82.0708 | 70 | 82.0708 | 82.0868 | 0 | 82.0868 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6143865741 | 2016-08-16 14:44:43 | 57358 | 2015-12-02 00:00:00 | 56989.5111689815 | 2014-11-28 12:16:05 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091441 | The source of energetic photons that reionized and heated the early universe remains uncertain. Early galaxies had low metallicity and the best local analogs are blue compact dwarf galaxies (BCDs) with low metallicity. We propose to observe two such galaxies known to be luminous in X-rays and accurately measure their spectrum with the Suzaku XIS. These observations are important to our understanding of the heating of the universe during the epoch of reionization. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | PHILIP KAARET | USA | 9 | AO9 | X-RAYS FROM LOW-METALLICITY BLUE COMPACT DWARF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709021020/ | Quick Look | ![]() |
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610 | A2061 | 230.3095 | 30.6453 | 229.795666 | 30.824015 | 216.361499 | 46.967712 | 48.13899774 | 57.1713197 | 293.2901 | 53943.6955092593 | 2006-07-27 16:41:32 | 53943.9946643518 | 2006-07-27 23:52:19 | 801081010 | 13.8887 | 14 | 13.9047 | 13.9047 | 13.8887 | 13.8967 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 11.8443 | 11.8443 | 25.8399 | 0 | PROCESSED | 57535.0552083333 | 2016-05-27 01:19:30 | 54401 | 2007-10-28 00:00:00 | 53955.6442939815 | 2006-08-08 15:27:47 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801081010/ | Quick Look | ![]() |
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611 | A2249 | 257.46 | 34.4851 | 257.00595 | 34.546595 | 250.753931 | 57.089244 | 57.64541352 | 34.94797305 | 129.9858 | 54114.5939467593 | 2007-01-14 14:15:17 | 54115.1252777778 | 2007-01-15 03:00:24 | 801082010 | 22.8156 | 15 | 22.8156 | 22.8236 | 0 | 22.8236 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19.7637 | 19.7637 | 45.9039 | 1 | PROCESSED | 57536.8308333333 | 2016-05-28 19:56:24 | 54695 | 2008-08-17 00:00:00 | 54133.0295833333 | 2007-02-02 00:42:36 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801082010/ | Quick Look | ![]() |
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612 | VELA PWN NE3 | 131.0442 | -44.0836 | 130.607036 | -43.901563 | 154.967747 | -58.624056 | 263.64329985 | -0.87547181 | 123.9937 | 55895.188900463 | 2011-11-30 04:32:01 | 55895.621724537 | 2011-11-30 14:55:17 | 506043010 | 17.7999 | 15 | 17.8066 | 17.7999 | 0 | 17.8066 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.012 | 13.012 | 37.3959 | 0 | PROCESSED | 57604.0129050926 | 2016-08-04 00:18:35 | 56274 | 2012-12-13 00:00:00 | 55907.1603703704 | 2011-12-12 03:50:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | C | SATORU KATSUDA | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506043010/ | Quick Look | ![]() |
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613 | VELA PWN E1 | 129.1398 | -45.2732 | 128.71724 | -45.098238 | 153.84788 | -60.334335 | 263.75797839 | -2.67419196 | 142.334 | 55916.0561226852 | 2011-12-21 01:20:49 | 55916.622337963 | 2011-12-21 14:56:10 | 506044010 | 17.718 | 15 | 17.718 | 17.718 | 0 | 17.718 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.6284 | 16.6284 | 48.8959 | 0 | PROCESSED | 57604.1814814815 | 2016-08-04 04:21:20 | 56305 | 2013-01-13 00:00:00 | 55937.7696527778 | 2012-01-11 18:28:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | C | SATORU KATSUDA | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506044010/ | Quick Look | ![]() |
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614 | HB9-WEST | 74.7057 | 46.2322 | 73.785793 | 46.156635 | 78.534376 | 23.399217 | 160.54700874 | 2.22396757 | 74.7402 | 56930.7930671296 | 2014-09-30 19:02:01 | 56931.9168518518 | 2014-10-01 22:00:16 | 509032010 | 49.7688 | 50 | 49.7688 | 49.7688 | 0 | 49.7688 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5952662037 | 2016-08-16 14:17:11 | 57345 | 2015-11-19 00:00:00 | 56979.4048611111 | 2014-11-18 09:43:00 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091312 | We propose to conduct two pointed observations of the Galactic supernova remnant (SNR) HB9 (G160.9+2.6) with Suzaku. HB9 is a member of the class of Galactic SNRs which are distinguished by their contrasting radio and X-ray morphologies. Prior X-ray observations of HB9 have suggested that the SNR may have a hard component to its X-ray emission, but the true nature of this emission and its origin (a background AGN, intercluster gas associated with the cluster that harbors the AGN or the SNR itself) remains elusive. Our proposed observations will help identify the true nature of the hard emission as well as search for spectral variations (and possible overionization) in the properties of the X-ray emitting plasma associated with the SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | THOMAS PANNUTI | USA | 9 | AO9 | SUZAKU OBSERVATIONS OF THE GALACTIC SUPERNOVA REMNANT HB9 (G160.9+2.6) | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509032010/ | Quick Look | ![]() |
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615 | 3C279 | 194.0685 | -5.7338 | 193.421343 | -5.463366 | 195.163667 | 0.26086 | 305.14803375 | 57.11713803 | 113.6423 | 54850.9795833333 | 2009-01-19 23:30:36 | 54853.9391203704 | 2009-01-22 22:32:20 | 703049010 | 134.1106 | 200 | 134.1106 | 134.1106 | 0 | 134.1106 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82.8563 | 82.8563 | 255.689 | 7 | PROCESSED | 57545.3939351852 | 2016-06-06 09:27:16 | 55328 | 2010-05-12 00:00:00 | 54880.5781365741 | 2009-02-18 13:52:31 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031346 | We propose a 200 ks observation of 3C279, the archetypal EGRET blazar to be conducted simultaneously with GLAST as well as many other facilities, with the goal of obtaining broadband spectra and light-curves. The flux in all observable bands is known to be rapidly variable, but the information regarding the correlation between the time history of flux in various bands is limited, and the proposed observations are designed to remedy this shortcoming. Such detailed spectral and variability studies are crucial to discriminate between different radiation scenarios responsible for production of X-rays and gamma-rays, and to constrain the matter content and by extension, the formation process of the jet, dissipation of the jet energy, and energization of the radiating particles. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GRZEGORZ MADEJSKI | USA | 3 | AO3 | SUZAKU AND GLAST OBSERVATIONS OF 3C279 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703049010/ | Quick Look | ![]() |
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616 | NGC 4258 | 184.7518 | 47.3153 | 184.134648 | 47.592794 | 160.376562 | 44.164981 | 138.28789039 | 68.83430148 | 139.1798 | 55511.1601388889 | 2010-11-11 03:50:36 | 55512.7112615741 | 2010-11-12 17:04:13 | 705051010 | 103.8332 | 100 | 103.8332 | 103.8412 | 0 | 103.837 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86.2257 | 86.2257 | 133.9688 | 1 | PROCESSED | 57554.0812384259 | 2016-06-15 01:56:59 | 55903 | 2011-12-08 00:00:00 | 55537.1754398148 | 2010-12-07 04:12:38 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051451 | We request a 100 ksec observation of the Low Luminosity AGN NGC 4258. This observation is meant to complement our existing 100 ksec Suzaku observation (Reynolds et al. 2009), and our 320 ksec Chandra-HETG observation (Murphy et al., in prep.). The goal is to further characterize the observed variability of the Fe Kalpha line and any associated changes in the continuum and/or absorption of NGC 4258. Given the unique constraints that we have on the mass, distance and accretion flow geometry in NGC 4258, as well as its role as a bridge between the most quiescent nuclei and powerful AGN, further Suzaku studies of NGC 4258 are clearly warranted. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | MICHAEL NOWAK | USA | 5 | AO5 | HUNTING FOR THE VARIABLE IRON LINE IN NGC 4258 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705051010/ | Quick Look | ![]() |
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617 | NGC 720 OFFSET | 28.2673 | -13.4983 | 27.658292 | -13.744232 | 21.049561 | -23.414412 | 172.55217141 | -70.17529179 | 242.404 | 55560.2543634259 | 2010-12-30 06:06:17 | 55565.2502083333 | 2011-01-04 06:00:18 | 805069010 | 223.9663 | 150 | 223.9722 | 223.9663 | 0 | 223.9722 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.3571 | 13.3571 | 28.3639 | 0 | PROCESSED | 57600.5655671296 | 2016-07-31 13:34:25 | 55994 | 2012-03-08 00:00:00 | 55627.1378009259 | 2011-03-07 03:18:26 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051503 | Models of galaxy formation suggest that as many as half the baryons may reside in an extended, hot halo. Detecting such a halo around a disk galaxy is, however, extremely challenging for current instrumentation. We propose instead to measure the baryon content of an isolated, X-ray bright elliptical galaxy (Mvir~6E12Msun), which provides the best opportunity to take a census of the baryons in a normal, galaxy-scale system. Currently little is known about the total baryon content of such objects, which are the likely end points of spiral galaxy merging. Combined with archival data, our offset pointing will enable the gas to be traced to ~0.75R500, comparable to what has been achieved for galaxy groups and clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | PHILIP HUMPHREY | USA | 5 | AO5 | THE BARYON FRACTION OF AN ISOLATED ELLIPTICAL GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805069010/ | Quick Look | ![]() |
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618 | MKW4 | 181.137 | 1.9141 | 180.496491 | 2.192466 | 180.278577 | 2.208157 | 276.9409609 | 62.39583381 | 136.3986 | 56655.392662037 | 2013-12-29 09:25:26 | 56656.271099537 | 2013-12-30 06:30:23 | 808066010 | 34.57 | 30 | 34.57 | 34.57 | 0 | 34.57 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.1435 | 30.1435 | 75.8879 | 0 | PROCESSED | 57613.7104861111 | 2016-08-13 17:03:06 | 57033 | 2015-01-11 00:00:00 | 56667.6362268518 | 2014-01-10 15:16:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081512 | We propose to observe the MKW4 group by leveraging existing observations to provide coverage from its center to its virial radius in two orthogonal directions. Three additional pointings, totaling 230 ksec, combined with two existing pointings, will allow us to determine radial profiles of gas temperature, density, entropy, pressure, and gas mass fraction, as well as their azimuthal variations. Comparing these properties to those of clusters will allow us to probe the role played by baryonic physics and assess the imprints of hierarchical structure formation. The stable and low background of the Suzaku XIS is crucial for the study of galaxy groups to their virial radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUANYUAN SU | USA | 8 | AO8 | PROBING A TYPICAL GALAXY GROUP TO ITS VIRAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808066010/ | Quick Look | ![]() |
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619 | JUPITER | 226.6349 | -16.1983 | 225.936085 | -16.00589 | 228.727521 | 1.247844 | 344.01962259 | 35.67652355 | 118.4908 | 53793.86 | 2006-02-27 20:38:24 | 53794.9585532407 | 2006-02-28 23:00:19 | 401001040 | 42.2558 | 36 | 42.2638 | 42.2638 | 42.2638 | 42.2558 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35.7067 | 35.7067 | 94.9059 | 2 | PROCESSED | 57533.1103819444 | 2016-05-25 02:38:57 | 54401 | 2007-10-28 00:00:00 | 53906.5712615741 | 2006-06-20 13:42:37 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011003 | We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure. | GALACTIC POINT SOURCES | 4 | C | RONALD ELSNER | USA | 1 | AO1 | JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401001040/ | Quick Look | ![]() |
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620 | 73P/SW3 | 18.1606 | -9.2654 | 17.534064 | -9.530431 | 13.093401 | -15.671197 | 139.58635244 | -71.44823165 | 59.3999 | 53894.1358333333 | 2006-06-08 03:15:36 | 53894.2085416667 | 2006-06-08 05:00:18 | 500014080 | 1.8637 | 35 | 1.8637 | 1.8637 | 1.8637 | 1.8637 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 1.9212 | 1.9212 | 6.2779 | 0 | PROCESSED | 57534.5937731482 | 2016-05-26 14:15:02 | 54267 | 2007-06-16 00:00:00 | 54052.5243171296 | 2006-11-13 12:35:01 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014080/ | Quick Look | ![]() |
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621 | 73P/SW3 | 18.3869 | -9.3535 | 17.760674 | -9.618192 | 13.270909 | -15.839893 | 140.33698221 | -71.47421859 | 59.3991 | 53894.4684490741 | 2006-06-08 11:14:34 | 53894.5356365741 | 2006-06-08 12:51:19 | 500014130 | 1.6939 | 35 | 1.6939 | 1.6939 | 1.6939 | 1.6939 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1.694 | 1.694 | 5.804 | 0 | PROCESSED | 57534.6023611111 | 2016-05-26 14:27:24 | 54267 | 2007-06-16 00:00:00 | 54052.5234722222 | 2006-11-13 12:33:48 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014130/ | Quick Look | ![]() |
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622 | 4U 1705-44 | 257.2313 | -44.1028 | 256.328133 | -44.039108 | 260.196098 | -21.094402 | 343.32206131 | -2.34487049 | 297.0793 | 54014.4242708333 | 2006-10-06 10:10:57 | 54015.0891087963 | 2006-10-07 02:08:19 | 401046030 | 20.065 | 20 | 20.065 | 20.065 | 20.065 | 20.065 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17.9196 | 17.9196 | 57.4239 | 2 | PROCESSED | 57535.7945138889 | 2016-05-27 19:04:06 | 54526 | 2008-03-01 00:00:00 | 54021.6765162037 | 2006-10-13 16:14:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011112 | We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state. | GALACTIC POINT SOURCES | 4 | A | ANDREW YOUNG | USA | 1 | AO1 | REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401046030/ | Quick Look | ![]() |
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623 | NGC3221 | 155.5344 | 21.5594 | 154.847338 | 21.812076 | 149.453825 | 10.59718 | 213.96748211 | 55.66659318 | 113.4999 | 56977.5304513889 | 2014-11-16 12:43:51 | 56980.5453125 | 2014-11-19 13:05:15 | 809051010 | 121.2459 | 120 | 121.2459 | 121.2459 | 0 | 121.2459 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8106018518 | 2016-08-16 19:27:16 | 57362 | 2015-12-06 00:00:00 | 56995.6190162037 | 2014-12-04 14:51:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091501 | Late-type galaxies in the Local Universe are missing over 70% of their baryonic mass, a large fraction of which is likely embedded in the extended, low density warm-hot gaseous halo. However, searches of hot diffuse halos around massive spiral galaxies found them to be relatively small and not very massive. The UV observations have shown that the baryonic halo mass depends on the specific star formation rate (sSFR) and not on the total mass of the galaxy. We propose to observe the halo emission of NGC3221 with very high sSFR. Detection and characterization of the hot halo around this galaxy will expand our understanding of the dependence of halo properties on galaxy properties, and advance our understanding of galaxy formation, feedback and metal enrichment proposed by theoretical models. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | ANJALI GUPTA | USA | 9 | AO9 | SEARCH FOR THE HOT GASEOUS HALO AROUND THE NEARBY SPIRAL GALAXY NGC3221 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809051010/ | Quick Look | ![]() |
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624 | OFF-FIELD2 | 156.3941 | 20.5095 | 155.710931 | 20.763905 | 150.605485 | 9.917753 | 216.1857144 | 56.11255364 | 112.0717 | 56982.1681018518 | 2014-11-21 04:02:04 | 56983.2640046296 | 2014-11-22 06:20:10 | 809053010 | 39.8287 | 40 | 39.8287 | 39.8287 | 0 | 39.8287 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8087847222 | 2016-08-16 19:24:39 | 57377 | 2015-12-21 00:00:00 | 57009.4169444444 | 2014-12-18 10:00:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091501 | Late-type galaxies in the Local Universe are missing over 70% of their baryonic mass, a large fraction of which is likely embedded in the extended, low density warm-hot gaseous halo. However, searches of hot diffuse halos around massive spiral galaxies found them to be relatively small and not very massive. The UV observations have shown that the baryonic halo mass depends on the specific star formation rate (sSFR) and not on the total mass of the galaxy. We propose to observe the halo emission of NGC3221 with very high sSFR. Detection and characterization of the hot halo around this galaxy will expand our understanding of the dependence of halo properties on galaxy properties, and advance our understanding of galaxy formation, feedback and metal enrichment proposed by theoretical models. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | ANJALI GUPTA | USA | 9 | AO9 | SEARCH FOR THE HOT GASEOUS HALO AROUND THE NEARBY SPIRAL GALAXY NGC3221 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809053010/ | Quick Look | ![]() |
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625 | GX 339-4 | 255.7025 | -48.7916 | 254.754666 | -48.72059 | 259.573177 | -25.865576 | 338.93635594 | -4.32587966 | 86.7489 | 54143.2316087963 | 2007-02-12 05:33:31 | 54146.2003009259 | 2007-02-15 04:48:26 | 401068010 | 77.2053 | 100 | 83.8935 | 77.2053 | 0 | 82.1138 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 94.026 | 94.026 | 256.484 | 4 | PROCESSED | 57537.4905208333 | 2016-05-29 11:46:21 | 54535 | 2008-03-10 00:00:00 | 54167.7751851852 | 2007-03-08 18:36:16 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011146 | Skewed iron emission lines from the inner accretion disk and broad-band disk reflection spectra are incisive diagnostics of relativistic effects and the inner accretion flow geometry in black hole binaries. With its high effective area, efficient instrument modes, and sensitivity in hard X-rays, Suzaku is ideally suited to fully exploit these diagnostics. We request a total of 154 ksec in up to four observations to observe a black hole transient in outburst, using a scheme tailored to accommodate different source fluxes and Suzaku's observing windows. We will support these observations with a global multi-wavelength network of observatories. Understanding accretion onto black holes is central to NASA's ``SEU'' research theme. | GALACTIC POINT SOURCES | 4 | A | JON MILLER | USA | 1 | AO1-TOO | SUZAKU OBSERVATIONS OF A BLACK HOLE TRANSIENT IN OUTBURST | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401068010/ | Quick Look | ![]() |
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626 | MKW4-WN | 181.4571 | 2.3391 | 180.816687 | 2.617439 | 180.402943 | 2.725316 | 277.2234025 | 62.91169747 | 110.2998 | 56994.5218865741 | 2014-12-03 12:31:31 | 56996.9723842593 | 2014-12-05 23:20:14 | 809062010 | 90.3652 | 100 | 90.3652 | 91.5172 | 0 | 91.5172 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 88.7385 | 88.7385 | 211.7057 | 1 | PROCESSED | 57617.4717361111 | 2016-08-17 11:19:18 | 56748 | 2014-04-01 00:00:00 | 57007.0908912037 | 2014-12-16 02:10:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091513 | We propose to observe the nearby group MKW4 by leveraging existing observations to provide coverage from its center to its virial radius in two orthogonal directions. Four additional pointings, combined with two existing pointings, will allow us to determine radial profiles of gas temperature, density, entropy, pressure, and gas mass fraction, as well as their azimuthal variation. Comparing these properties to those of clusters will allow us to probe the role played by baryonic physics and assess the imprints of hierarchical structure formation. The stable and low background of the Suzaku XIS is crucial for the study of galaxy groups to their virial radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUANYUAN SU | USA | 9 | AO9 | PROBING A TYPICAL GALAXY GROUP TO ITS VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809062010/ | Quick Look | ![]() |
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627 | MCG-6-30-15 | 203.9717 | -34.2976 | 203.255303 | -34.04246 | 215.173232 | -22.546653 | 313.28966663 | 27.67858669 | 102.4356 | 53758.5062962963 | 2006-01-23 12:09:04 | 53761.0835648148 | 2006-01-26 02:00:20 | 700007020 | 98.4834 | 300 | 98.4834 | 98.4834 | 98.4834 | 98.4834 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 81.8922 | 81.8922 | 222.6497 | 3 | PROCESSED | 57532.8430902778 | 2016-05-24 20:14:03 | 54247 | 2007-05-27 00:00:00 | 54059.5463773148 | 2006-11-20 13:06:47 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001035 | The broad iron line in the Seyfert 1 galaxy MCG-6-30-15 shows that most of the power is released at 2--4 gravitational radii enabling the strong gravity, accretion flow and energy release in that exciting regime to be studied. The spectral variability of the source decomposes into a highly variable power law and a reflection-dominated component, containing the iron line and Compton hump, which varies significantly but with much less amplitude. This can be explained by the extreme gravitational light bending occuring in this region. We propose to observe MCG--6-30-15 for 4 x 50~ks in order to determine for the first time the variability of the reflection over a wide range of energies from below 1 keV to above 40 keV and timescales . | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ANDREW FABIAN | JAP | 0 | SWG | REFLECTION, ABSORPTION AND STRONG GRAVITY AROUND THE SPINNING BLACK HOLE IN MCG--6-30-15 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700007020/ | Quick Look | ![]() |
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628 | IGR J16207-5129 | 245.1895 | -51.5038 | 244.232877 | -51.38483 | 252.516177 | -29.556104 | 332.45599844 | -1.05021687 | 88.1855 | 54499.8231365741 | 2008-02-03 19:45:19 | 54500.7841898148 | 2008-02-04 18:49:14 | 402065010 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 49.5955 | 49.5955 | 83.0319 | 1 | PROCESSED | 57541.498587963 | 2016-06-02 11:57:58 | 54883 | 2009-02-21 00:00:00 | 54515.6347800926 | 2008-02-19 15:14:05 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021122 | We propose to observe 3 INTEGRAL-discovered High Mass X-ray Binaries (IGR HMXBs) to search for X-ray pulsations and to study their broadband spectra. Over the past few years, INTEGRAL has found a surprising number of HMXBs, and the large number of new, locally absorbed supergiant HMXBs indicate that these wind-accretors are more common than previously thought. In addition to high column densities, some of these systems have other extreme properties such as slowly rotating neutron stars (NSs) or rapid X-ray flares. For the systems we propose to observe, detection of pulsations is important for establishing the presence of a NS and for constraining the spin period distribution for HMXB NSs. As these are strong hard X-ray emitters, we will take advantage of Suzaku's broadband capabilities. | GALACTIC POINT SOURCES | 4 | B | JOHN TOMSICK | USA | 2 | AO2 | LOOKING FOR SIGNATURES OF HIGH MAGNETIC FIELD NEUTRON STARS IN INTEGRAL HMXBS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402065010/ | Quick Look | ![]() |
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629 | NGC 4151 | 182.6375 | 39.4139 | 182.006166 | 39.692011 | 164.091601 | 36.628069 | 155.05374688 | 75.05753801 | 112.1087 | 54087.8369097222 | 2006-12-18 20:05:09 | 54090.3848726852 | 2006-12-21 09:14:13 | 701034010 | 124.9796 | 125 | 124.9796 | 124.9796 | 0 | 124.9796 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 131.2741 | 131.2741 | 220.1059 | 3 | PROCESSED | 57536.4582060185 | 2016-05-28 10:59:49 | 54702 | 2008-08-24 00:00:00 | 54132.849537037 | 2007-02-01 20:23:20 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011327 | We propose a 100 ks Suzaku observation of the brightest Seyfert Galaxy in the sky. Given the broad band-pass, and high sensitivity, the proposed observations will provide a high-quality spectrum which will allow us to search for variability in the high-ionized absorber (compared to previous observations). We will be able to obtain stringent constraints on the "Reflection Hump" and compare it to the strength of the Fe Kalpha emission line - thus providing a direct test of Reflection models. The proposed program will also complement observations of fainter and more exotic Seyferts likely to be observed during AO-1. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | IAN GEORGE | USA | 1 | AO1 | DECOUPLING THE COMPONENTS IN THE BRIGHTEST SEYFERT: NGC 4151 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701034010/ | Quick Look | ![]() |
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630 | APM 08279+5255 | 127.9229 | 52.7639 | 126.990699 | 52.933179 | 116.237243 | 32.72103 | 165.74356471 | 36.23970609 | 100.0676 | 54040.3996643518 | 2006-11-01 09:35:31 | 54041.9690277778 | 2006-11-02 23:15:24 | 701057020 | 102.295 | 100 | 102.303 | 102.311 | 102.311 | 102.295 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 95.624 | 95.624 | 135.5778 | 1 | PROCESSED | 57536.0492592593 | 2016-05-28 01:10:56 | 54695 | 2008-08-17 00:00:00 | 54088.5241782407 | 2006-12-19 12:34:49 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011353 | Motivated by the detection of a relativistic outflow of highly ionized gas in previous XMM-Newton and Chandra observations of the lensed quasar APM08279+5255 we propose to monitor this object with three 100ks observations with the aim of improving our understanding of the significance of such outflows in regulating black hole growth and in influencing structure formation. The main scientific goals are : (a) verify the present interpretations of Fe line features in this quasar, (b) monitor the time variability of the Fe absorption features and thus constrain the acceleration mechanism, (c) constrain the kinematic, ionization and absorbing properties of the outflow, and (d) show whether the low-energy ionized absorber is part of the relativistic outflow. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GEORGE CHARTAS | USA | 1 | AO1 | VIEWS OF RELATIVISTIC WINDS THROUGH NATURAL LENSES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701057020/ | Quick Look | ![]() |
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631 | 1RX J154814.5-452845 | 237.0511 | -45.4226 | 236.175049 | -45.269354 | 245.126412 | -24.783918 | 332.46961393 | 7.07040697 | 85.7358 | 54132.6368518518 | 2007-02-01 15:17:04 | 54135.3543865741 | 2007-02-04 08:30:19 | 401037010 | 99.4541 | 100 | 99.4541 | 99.4621 | 0 | 99.4701 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86.8552 | 86.8552 | 234.7838 | 3 | PROCESSED | 57537.0252777778 | 2016-05-29 00:36:24 | 54702 | 2008-08-24 00:00:00 | 54139.4767939815 | 2007-02-08 11:26:35 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011102 | Intermediate Polars (IPs) are strong soft and hard X-ray sources and Suzaku is therefore ideally suited to their study. We have selected three IPs that are of particularly high priority. They have all been detected as hard (E>10 keV) X-ray sources; they all have a hot (kT~100 eV), blackbody-like component; none have been studied simultaneously over a wide band-pass. We therefore propose 80 ksec observations each of V2400 Oph, 1RXS J154814.5-452845, and 1RXS J213344.1+510725, with an additional 40 ksec background observation for V2400 Oph. We plan to analyze the average and phase-resolved spectra to determine the strength of the reflection continuum; the highest temperature present in the plasma; and the details of the complex absorber. | GALACTIC POINT SOURCES | 4 | A | KOJI MUKAI | USA | 1 | AO1 | BROAD-BAND SPECTROSCOPY OF INTERMEDIATE POLARS: FROM THE SOFT COMPONENT TO REFLECTION | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401037010/ | Quick Look | ![]() |
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632 | 4U 1705-44 | 257.2281 | -44.1019 | 256.324944 | -44.038193 | 260.193555 | -21.093723 | 343.32141433 | -2.34248879 | 264.0666 | 53996.5173611111 | 2006-09-18 12:25:00 | 53996.8619675926 | 2006-09-18 20:41:14 | 401046020 | 17.134 | 20 | 17.342 | 17.134 | 17.334 | 17.334 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 15.4477 | 15.4477 | 29.7679 | 0 | PROCESSED | 57535.6082175926 | 2016-05-27 14:35:50 | 54526 | 2008-03-01 00:00:00 | 54020.9055555556 | 2006-10-12 21:44:00 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011112 | We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state. | GALACTIC POINT SOURCES | 4 | A | ANDREW YOUNG | USA | 1 | AO1 | REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401046020/ | Quick Look | ![]() |
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633 | LMC X-4 | 83.1883 | -66.3595 | 83.179882 | -66.392572 | 1.044909 | -87.279168 | 276.32310713 | -32.53751505 | 226.9099 | 54507.0294560185 | 2008-02-11 00:42:25 | 54507.6043287037 | 2008-02-11 14:30:14 | 702037010 | 23.3814 | 20 | 23.3894 | 23.3974 | 0 | 23.3814 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20.047 | 20.047 | 49.662 | 1 | PROCESSED | 57541.5628356482 | 2016-06-02 13:30:29 | 54883 | 2009-02-21 00:00:00 | 54515.5898842593 | 2008-02-19 14:09:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021127 | We propose for a series of three 20ks observations of the binary X-ray pulsar LMC X-4. This source shows 13.5 s pulsations, a 1.4 d orbital period, and a long-period (~30 d) variability due to a warped, precessing accretion disk. The proposed analysis will use pulse-phase spectroscopy with XIS to explore changes in the X-ray pulses and spectra at three different phases in the disk precession. This work will give us a detailed picture of the accretion flow, particularly for the inner regions of the accretion disk that are illuminated by the X-rays from the neutron star. This project takes advantage of the strengths of the XIS, particularly its excellent spectral resolution, sufficient (1s) time resolution in Window mode, and wide PSF that limits pile-up effects. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RYAN HICKOX | USA | 2 | AO2 | SUPERORBITAL VARIATION OF LMC X-4: EXPLORING THE ACCRETION FLOW | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702037010/ | Quick Look | ![]() |
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634 | COMET_8P_TUTTLE-P2_17 | 40.6015 | -37.8518 | 40.101512 | -38.064027 | 20.766573 | -50.125126 | 244.68288405 | -64.39021906 | 254.0645 | 54492.1630439815 | 2008-01-27 03:54:47 | 54492.2959953704 | 2008-01-27 07:06:14 | 502063170 | 5.1495 | 5 | 5.1495 | 5.1495 | 0 | 5.1495 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 5.4142 | 5.4142 | 11.432 | 0 | PROCESSED | 57541.4188425926 | 2016-06-02 10:03:08 | 54912 | 2009-03-22 00:00:00 | 54546.2465509259 | 2008-03-21 05:55:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063170/ | Quick Look | ![]() |
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635 | 3C 445 | 335.9528 | -2.0995 | 335.30761 | -2.353112 | 336.949965 | 7.376595 | 61.86726076 | -46.70852053 | 68.9567 | 54245.2015046296 | 2007-05-25 04:50:10 | 54248.9169444444 | 2007-05-28 22:00:24 | 702056010 | 139.7691 | 125 | 139.7691 | 139.7691 | 0 | 139.7691 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 117.2412 | 117.2412 | 320.9918 | 4 | PROCESSED | 57538.8276967593 | 2016-05-30 19:51:53 | 54702 | 2008-08-24 00:00:00 | 54256.717662037 | 2007-06-05 17:13:26 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021352 | It is well known that the circum-black hole environ of Seyferts contain warm, photoionized gas responsible for complex absorption/emission at X-rays. Evidence for such components in radio-loud AGN is, instead, rare. And yet, presence of an ionized, scattering medium is postulated by unification models for these sources, and some models for jet formation. Here we tackle this problem by proposing sensitive Suzaku observations of 3C445, the only Broad-Line Radio Galaxy exhibiting soft X-ray emission lines from 0.4-3 keV in an archival EPIC spectrum. We will: 1) Determine the broad-band continuum; 2) Study the properties of the soft emission lines, determining the gas density and location, and thus its role in jet collimation; and 3) Confirm the strong reflection component suggested by EPIC. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RITA SAMBRUNA | USA | 2 | AO2 | WARM GAS IN THE INNER REGIONS OF RADIO-LOUD AGN: THE CASE OF 3C445 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702056010/ | Quick Look | ![]() |
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636 | SWIFTJ2000.6+3210 | 300.0869 | 32.2033 | 299.597811 | 32.064769 | 312.685822 | 51.280995 | 68.99570836 | 1.1443147 | 87.4233 | 53837.6619212963 | 2006-04-12 15:53:10 | 53837.9139351852 | 2006-04-12 21:56:04 | 401053010 | 12.4384 | 20 | 12.444 | 12.4512 | 12.4512 | 12.4384 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 9.8767 | 9.8767 | 21.7679 | 0 | PROCESSED | 57533.4456134259 | 2016-05-25 10:41:41 | 54775 | 2008-11-05 00:00:00 | 53927.3549189815 | 2006-07-11 08:31:05 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011132 | INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. | GALACTIC POINT SOURCES | 4 | A | RANDALL SMITH | USA | 1 | AO1 | HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401053010/ | Quick Look | ![]() |
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637 | Q0450-1310 | 73.3011 | -13.0912 | 72.722633 | -13.172561 | 69.927484 | -35.377207 | 211.74785299 | -32.06702416 | 263.6423 | 54535.8878240741 | 2008-03-10 21:18:28 | 54536.2502314815 | 2008-03-11 06:00:20 | 702062010 | 15.5102 | 13 | 15.5102 | 15.5102 | 0 | 15.5102 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.9887 | 14.9887 | 31.3059 | 0 | PROCESSED | 57541.8181828704 | 2016-06-02 19:38:11 | 54916 | 2009-03-26 00:00:00 | 54550.1640277778 | 2008-03-25 03:56:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021361 | The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | GEORGE CHARTAS | USA | 2 | AO2 | AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702062010/ | Quick Look | ![]() |
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638 | HCG62 | 193.274 | -9.2022 | 192.623373 | -8.930867 | 195.778851 | -3.241931 | 303.62256693 | 53.66732525 | 113.6407 | 53755.3883333333 | 2006-01-20 09:19:12 | 53758.5002199074 | 2006-01-23 12:00:19 | 800013020 | 114.8488 | 100 | 114.8568 | 114.8488 | 114.8488 | 114.8568 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 98.7836 | 98.7836 | 268.8498 | 4 | PROCESSED | 57532.7777199074 | 2016-05-24 18:39:55 | 54247 | 2007-05-27 00:00:00 | 54040.4546064815 | 2006-11-01 10:54:38 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001057 | We propose to obtain high-quality spectra of the X-ray brightest, compact group of galaxies HCG62 with Suzaku. The previous ASCA observation has reported that this group has a hard tail in the spectrum. With 100 ksec exposure, we can constrain the flux of the hard component above ~3 keV with much higher accuracy. This will give a great impact in understanding the origin of the hard emission and non-thermal populations in the IGM. Furhtermore determining the metal abundance, particularly Oxygen, in the central and outer regions will give us new, valuable information on metal enrichment processes in the group that is not dominated by a cD galaxy. Suzaku/XIS is the best-suited for our scientific objectives since it has a low background level and the unprecedented high sensitivity. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NAOMI OTA | JAP | 0 | SWG | MEASURING HARD TAILS AND METAL DISTRIBUTIONS IN THE GALAXY GROUP HCG62 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800013020/ | Quick Look | ![]() |
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639 | SS AUR | 93.3423 | 47.7333 | 92.395757 | 47.74724 | 92.468681 | 24.321363 | 166.0127795 | 13.79596984 | 289.1089 | 54529.7508796296 | 2008-03-04 18:01:16 | 54530.180775463 | 2008-03-05 04:20:19 | 402045010 | 19.4714 | 20 | 19.4714 | 19.4714 | 0 | 19.4714 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17.378 | 17.378 | 37.1359 | 0 | PROCESSED | 57541.7699074074 | 2016-06-02 18:28:40 | 54905 | 2009-03-15 00:00:00 | 54539.2223726852 | 2008-03-14 05:20:13 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021105 | Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose short Suzaku observations of dwarf novae with secure, parallax-based distance estimates that have not been the subject of pointed, imaging, X-ray observations in the 0.5-10 keV band. This will be an important check of potential biases in earlier studies. | GALACTIC POINT SOURCES | 4 | C | KOJI MUKAI | USA | 2 | AO2 | BUILDING UP AN UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A PARALLAX SELECTED SAMPLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402045010/ | Quick Look | ![]() |
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640 | 4U1705-44 | 257.2244 | -44.1021 | 256.321247 | -44.038375 | 260.19074 | -21.094172 | 343.31966899 | -2.34047423 | 86.9924 | 54516.9847569444 | 2008-02-20 23:38:03 | 54517.6182175926 | 2008-02-21 14:50:14 | 402051030 | 25.9956 | 15 | 26.0516 | 25.9956 | 0 | 26.0516 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.8205 | 20.8205 | 54.7239 | 1 | PROCESSED | 57541.7148611111 | 2016-06-02 17:09:24 | 54901 | 2009-03-11 00:00:00 | 54535.2030439815 | 2008-03-10 04:52:23 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021113 | We recently proposed a solution to the problem of model ambiguity for the spectra of atoll-type neutron stars. This work was performed on X-ray transient, and we need to test the model on the main population of persistent atolls. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. We propose to supplement the Suzaku monitoring archive begun in AO-1 by targeting the two persistent atolls with the greatest X-ray variability. | GALACTIC POINT SOURCES | 4 | A | RONALD REMILLARD | USA | 2 | AO2 | X-RAY SPECTRA OF ATOLL-TYPE NEUTRON STARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402051030/ | Quick Look | ![]() |
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641 | IGR J17544-2619 | 268.6038 | -26.3314 | 267.825334 | -26.322724 | 268.737527 | -2.896537 | 3.23518966 | -0.33446224 | 84.5765 | 54544.5263425926 | 2008-03-19 12:37:56 | 54547.2640509259 | 2008-03-22 06:20:14 | 402061010 | 103.4173 | 72 | 103.8115 | 103.8275 | 0 | 103.4173 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 65.5656 | 65.5656 | 236.5059 | 3 | PROCESSED | 57541.9752314815 | 2016-06-02 23:24:20 | 54933 | 2009-04-12 00:00:00 | 54566.6106134259 | 2008-04-10 14:39:17 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021121 | Supergiant Fast X-ray Transients are a newly-discovered class of x-ray binary with short outbursts and late O to early B supergiant companions. They are not persistently bright, but the nature of their low-level variability is not well known. Similarly short outbursts are also seen in bright HMXBs with supergiant companions such as Cyg X-1 and Vel X-1. The mechanism of these outbursts is unknown in all cases. We propose long pointings to the two best-studied SFXTs and a third object, XTE J1743-363, which seems to be transitional between SFXTs and persistent supergiant HMXBs. We will characterize their variability at low flux levels, both to understand the accretion mechanism and to enable surveys of archival data for new SFXTs. | GALACTIC POINT SOURCES | 4 | C | DAVID SMITH | USA | 2 | AO2 | CHARACTERIZING THE SPECTRUM AND VARIABILITY OF THE SUPERGIANT FAST X-RAY TRANSIENTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402061010/ | Quick Look | ![]() |
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642 | RXJ_0852-4622_NW_offset | 135.1284 | -47.9102 | 134.705364 | -47.713589 | 163.727844 | -60.335158 | 268.39892579 | -1.13950817 | 140.267 | 53727.3040393518 | 2005-12-23 07:17:49 | 53728.368912037 | 2005-12-24 08:51:14 | 500010020 | 59.1784 | 50 | 59.1784 | 59.1925 | 59.2026 | 59.1925 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 63.4821 | 63.4821 | 91.9959 | 0 | PROCESSED | 57532.4967708333 | 2016-05-24 11:55:21 | 54247 | 2007-05-27 00:00:00 | 54039.2486226852 | 2006-10-31 05:58:01 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001048 | We propose to observe two lobes of X-ray and gamma-ray emission from the shell remnant RXJ 0852-4622 (Vela Jr) with HXD. The 1-10 keV spectrum of this remnant is essentially a featureless continuum attributed to synchrotron emission from accelerated electrons, with the X-ray and gamma-ray morphologies being very well matched. Observations at energies above 10 keV with HXD will probe the cut-off energy of the synchrotron spectrum, shedding light on the electron acceleration efficiency. The large size of the remnant makes it possible to observe different portions of the limb with separate HXD PIN observations. | GALACTIC DIFFUSE EMISSION | 5 | A | UNA HWANG | JAP | 0 | SWG | HXD OBSERVATION OF NONTHERMAL EMISSION FROM RXJ 0852-4622 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500010020/ | Quick Look | ![]() |
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643 | XBONGBLUE2 | 217.7653 | 34.3413 | 217.240861 | 34.56211 | 200.146538 | 45.945194 | 57.71878971 | 67.47993323 | 130.3787 | 54454.1686921296 | 2007-12-20 04:02:55 | 54454.5050694445 | 2007-12-20 12:07:18 | 702084010 | 14.8162 | 13 | 14.8162 | 14.8162 | 0 | 14.8162 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14.5794 | 14.5794 | 29.0559 | 0 | PROCESSED | 57540.9126851852 | 2016-06-01 21:54:16 | 54828 | 2008-12-28 00:00:00 | 54460.6654398148 | 2007-12-26 15:58:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021376 | We propose to use Suzaku's large collecting area and excellent energy response to measure accurate X-ray spectra for 9 XBONGs and 8 luminous Type 2 AGN selected from very large samples of identified XBONGs and Type 2 AGN found in our Chandra XBootes survey. We have obtained optical spectra for 258 XBONGs and identified ~700 X-ray luminous Type 2 AGN at z>0.7. With known source positions and X-ray fluxes, we select sources that are relatively bright with little or no contamination from other X-ray sources. Thus we will measure individual spectra for these bright sources. We propose eight 15 ksec Suzaku XIS observations to measure the absorption in 8 luminous z > 0.8 Type 2 AGN and eight 10 ksec observations to measure the absorption and iron emission for nine XBONGs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | CHRISTINE JONES | USA | 2 | AO2 | OBSCURED AGN AND XBONGS IN BOOTES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702084010/ | Quick Look | ![]() |
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644 | EXO 2030+375 | 308.0118 | 37.6951 | 307.540549 | 37.524573 | 325.984128 | 54.001657 | 77.17399477 | -1.17458429 | 56.3502 | 54234.8591666667 | 2007-05-14 20:37:12 | 54236.1565277778 | 2007-05-16 03:45:24 | 402068010 | 57.6071 | 40 | 57.6071 | 57.6071 | 0 | 57.6071 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53.3954 | 53.3954 | 112.0678 | 2 | PROCESSED | 57538.7243055556 | 2016-05-30 17:23:00 | 54702 | 2008-08-24 00:00:00 | 54242.497962963 | 2007-05-22 11:57:04 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021124 | We propose a 40 ks Suzaku observation to confirm EXO 2030+375's recently discovered ~10 keV cyclotron feature and constrain its second harmonic at ~20 keV. EXO 2030+375 is a 42-second Be/X-ray pulsar in an eccentric 46-day orbit. If confirmed the ~10 keV cyclotron feature will be the lowest in energy known for an accreting pulsar and will provide the missing piece to make EXO 2030+375 an ideal candidate to observationally test accretion theory. In addition, we will measure EXO 2030+375's spin frequency, study its pulse shape versus energy, and perform phase resolved spectroscopy. Suzaku will allow these studies to reach lower energies and provide high quality spectra at lower luminosities than in any previous observations. | GALACTIC POINT SOURCES | 4 | A | COLLEEN WILSON | USA | 2 | AO2 | CONSTRAINING CYCLOTRON FEATURES IN A NORMAL OUTBURST OF EXO 2030+375 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402068010/ | Quick Look | ![]() |
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645 | V2491 CYG | 295.7679 | 32.3068 | 295.285617 | 32.186831 | 307.093304 | 52.481406 | 67.2208484 | 4.33923679 | 253.6206 | 55503.4390162037 | 2010-11-03 10:32:11 | 55505.2709837963 | 2010-11-05 06:30:13 | 405036010 | 74.4004 | 70 | 74.4004 | 74.4004 | 0 | 74.4004 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57.2065 | 57.2065 | 158.2519 | 2 | PROCESSED | 57553.9866087963 | 2016-06-14 23:40:43 | 55885 | 2011-11-20 00:00:00 | 55518.4178356482 | 2010-11-18 10:01:41 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051213 | We propose to observe again one of the most luminous and intriguing classical novae of the last two years, after it has returned to quiescence. The goala are to understand how accretion is re-estabilished, investigate the claim that the white dwarf an intermediate polar (IP), estimate mass accretion are and white dwarf mass. IP are a class of X-ray sources that Suzaku is ideally suited to study, and we want to study the influence of the magnetic field on the nova evolution. | GALACTIC POINT SOURCES | 4 | C | MARINA ORIO | USA | 5 | AO5 | REVISITING AN X-RAY LUMINOUS NOVA NOVA AFTER THE ERUPTION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405036010/ | Quick Look | ![]() |
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646 | RXCJ0605 | 91.2587 | -35.3175 | 90.815345 | -35.312478 | 91.987157 | -58.750453 | 241.74700639 | -24.18215725 | 309.9853 | 55322.2226041667 | 2010-05-06 05:20:33 | 55323.0307060185 | 2010-05-07 00:44:13 | 805065020 | 40.0231 | 40 | 40.0231 | 40.0231 | 0 | 40.0231 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33.1762 | 33.1762 | 69.7899 | 0 | PROCESSED | 57551.4119097222 | 2016-06-12 09:53:09 | 55287 | 2010-04-01 00:00:00 | 55341.5093981482 | 2010-05-25 12:13:32 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805065020/ | Quick Look | ![]() |
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647 | TAU SCO | 248.9714 | -28.2185 | 248.191858 | -28.116816 | 251.449018 | -6.120961 | 351.53328031 | 12.80600635 | 277.9748 | 54710.0436689815 | 2008-09-01 01:02:53 | 54710.3697222222 | 2008-09-01 08:52:24 | 403034010 | 14.6171 | 10 | 14.6171 | 14.6171 | 0 | 14.6171 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.0855 | 12.0855 | 28.1359 | 0 | PROCESSED | 57543.4427777778 | 2016-06-04 10:37:36 | 55148 | 2009-11-13 00:00:00 | 54780.4170138889 | 2008-11-10 10:00:30 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031121 | We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars. | GALACTIC POINT SOURCES | 4 | A | RICHARD IGNACE | USA | 3 | AO3 | X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403034010/ | Quick Look | ![]() |
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648 | MRK 421 | 166.1081 | 38.2021 | 165.413329 | 38.471893 | 151.215505 | 29.492571 | 179.85015534 | 65.02934628 | 313.5582 | 54591.1196527778 | 2008-05-05 02:52:18 | 54595.3502199074 | 2008-05-09 08:24:19 | 703043010 | 180.7851 | 150 | 180.7931 | 180.7851 | 0 | 180.7931 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 163.5507 | 163.5507 | 343.6517 | 9 | PROCESSED | 57542.5998842593 | 2016-06-03 14:23:50 | 54972 | 2009-05-21 00:00:00 | 54606.5618287037 | 2008-05-20 13:29:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031341 | We propose one 150 ksec Suzaku ToO observations of one of the three strong GeV-TeV gamma-ray blazars Mrk 421, Mrk 501, or 1ES 1959+650 during a 10 day multiwavelength campaign with coverage from radio to gamma-rays. The proposal is submitted by the VERITAS collaboration, assuring excellent TeV gamma-ray coverage. The Suzaku observations will play a key-role in interpreting the multiwavelength data set, allowing us to measure the time lag between the X-ray and gamma-ray flux variability and to scrutinize the correlation of the X-ray and gamma-ray spectral indices. The Suzaku and gamma-ray energy spectra will allow us to constrain the intensity of the IR Diffuse Extragalactic Background Radiation which absorbs TeV gamma-rays in extragalactic pairproduction processes. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HENRIC KRAWCZYNSKI | USA | 3 | AO3-TOO | TARGET OF OPPORTUNITY OBSERVATIONS OF THE BLAZARS MRK 421, MRK 501, AND 1ES 1959+650 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703043010/ | Quick Look | ![]() |
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649 | ETA CARINAE | 161.3407 | -59.6518 | 160.853368 | -59.388342 | 202.155822 | -58.871724 | 287.61551185 | -0.58277566 | 142.0006 | 54856.1332291667 | 2009-01-25 03:11:51 | 54856.6821064815 | 2009-01-25 16:22:14 | 403037010 | 28.8053 | 30 | 28.8053 | 28.8053 | 0 | 28.8053 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17.4539 | 17.4539 | 47.4079 | 0 | PROCESSED | 57545.3235185185 | 2016-06-06 07:45:52 | 55328 | 2010-05-12 00:00:00 | 54880.533587963 | 2009-02-18 12:48:22 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031124 | X-ray observations of Eta Carinae near the 2003 periastron passage confirmed that the X-ray emission primarily arises from collision of winds in a binary system, but raised fundamental questions about the cause of the 3 month-long X-ray minimum and an excess above ~10 keV (possibly up to 50 keV) in addition to the thermal emission with kT ~3-5 keV. These features would originate from plasma extremely embedded in the primary winds and acceleration of high energy particles at the wind colliding region. To resolve these features clearly, broad band Suzaku observations around the periastron passage are crucial. We propose four 30 ksec Suzaku observations of Eta Carinae during AO3, which will cover the next X-ray maximum (in late 2008) and minimum (in early 2009). | GALACTIC POINT SOURCES | 4 | A | KENJI HAMAGUCHI | USA | 3 | AO3 | X-RAY EMISSION FROM ETA CARINAE DURING THE X-RAY MAXIMUM AND MINIMUM | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403037010/ | Quick Look | ![]() |
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650 | CEN X-4 | 224.5893 | -31.6684 | 223.829289 | -31.468804 | 231.309524 | -14.121168 | 332.24097668 | 23.88258751 | 104.6233 | 54847.9102314815 | 2009-01-16 21:50:44 | 54850.9717939815 | 2009-01-19 23:19:23 | 403057010 | 146.6704 | 150 | 146.6876 | 146.6704 | 0 | 146.6916 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 133.6185 | 133.6185 | 264.4539 | 2 | PROCESSED | 57545.3354513889 | 2016-06-06 08:03:03 | 55328 | 2010-05-12 00:00:00 | 54880.5460069444 | 2009-02-18 13:06:15 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031161 | Observations of thermal emission from the surface of quiescent neutron star low-mass X-ray binaries (LMXBs) can be used to measure neutron star radii. However, their quiescent spectra are complicated due to the presence of an additional power-law, and because variability has been seen on timescales as short as 100s. The nearest known neutron star LMXB Cen X-4 gives us the clearest view of these objects. But, the best observation so far lacked the sensitivity to determine the cause of the variability. Yet, the cause has important ramifications for measuring neutron star radii - if it is the thermal (rather than power-law) component that is varying our picture of quiescent emission may be wrong. To solve this critical problem we propose a 150 ksec observation of Cen X-4 with Suzaku. | GALACTIC POINT SOURCES | 4 | A | EDWARD CACKETT | USA | 3 | AO3 | UNCOVERING VARIABLE QUIESCENT EMISSION IN THE NEUTRON STAR CEN X-4 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403057010/ | Quick Look | ![]() |
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651 | G18.0-0.7 | 276.56 | -13.5781 | 275.85231 | -13.608204 | 276.459314 | 9.715522 | 18.00442084 | -0.69482715 | 92.0001 | 54909.8982060185 | 2009-03-19 21:33:25 | 54911.080775463 | 2009-03-21 01:56:19 | 503086010 | 52.0592 | 50 | 52.0592 | 52.0672 | 0 | 52.0672 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.3036 | 46.3036 | 102.1458 | 2 | PROCESSED | 57547.7369560185 | 2016-06-08 17:41:13 | 55329 | 2010-05-13 00:00:00 | 54923.3684490741 | 2009-04-02 08:50:34 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031203 | By studying pulsar wind nebulae, the synchrotron nebulae powered by a neutron star's loss of rotational energy, it is possible to determine the energetics of both the progenitor supernova and central neutron star. This requires estimates of the expansion velocity and mass swept-up the pulsar wind nebulae, best obtained by analyzing the spectrum of the thermal X-rays emitting by this material. In the proposal, we request a 50ks observation of four of the most energetic pulsar wind nebulae in the Milky Way to both detect such thermal X-ray emission and use the measured spectral properties to infer the ejecta mass and kinetic energy of their progenitor supernova and the initial spin period of the central neutron star -- all currently unmeasurable using the currently available information. | GALACTIC DIFFUSE EMISSION | 5 | C | JOSEPH GELFAND | USA | 3 | AO3 | STUDYING THE PROGENITOR SUPERNOVA AND CENTRAL NEUTRON STAR OF PULSAR WIND NEBULAE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503086010/ | Quick Look | ![]() |
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652 | IGRJ01528 | 28.2011 | -3.4464 | 27.56858 | -3.692494 | 24.925792 | -14.053354 | 157.35013019 | -62.14500791 | 77.3667 | 55007.0338078704 | 2009-06-25 00:48:41 | 55008.1426388889 | 2009-06-26 03:25:24 | 704043010 | 46.9159 | 40 | 46.9159 | 47.6119 | 0 | 47.6248 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 42.1043 | 42.1043 | 95.7918 | 0 | PROCESSED | 57547.6882407407 | 2016-06-08 16:31:04 | 55386 | 2010-07-09 00:00:00 | 55019.1922337963 | 2009-07-07 04:36:49 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041414 | We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | EZEQUIEL TREISTER | USA | 4 | AO4 | THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704043010/ | Quick Look | ![]() |
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653 | 4U 1608-52 | 243.2309 | -52.3757 | 242.269732 | -52.248184 | 251.350346 | -30.651804 | 330.98178647 | -0.83761569 | 125.7606 | 55273.9986689815 | 2010-03-18 23:58:05 | 55274.9154166667 | 2010-03-19 21:58:12 | 404044030 | 31.7568 | 30 | 31.7568 | 31.7568 | 0 | 31.7568 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.3094 | 15.3094 | 79.1938 | 0 | PROCESSED | 57550.9191898148 | 2016-06-11 22:03:38 | 55652 | 2011-04-01 00:00:00 | 55286.259849537 | 2010-03-31 06:14:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041223 | The true nature of X-ray emission from neutron star X-ray binaries (NSXRBs) has not been clear for sometime and there are many possibilities for the spectral model. Recent progress has been made, but relies on RXTE data which lacks the low energy sensitivity where disk emission is most prominent. Using Suzaku we propose four 30 ksec observations of the transient 4U 1608-52 throughout an outburst. We will test how spectral parameters change with luminosity, allowing us to untangle the correct model. An essential part of this proposal is the unique ability of Suzaku to detect asymmetric broad iron emission lines in NSXRBs. We will study how the iron line varies throughout the outburst, which combined with the spectral fits will test the interaction between the accretion disk and corona. | GALACTIC POINT SOURCES | 4 | A | EDWARD CACKETT | USA | 4 | AO4-TOO | ACCRETION DISK EVOLUTION THROUGHOUT A NEUTRON STAR LMXB OUTBURST | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404044030/ | Quick Look | ![]() |
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654 | BF ERI | 69.8754 | -4.5962 | 69.256008 | -4.693413 | 67.473114 | -26.478101 | 201.0367912 | -31.29845078 | 262.0133 | 56350.9190625 | 2013-02-27 22:03:27 | 56351.6253009259 | 2013-02-28 15:00:26 | 407045010 | 32.8177 | 30 | 32.8177 | 32.8177 | 0 | 32.8178 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 32.0161 | 32.0161 | 61.0099 | 1 | PROCESSED | 57610.6930092593 | 2016-08-10 16:37:56 | 56738 | 2014-03-22 00:00:00 | 56372.5138773148 | 2013-03-21 12:19:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071212 | The mass of an accreting white dwarf is a key parameter governing its X-ray emission. We expect that the higher the mass, the higher the temperature and luminosity. Existing data appear consistent with this expectation, given the considerable uncertainties usually associated with the white dwarf masses of individual systems. Here we propose Suzaku observations of 5 dwarf novae for which very high or very low white dwarf mass estimates have been published. These targets provide the best opportunity of further establishing the mass-temperature correlation. Moreover, if the mass estimates are reliable, these targets are of interest from evolutionary considerations - how did these systems form with such high/low mass white dwarfs, and what are their ultimate fates? | GALACTIC POINT SOURCES | 4 | C | KOJI MUKAI | USA | 7 | AO7 | DWARF NOVAE WITH EXTREME WHITE DWARF MASSES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407045010/ | Quick Look | ![]() |
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655 | 1RXS J032613.6+02252 | 51.5615 | 2.4213 | 50.912043 | 2.246984 | 49.792333 | -15.817317 | 180.7494445 | -42.4285339 | 253.9336 | 55596.8403356482 | 2011-02-04 20:10:05 | 55597.6203125 | 2011-02-05 14:53:15 | 705038010 | 32.1971 | 32 | 32.1971 | 32.1971 | 0 | 32.1971 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.6441 | 22.6441 | 67.3879 | 1 | PROCESSED | 57600.8622106482 | 2016-07-31 20:41:35 | 55983 | 2012-02-26 00:00:00 | 55614.1886342593 | 2011-02-22 04:31:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051402 | High frequency peaked BL Lacs are a peculiar subclass of Blazars characterized by non-thermal emission across the whole electromagnetic spectrum. Their spectral energy distributions (SEDs) include two main components: a low-energy component with power peaking in the range from the UV to the X-ray band, and a substantial high-energy component often dominated by gamma-rays. We propose 3 observations (32 ks each) of a selected sample of HBLs to study the behavior of the first component, widely interpreted as synchrotron radiation. First, we will be able to disentangle between different spectral shapes of the synchrotron SED of HBLs. Second, we will use the proposed observations to investigate the properties of the most representative sample of TeV candidate HBLs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | FRANCESCO MASSARO | USA | 5 | AO5 | X-RAY CURVED SPECTRA IN HIGH FREQUENCY PEAKED BL LACS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705038010/ | Quick Look | ![]() |
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656 | 4U 1957+11 | 299.8418 | 11.7197 | 299.250981 | 11.582408 | 304.890304 | 31.617141 | 51.31351001 | -9.31745051 | 63.9325 | 55333.5190277778 | 2010-05-17 12:27:24 | 55334.4675 | 2010-05-18 11:13:12 | 405057020 | 34.9353 | 35 | 34.9433 | 34.9513 | 0 | 34.9353 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.2625 | 28.2625 | 81.9118 | 0 | PROCESSED | 57551.562650463 | 2016-06-12 13:30:13 | 55714 | 2011-06-02 00:00:00 | 55347.2466898148 | 2010-05-31 05:55:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051254 | We propose three observations of the black hole candidate 4U 1957+11. It is one of only two persistently soft state BHC, and has the highest fitted temperature, and highest fitted spin parameter, of any observed BHC. The question arises of whether this high spin is a good estimate of the true spin, or whether this high temperature is evidence of a low level or corona or wind. The multiple Suzaku observations will allow us to track how the disk parameters change, and offer us a 40% chance of observing a state with a large coronal component. The latter might be indicative of launching of a disk wind. | GALACTIC POINT SOURCES | 4 | B | MICHAEL NOWAK | USA | 5 | AO5 | 4U1957+11: THE MOST RAPIDLY SPINNING BLACK HOLE? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405057020/ | Quick Look | ![]() |
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657 | CBS 126 | 153.2712 | 35.8701 | 152.538495 | 36.117901 | 141.901695 | 23.115205 | 188.30426979 | 55.38335717 | 124.145 | 55487.3144907407 | 2010-10-18 07:32:52 | 55489.5529861111 | 2010-10-20 13:16:18 | 705042010 | 101.542 | 100 | 101.566 | 101.542 | 0 | 101.566 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 90.7438 | 90.7438 | 193.3897 | 2 | PROCESSED | 57553.8238541667 | 2016-06-14 19:46:21 | 55867 | 2011-11-02 00:00:00 | 55498.3270949074 | 2010-10-29 07:51:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051432 | We propose to carry out a 100 ks Suzaku observation of Broad Line Seyfert 1 (BLS1) galaxy CBS 126. This source exhibits many properties which are thought to be typical of a Narrow Line Seyfert 1 (NLS1), such as a large soft X-ray excess and strong spectral variability, but unusual for a BLS1. Taking advantage of Suzaku's unique broad band X-ray energy window, our main goal is to clarify the nature of the unusual, variable, optically polarized spectrum of CBS 126. These interesting spectral features cover a wide energy range where Suzaku is ideal. With these proposed studies we will gain better understanding of accretion-powered AGN in general. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | SACHIKO TSURUTA | USA | 5 | AO5 | SPECTRAL AND TEMPORAL STUDIES OF THE SEYFERT 1 GALAXY CBS 126 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705042010/ | Quick Look | ![]() |
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658 | SGR 1806-20 | 272.1607 | -20.4008 | 271.416415 | -20.409492 | 272.01832 | 3.024829 | 10.00344249 | -0.23433657 | 89.0334 | 56010.449837963 | 2012-03-24 10:47:46 | 56012.5314814815 | 2012-03-26 12:45:20 | 406069010 | 70.5964 | 70 | 70.5964 | 70.5964 | 0 | 70.5964 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 63.9571 | 63.9571 | 179.8279 | 2 | PROCESSED | 57605.0500462963 | 2016-08-05 01:12:04 | 56399 | 2013-04-17 00:00:00 | 56023.2387384259 | 2012-04-06 05:43:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061301 | Recent Suzaku investigations revealed that a broad-band (0.8-70 keV) spectra of known magnetars systematically change depending on their characteristic ages. The hard X-rays of magnetars become weaker but harder for older objects. In order to accomplish this picture, we have to verify that this correlation is rather free from selection effects, and holds even when the sources vary on long time scales. Here we propose a 70 ks observation of SGR 1806-20. If we detect the hard X-rays from this source at a rather intensity, the above correlation will be much reinforced. | GALACTIC POINT SOURCES | 4 | C | TERUAKI ENOTO | USA | 6 | AO6 | VARIABILITY OF HARD X-RAYS FROM MAGNETARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406069010/ | Quick Look | ![]() |
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659 | 1FGL J1018.6-5856 | 154.7397 | -58.9449 | 154.297065 | -58.693515 | 196.565416 | -60.867795 | 284.35462729 | -1.68677577 | 302.8974 | 56098.9298611111 | 2012-06-20 22:19:00 | 56100.4612384259 | 2012-06-22 11:04:11 | 407069010 | 72.8412 | 70 | 72.8412 | 72.8412 | 0 | 72.8412 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57.6773 | 57.6773 | 132.25 | 0 | PROCESSED | 57605.7791087963 | 2016-08-05 18:41:55 | 56479 | 2013-07-06 00:00:00 | 56113.258900463 | 2012-07-05 06:12:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071234 | We propose Suzaku observations of a newly discovered gamma-ray binary 1FGL J1018.6-5856. Recent observations by the Fermi Gamma-ray Space Telescope and follow-up observations in other wavelengths revealed that the gamma-ray source is a new member of the rare gamma-ray binary class with an orbital period of 16 days. We propose two types of observations with Suzaku. One is a continuous observation of a sharp X-ray peak found in the lightcurve by the Swift XRT. Another is a series of snap shot observations in orbital phase between the peaks. We aim to perform phase-resolved spectral analysis which is not possible with the Swift XRT data. We also compare the Swift XRT lightcurve with new lightcurves taken by Suzaku in order to test the repeatability of the X-ray orbital modulation. | GALACTIC POINT SOURCES | 4 | B | TAKAAKI TANAKA | USA | 7 | AO7 | SUZAKU OBSERVATIONS OF A NEWLY DISCOVERED GAMMA-RAY BINARY: 1FGL J1018.6-5856 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407069010/ | Quick Look | ![]() |
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660 | NGC 2403 | 114.2007 | 65.5918 | 112.996594 | 65.703234 | 103.458828 | 43.277316 | 150.58117971 | 29.1798975 | 310.3004 | 53810.5896875 | 2006-03-16 14:09:09 | 53811.5884143518 | 2006-03-17 14:07:19 | 800021010 | 72.3687 | 70 | 72.3767 | 72.3687 | 72.3767 | 72.3767 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 59.3591 | 59.3591 | 86.2779 | 0 | PROCESSED | 57533.2480439815 | 2016-05-25 05:57:11 | 54247 | 2007-05-27 00:00:00 | 54042.0667708333 | 2006-11-03 01:36:09 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001101 | We propose to observe NGC 2403, which is a nearby luminous normal spiral. Our main objective is to search and investigation of diffuse emission components. These include both rather soft (kT = 0.1 - 1 keV) ones already detected from a fair number of spirals, and hot (kT = a few keV) emission which, if established, may become an analogue to the Galactic ridge emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAZUO MAKISHIMA | JAP | 0 | SWG | A PROPOSAL FOR A 70 KSEC SUZAKU OBSERVATION OF THE NORMAL SPIRAL GALAXY NGC 2403 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800021010/ | Quick Look | ![]() |
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661 | A426VIR S | 48.9041 | 42.4908 | 48.073152 | 42.306326 | 58.095587 | 23.496379 | 149.35896709 | -12.86322568 | 271.5007 | 56708.3862962963 | 2014-02-20 09:16:16 | 56709.0453009259 | 2014-02-21 01:05:14 | 808085010 | 26.26 | 25 | 26.284 | 26.276 | 0 | 26.26 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.0267 | 21.0267 | 56.9339 | 1 | PROCESSED | 57613.8719560185 | 2016-08-13 20:55:37 | 57086 | 2015-03-05 00:00:00 | 56720.6405902778 | 2014-03-04 15:22:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081526 | Our analysis of Suzaku Key Project data of the Perseus Cluster of galaxies has uncovered a significant drop in temperature, density and derived thermodynamic properties of the intra-cluster medium in the NW direction at the cluster's virial radius, suggesting the presence of a strong shock. In order to firmly confirm and further explore this feature we propose to expand upon the observation of this region. Confirmation of a shock at the virial radius will provide the first ever direct observation of the formation of a galaxy cluster and virialization of the in-falling hot gas. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ONDREJ URBAN | USA | 8 | AO8 | SHOCK FRONT AT THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808085010/ | Quick Look | ![]() |
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662 | LMC X-4 | 83.1886 | -66.3594 | 83.180179 | -66.392471 | 1.047321 | -87.279275 | 276.32297371 | -32.53740633 | 226.9086 | 54500.7929513889 | 2008-02-04 19:01:51 | 54501.0521875 | 2008-02-05 01:15:09 | 702036010 | 0 | 20 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 5.6729 | 5.6729 | 22.3779 | 1 | PROCESSED | 57541.4899537037 | 2016-06-02 11:45:32 | 54883 | 2009-02-21 00:00:00 | 54515.6401851852 | 2008-02-19 15:21:52 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021127 | We propose for a series of three 20ks observations of the binary X-ray pulsar LMC X-4. This source shows 13.5 s pulsations, a 1.4 d orbital period, and a long-period (~30 d) variability due to a warped, precessing accretion disk. The proposed analysis will use pulse-phase spectroscopy with XIS to explore changes in the X-ray pulses and spectra at three different phases in the disk precession. This work will give us a detailed picture of the accretion flow, particularly for the inner regions of the accretion disk that are illuminated by the X-rays from the neutron star. This project takes advantage of the strengths of the XIS, particularly its excellent spectral resolution, sufficient (1s) time resolution in Window mode, and wide PSF that limits pile-up effects. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RYAN HICKOX | USA | 2 | AO2 | SUPERORBITAL VARIATION OF LMC X-4: EXPLORING THE ACCRETION FLOW | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702036010/ | Quick Look | ![]() |
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663 | GX 339-4 | 255.7085 | -48.7866 | 254.760711 | -48.715619 | 259.576938 | -25.860175 | 338.94274721 | -4.32598042 | 275.4008 | 56526.5726967593 | 2013-08-22 13:44:41 | 56529.3592476852 | 2013-08-25 08:37:19 | 408034010 | 101.0196 | 100 | 101.0196 | 101.0196 | 0 | 101.0196 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 90.3169 | 90.3169 | 240.7097 | 1 | PROCESSED | 57612.5083680556 | 2016-08-12 12:12:03 | 56956 | 2014-10-26 00:00:00 | 56588.9590046296 | 2013-10-23 23:00:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081242 | Due to the presence of a steady jet, constraining the properties of black hole systems in their hard state is important for understanding accretion disks and jets. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? This proposal includes the use of Suzaku, NuSTAR, and radio observations to address these questions. A main diagnostic of the accretion geometry is the Compton reflection component, and the combination of Suzaku and NuSTAR covers, with very good energy resolution and sensitivity, the iron emission line, the absorption edges, and the hard X-ray reflection bump. | GALACTIC POINT SOURCES | 4 | A | JOHN TOMSICK | USA | 8 | AO8-TOO | CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408034010/ | Quick Look | ![]() |
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664 | 1H0419-577 | 66.5116 | -57.211 | 66.267931 | -57.322556 | 29.331877 | -75.671402 | 266.99901337 | -41.98911345 | 55.5914 | 54306.2319328704 | 2007-07-25 05:33:59 | 54309.0835532407 | 2007-07-28 02:00:19 | 702041010 | 205.8628 | 200 | 205.8708 | 205.8708 | 0 | 205.8628 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 152.8317 | 152.8317 | 246.3578 | 2 | PROCESSED | 57539.3963888889 | 2016-05-31 09:30:48 | 54706 | 2008-08-28 00:00:00 | 54339.7211111111 | 2007-08-27 17:18:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021304 | A hotly debated question is whether Seyfert X-ray spectra are dominated by components that are blurred by strong gravitational effects close (< 20rg) to the central black hole. Models featuring either complex absorption or blurred disk spectra provide equally good parameterizations of the mean X-ray spectrum of many objects. To make progress with current instruments we require observations with a temporal baseline and flux that will allow us to look for key parameter correlations, as the two scenarios predict different time-dependent behavior. To that end, we propose a Suzaku observation of 1H0419-577, a target that exhibits a remarkable degree of spectral variability in the X-ray regime promising some definitive results in this important area. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TRACEY TURNER | USA | 2 | AO2 | HOW IMPORTANT IS STRONG RELATIVISTIC BLURRING IN SPECTRA OF SEYFERT GALAXIES? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702041010/ | Quick Look | ![]() |
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665 | NGC5548 | 214.4931 | 25.1252 | 213.926181 | 25.355393 | 201.995661 | 36.403773 | 31.92399813 | 70.49805067 | 305.6592 | 54275.9121643518 | 2007-06-24 21:53:31 | 54276.6918055556 | 2007-06-25 16:36:12 | 702042020 | 35.9152 | 30 | 35.9152 | 35.9152 | 0 | 35.9152 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33.175 | 33.175 | 67.3419 | 3 | PROCESSED | 57539.0421759259 | 2016-05-31 01:00:44 | 54695 | 2008-08-17 00:00:00 | 54322.4919675926 | 2007-08-10 11:48:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021307 | We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARTIN ELVIS | USA | 2 | AO2 | NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702042020/ | Quick Look | ![]() |
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666 | 1RXS J032540.0-08144 | 51.413 | -8.2453 | 50.804131 | -8.420115 | 46.598209 | -26.061844 | 192.86854593 | -48.95490782 | 66.7974 | 56869.0655208333 | 2014-07-31 01:34:21 | 56869.9960532407 | 2014-07-31 23:54:19 | 409029010 | 39.5408 | 40 | 39.5408 | 39.9168 | 0 | 39.9248 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.9289 | 18.9289 | 53.612 | 0 | PROCESSED | 57616.4538425926 | 2016-08-16 10:53:32 | 57264 | 2015-08-30 00:00:00 | 56898.3797453704 | 2014-08-29 09:06:50 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091211 | Cataclysmic variables (CVs) detected in the INTEGRAL and Swift BAT hard X-ray surveys are predominantly magnetic systems of the intermediate polar subtype. However, as the survey sensitivity improves, an increasing number of polars are also detected as hard X-ray sources, even though the majority of polars are soft X-ray bright and hard X-ray faint. Over the long term, we hope to understand why most polars are soft X-ray dominated, and why a subset is hard X-ray bright. Here we propose Suzaku observations of four poorly studied BAT-detected polars, 1RXS J032540.0-081442, Swift J2319.4+2619, IW Eri, and IGR J14536-5522, supported by ground-based observations including optical polarimetry, to determine their system parameters. | GALACTIC POINT SOURCES | 4 | A | KOJI MUKAI | USA | 9 | AO9 | HARD X-RAY BRIGHT POLARS: WHY ARE THEY DIFFERENT? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409029010/ | Quick Look | ![]() |
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667 | NGC7582 | 349.5634 | -42.322 | 348.875032 | -42.595557 | 331.740868 | -34.366673 | 348.21143031 | -65.69925686 | 64.738 | 54248.9237152778 | 2007-05-28 22:10:09 | 54249.7328587963 | 2007-05-29 17:35:19 | 702052020 | 28.769 | 25 | 28.769 | 28.769 | 0 | 28.769 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24.6824 | 24.6824 | 69.9059 | 0 | PROCESSED | 57538.7538541667 | 2016-05-30 18:05:33 | 54695 | 2008-08-17 00:00:00 | 54255.6928472222 | 2007-06-04 16:37:42 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021332 | We propose to perform 4 Suzaku observations of 25 ks each (for a total of 100 ks) of the bright Seyfert 2 galaxy,NGC 7582.The aim of this proposal is to measure the distance of the gas that absorbs the nuclear radiation, by analyzing the pattern of variability of its column density.NGC7582 is the ideal target for this kind of analysis, because it already showed large variations of the column density of the absorber between X-ray observations taken a few years apart.With the present proposal, we intend to probe a wider range of timescales, from a week to about six months, in order to measure the distance of the absorber from the nucleus. This measure is crucial to understand the nature of the absorber in type 2 objects and the validity of the torus paradigm. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARCO CHIABERGE | USA | 2 | AO2 | MEASURING THE DISTANCE OF THE ABSORBER IN NGC 7582 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702052020/ | Quick Look | ![]() |
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668 | 4C+74.26 | 310.5668 | 75.0616 | 310.712656 | 74.880312 | 50.693329 | 74.661974 | 108.92036641 | 19.50581044 | 289.6922 | 54401.4314467593 | 2007-10-28 10:21:17 | 54403.2606944444 | 2007-10-30 06:15:24 | 702057010 | 91.583 | 100 | 91.583 | 91.583 | 0 | 91.591 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 94.114 | 94.114 | 158.0298 | 1 | PROCESSED | 57540.3825925926 | 2016-06-01 09:10:56 | 54776 | 2008-11-06 00:00:00 | 54409.2446064815 | 2007-11-05 05:52:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021354 | We propose a 100 ks observation of the bright broad-line radio galaxy 4C+74.26. A previous 35 ks XMM-Newton observation of 4C+74.26 yielded the first indication of a relativistically broadened Fe K line in a radio-loud AGN as well as other typical AGN properties (e.g., a warm absorber). The long observation proposed here will allow a detailed investigation of the Fe K line profile and improve significantly on the previous observation by detecting the associated Compton reflection hump with the HXD/PIN instrument. Modeling of these features will allow the first accurate determination of the geometry and structure of the inner accretion disk in a radio-loud AGN, and hence provide invaluable information for modeling the physics of the disk/jet interaction. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | DAVID BALLANTYNE | USA | 2 | AO2 | A CLOSE LOOK AT 4C+74.26 WITH SUZAKU: FOCUSING IN ON THE DISK/JET INTERACTION | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702057010/ | Quick Look | ![]() |
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669 | CYGNUS X-1 | 299.5796 | 35.2119 | 299.109658 | 35.075474 | 313.654707 | 54.262131 | 71.33922039 | 3.07967202 | 58.5817 | 56796.2767476852 | 2014-05-19 06:38:31 | 56799.3266203704 | 2014-05-22 07:50:20 | 409049010 | 14.5127 | 30 | 0 | 14.5127 | 0 | 0 | 0 | 3 | 0 | 0 | 1 | 0 | 0 | 113.8259 | 113.8259 | 263.4619 | 1 | PROCESSED | 57615.2053703704 | 2016-08-15 04:55:44 | 57180 | 2015-06-07 00:00:00 | 56811.8023958333 | 2014-06-03 19:15:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091241 | We propose for a 30 ks observation of the accreting black hole Cygnus X-1 to occur simultaneously with NuSTAR. In mid-2012, we obtained a joint Suzaku/NuSTAR observation of Cyg X-1 in the soft state, and we clearly see reflection features with a relativistically broadened iron line that we have used to constrain the geometry of the accretion disk, including finding possible evidence for a warped accretion disk, and the black hole spin. This TOO proposal is to observe the source in the hard state to constrain how the accretion geometry changes between states. The combination of Suzaku and NuSTAR covers, with very good energy resolution and throughput, the thermal component, the iron line complex, the iron absorption edge, and the hard X-ray reflection hump. | GALACTIC POINT SOURCES | 4 | A | JOHN TOMSICK | USA | 9 | AO9-TOO | CYGNUS X-1 IN THE HARD STATE WITH SUZAKU AND NUSTAR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409049010/ | Quick Look | ![]() |
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670 | 73P/SW3 | 317.9167 | 24.1666 | 317.359719 | 23.9609 | 329.535722 | 38.234901 | 71.86402338 | -16.24383714 | 72.7109 | 53868.3425 | 2006-05-13 08:13:12 | 53868.4085532407 | 2006-05-13 09:48:19 | 500013040 | 3.225 | 20 | 3.225 | 3.225 | 3.225 | 3.225 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.677 | 2.677 | 5.7039 | 0 | PROCESSED | 57534.2934143518 | 2016-05-26 07:02:31 | 54256 | 2007-06-05 00:00:00 | 54042.2977430556 | 2006-11-03 07:08:45 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013040/ | Quick Look | ![]() |
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671 | NGC 3079 | 150.4972 | 55.6116 | 149.652795 | 55.852826 | 130.116379 | 40.274577 | 157.90048948 | 48.39234685 | 268.6689 | 54612.8709722222 | 2008-05-26 20:54:12 | 54615.4362731482 | 2008-05-29 10:28:14 | 803039020 | 102.34 | 100 | 102.348 | 102.34 | 0 | 102.348 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102.0031 | 102.0031 | 221.6019 | 2 | PROCESSED | 57542.6909027778 | 2016-06-03 16:34:54 | 54999 | 2009-06-17 00:00:00 | 54633.7055439815 | 2008-06-16 16:55:59 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031303 | We will determine whether AGN can drive galactic-scale winds by observing NGC 3079, the best nearby candidate for such a wind. The edge-on spiral NGC 3079 hosts a Compton-thick AGN and is surrounded by a 40 kpc-scale soft X-ray nebula, the largest manifestation of outflow activity also seen in the optical and radio. Proving the outflow is AGN-driven requires Suzaku's unique abilities. We will measure the AGN luminosity using the HXD in the 15-40 keV range and the 2-10 keV band reflection spectrum to assess whether the AGN can radiatively-or-mechanically power the observed superwind. We will determine the origin of the soft X-ray nebula using the relative elemental abundances in the plasma. We can also detect any significant starburst through the 6.7 keV line emission it would create. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | DAVID STRICKLAND | USA | 3 | AO3 | NGC 3079'S 40 KPC-SCALE OUTFLOW: AGN OR STARBURST-DRIVEN? | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803039020/ | Quick Look | ![]() |
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672 | 3C 452 | 341.4131 | 39.7498 | 340.846907 | 39.486403 | 2.315539 | 43.172801 | 98.13461856 | -16.98917572 | 65.3539 | 54267.3964351852 | 2007-06-16 09:30:52 | 54268.8294444444 | 2007-06-17 19:54:24 | 702073010 | 66.68 | 53 | 66.696 | 66.68 | 0 | 66.696 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61.4487 | 61.4487 | 123.8018 | 3 | PROCESSED | 57538.9941550926 | 2016-05-30 23:51:35 | 54695 | 2008-08-17 00:00:00 | 54319.4923032407 | 2007-08-07 11:48:55 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021372 | The nature and even the existence of type II quasars is highly controversial. Due to their highly obscured nature, very hard (> 15 keV) observations are needed to probe their properties. With the 9-month SWIFT BAT all-sky AGN survey, detection of heavily obscured sources is now possible. Indeed, 6 type II quasars have been identified. Their properties, however, are a challenge to standard AGN models e.g., all but one of these sources are strong radio sources and several have optical spectra indicative of an un-absorbed source. We propose Suzaku observations of the 5 without broadband high signal to noise x-ray data to perform a detailed analysis of their x-ray properties and to understand their relationship to the lower luminosity well studied Seyfert IIs. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RICHARD MUSHOTZKY | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF SWIFT BAT TYPE II QUASARS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702073010/ | Quick Look | ![]() |
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673 | LMC X-3 OFF FIELD 1 | 85.5783 | -64.5441 | 85.521216 | -64.565729 | 45.792643 | -87.283954 | 274.09377866 | -31.6918405 | 324.0002 | 53847.1442361111 | 2006-04-22 03:27:42 | 53848.0099421296 | 2006-04-23 00:14:19 | 501097010 | 43.6067 | 50 | 43.6067 | 43.6067 | 43.6067 | 43.6067 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 42.0261 | 42.0261 | 74.7459 | 0 | PROCESSED | 57533.5339583333 | 2016-05-25 12:48:54 | 54526 | 2008-03-01 00:00:00 | 53907.3335763889 | 2006-06-21 08:00:21 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011256 | The Galactic corona is believed to play an essential role in the ``eco-system'' of the Galaxy. But the extent as well as the physical properties of the corona are yet to be determined. We request deep Suzaku XIS observations of the soft X-ray background in the vicinity of LMC X-3, toward which we have already conducted far-UV and X-ray absorption line spectroscopy. We have developed a software tool for a joint model fit to the absorption and emission data, allowing for statistical tests of various models and constraints on such parameters as hot gas temperature, density, and scale. The results will provide a unique calibration of our understanding of the corona. | GALACTIC DIFFUSE EMISSION | 5 | A | Q. DANIEL WANG | USA | 1 | AO1 | A JOINT EMISSION AND ABSORPTION STUDY OF THE GALACTIC CORONA | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501097010/ | Quick Look | ![]() |
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674 | VELA SNR CB3 | 129.7826 | -44.6964 | 129.353744 | -44.51903 | 154.049323 | -59.60688 | 263.57338638 | -1.96329272 | 278.1748 | 55318.927974537 | 2010-05-02 22:16:17 | 55319.3418402778 | 2010-05-03 08:12:15 | 505070010 | 18.1718 | 20 | 18.1718 | 18.1718 | 0 | 18.1718 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.1544 | 17.1544 | 35.7539 | 1 | PROCESSED | 57551.3562847222 | 2016-06-12 08:33:03 | 55696 | 2011-05-15 00:00:00 | 55330.1275925926 | 2010-05-14 03:03:44 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051304 | The Vela SNR is known to have ejecta bullets outside the main shell. In addition to these bullets, signatures of ejecta inside the main shell have been uncovered in recent X-ray studies. Mostly, these are rich in light metals such as O, Ne, or Mg, whereas no Fe-rich ejecta had yet been detected. Based on archival XMM-Newton data, we found a possible Fe-rich ejecta bullet headed roughly in the opposite direction of Vela pulsar's motion. This would provide us with a window into the core-collapse SN explosion of the Vela SNR. Since its electron temperature is very low (~0.1 keV), the good Suzaku XIS response below 0.5 keV is suitable to study this object. We propose to observe it in four pointings. The requested exposure time is 20 ks each, resulting in a total exposure time of 80 ks. | GALACTIC DIFFUSE EMISSION | 5 | B | SATORU KATSUDA | USA | 5 | AO5 | IRON-RICH EJECTA BULLET IN THE VELA SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505070010/ | Quick Look | ![]() |
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675 | MONOGEM RING W1 | 100.4191 | 15.2834 | 99.703498 | 15.332031 | 100.143287 | -7.791413 | 198.20484712 | 4.79777248 | 269.9998 | 55998.5603356482 | 2012-03-12 13:26:53 | 56000.0002314815 | 2012-03-14 00:00:20 | 506053010 | 61.1266 | 60 | 61.1267 | 61.1266 | 0 | 61.1266 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 59.074 | 59.074 | 124.3739 | 1 | PROCESSED | 57604.899849537 | 2016-08-04 21:35:47 | 56382 | 2013-03-31 00:00:00 | 56016.6737152778 | 2012-03-30 16:10:09 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061316 | We propose to observe the oldest, nearby SNR, the Monogem Ring, with the Suzaku XIS to study the plasma conditions in two locations which are near the Galactic plane and where there is evidence of a significant interaction with cooler (10^4 - 10^5 K), denser material. We chose one pointing where the turbulent mixing of hot and cooler gas should be large, and an adjacent pointing where the mixing should be small. From our previous Suzaku observation at a region far from the plane, we derived an ionization timescale for the non-equilibrium plasma which is apparently inconsistent with the age of the SNR. Our proposed observations will allow a detailed comparison of the plasma conditions in these regions with very different histories, and initial and current conditions. | GALACTIC DIFFUSE EMISSION | 5 | C | PAUL PLUCINSKY | USA | 6 | AO6 | STUDYING THE PLASMA EVOLUTION IN THE MONOGEM RING | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506053010/ | Quick Look | ![]() |
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676 | G236+38 ON | 146.5345 | 0.5057 | 145.892219 | 0.737078 | 148.588681 | -12.195052 | 235.93345442 | 38.21375915 | 307.3884 | 55713.4761574074 | 2011-06-01 11:25:40 | 55715.0002314815 | 2011-06-03 00:00:20 | 506055010 | 69.8025 | 70 | 69.8025 | 69.8025 | 0 | 69.8025 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64.3488 | 64.3488 | 131.674 | 0 | PROCESSED | 57602.2264351852 | 2016-08-02 05:26:04 | 56127 | 2012-07-19 00:00:00 | 55757.6954050926 | 2011-07-15 16:41:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061321 | Interstellar clouds cast shadows in the soft X-ray background (SXRB). Observations of these shadows enable us to disentangle the various components of the SXRB. Unfortunately, to date, shadowing observations with XMM or Suzaku have only been published for three directions, all in the southern Galactic hemisphere. We propose two new pairs of on- and off-cloud shadowing observations, in order to sample the northern Galactic hemisphere. Our particular goal is to obtain accurate X-ray spectra of the Galactic halo, which we will compare with the predictions of models of galactic fountains and infalling extragalactic material. | GALACTIC DIFFUSE EMISSION | 5 | B | DAVID HENLEY | USA | 6 | AO6 | UNDERSTANDING THE ORIGIN OF THE GALACTIC HALO USING SHADOWING OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506055010/ | Quick Look | ![]() |
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677 | COMET_8P_TUTTLE-P1-3 | 28.0473 | 7.5049 | 27.389882 | 7.258447 | 28.728614 | -3.762405 | 148.10975305 | -52.37174422 | 248.4997 | 54470.6493055556 | 2008-01-05 15:35:00 | 54470.7154861111 | 2008-01-05 17:10:18 | 502062030 | 1.9633 | 2 | 1.9633 | 1.9633 | 0 | 1.9633 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1.905 | 1.905 | 5.718 | 0 | PROCESSED | 57540.9903935185 | 2016-06-01 23:46:10 | 54908 | 2009-03-18 00:00:00 | 54542.2294791667 | 2008-03-17 05:30:27 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062030/ | Quick Look | ![]() |
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678 | SNR HB3 SE-A | 35.6022 | 61.9246 | 34.662678 | 61.696985 | 57.575576 | 44.47157 | 133.41628397 | 0.91883689 | 247.499 | 56322.7203935185 | 2013-01-30 17:17:22 | 56323.4079050926 | 2013-01-31 09:47:23 | 507056010 | 46.748 | 40 | 46.748 | 46.7517 | 0 | 46.7597 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.9628 | 43.9628 | 59.3939 | 0 | PROCESSED | 57608.6541666667 | 2016-08-08 15:42:00 | 56709 | 2014-02-21 00:00:00 | 56342.6336921296 | 2013-02-19 15:12:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071316 | We propose to study the large SNR HB3, which is classified as the mixed-morphology SNRs. The Fermi LAT revealed recently bright gamma-ray emissions adjacent to the southeastern shell of HB3, indicating the gamma rays originate in shocked molecular clouds associated with the nearby HII region W3/W4. However it is difficult to determine the gamma-ray origins since the HII regions are dominant in all energy bands except for X-ray. Our aim is to obtain the spatial structure and the temperature of thermal X-ray emissions at this site. These information will help us to understand whether HB3 interacts with molecular clouds. For this purpose, we require high sensitivities and the wide field of view to cover the southeastern shell. Suzaku is an ideal X-ray observatory to achieve this objective. | GALACTIC DIFFUSE EMISSION | 5 | C | JUNICHIRO KATSUTA | USA | 7 | AO7 | SUZAKU OBSERVATION OF A GAMMA-RAY EMISSION SNR, HB3 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507056010/ | Quick Look | ![]() |
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679 | NGC3227 | 155.8766 | 19.8689 | 155.194036 | 20.122276 | 150.387342 | 9.143225 | 216.98457422 | 55.44588075 | 115.8562 | 54767.3422685185 | 2008-10-28 08:12:52 | 54768.8487731482 | 2008-10-29 20:22:14 | 703022010 | 58.9172 | 50 | 58.9172 | 58.9172 | 0 | 58.9172 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52.0337 | 52.0337 | 130.1478 | 1 | PROCESSED | 57544.2886689815 | 2016-06-05 06:55:41 | 54557 | 2008-04-01 00:00:00 | 54788.4566203704 | 2008-11-18 10:57:32 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031013 | We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARTIN ELVIS | USA | 3 | AO3 | NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703022010/ | Quick Look | ![]() |
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680 | NGC741S2_P2 | 29.0179 | 5.3952 | 28.364923 | 5.150978 | 28.892288 | -6.076565 | 150.99426375 | -53.91742537 | 71.6631 | 55053.608287037 | 2009-08-10 14:35:56 | 55053.8425347222 | 2009-08-10 20:13:15 | 804055020 | 10.5481 | 10 | 10.5481 | 10.5481 | 0 | 10.5481 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9.548 | 9.548 | 20.2299 | 0 | PROCESSED | 57548.1047800926 | 2016-06-09 02:30:53 | 55465 | 2010-09-26 00:00:00 | 55098.1704166667 | 2009-09-24 04:05:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JOEL BREGMAN | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804055020/ | Quick Look | ![]() |
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681 | NGC3227 | 155.8768 | 19.8689 | 155.194236 | 20.122276 | 150.38752 | 9.143295 | 216.98468368 | 55.44605831 | 113.2489 | 54782.1173032407 | 2008-11-12 02:48:55 | 54783.7293865741 | 2008-11-13 17:30:19 | 703022030 | 56.5715 | 50 | 56.5772 | 56.5852 | 0 | 56.5715 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50.2231 | 50.2231 | 139.2698 | 1 | PROCESSED | 57544.401724537 | 2016-06-05 09:38:29 | 54557 | 2008-04-01 00:00:00 | 54797.3603356482 | 2008-11-27 08:38:53 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031013 | We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARTIN ELVIS | USA | 3 | AO3 | NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703022030/ | Quick Look | ![]() |
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682 | RX J1713 CENTER | 258.5686 | -39.6657 | 257.702123 | -39.608442 | 260.830462 | -16.587092 | 347.49241435 | -0.52884605 | 86.0002 | 56713.2203125 | 2014-02-25 05:17:15 | 56714.6669212963 | 2014-02-26 16:00:22 | 508068010 | 82.0615 | 80 | 82.0695 | 82.0695 | 0 | 82.0615 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.8059 | 34.8059 | 50.3319 | 0 | PROCESSED | 57613.9125231482 | 2016-08-13 21:54:02 | 57089 | 2015-03-08 00:00:00 | 56723.6064699074 | 2014-03-07 14:33:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081313 | Detecting thermal emission and determining the ambient density are the missing keys to constrain hadronic acceleration in X-ray synchrotron-dominated SNRs. In the prototypical CR accelerator RX J1713.7-3946, X-ray thermal emission has been sought for over a decade, without success. Deep Suzaku observations will constrain either the conditions of the ambient medium in which the SNR is evolving, or the SN progenitor type (core-collapse or thermonuclear) and nucleosynthesis yield. | GALACTIC DIFFUSE EMISSION | 5 | B | FABIO ACERO | USA | 8 | AO8 | STUDY OF THE THERMAL EMISSION IN THE SYNCHROTRON DOMINATED SNR RX J1713.7-3946 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508068010/ | Quick Look | ![]() |
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683 | COMET_8P_TUTTLE-P2_BGD-1 | 40.599 | -37.8517 | 40.099004 | -38.063935 | 20.76393 | -50.124108 | 244.68396515 | -64.39213957 | 254.2787 | 54492.4296643518 | 2008-01-27 10:18:43 | 54492.562662037 | 2008-01-27 13:30:14 | 502064010 | 6.5707 | 5 | 6.5707 | 6.6024 | 0 | 6.5867 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6.6293 | 6.6293 | 11.4879 | 0 | PROCESSED | 57541.4243518518 | 2016-06-02 10:11:04 | 54912 | 2009-03-22 00:00:00 | 54546.2413888889 | 2008-03-21 05:47:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502064010/ | Quick Look | ![]() |
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684 | NGC 4051 | 180.7984 | 44.5394 | 180.160059 | 44.817725 | 159.257872 | 40.347523 | 148.85547697 | 70.08163582 | 138.344 | 54776.3187847222 | 2008-11-06 07:39:03 | 54782.1112731482 | 2008-11-12 02:40:14 | 703023010 | 274.5305 | 340 | 274.5305 | 274.5305 | 0 | 274.5305 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 220.1993 | 220.1993 | 441.4488 | 3 | PROCESSED | 57544.5089930556 | 2016-06-05 12:12:57 | 54557 | 2008-04-01 00:00:00 | 54795.7746527778 | 2008-11-25 18:35:30 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031014 | The powerful combination of Principal Components Analysis with time-resolved X-ray spectroscopy of Seyfert AGN has shown strong evidence that changes in a complex absorber are the origin of much of observed AGN spectral and flux variability. Large column, high ionization layers of gas may arise in a disk wind, representing a significant new, and possibly dominant, component, responsible for shaping the X-ray spectrum of AGN. The broad bandpass of Suzaku gives us a unique opportunity to model primary and reflected continua and the effects of variable absorbing zones, and test wind and other models. We propose a long 340 ks exposure on the NLSy1 NGC 4051 whose large amplitude of variability and well-studied complex absorption will test those models to the limit | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TRACEY TURNER | USA | 3 | AO3 | DECONSTRUCTING SEYFERT SPECTRA - TIME FOR A PARADIGM SHIFT? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703023010/ | Quick Look | ![]() |
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685 | PDS 456 | 262.0806 | -14.2617 | 261.369911 | -14.221632 | 262.221213 | 8.965556 | 10.39448289 | 11.16711992 | 96.2509 | 56359.500150463 | 2013-03-08 12:00:13 | 56362.375162037 | 2013-03-11 09:00:14 | 707035030 | 108.3397 | 450 | 108.3477 | 108.3477 | 0 | 108.3397 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 94.226 | 94.226 | 248.3918 | 3 | PROCESSED | 57610.7991435185 | 2016-08-10 19:10:46 | 56018 | 2012-04-01 00:00:00 | 56373.5603125 | 2013-03-22 13:26:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071431 | PDS 456 is the most luminous nearby (z=0.184) AGN, more typical of quasars at high redshift. A 2007 Suzaku observation resolved iron K absorption at 9 keV in the QSO frame, moving at near relativistic velocities (0.25c). A follow-up 2011 observation was highly absorbed and showed a direct response of the iron K absorber to a decrease in the ionizing flux, while the harder photons lag behind the soft, by 10^4 secs. We propose to monitor the remarkable spectral variability and outflow from PDS 456, through a deep 450ks Suzaku observation. We wish to:- (i) quantify the time lags and determine the location of the reprocessor, (ii) determine the origin and timescale of the absorber variability and (iii) measure the hard X-ray variability from a Compton thick absorber in PDS 456. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | JAMES REEVES | USA | 7 | AO7 | VARIABILITY AND REVERBERATION OF THE QUASAR WIND IN PDS 456 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707035030/ | Quick Look | ![]() |
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686 | ARC1 | 40.8605 | -42.0069 | 40.383748 | -42.218277 | 17.737941 | -53.844666 | 253.28744097 | -62.75503946 | 235.1247 | 54480.7980787037 | 2008-01-15 19:09:14 | 54482.7640509259 | 2008-01-17 18:20:14 | 502070010 | 104.3694 | 100 | 104.3774 | 104.3854 | 0 | 104.3694 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 115.4202 | 115.4202 | 169.8377 | 3 | PROCESSED | 57541.3640277778 | 2016-06-02 08:44:12 | 54860 | 2009-01-29 00:00:00 | 54490.7270717593 | 2008-01-25 17:26:59 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021222 | Outside of the largest loops in the northern sky, few X-ray bright regions in the Galactic halo are understood. Here, we propose to study of a medium sized (~10 degree) bright feature in the southern sky. The feature is arc-shaped, suspiciously like the edge of a hot bubble. We propose to make three Suzaku observations along a radial line through the arc. With them, we will be able to determine the thermal properties of the region and whether or not the plasma temperature decreases with radius from the projected center, as expected for middle aged supernova remnants. | GALACTIC DIFFUSE EMISSION | 5 | C | ROBIN SHELTON | USA | 2 | AO2 | A CLOSER LOOK AT HOT HALO GAS: AN EXAMINATION OF AN X-RAY BRIGHT ARC | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502070010/ | Quick Look | ![]() |
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687 | SN 2005KD | 60.8552 | 71.7156 | 59.486745 | 71.577171 | 76.353108 | 49.655537 | 136.84988934 | 14.24754739 | 218.8053 | 54568.8904976852 | 2008-04-12 21:22:19 | 54570.0348842593 | 2008-04-14 00:50:14 | 703025010 | 51.6289 | 50 | 51.6289 | 51.6369 | 0 | 51.6449 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 63.5726 | 63.5726 | 98.8639 | 1 | PROCESSED | 57542.2950694444 | 2016-06-03 07:04:54 | 54947 | 2009-04-26 00:00:00 | 54581.1998842593 | 2008-04-25 04:47:50 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031241 | Supernovae (SNe) 2005kd and 2006jd are some of the brightest SNe ever detected in X-rays. The high X-ray luminosities (>E41 erg/s) are the results of the SN shock interacting with dense material in the environment of the SNe. We propose one Suzaku observation of each SN to obtain high-quality spectra that will be used to measure the temperature of the forward and reverse shock and to establish the rate of decline in comparison with existing Swift, Chandra and XMM-Newton data. The data will further be used to measure the circumstellar matter density and mass-loss rate of the progenitors to probe the nature of the SN progenitors. Our science objectives rely on Suzaku's uniqueness, i.e. the large collecting area, good spectral resolution, and the high sensitivity in the hard X-ray band. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | STEFAN IMMLER | USA | 3 | AO3 | SUZAKU OBSERVATIONS OF X-RAY BRIGHT SUPERNOVAE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703025010/ | Quick Look | ![]() |
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688 | ARC_BACKGROUND | 39.8321 | -35.8483 | 39.320146 | -36.062945 | 21.353527 | -48.064568 | 240.48423372 | -65.50115915 | 257.6627 | 54496.6274537037 | 2008-01-31 15:03:32 | 54499.812662037 | 2008-02-03 19:30:14 | 502072010 | 0 | 100 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 105.161 | 105.161 | 275.1537 | 4 | PROCESSED | 57541.5227314815 | 2016-06-02 12:32:44 | 54883 | 2009-02-21 00:00:00 | 54515.6371875 | 2008-02-19 15:17:33 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021222 | Outside of the largest loops in the northern sky, few X-ray bright regions in the Galactic halo are understood. Here, we propose to study of a medium sized (~10 degree) bright feature in the southern sky. The feature is arc-shaped, suspiciously like the edge of a hot bubble. We propose to make three Suzaku observations along a radial line through the arc. With them, we will be able to determine the thermal properties of the region and whether or not the plasma temperature decreases with radius from the projected center, as expected for middle aged supernova remnants. | GALACTIC DIFFUSE EMISSION | 5 | C | ROBIN SHELTON | USA | 2 | AO2 | A CLOSER LOOK AT HOT HALO GAS: AN EXAMINATION OF AN X-RAY BRIGHT ARC | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502072010/ | Quick Look | ![]() |
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689 | MBM20 | 68.9409 | -14.6227 | 68.368213 | -14.724058 | 64.473913 | -36.217726 | 211.39642208 | -36.55928879 | 252.4258 | 54507.612025463 | 2008-02-11 14:41:19 | 54510.6980439815 | 2008-02-14 16:45:11 | 502075010 | 107.0668 | 100 | 107.0668 | 107.0668 | 0 | 107.0668 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92.8036 | 92.8036 | 266.6036 | 2 | PROCESSED | 57541.6362847222 | 2016-06-02 15:16:15 | 54889 | 2009-02-27 00:00:00 | 54522.4496527778 | 2008-02-26 10:47:30 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021224 | We propose a study of the X-ray Emission from the Local Bubble (LB) and the Galactic Halo pointing toward the neutral hydrogen cloud MBM20 and a nearby low hydrogen column density, high latitude line of sight (called the Eridanus Hole). MBM20 absorbs about 75% of the foreground emission in the keV energy band, while the Eridanus Hole absorbs only 8%. The shadow of the cloud will be used to study the energy distribution of the X-ray foreground in the energy range 0.4-2 keV, to separate O VII and O VIII lines and study the composition and evolution of the LB. The comparison with the spectrum from the Eridanus Hole will be used to estimate the background emission due to the galactic halo and extragalactic source. | GALACTIC DIFFUSE EMISSION | 5 | B | MASSIMILIANO GALEAZZI | USA | 2 | AO2 | STUDYING THE PROPERTIES OF THE LOCAL BUBBLE AND GALACTIC HALO TOWARD MBM20 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502075010/ | Quick Look | ![]() |
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690 | MRK 348 | 12.1911 | 31.9636 | 11.514938 | 31.691174 | 24.328489 | 24.485278 | 122.27104531 | -30.90471809 | 71.8836 | 54645.9325694444 | 2008-06-28 22:22:54 | 54648.0591203704 | 2008-07-01 01:25:08 | 703029010 | 87.4614 | 80 | 88.5334 | 87.4614 | 0 | 88.5334 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 78.5504 | 78.5504 | 183.7239 | 0 | PROCESSED | 57542.9708333333 | 2016-06-03 23:18:00 | 55031 | 2009-07-19 00:00:00 | 54664.7845601852 | 2008-07-17 18:49:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031322 | X-ray observations of Seyfert 2 have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by the AGN Unification Scheme. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (80 ksec each) of three bright Compton-thin Seyfert 2 galaxies, selected from the Swift/BAT survey, with a hard X-ray flux exceeding 9e-11cgs, to form a flux-limited sample. The unprecedented bandpass of Suzaku offers a unique tool to investigate the X-ray emission of these sources, allowing us to put strong constraints on the reprocessing matter in Seyfert 2s. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | VALENTINA BRAITO | USA | 3 | AO3 | THE NATURE OF THE X-RAY ABSORBER IN SEYFERT 2 GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703029010/ | Quick Look | ![]() |
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691 | 3C 396 | 285.987 | 5.4347 | 285.37156 | 5.359452 | 288.059681 | 27.878529 | 39.1930056 | -0.29514711 | 64.6066 | 56773.2792592593 | 2014-04-26 06:42:08 | 56775.1223726852 | 2014-04-28 02:56:13 | 509038010 | 82.7922 | 80 | 82.7922 | 82.7922 | 0 | 82.7922 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 1.0111 | 1.0111 | 1.744 | 0 | PROCESSED | 57614.9978703704 | 2016-08-14 23:56:56 | 57157 | 2015-05-15 00:00:00 | 56789.6241782407 | 2014-05-12 14:58:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091315 | We propose to conduct Suzaku observations of the Galactic supernova remnants (SNRs) Kes 69 (G21.8-0.6) and 3C 396 (G39.2-0.3). These SNRs were detected in the infrared by Spitzer and their infrared colors suggest that shocked molecules produce the observed emission. Published analyses of the X-ray emission from these SNRs (along with our own analysis of archival XMM-Newton and Chandra observations of these sources) reveals that the emission from both Kes 69 and 3C 396 is thermal and that they may both be mixed-morphology SNRs (MMSNRs) but deeper observations are needed to clarify their X-ray spectral properties. In particular, we will investigate whether these X-ray emitting plasmas are overionized, which is observed for other MMSNRs. | GALACTIC DIFFUSE EMISSION | 5 | B | THOMAS PANNUTI | USA | 9 | AO9 | SUZAKU OBSERVATIONS OF THE SPITZER-DETECTED GALACTIC SUPERNOVA REMNANTS KES 69 (G21.8-0.6) AND 3C 396 (G39.2-0.3) | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509038010/ | Quick Look | ![]() |
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692 | PKS 0326-288 | 52.1551 | -28.6965 | 51.63485 | -28.868348 | 39.555316 | -45.73648 | 224.90475513 | -55.39691379 | 250.3682 | 55226.8889699074 | 2010-01-30 21:20:07 | 55228.3266087963 | 2010-02-01 07:50:19 | 704039010 | 58.0237 | 60 | 58.0238 | 58.0237 | 0 | 58.0237 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 49.6247 | 49.6247 | 124.1859 | 3 | PROCESSED | 57550.4794560185 | 2016-06-11 11:30:25 | 55616 | 2011-02-24 00:00:00 | 55249.7586805556 | 2010-02-22 18:12:30 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041413 | We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195~keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log($L_x$) $> 45.5$~ergs~sec$^{-1}$) absorbed tyoe II QSOs in the local universe and the most ripe for study with suzaku. 3C~332 is believed to be Compton-thick as suggested by chandra observations, and the newly discovered source SWIFT~J2344.6-4233 at a redshift of $z=0.6$ is the most luminous object in the BAT sample with log($L_x$) $=46.5$~ergs~sec$^{-1}$. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | WAYNE BAUMGARTNER | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704039010/ | Quick Look | ![]() |
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693 | 3C 332 | 244.4239 | 32.3632 | 243.942335 | 32.484407 | 233.11322 | 52.57597 | 52.6372471 | 45.34839384 | 292.5008 | 55051.0341782407 | 2009-08-08 00:49:13 | 55052.4655092593 | 2009-08-09 11:10:20 | 704038010 | 59.8339 | 60 | 59.8339 | 59.8339 | 0 | 59.8339 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.0491 | 46.0491 | 123.652 | 0 | PROCESSED | 57548.1132407407 | 2016-06-09 02:43:04 | 55437 | 2010-08-29 00:00:00 | 55067.2557986111 | 2009-08-24 06:08:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041413 | We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195~keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log($L_x$) $> 45.5$~ergs~sec$^{-1}$) absorbed tyoe II QSOs in the local universe and the most ripe for study with suzaku. 3C~332 is believed to be Compton-thick as suggested by chandra observations, and the newly discovered source SWIFT~J2344.6-4233 at a redshift of $z=0.6$ is the most luminous object in the BAT sample with log($L_x$) $=46.5$~ergs~sec$^{-1}$. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | WAYNE BAUMGARTNER | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704038010/ | Quick Look | ![]() |
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694 | Q0940-1050 | 145.7249 | -11.0726 | 145.114895 | -10.843374 | 152.028873 | -23.330401 | 246.39011763 | 30.43738638 | 275.7617 | 54616.2125578704 | 2008-05-30 05:06:05 | 54617.1321064815 | 2008-05-31 03:10:14 | 703040010 | 32.3623 | 28 | 32.3623 | 32.3623 | 0 | 32.3623 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.7776 | 26.7776 | 79.4378 | 1 | PROCESSED | 57542.689212963 | 2016-06-03 16:32:28 | 54999 | 2009-06-17 00:00:00 | 54633.6981828704 | 2008-06-16 16:45:23 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031334 | Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GEORGE CHARTAS | USA | 3 | AO3 | A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703040010/ | Quick Look | ![]() |
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695 | PKS 0528+134 | 82.7307 | 13.5905 | 82.023508 | 13.553568 | 82.834667 | -9.669991 | 191.31463869 | -10.98486414 | 89.0231 | 54736.1098611111 | 2008-09-27 02:38:12 | 54741.6752777778 | 2008-10-02 16:12:24 | 703048010 | 203.4574 | 200 | 203.4654 | 203.4654 | 0 | 203.4574 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 135.3629 | 135.3629 | 443.8619 | 4 | PROCESSED | 57544.2063888889 | 2016-06-05 04:57:12 | 55148 | 2009-11-13 00:00:00 | 54780.7843287037 | 2008-11-10 18:49:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031345 | We propose a Suzaku observation of bright gamma-ray blazar PKS 0528+134, to be conducted jointly with GLAST, radio, and optical telescopes. This observation was accepted in the previous AO, but was not conducted due to GLAST launch delays. The goal is to obtain time-resolved broadband spectra. The X-ray and gamma-ray fluxes are known to be rapidly variable, but the information regarding the correlation between the X-ray and gamma-ray flux is limited. Such detailed spectral and variability studies are crucial to discriminate between different radiation scenarios responsible for production of X-rays and gamma-rays, and to constrain the matter content and by extension, the formation process of the jet, dissipation of the jet energy, and energization of the radiating particles. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GRZEGORZ MADEJSKI | USA | 3 | AO3 | SUZAKU AND GLAST OBSERVATIONS OF PKS 0528+134 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703048010/ | Quick Look | ![]() |
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696 | 3C120 | 68.298 | 5.3556 | 67.633455 | 5.25115 | 67.433074 | -16.401934 | 190.3728125 | -27.39468757 | 237.4583 | 53782.5602199074 | 2006-02-16 13:26:43 | 53783.5876967593 | 2006-02-17 14:06:17 | 700001020 | 41.5545 | 160 | 41.5545 | 41.5545 | 41.5545 | 41.5545 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 36.8461 | 36.8461 | 88.772 | 2 | PROCESSED | 57533.0172685185 | 2016-05-25 00:24:52 | 54247 | 2007-05-27 00:00:00 | 54041.2956365741 | 2006-11-02 07:05:43 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001003 | Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 0 | SWG | BROAD-BAND MONITORING OF 3C120 IN VARIOUS ACCRETING STATES | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700001020/ | Quick Look | ![]() |
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697 | 3C120 | 68.2979 | 5.3541 | 67.633361 | 5.249649 | 67.432732 | -16.403401 | 190.37414386 | -27.39561637 | 262.5053 | 53796.9456828704 | 2006-03-02 22:41:47 | 53797.8606365741 | 2006-03-03 20:39:19 | 700001040 | 40.9051 | 160 | 40.9131 | 40.9211 | 40.9211 | 40.9051 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 40.3118 | 40.3118 | 79.0459 | 0 | PROCESSED | 57533.1408912037 | 2016-05-25 03:22:53 | 54247 | 2007-05-27 00:00:00 | 54041.627025463 | 2006-11-02 15:02:55 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001003 | Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JUN KATAOKA | JAP | 0 | SWG | BROAD-BAND MONITORING OF 3C120 IN VARIOUS ACCRETING STATES | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700001040/ | Quick Look | ![]() |
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698 | NGC 5506 | 213.312 | -3.2124 | 212.663098 | -2.97888 | 212.190832 | 9.596053 | 339.14600253 | 53.80603682 | 287.3743 | 53955.6875578704 | 2006-08-08 16:30:05 | 53957.003900463 | 2006-08-10 00:05:37 | 701030010 | 47.7531 | 150 | 47.7531 | 47.7531 | 47.7531 | 47.7531 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 41.0973 | 41.0973 | 113.7259 | 2 | PROCESSED | 57535.2578587963 | 2016-05-27 06:11:19 | 54695 | 2008-08-17 00:00:00 | 54116.2715740741 | 2007-01-16 06:31:04 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011312 | NGC 5506 is one of the brightest Seyferts in the X-ray sky, the second brightest in the PIN bandpass. Obscuring gas has kept the true nature of this AGN secret until recent optical and infrared studies have unmasked the narrow-line-seyfert 1 nucleus. With this knowledge, NGC 5506 is the perfect candidate for confirming the generality of a new result based on a recent XMM observation of Mkn 766, ie that the ionized component of Fe K emission originates from the inner accretion disk and closely tracks the hard X-ray continuum flux. This immediately gives us the ionization-state and size-scale of the inner disk. We request a 150 ks Suzaku observation to see whether a similar result holds for NGC 5506 and, by extension, may be a property of NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TRACEY TURNER | USA | 1 | AO1 | SUZAKU STUDY OF THE BRIGHTEST NARROW LINE SEYFERT 1: NGC 5506 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701030010/ | Quick Look | ![]() |
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699 | COMA E5.5 | 196.6115 | 27.8944 | 196.012448 | 28.161547 | 183.085886 | 31.985086 | 46.75951976 | 86.58537166 | 280.0017 | 55730.7852546296 | 2011-06-18 18:50:46 | 55731.2738657407 | 2011-06-19 06:34:22 | 806035010 | 10.8791 | 15 | 10.8871 | 10.8871 | 0 | 10.8791 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.5597 | 12.5597 | 42.1979 | 0 | PROCESSED | 57602.3474537037 | 2016-08-02 08:20:20 | 55652 | 2011-04-01 00:00:00 | 55770.1742939815 | 2011-07-28 04:10:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806035010/ | Quick Look | ![]() |
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700 | IRAS08572+3915 | 135.0664 | 39.0091 | 134.264876 | 39.204772 | 126.11779 | 21.048672 | 183.47368885 | 40.96543811 | 300.022 | 53839.0903240741 | 2006-04-14 02:10:04 | 53840.7752199074 | 2006-04-15 18:36:19 | 701053010 | 77.1974 | 75 | 77.2214 | 77.1974 | 77.2134 | 77.2214 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 62.3339 | 62.3339 | 145.4999 | 9 | PROCESSED | 57533.486875 | 2016-05-25 11:41:06 | 54401 | 2007-10-28 00:00:00 | 53906.2114699074 | 2006-06-20 05:04:31 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011344 | Ultraluminous infrared galaxies (ULIRGs) produce the energy outputs of quasars with nearly all the power emerging in the far-IR via reprocessing of optical, UV, and X-ray radiation by dust. The ultimate nuclear power source, be it AGN or compact starburst, of ULIRGs has been the focus of much debate since their discovery with the IRAS mission. While observations with Spitzer are unlocking the secrets of many nearby ULIRGs, some have nuclei that are apparently so obscured as to be optically thick even in the mid-IR. We have chosen three local ULIRGs, IRAS 08572+3915, IRAS15250+3609, and IRAS20551-4250 that are IR-bright, yet highly obscured for deep Suzaku observations to search for the tell-tale signs of a buried AGN: hard X-ray emission behind significant column densities of HI gas. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | SARAH GALLAGHER | USA | 1 | AO1 | ULTRAHARD X-RAY CASE STUDIES OF ULIRGS WITH DEEP SILICATE ABSORPTION | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701053010/ | Quick Look | ![]() |
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701 | MRK 352 | 14.9991 | 31.7575 | 14.31506 | 31.488197 | 26.597079 | 23.289939 | 125.05610732 | -31.07894727 | 255.5628 | 55202.4718402778 | 2010-01-06 11:19:27 | 55203.6009143518 | 2010-01-07 14:25:19 | 704025010 | 45.6717 | 40 | 45.6877 | 45.6717 | 0 | 45.6872 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.3693 | 22.3693 | 97.5358 | 1 | PROCESSED | 57550.0955439815 | 2016-06-11 02:17:35 | 55602 | 2011-02-10 00:00:00 | 55235.27125 | 2010-02-08 06:30:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041402 | The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | LISA WINTER | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704025010/ | Quick Look | ![]() |
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702 | SWIFT J0904.3+5538 | 136.117 | 55.5749 | 135.191467 | 55.77395 | 120.650833 | 36.933195 | 161.50516347 | 40.6960792 | 282.0039 | 54949.092025463 | 2009-04-28 02:12:31 | 54949.700162037 | 2009-04-28 16:48:14 | 704027010 | 41.9438 | 40 | 41.9438 | 41.9438 | 0 | 41.9438 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 35.8838 | 35.8838 | 52.5359 | 1 | PROCESSED | 57546.4424537037 | 2016-06-07 10:37:08 | 55343 | 2010-05-27 00:00:00 | 54973.440474537 | 2009-05-22 10:34:17 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041402 | The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | LISA WINTER | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704027010/ | Quick Look | ![]() |
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703 | UGC 6728 | 176.2197 | 79.6106 | 175.467594 | 79.888182 | 114.113262 | 63.856037 | 126.64092866 | 37.03371002 | 285.5693 | 54988.5646759259 | 2009-06-06 13:33:08 | 54989.5125925926 | 2009-06-07 12:18:08 | 704029010 | 49.0039 | 40 | 49.0039 | 49.0039 | 0 | 49.0039 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.5347 | 41.5347 | 81.8839 | 0 | PROCESSED | 57547.4998726852 | 2016-06-08 11:59:49 | 55364 | 2010-06-17 00:00:00 | 54998.3390740741 | 2009-06-16 08:08:16 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041402 | The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | LISA WINTER | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704029010/ | Quick Look | ![]() |
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704 | MCG-2-58-22 | 346.1839 | -8.6878 | 345.532632 | -8.95779 | 343.915361 | -2.560866 | 64.09176202 | -58.7610593 | 247.1128 | 55167.9420486111 | 2009-12-02 22:36:33 | 55170.9356365741 | 2009-12-05 22:27:19 | 704032010 | 138.9688 | 130 | 139.0088 | 138.9688 | 0 | 139.0088 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 105.4957 | 105.4957 | 258.6277 | 2 | PROCESSED | 57549.8017361111 | 2016-06-10 19:14:30 | 55553 | 2010-12-23 00:00:00 | 55187.5510763889 | 2009-12-22 13:13:33 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041404 | We propose a 130 ks Suzaku long-look to study the Fe K emission complex of the Seyfert 1.5 AGN MCG--2-58-22, which has the unique combination of being X-ray bright, ``bare'' (i.e., lacking a strong ionized absorber), and possibly hosting both a truncated accretion disk and ionized circumnuclear material. We aim to accurately constrain the geometry and ionization state of the accreting circumnuclear material of this likely low-Compton reflection source by resolving the Fe K alpha line and constraining its origin, which may likely be a truncated thin disk, and verifying a previous claim of emission from H-like Fe. We will also determine the origin of this object's soft excess. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | ALEX MARKOWITZ | USA | 4 | AO4 | A SUZAKU OBSERVATION OF MCG--2-58-22: A TRUNCATED OR IONIZED ACCRETION DISK? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704032010/ | Quick Look | ![]() |
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705 | MRK1018 | 31.5471 | -0.2351 | 30.907355 | -0.473179 | 29.3057 | -12.234469 | 159.73232745 | -57.66458833 | 73.6945 | 55015.0121759259 | 2009-07-03 00:17:32 | 55016.0939699074 | 2009-07-04 02:15:19 | 704044010 | 43.9014 | 40 | 43.9094 | 43.9014 | 0 | 43.9094 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.6884 | 37.6884 | 93.4578 | 5 | PROCESSED | 57547.7689467593 | 2016-06-08 18:27:17 | 55395 | 2010-07-18 00:00:00 | 55027.1070023148 | 2009-07-15 02:34:05 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041414 | We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | EZEQUIEL TREISTER | USA | 4 | AO4 | THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704044010/ | Quick Look | ![]() |
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706 | NGC 3718 | 173.2341 | 53.1118 | 172.54734 | 53.387989 | 147.276263 | 44.880657 | 146.87581124 | 60.21394242 | 142.7392 | 55128.8497800926 | 2009-10-24 20:23:41 | 55130.255775463 | 2009-10-26 06:08:19 | 704048010 | 59.8882 | 60 | 59.9202 | 59.8882 | 0 | 59.9202 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52.4392 | 52.4392 | 121.4599 | 0 | PROCESSED | 57548.9845138889 | 2016-06-09 23:37:42 | 55507 | 2010-11-07 00:00:00 | 55141.3212384259 | 2009-11-06 07:42:35 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041415 | The SWIFT BAT hard (14-195 KeV) survey is performing the first unbiased hard X-ray survey of the entire sky with follow-up observations with the Swift XRT to fully identify the sample. In this survey we have found two very low luminosity nearby hard X-ray sources which show little, if any, evidence for nuclear activity in the optical or UV band, and have very low apparent Eddington ratios. We propose Suzaku observations of these objects to determine whether there is an X-ray spectral signature of a low Eddington ratio, as predicted if these objects are indeed in a radiatively inefficient accretion flow. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RICHARD MUSHOTZKY | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF NGC4138 AND NGC3718 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704048010/ | Quick Look | ![]() |
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707 | N44 SB | 80.6234 | -67.9392 | 80.661581 | -67.984502 | 334.827675 | -86.129494 | 278.35092966 | -33.30497245 | 311.8533 | 54565.7359143518 | 2008-04-09 17:39:43 | 54566.5084953704 | 2008-04-10 12:12:14 | 803036010 | 30.5568 | 30 | 30.5568 | 30.5568 | 0 | 30.5568 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.9118 | 26.9118 | 66.748 | 1 | PROCESSED | 57542.2791898148 | 2016-06-03 06:42:02 | 54946 | 2009-04-25 00:00:00 | 54580.4450810185 | 2008-04-24 10:40:55 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031238 | Clusters of massive stars, through their stellar winds and supernovae, form large diffuse structures known as superbubbles (SBs), which play an essential role in shaping the local interstellar medium. Most SB models indicate that these objects should be dominated by thermal plasma processes. However, observations of 3 SBs have detected significant nonthermal contributions to their X-ray emission, which raises many questions. Is it generated by synchrotron, inverse-Compton, or nonthermal Bremsstrahlung processes? Are colliding stellar winds or internal supernova remnants responsible? We therefore propose to examine the X-ray emission from 3 X-ray bright SBs, to search for nonthermal X-ray emission, and if possible place strong constraints on the source of this emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | LARRY MADDOX | USA | 3 | AO3 | A SEARCH FOR NONTHERMAL X-RAY EMISSION FROM SUPERBUBBLES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803036010/ | Quick Look | ![]() |
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708 | NGC 4406 | 186.5483 | 12.9401 | 185.91466 | 13.216832 | 180.759915 | 14.456271 | 279.08850556 | 74.63107328 | 294.6659 | 55001.7603125 | 2009-06-19 18:14:51 | 55004.4793287037 | 2009-06-22 11:30:14 | 803043010 | 101.7736 | 90 | 101.7736 | 101.7736 | 0 | 101.7736 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86.5545 | 86.5545 | 234.8981 | 2 | PROCESSED | 57547.6610300926 | 2016-06-08 15:51:53 | 55384 | 2010-07-07 00:00:00 | 55015.2472569445 | 2009-07-03 05:56:03 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031404 | We propose Suzaku observations of three elliptical galaxies, selected on brightness and the availability of XMM-Newton RGS data, as part of a program to investigate their star formation history and chemical evolution via abundance studies of the hot interstellar medium. The low-energy sensitivity, spectral resolution, and low background of the Suzaku XIS enables the first accurate model-independent measurements of the abundance pattern while expanding the number of measurable temperature diagnostic features. Analysis of XIS spectra (critically, with SCI on), exclusively and in combination with RGS data, demonstrates the unique power of Suzaku to contribute to our understanding of the thermal and chemical properties of these systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MICHAEL LOEWENSTEIN | USA | 3 | AO3 | UNCOVERING THE TRUE ABUNDANCES OF ELLIPTICAL GALAXIES WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803043010/ | Quick Look | ![]() |
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709 | NGC 5174 | 202.3569 | 11.0203 | 201.73681 | 11.278322 | 196.356635 | 18.897363 | 333.76702191 | 71.58014685 | 102.4436 | 55219.0472685185 | 2010-01-23 01:08:04 | 55220.5835532407 | 2010-01-24 14:00:19 | 804048010 | 54.5151 | 50 | 54.5231 | 54.5151 | 0 | 54.5231 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.0362 | 44.0362 | 132.6979 | 0 | PROCESSED | 57550.3479050926 | 2016-06-11 08:20:59 | 55595 | 2011-02-03 00:00:00 | 55229.1361226852 | 2010-02-02 03:16:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041504 | Galaxies are missing most of their baryons when compared to the cosmological baryon to dark matter ratio: the Milky Way retained only 30% of its baryons while lower mass galaxies retain less than 10%. Probably, these baryons were expelled by intense galactic winds during the early star formation period at z = 1-3. These galactic winds can carry gas far beyond the virial radius of small and modest galaxies, but the most massive galaxies should retain much of this gas. We propose to test this picture by searching for the missing baryons surrounding two extremely massive spiral galaxies, with 6-8 times the stellar content of M31 and with v_rot = 370, 420 km/s. If successful, we will detect a significant fraction of the 3-4E11 Msun of the missing baryons as hot gas. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | JOEL BREGMAN | USA | 4 | AO4 | THE BARYON CONTENT OF MASSIVE SPIRAL GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804048010/ | Quick Look | ![]() |
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710 | NGC 1365 | 53.3909 | -36.1409 | 52.913513 | -36.307906 | 36.789839 | -53.036651 | 237.95774893 | -54.60665436 | 30.5416 | 55374.0284143518 | 2010-06-27 00:40:55 | 55377.9834606482 | 2010-06-30 23:36:11 | 705031010 | 151.6134 | 450 | 151.6294 | 151.6134 | 0 | 151.6214 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 123.2422 | 123.2422 | 341.6577 | 2 | PROCESSED | 57552.5171064815 | 2016-06-13 12:24:38 | 55287 | 2010-04-01 00:00:00 | 55434.2469444445 | 2010-08-26 05:55:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051112 | We propose 3 observations (~4 days each) of the Seyfert galaxy NGC 1365, at 2-week intervals. We aim to use eclipses to unambiguously identify the broad Fe K line, examine variability of the HXD/PIN excess, and to search for changes in the physical properties of the ionized absorber in this bright, nearby AGN. Shorter observations of this galaxy with XMM-Newton, Chandra and Suzaku showcase several remarkable physical traits: (1) FeXXV and FeXXVI K-shell absorption lines (the highest s/n detection so far among AGN), (2) rapidly varying cold absorption, (3) a highly significant relativistic Fe K emission line, and (4) a factor ~4 excess flux at high energies. The proposed observations will provide legacy spectra for what is arguably the single most physically-revealing obscured AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | LAURA BRENNEMAN | USA | 5 | AO5 | A LONG LOOK AT NGC 1365: DISC TOMOGRAPHY, IONIZED ABSORPTION AND HIGH ENERGY EXCESS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705031010/ | Quick Look | ![]() |
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711 | SNR G106.3+2.7 P3 | 336.5055 | 60.7692 | 336.063779 | 60.514367 | 20.620799 | 61.417005 | 106.0859109 | 2.74547808 | 12.2692 | 55424.0215509259 | 2010-08-16 00:31:02 | 55424.9841782407 | 2010-08-16 23:37:13 | 505073010 | 50.4548 | 50 | 50.4628 | 50.4548 | 0 | 50.4632 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50.2105 | 50.2105 | 83.1639 | 1 | PROCESSED | 57553.1155439815 | 2016-06-14 02:46:23 | 55805 | 2011-09-01 00:00:00 | 55439.1312037037 | 2010-08-31 03:08:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051305 | After two decades searching for the origin of the GeV emission from 3EG J2227+6122, it is now identified with PSR J2229+6114 and its PWN.~This highly energetic young pulsar lies within the arcmin diameter Boomerang radio nebula. Now, recently discovered nearby extended TeV emission suggest a second Vela-like "cocoon" feed by relic electrons from the PWN, blowing out the vast degree-scale radio feature.~Interactions of the SNR shock front with overlapping molecular cloud material can also contribute in the gamma-ray production.~An XIS mosaic will allow us to search for soft and hard X-ray emission similar to Vela's "Cocoon" and resolve the nature of the TeV emission and its connection to the Boomerang and the radio feature. | GALACTIC DIFFUSE EMISSION | 5 | C | ESTER ALIU | USA | 5 | AO5 | ORIGIN OF THE VHE GAMMA-RAY EMISSION FROM SNR G106.3+2.7 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505073010/ | Quick Look | ![]() |
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712 | NGC 6251 | 248.2903 | 82.5391 | 249.646931 | 82.638978 | 99.623854 | 73.274498 | 115.75265542 | 31.17774629 | 182.5432 | 55532.2390625 | 2010-12-02 05:44:15 | 55534.0341898148 | 2010-12-04 00:49:14 | 705039010 | 87.0706 | 85 | 87.0706 | 87.0706 | 0 | 87.0706 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 75.8074 | 75.8074 | 155.0879 | 1 | PROCESSED | 57554.3327546296 | 2016-06-15 07:59:10 | 55931 | 2012-01-05 00:00:00 | 55565.375162037 | 2011-01-04 09:00:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051411 | We propose an 85-ks Suzaku observation of NGC 6251, the brightest example of a low-excitation radio galaxy (LERG). We have previously suggested that LERGs violate conventional AGN unification schemes: they may lack an obscuring torus and are likely to accrete in a radiatively inefficient manner, with almost all of the energy released by the accretion process being channeled into powerful jets. However, Suzaku observations at low and high energies are needed to test this model directly. We will use the XIS and HXD to search for the signatures of accretion-related X-ray emission: (1) the 6.4 keV Fe Ka line, (2) heavily absorbed X-ray emission, and (3) the >10 keV Compton reflection bump. These results will have important implications for models of accretion and feedback in radio-loud AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | DANIEL EVANS | USA | 5 | AO5 | A DIRECT TEST OF THE NUCLEAR X-RAY DICHOTOMY IN RADIO-LOUD AGN | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705039010/ | Quick Look | ![]() |
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713 | A1795_FAR_SOUTHWEST | 206.9673 | 26.3143 | 206.388758 | 26.56302 | 193.820617 | 34.636362 | 32.43951308 | 77.37921169 | 300.5685 | 55011.5565162037 | 2009-06-29 13:21:23 | 55012.4849537037 | 2009-06-30 11:38:20 | 804083010 | 38.3573 | 35 | 38.3573 | 38.6253 | 0 | 38.6333 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57598.4742013889 | 2016-07-29 11:22:51 | 55395 | 2010-07-18 00:00:00 | 55027.5898726852 | 2009-07-15 14:09:25 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041528 | The outer regions of clusters beyond 0.5 r200 contain a large amount of the dark matter, baryons and metals in the system, yet they are poorly understood. We propose to conduct a new test of cluster and structure formation by probing the distribution of dark matter and the thermodynamic history of the ICM in the outskirts of the cluster Abell 1795. Our previous Suzaku observations of Abell 1795 indicate deviations from hydrostatic equilibrium; we sample two disjoint regions beyond r500, detecting cluster emission in one but not the other (a difference of 5-sigma). With the proposed observations spanning r500-r200, we will obtain a more sensitive measurement of the azimuthally averaged temperature and density at this radius and search for variations over a wider range of azimuth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 4 | AO4 | ABELL 1795 WITH SUZAKU: A NEW WINDOW ON CLUSTER FORMATION AND STRUCTURE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804083010/ | Quick Look | ![]() |
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714 | PDS 456 | 262.0809 | -14.2537 | 261.370252 | -14.213634 | 262.221057 | 8.97356 | 10.4015562 | 11.17111116 | 96.1694 | 55636.625462963 | 2011-03-16 15:00:40 | 55639.3564930556 | 2011-03-19 08:33:21 | 705041010 | 125.5272 | 130 | 125.5352 | 125.5272 | 0 | 125.5327 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 100.875 | 100.875 | 235.9276 | 2 | PROCESSED | 57601.2862615741 | 2016-08-01 06:52:13 | 56050 | 2012-05-03 00:00:00 | 55677.3183564815 | 2011-04-26 07:38:26 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051421 | PDS 456 is the most luminous nearby AGN and a recent Suzaku observation revealed a powerful ionized outflow moving at 0.25c with kinetic output matching the quasar bolometric luminosity. Above 10 keV the HXD appears to show a factor 3 rise in flux over the XIS, implying that a high column density absorber (>10^24 cm^-2) is located close to the X-ray source in order to partially covers its emission. We propose to study the remarkable X-ray absorption towards PDS 456 through two further 130 ks Suzaku observations. This will:-i) confirm the nature of the hard excess, ii) determine whether spectral variability can be explained by variable partial covering and iii) enable us to measure the imprint of the ionized outflow at Fe K with unprecedented accuracy. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TRACEY TURNER | USA | 5 | AO5 | THE COMPTON-THICK OUTFLOW IN THE TYPE I QSO PDS 456 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705041010/ | Quick Look | ![]() |
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715 | A2204_FIELD_1 | 248.3552 | 5.4547 | 247.739346 | 5.558766 | 245.63481 | 27.082232 | 21.05505633 | 33.03914402 | 261.0004 | 55440.0008217593 | 2010-09-01 00:01:11 | 55441.1467013889 | 2010-09-02 03:31:15 | 805056010 | 40.6674 | 40 | 40.6674 | 40.6674 | 0 | 40.6674 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.488 | 37.488 | 98.9941 | 1 | PROCESSED | 57553.2764699074 | 2016-06-14 06:38:07 | 55287 | 2010-04-01 00:00:00 | 55456.099849537 | 2010-09-17 02:23:47 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805056010/ | Quick Look | ![]() |
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716 | NGC3402 OFF-CENTER | 162.4923 | -13.1954 | 161.871445 | -12.930338 | 169.151232 | -19.021161 | 262.91388856 | 40.05493452 | 124.5885 | 55557.4779513889 | 2010-12-27 11:28:15 | 55558.1231134259 | 2010-12-28 02:57:17 | 805070010 | 27.8664 | 30 | 27.8744 | 27.8744 | 0 | 27.8664 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.0294 | 25.0294 | 55.74 | 1 | PROCESSED | 57554.5274421296 | 2016-06-15 12:39:31 | 55961 | 2012-02-04 00:00:00 | 55595.0278703704 | 2011-02-03 00:40:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051512 | Using the composite data from dwarf galaxies to rich clusters, we find that the baryon fraction is mainly set by the system's potential well depth. The small scatter of baryon fractions as a function of the gravitational potential well depth indicates a universal baryon loss mechanism for these systems. However, the relation is most poorly constrained in the poor galaxy group regime below 1keV, where few individual measurements exists. Since most galaxies reside in these groups, it is also important to test whether the missing baryons from the galaxies are actually in these poor groups. We propose deep, off-center observations of two such groups, doubling the sample, to better delineate and understand the transition of the baryon loss from clusters to galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | XINYU DAI | USA | 5 | AO5 | BARYON LOSS IN POOR GALAXY GROUPS: DISTINGUISHING PRE-HEATING AND FEEDBACK MODELS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805070010/ | Quick Look | ![]() |
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717 | ABELL 115 | 13.9939 | 26.3802 | 13.320825 | 26.109701 | 23.360956 | 18.75409 | 124.19588168 | -36.48041221 | 44.0022 | 55401.606087963 | 2010-07-24 14:32:46 | 55403.0529398148 | 2010-07-26 01:16:14 | 805077010 | 66.1556 | 65 | 66.1629 | 66.1556 | 0 | 66.1829 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61.8298 | 61.8298 | 124.968 | 2 | PROCESSED | 57552.6853472222 | 2016-06-13 16:26:54 | 55780 | 2011-08-07 00:00:00 | 55414.1298148148 | 2010-08-06 03:06:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051521 | We propose central and offset pointed observations of the strongly merging ``double'' cluster A115 to study the properties of the intracluster gas at the virial radius. Ultimately, the results can be compared with results from both relaxed and other merging systems to determine the effects of mergers on the extended gas halos of clusters (e.g., departures from hydrostatic equilibrium, and the level of non-thermal pressure support). Additionally, we will verify the presence of hard X-ray emission between the subclusters, marginally detected in Chandra observations, accurately measure its temperature, and determine its origin by confirming it as hot thermal (shock heated gas) or non-thermal (shock or turbulent accelerated particles) emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SCOTT RANDALL | USA | 5 | AO5 | THE EXTENDED ATMOSPHERES OF STRONGLY MERGING GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805077010/ | Quick Look | ![]() |
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718 | MKN 590 | 33.6446 | -0.7698 | 33.006332 | -1.002435 | 31.137585 | -13.457637 | 163.50990373 | -56.94179664 | 250.4206 | 55584.0937615741 | 2011-01-23 02:15:01 | 55585.6252083333 | 2011-01-24 15:00:18 | 705043010 | 61.5547 | 150 | 61.5867 | 61.5547 | 0 | 61.5707 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 55.1599 | 55.1599 | 132.2758 | 0 | PROCESSED | 57600.7325 | 2016-07-31 17:34:48 | 55965 | 2012-02-08 00:00:00 | 55599.1867824074 | 2011-02-07 04:28:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051433 | We propose a 150 ks Suzaku long-look to study the Compton reflection component, soft excess, ionized emission and possible ionized reflection of the Seyfert 1.2 AGN Mkn 590, which has an unobscured line of sight or "bare nucleus" and as of yet unquantified reflection. We aim to accurately constrain the geometry of the circumnuclear material and determine the ionization states of both the Compton-thin and Compton-thick material surrounding the black hole by studying the origin of the soft excess, determining the likelihood of ionized reflection and accurately measuring the intensity of neutral, H-like and He-like Fe emission lines. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | ELIZABETH RIVERS | USA | 5 | AO5 | QUANTIFYING THE COMPTON REFLECTION AND IONIZED EMISSION IN MKN 590 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705043010/ | Quick Look | ![]() |
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719 | NGC 2992 | 146.4352 | -14.2714 | 145.83373 | -14.040218 | 154.019094 | -26.058459 | 249.66741784 | 28.82528499 | 102.6298 | 53680.5956481482 | 2005-11-06 14:17:44 | 53681.5850925926 | 2005-11-07 14:02:32 | 700005010 | 37.5029 | 120 | 37.5029 | 38.7568 | 37.518 | 37.715 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 32.073 | 32.073 | 85.4859 | 1 | PROCESSED | 57527.9475231482 | 2016-05-19 22:44:26 | 54247 | 2007-05-27 00:00:00 | 54037.5593518518 | 2006-10-29 13:25:28 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001013 | NGC 2992 is a nearby Seyfert 1.9 galaxy showing long-term (20 yrs) large amplitude (factor of 20) variability. This object showed switching between Compton-thick and -thin. Recent RXTE monitoring has shown that this object is highly variable on shorter time scales (2 weeks). We propose three Suzaku observations to monitor the variability of absorption column, broad band continuum shape, and Fe line intensity to understand the cause of the remarkable variability. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YUICHI TERASHIMA | JAP | 0 | SWG | THE SPECTRAL VARIABILITY IN NGC 2992: FE-LINE, REFLECTION, AND COMPTON-THIN/THICK SWITCHING | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700005010/ | Quick Look | ![]() |
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720 | VELA SNR CB1 | 130.2067 | -44.4709 | 129.774891 | -44.291952 | 154.339696 | -59.260079 | 263.57895082 | -1.58638955 | 294.2634 | 55318.1574074074 | 2010-05-02 03:46:40 | 55318.5738425926 | 2010-05-02 13:46:20 | 505068010 | 23.6665 | 20 | 23.6665 | 23.678 | 0 | 23.6665 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.818 | 18.818 | 35.9759 | 1 | PROCESSED | 57551.3448842593 | 2016-06-12 08:16:38 | 55696 | 2011-05-15 00:00:00 | 55330.1358449074 | 2010-05-14 03:15:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051304 | The Vela SNR is known to have ejecta bullets outside the main shell. In addition to these bullets, signatures of ejecta inside the main shell have been uncovered in recent X-ray studies. Mostly, these are rich in light metals such as O, Ne, or Mg, whereas no Fe-rich ejecta had yet been detected. Based on archival XMM-Newton data, we found a possible Fe-rich ejecta bullet headed roughly in the opposite direction of Vela pulsar's motion. This would provide us with a window into the core-collapse SN explosion of the Vela SNR. Since its electron temperature is very low (~0.1 keV), the good Suzaku XIS response below 0.5 keV is suitable to study this object. We propose to observe it in four pointings. The requested exposure time is 20 ks each, resulting in a total exposure time of 80 ks. | GALACTIC DIFFUSE EMISSION | 5 | B | SATORU KATSUDA | USA | 5 | AO5 | IRON-RICH EJECTA BULLET IN THE VELA SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505068010/ | Quick Look | ![]() |
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721 | NGC 4945 | 196.3459 | -49.5284 | 195.615808 | -49.260687 | 217.044106 | -38.699389 | 305.256234 | 13.28040137 | 283.285 | 55381.636087963 | 2010-07-04 15:15:58 | 55382.6765856482 | 2010-07-05 16:14:17 | 705047010 | 39.0737 | 40 | 39.0817 | 39.0817 | 0 | 39.0737 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 34.0751 | 34.0751 | 89.8719 | 1 | PROCESSED | 57552.4706481482 | 2016-06-13 11:17:44 | 55770 | 2011-07-28 00:00:00 | 55404.2681134259 | 2010-07-27 06:26:05 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051442 | We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GUIDO RISALITI | USA | 5 | AO5 | HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705047010/ | Quick Look | ![]() |
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722 | NGC 4945 | 196.3265 | -49.5207 | 195.596537 | -49.252961 | 217.025208 | -38.698833 | 305.24375345 | 13.28878787 | 296.6587 | 55403.0670717593 | 2010-07-26 01:36:35 | 55404.1745717593 | 2010-07-27 04:11:23 | 705047030 | 40.3266 | 40 | 40.3426 | 40.3266 | 0 | 40.3426 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.6182 | 34.6182 | 95.6358 | 0 | PROCESSED | 57552.7156134259 | 2016-06-13 17:10:29 | 55780 | 2011-08-07 00:00:00 | 55414.0832407407 | 2010-08-06 01:59:52 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051442 | We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GUIDO RISALITI | USA | 5 | AO5 | HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705047030/ | Quick Look | ![]() |
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723 | A1795_NEAR_WEST | 206.9975 | 26.5902 | 206.419777 | 26.838853 | 193.705375 | 34.896895 | 33.70837645 | 77.38236805 | 300.5681 | 55009.4637962963 | 2009-06-27 11:07:52 | 55010.100162037 | 2009-06-28 02:24:14 | 804085010 | 24.2664 | 20 | 24.2664 | 24.5363 | 0 | 24.5203 | 5 | 2 | 0 | 2 | 1 | 0 | 0 | 9.9711 | 9.9711 | 22.7619 | 0 | PROCESSED | 57598.4788425926 | 2016-07-29 11:29:32 | 55386 | 2010-07-09 00:00:00 | 55020.3655555556 | 2009-07-08 08:46:24 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041528 | The outer regions of clusters beyond 0.5 r200 contain a large amount of the dark matter, baryons and metals in the system, yet they are poorly understood. We propose to conduct a new test of cluster and structure formation by probing the distribution of dark matter and the thermodynamic history of the ICM in the outskirts of the cluster Abell 1795. Our previous Suzaku observations of Abell 1795 indicate deviations from hydrostatic equilibrium; we sample two disjoint regions beyond r500, detecting cluster emission in one but not the other (a difference of 5-sigma). With the proposed observations spanning r500-r200, we will obtain a more sensitive measurement of the azimuthally averaged temperature and density at this radius and search for variations over a wider range of azimuth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 4 | AO4 | ABELL 1795 WITH SUZAKU: A NEW WINDOW ON CLUSTER FORMATION AND STRUCTURE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804085010/ | Quick Look | ![]() |
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724 | X1630-472 | 248.5239 | -47.3401 | 247.603368 | -47.236061 | 254.092996 | -25.076506 | 336.95804041 | 0.27755382 | 107.6616 | 53809.226412037 | 2006-03-15 05:26:02 | 53809.743912037 | 2006-03-15 17:51:14 | 400010050 | 23.1671 | 200 | 23.1751 | 23.1769 | 23.1768 | 23.1671 | 2 | 1 | 2 | 2 | 1 | 0 | 0 | 18.8605 | 18.8605 | 44.706 | 0 | PROCESSED | 57533.2189930556 | 2016-05-25 05:15:21 | 54247 | 2007-05-27 00:00:00 | 54041.9302662037 | 2006-11-02 22:19:35 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001058 | We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active. | GALACTIC POINT SOURCES | 4 | A | JEAN COTTAM | JAP | 0 | SWG-TOO | FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400010050/ | Quick Look | ![]() |
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725 | CH CYG | 291.1168 | 50.2494 | 290.78804 | 50.14985 | 313.638835 | 70.5089 | 81.85997028 | 15.59541424 | 38.1861 | 53883.3112962963 | 2006-05-28 07:28:16 | 53884.1502199074 | 2006-05-29 03:36:19 | 400016030 | 35.144 | 35 | 35.152 | 35.16 | 35.16 | 35.144 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 37.459 | 37.459 | 72.4479 | 1 | PROCESSED | 57534.4573726852 | 2016-05-26 10:58:37 | 54258 | 2007-06-07 00:00:00 | 54109.7043981482 | 2007-01-09 16:54:20 | 3.0.22.43 | 9 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001082 | CH Cygni is a symbiotic star in which a white dwarf is believed to be accreting the wind of the red giant. ASCA observation revealed a complex X-ray spectrum consisting of a heavily absorbed hard component and a relatively unabsorbed soft component. We propose to obtain the spectrum of CH Cyg above 10 keV for the first time using Suzaku HXD (PIN), while simultaneously obtaining high quality spectrum below 10 keV with the XIS. | GALACTIC POINT SOURCES | 4 | A | KOJI MUKAI | JAP | 0 | SWG | SUZAKU OBSERVATION OF THE SYMBIOTIC SYSTEM CH CYGNI | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400016030/ | Quick Look | ![]() |
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726 | FORNAX CLUSTER NORTH | 54.7043 | -35.2293 | 54.224181 | -35.391159 | 39.001198 | -52.608062 | 236.34100564 | -53.57224957 | 244.9996 | 53741.5137847222 | 2006-01-06 12:19:51 | 53742.3336111111 | 2006-01-07 08:00:24 | 800002020 | 37.1921 | 80 | 37.1921 | 37.2161 | 37.2081 | 37.2001 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39.2874 | 39.2874 | 70.8159 | 1 | PROCESSED | 57532.6432291667 | 2016-05-24 15:26:15 | 54247 | 2007-05-27 00:00:00 | 54039.8151041667 | 2006-10-31 19:33:45 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001018 | The center of the Fornax cluster was observed with Suzaku with a 80 ks exposure. We have detected excess hard-emission and derived O abundances of the ISM of NGC 1399 and NGC 1404, and the intracluster medium (ICM). Here, we propose to observe two offset pointings of the Fornax cluster for 160 ks (80 ks times 2) to study the distribution of the hard emission and the abundance distribution of O, Mg, Si, S and Fe. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | JAP | 0 | SWG | MAPPING HARD EXCESS EMISSION AND OXYGEN IN THE INTRACLUSTER MEDIUM OF THE FORNAX CLUSTER | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800002020/ | Quick Look | ![]() |
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727 | CYGNUS X-2 | 326.1653 | 38.3323 | 325.647427 | 38.10178 | 346.69525 | 47.972917 | 87.3318132 | -11.3049847 | 76.3142 | 53871.8636805556 | 2006-05-16 20:43:42 | 53872.7293171296 | 2006-05-17 17:30:13 | 401049010 | 39.3903 | 37 | 39.3903 | 39.4063 | 39.3903 | 39.3903 | 2 | 1 | 2 | 2 | 1 | 0 | 0 | 36.8804 | 36.8804 | 74.786 | 1 | PROCESSED | 57534.3858217593 | 2016-05-26 09:15:35 | 54401 | 2007-10-28 00:00:00 | 53927.6429166667 | 2006-07-11 15:25:48 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011113 | The potential well around low-magnetic field neutron stars is very similar to that around Schwarzschild black holes. Doppler shifts expected at the inner disk around such neutron stars should be very similar, and should produce relativistic FeK-alpha emission lines like those observed in some black hole systems. To date, however, relativistically broadened FeK-alpha emission lines have not been clearly detected in neutron star systems, in part because their lines are generally weaker than those found in black hole systems. We propose to observe the neutron star binaries 4U 1820-30, Cygnus X-2, and Serpens X-1 for 37 ksec each in Suzaku Cycle 1, to confirm possible evidence of relativistic broadening. Relativistic phenomena and accretion studies are central to NASA's ``SEU'' theme. | GALACTIC POINT SOURCES | 4 | B | JON MILLER | USA | 1 | AO1 | A SUZAKU STUDY OF BROAD IRON LINES IN NEUTRON STAR BINARIES | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401049010/ | Quick Look | ![]() |
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728 | MONOGEM RING W2 | 97.483 | 17.0349 | 96.757694 | 17.069404 | 97.197447 | -6.219287 | 195.35325463 | 3.08684005 | 270 | 56001.1430439815 | 2012-03-15 03:25:59 | 56002.5487384259 | 2012-03-16 13:10:11 | 506054010 | 62.5933 | 60 | 62.5933 | 62.5933 | 0 | 62.5933 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 59.9669 | 59.9669 | 121.4439 | 1 | PROCESSED | 57604.9251967593 | 2016-08-04 22:12:17 | 56385 | 2013-04-03 00:00:00 | 56019.3467592593 | 2012-04-02 08:19:20 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061316 | We propose to observe the oldest, nearby SNR, the Monogem Ring, with the Suzaku XIS to study the plasma conditions in two locations which are near the Galactic plane and where there is evidence of a significant interaction with cooler (10^4 - 10^5 K), denser material. We chose one pointing where the turbulent mixing of hot and cooler gas should be large, and an adjacent pointing where the mixing should be small. From our previous Suzaku observation at a region far from the plane, we derived an ionization timescale for the non-equilibrium plasma which is apparently inconsistent with the age of the SNR. Our proposed observations will allow a detailed comparison of the plasma conditions in these regions with very different histories, and initial and current conditions. | GALACTIC DIFFUSE EMISSION | 5 | C | PAUL PLUCINSKY | USA | 6 | AO6 | STUDYING THE PLASMA EVOLUTION IN THE MONOGEM RING | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506054010/ | Quick Look | ![]() |
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729 | SIGMA GEM | 115.843 | 28.9438 | 115.063071 | 29.063433 | 112.630716 | 7.510513 | 191.13214337 | 23.30670736 | 104.4403 | 54394.4090162037 | 2007-10-21 09:48:59 | 54397.9690162037 | 2007-10-24 23:15:23 | 402033010 | 142.8897 | 125 | 142.8897 | 142.9936 | 0 | 142.9856 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 124.4471 | 124.4471 | 307.5416 | 1 | PROCESSED | 57540.4020138889 | 2016-06-01 09:38:54 | 54776 | 2008-11-06 00:00:00 | 54407.830474537 | 2007-11-03 19:55:53 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021014 | Suzaku is a powerful instrument for studying the hot (>100 MK) coronal quiescent and flare emission on RS CVn binaries. We propose a 125 ksec (3-4 day elapsed time) observation of the RS CVn binary Sigma Gem. Our goals are i) to better characterize its hard (>10 keV) emission, ii) to understand the origin of coronal thermal and nonthermal plasma by studying the evolution of the coronal thermal structure, iii) to investigate the persistent and flaring nonthermal electron population using a combination of X-ray and radio cm+mm continuum data, and iv) compare long duration flares on Sigma Gem with the 6 hour flares of Sigma2 CrB. Such studies require the long duty cycle of Suzaku observations and its high sensitivity, particularly the greatly enhanced capability at 10-25 keV provided by HXD. | GALACTIC POINT SOURCES | 4 | C | ALEXANDER BROWN | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF THERMAL AND NONTHERMAL CORONAL STRUCTURE ON THE RS CVN BINARY SIGMA GEM (K0III +?) | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402033010/ | Quick Look | ![]() |
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730 | COMA NW3.5 | 194.5289 | 28.7386 | 193.925957 | 29.008414 | 180.709004 | 31.910374 | 80.83345269 | 87.81635354 | 116.0021 | 55917.9522685185 | 2011-12-22 22:51:16 | 55918.5091898148 | 2011-12-23 12:13:14 | 806040020 | 16.7407 | 15 | 16.7407 | 16.7631 | 0 | 16.7487 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.8051 | 15.8051 | 48.1159 | 0 | PROCESSED | 57604.2115509259 | 2016-08-04 05:04:38 | 55652 | 2011-04-01 00:00:00 | 55972.6802662037 | 2012-02-15 16:19:35 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806040020/ | Quick Look | ![]() |
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731 | AQL X-1 | 287.8181 | 0.5776 | 287.17982 | 0.493878 | 289.379 | 22.827401 | 35.7124509 | -4.14763067 | 265.5384 | 54392.3838310185 | 2007-10-19 09:12:43 | 54392.7918287037 | 2007-10-19 19:00:14 | 402053050 | 17.8899 | 15 | 17.8899 | 17.8899 | 0 | 17.8899 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.9278 | 16.9278 | 35.2319 | 1 | PROCESSED | 57540.3079513889 | 2016-06-01 07:23:27 | 54769 | 2008-10-30 00:00:00 | 54402.4178935185 | 2007-10-29 10:01:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021114 | We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. | GALACTIC POINT SOURCES | 4 | A | RONALD REMILLARD | USA | 2 | AO2-TOO | X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402053050/ | Quick Look | ![]() |
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732 | 4 DRA | 187.4841 | 69.1938 | 186.936079 | 69.469913 | 136.91907 | 61.165888 | 125.77229084 | 47.81569563 | 339.9969 | 55304.8913773148 | 2010-04-18 21:23:35 | 55305.8557291667 | 2010-04-19 20:32:15 | 405035010 | 42.2602 | 40 | 42.2682 | 42.2682 | 0 | 42.2602 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.792 | 43.792 | 83.2778 | 1 | PROCESSED | 57551.2555439815 | 2016-06-12 06:07:59 | 55693 | 2011-05-12 00:00:00 | 55327.2173958333 | 2010-05-11 05:13:03 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051212 | The symbiotic star, 4 Dra, has been poorly studied in X-rays. Based on the ROSAT data, we argue that it is a nearby, lower accretion rate analogue of the hard X-ray bright symibiotic stars that have been detected above 10 keV. We propose the first pointed observation of 4 Dra that covers the entire 0.4-10 keV band to test our interpretation: we expect it to be bright above 2 keV, with an optically thin thermal spectrum, likely with a strong and complex intrinsic absorber. If confirmed, 4 Dra may turn out to be a key object in the study of hard X-ray emitting symbiotic stars. | GALACTIC POINT SOURCES | 4 | B | KOJI MUKAI | USA | 5 | AO5 | THE FIRST LOOK AT THE SYMBIOTIC STAR 4 DRA ABOVE 2 KEV | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405035010/ | Quick Look | ![]() |
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733 | SMC X-1 | 19.2772 | -73.44 | 18.945719 | -73.703155 | 312.351206 | -66.472298 | 300.41207357 | -43.56242986 | 167.9636 | 55825.1720949074 | 2011-09-21 04:07:49 | 55825.6536805556 | 2011-09-21 15:41:18 | 706030070 | 18.1239 | 18 | 18.2772 | 18.2852 | 0 | 18.1239 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 18.3687 | 18.3687 | 41.5959 | 0 | PROCESSED | 57603.2202662037 | 2016-08-03 05:17:11 | 56218 | 2012-10-18 00:00:00 | 55851.4509027778 | 2011-10-17 10:49:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JOSEPH NEILSEN | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030070/ | Quick Look | ![]() |
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734 | SMC X-1 | 19.2766 | -73.4376 | 18.945062 | -73.700756 | 312.356716 | -66.471322 | 300.41185267 | -43.56483062 | 244.987 | 55907.8985069444 | 2011-12-12 21:33:51 | 55908.2709722222 | 2011-12-13 06:30:12 | 706030090 | 17.3055 | 18 | 17.4079 | 17.4079 | 0 | 17.3055 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.413 | 18.413 | 32.1719 | 0 | PROCESSED | 57604.1197685185 | 2016-08-04 02:52:28 | 56289 | 2012-12-28 00:00:00 | 55920.9743981482 | 2011-12-25 23:23:08 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JOSEPH NEILSEN | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030090/ | Quick Look | ![]() |
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735 | H1821+643 | 275.4676 | 64.3592 | 275.403785 | 64.332814 | 318.33431 | 86.843842 | 94.01912066 | 27.4276768 | 65.0012 | 56398.4117013889 | 2013-04-16 09:52:51 | 56402.5419328704 | 2013-04-20 13:00:23 | 708037010 | 246.5839 | 400 | 246.5839 | 246.5919 | 0 | 246.5999 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 251.0273 | 251.0273 | 356.8299 | 0 | PROCESSED | 57611.1526273148 | 2016-08-11 03:39:47 | 56383 | 2013-04-01 00:00:00 | 56425.7059606482 | 2013-05-13 16:56:35 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081436 | H1821+643 (z=0.297) is not "just another quasar". This luminous active galactic nucleus (AGN) is an extremely rare example of a powerful quasar at the center of a rich, cooling-core cluster of galaxies. As such, it may represent a key evolutionary stage in the complex interplay between AGN and the core regions of the intracluster medium (ICM). Our analysis of archival XMM-Newton data has found evidence for a relativistically broad iron line. Here, we build on this request deep (400ks) Suzaku spectroscopy of H1821+643 to (1) measure the spin of this supermassive black hole and (2) search for powerful highly ionized outflows. In addition to measuring spin in the most luminous and distant object yet, this will enable us to test key predictions of recent models for AGN feedback. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | CHRISTOPHER REYNOLDS | USA | 8 | AO8 | THE BLACK HOLE SPIN AND IONIZED OUTFLOWS IN THE COOLING-FLOW QUASAR H1821+643 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708037010/ | Quick Look | ![]() |
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736 | 1A1118-61 | 170.3073 | -61.878 | 169.75636 | -61.603723 | 210.888825 | -57.212599 | 292.515895 | -0.84430143 | 131.7127 | 54846.5144328704 | 2009-01-15 12:20:47 | 54847.9029976852 | 2009-01-16 21:40:19 | 403049010 | 49.6674 | 45 | 49.6674 | 49.6674 | 0 | 49.6674 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.8159 | 46.8159 | 119.9538 | 0 | PROCESSED | 57545.2346296296 | 2016-06-06 05:37:52 | 55328 | 2010-05-12 00:00:00 | 54858.6603125 | 2009-01-27 15:50:51 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031155 | We propose to perform Target of Opportunity Observations of one accreting neutron star in outburst during Suzaku AO3. The aim of the observations is to observe the source at a level of 40 and 200mCrab, to determine the properties of the cyclotron line in this system and to determine its broad band spectrum. | GALACTIC POINT SOURCES | 4 | A | KATJA POTTSCHMIDT | USA | 3 | AO3-TOO | SEARCHING FOR CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403049010/ | Quick Look | ![]() |
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737 | RXCJ0605 | 91.4642 | -35.1179 | 91.019375 | -35.111883 | 92.302761 | -58.547808 | 241.59260677 | -23.96271915 | 309.9856 | 55323.8555555556 | 2010-05-07 20:32:00 | 55324.6821412037 | 2010-05-08 16:22:17 | 805065040 | 43.6946 | 40 | 43.6946 | 43.6946 | 0 | 43.7106 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.3321 | 39.3321 | 71.4139 | 0 | PROCESSED | 57551.4409837963 | 2016-06-12 10:35:01 | 55287 | 2010-04-01 00:00:00 | 55341.5146990741 | 2010-05-25 12:21:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805065040/ | Quick Look | ![]() |
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738 | ETA CARINAE | 161.2769 | -59.635 | 160.789962 | -59.371642 | 202.089433 | -58.883736 | 287.57915278 | -0.58292483 | 99.9027 | 54810.21125 | 2008-12-10 05:04:12 | 54811.2084953704 | 2008-12-11 05:00:14 | 403036010 | 48.5016 | 30 | 48.5016 | 48.5016 | 0 | 48.5016 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.4259 | 42.4259 | 86.1518 | 2 | PROCESSED | 57544.6853125 | 2016-06-05 16:26:51 | 55198 | 2010-01-02 00:00:00 | 54828.3640972222 | 2008-12-28 08:44:18 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031124 | X-ray observations of Eta Carinae near the 2003 periastron passage confirmed that the X-ray emission primarily arises from collision of winds in a binary system, but raised fundamental questions about the cause of the 3 month-long X-ray minimum and an excess above ~10 keV (possibly up to 50 keV) in addition to the thermal emission with kT ~3-5 keV. These features would originate from plasma extremely embedded in the primary winds and acceleration of high energy particles at the wind colliding region. To resolve these features clearly, broad band Suzaku observations around the periastron passage are crucial. We propose four 30 ksec Suzaku observations of Eta Carinae during AO3, which will cover the next X-ray maximum (in late 2008) and minimum (in early 2009). | GALACTIC POINT SOURCES | 4 | A | KENJI HAMAGUCHI | USA | 3 | AO3 | X-RAY EMISSION FROM ETA CARINAE DURING THE X-RAY MAXIMUM AND MINIMUM | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403036010/ | Quick Look | ![]() |
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739 | ESO 511-G030 | 214.8452 | -26.6475 | 214.125784 | -26.417987 | 221.40413 | -12.023995 | 326.22882256 | 32.21510552 | 286.6511 | 56128.5082523148 | 2012-07-20 12:11:53 | 56128.7501388889 | 2012-07-20 18:00:12 | 707023010 | 5.7461 | 270 | 5.7461 | 5.7541 | 0 | 5.7621 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3.9886 | 3.9886 | 20.8879 | 0 | PROCESSED | 57606.6388194444 | 2016-08-06 15:19:54 | 56646 | 2013-12-20 00:00:00 | 56214.9581944445 | 2012-10-14 22:59:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071413 | The study of "bare" Seyfert 1 AGN is essential to measure the true properties of the inner regions of the accretion disk. The nearby Seyfert ESO 511-G30 is a prime candidate for fulfilling this role due to its broad Fe K component and lack of any intrinsic warm absorption. It is also one of the X-ray brightest bare Seyferts featured in the Swift 58 month BAT catalogue as yet unobserved with Suzaku. We propose a 270 ks Suzaku observation of ESO 511-G30 to unambiguously constrain the properties of the accretion disk and subsequently the black hole spin. In addition, the HXD data will allow us to measure the Compton reflection hump, while the excellent soft X-ray spectral resolution of XIS will allow the origin of the soft excess to be determined. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JAMES REEVES | USA | 7 | AO7 | MEASURING THE ACCRETION DISK AND BLACK HOLE PROPERTIES OF ESO 511-G30 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707023010/ | Quick Look | ![]() |
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740 | PG 1404+226 | 211.5943 | 22.4043 | 211.013582 | 22.642135 | 200.388612 | 32.841534 | 21.50519934 | 72.36517417 | 124.2434 | 56284.2179398148 | 2012-12-23 05:13:50 | 56286.1272453704 | 2012-12-25 03:03:14 | 707026010 | 80.2969 | 80 | 80.3129 | 80.2969 | 0 | 80.3049 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.5848 | 70.5848 | 164.9457 | 1 | PROCESSED | 57608.3815972222 | 2016-08-08 09:09:30 | 56687 | 2014-01-30 00:00:00 | 56320.7751157407 | 2013-01-28 18:36:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071419 | We propose a 80 ks observation of a NLS galaxy, PG1404+226, with Suzaku/XIS to investigate the physical conditions of extreme absorbers known as the ultra-fast-outflows (UFOs; v/c~0.1-0.2) of variable resonant absorption features from many ions (e.g. Ne IX, Ne X, Mg XII and S XVI) in the soft X-ray band (~0.5-3.5 keV), and we propose the first Suzaku observation of this object to (i) independently confirm/refute the previous claims of the presence of these UFOs including a potential detection of Fe K-shell absorbers, (ii) examine their variabilities and compare the outflow properties at low and high XIS-flux states, (iii) compare its outflow rate and kinetic power with those in other AGN UFOs, and (iv) utilize a high-quality Suzaku data to improve our MHD disk-wind model. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | KEIGO FUKUMURA | USA | 7 | AO7 | PROBING THE ULTRA-FAST-OUTFLOWS OF PG1404+226 WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707026010/ | Quick Look | ![]() |
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741 | SBS 1301+540 | 196.0153 | 53.8063 | 195.478385 | 54.074176 | 163.182611 | 53.62856 | 118.79430047 | 63.22042238 | 133.9261 | 56991.9979976852 | 2014-11-30 23:57:07 | 56994.5141435185 | 2014-12-03 12:20:22 | 709018010 | 94.3176 | 100 | 94.3176 | 95.1576 | 0 | 95.1736 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 105.4641 | 105.4641 | 217.3498 | 5 | PROCESSED | 57617.4634143518 | 2016-08-17 11:07:19 | 57451 | 2016-03-04 00:00:00 | 57084.1361574074 | 2015-03-03 03:16:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091411 | We propose to carry out Suzaku observations, 100 ks each, of two Seyfert I nuclei, IGR J16558-5203 and SBS 1301+540, hard X-ray selected by Swift. Our goal is to distinguish between various competing models proposed for the X-ray spectra of Seyfert I nuclei. Specifically we will explore the effects of strong gravity, by testing the ionized relativistic reflection (hereafter IRR) and by measuring the spin of the black hole. We will take advantage of Suzaku s excellent capability in the broad bands from the soft through medium to hard X-ray bands. With our proposed studies we will gain deeper understanding of accretion-powered AGN in general. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | SACHIKO TSURUTA | USA | 9 | AO9 | SPECTRAL STUDIES OF SOME HARD X RAY SELECTED SEYFERT NUCLEI | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709018010/ | Quick Look | ![]() |
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742 | IRAS 05078+1626 | 77.6911 | 16.4922 | 76.970259 | 16.431142 | 78.130409 | -6.443089 | 186.12002752 | -13.50176431 | 259.3263 | 56351.6301736111 | 2013-02-28 15:07:27 | 56352.6112847222 | 2013-03-01 14:40:15 | 707029010 | 46.0167 | 45 | 46.0167 | 46.0167 | 0 | 46.0167 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.1101 | 44.1101 | 84.7558 | 1 | PROCESSED | 57610.7197916667 | 2016-08-10 17:16:30 | 56749 | 2014-04-02 00:00:00 | 56372.578287037 | 2013-03-21 13:52:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071424 | A hard X-ray-selected (BAT) AGN sample shows a remarkable 70% of the local population of type 1 AGN to have extreme hard excesses above 20 keV, likely caused by Compton-thick gas in the line-of-sight, covering at least 50% of the source. We request six snapshot observations to complete a Suzaku survey of a BAT-flux-limited sample and make a complete and unbiased measurement of the incidence. Analysis of the new sources will be performed in conjunction with existing exposures, providing exciting new insight into the previously unknown structures in hard X-ray selected AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TRACEY TURNER | USA | 7 | AO7 | INVESTIGATING COMPTON-THICK ABSORBERS IN TYPE 1 AGN: OVERHAULING THE AGN PARADIGM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707029010/ | Quick Look | ![]() |
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743 | COMA E3 | 195.8278 | 27.896 | 195.226801 | 28.164193 | 182.356899 | 31.675143 | 49.87218267 | 87.25778961 | 279.9974 | 55729.4896064815 | 2011-06-17 11:45:02 | 55729.6863078704 | 2011-06-17 16:28:17 | 806032010 | 7.9801 | 10 | 7.9801 | 7.9801 | 0 | 7.9801 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 5.764 | 5.764 | 16.9839 | 0 | PROCESSED | 57602.3229976852 | 2016-08-02 07:45:07 | 55652 | 2011-04-01 00:00:00 | 55770.1022453704 | 2011-07-28 02:27:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806032010/ | Quick Look | ![]() |
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744 | MCG-5-23-16 | 146.9228 | -30.9448 | 146.373555 | -30.712217 | 162.622685 | -41.142645 | 262.74496877 | 17.23993252 | 295.4404 | 56448.2467476852 | 2013-06-05 05:55:19 | 56450.9584606482 | 2013-06-07 23:00:11 | 708021020 | 138.8466 | 300 | 138.8466 | 138.8466 | 0 | 138.8466 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 140.4914 | 140.4914 | 234.282 | 2 | PROCESSED | 57611.5159490741 | 2016-08-11 12:22:58 | 56383 | 2013-04-01 00:00:00 | 56461.7776736111 | 2013-06-18 18:39:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081416 | Significant recent developments in probing environments around AGN black holes has been achieved using X-ray reverberation. They were initially detected in the soft excess of several NLS1s, then recently, the first Fe K reverberation was also seen. In addition to measuring x-rays reverberating a few r_g from the event horizon, short/long delays from different radii have been separated for the first time in NGC4151. Here we propose to observe MCG-5-23-1 for 300 ks in order to study its iron K reverberation. It is optimally one of the brightest and most variable AGN in X-rays. Archival data already show very exciting signatures of Fe K reverberation. With new observations we aim to constrain the emitting region size and study the emission originating at different distances from of the hole. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ABDERAHMEN ZOGHBI | USA | 8 | AO8 | IRON K REVERBERATION IN MCG 5-23-16 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708021020/ | Quick Look | ![]() |
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745 | MKN 915 | 339.1982 | -12.5468 | 338.534901 | -12.806507 | 336.087416 | -3.520949 | 51.05925373 | -55.2984956 | 243.0396 | 56622.9636458333 | 2013-11-26 23:07:39 | 56624.1320601852 | 2013-11-28 03:10:10 | 708029010 | 41.22 | 40 | 41.22 | 41.22 | 0 | 41.22 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.3893 | 37.3893 | 100.9399 | 0 | PROCESSED | 57613.4605787037 | 2016-08-13 11:03:14 | 56383 | 2013-04-01 00:00:00 | 56637.6375347222 | 2013-12-11 15:18:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081419 | The BAT AGN sample constitutes an unprecedented all-sky hard X-ray survey of the local AGN population. However, to properly model the X-ray absorption & reflection, coverage below 10 keV is needed with CCD spectral resolution and adequate signal-to-noise. We propose to observe 11 AGN with Suzaku, which will increase the completeness of a flux-limited sample with such coverage from 85 to 158 sources. The 11 AGN only have severely underexposed Swift XRT coverage below 10 keV whereas the remaining sources have either Suzaku or XMM coverage. The Suzaku data have the additional advantage of sensitivity above 10 keV that helps to mitigate the long time-baseline of the BAT spectra. The new observations will create a significantly enhanced legacy data set that will provide value for years to come. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TAHIR YAQOOB | USA | 8 | AO8 | ROBUST CHARACTERIZATION OF ABSORPTION AND REFLECTION IN A LOCAL FLUX-LIMITED AGN POPULATION FROM THE SWIFT BAT SURVEY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708029010/ | Quick Look | ![]() |
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746 | OFF-FIELD5 | 318.3256 | -10.4856 | 317.650019 | -10.692475 | 317.524522 | 5.342962 | 39.92155172 | -36.21028826 | 81.4906 | 56787.0661226852 | 2014-05-10 01:35:13 | 56789.4168171296 | 2014-05-12 10:00:13 | 509046010 | 80.908 | 80 | 80.908 | 80.908 | 0 | 80.908 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71.3404 | 71.3404 | 203.0697 | 2 | PROCESSED | 57615.126724537 | 2016-08-15 03:02:29 | 56748 | 2014-04-01 00:00:00 | 56806.674212963 | 2014-05-29 16:10:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091321 | Our special vantage point in our Galaxy allows us to study the Galactic warm-hot halo along several sightlines and determine its physical properties. The combination of absorption and emission measurements provides a powerful tool in this regard. Instead of average emission and absorption measures used in previous studies, one immediate step forward would be to use emission measures close to absorption sightlines. With proposed observations we will determine emission measures close to five sightlines in which we have the most accurate absorption measurements with Chandra. This will break the degeneracy between density and path-length and robustly measure the extent and mass of the warm-hot halo, placing strongest constraints yet on the fraction of missing baryons in the warm-hot plasma. | GALACTIC DIFFUSE EMISSION | 5 | A | ANJALI GUPTA | USA | 9 | AO9 | CIRCUM-GALACTIC MEDIUM OF THE MILKY WAY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509046010/ | Quick Look | ![]() |
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747 | MKN 1148 | 12.9805 | 17.4231 | 12.320857 | 17.151473 | 18.75445 | 10.92233 | 123.09650608 | -45.44849404 | 266.997 | 56656.2855555556 | 2013-12-30 06:51:12 | 56657.0627662037 | 2013-12-31 01:30:23 | 708033010 | 28.3189 | 30 | 28.3189 | 28.3269 | 0 | 28.3269 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23.1005 | 23.1005 | 67.1379 | 2 | PROCESSED | 57613.7155324074 | 2016-08-13 17:10:22 | 56383 | 2013-04-01 00:00:00 | 56702.7526273148 | 2014-02-14 18:03:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081419 | The BAT AGN sample constitutes an unprecedented all-sky hard X-ray survey of the local AGN population. However, to properly model the X-ray absorption & reflection, coverage below 10 keV is needed with CCD spectral resolution and adequate signal-to-noise. We propose to observe 11 AGN with Suzaku, which will increase the completeness of a flux-limited sample with such coverage from 85 to 158 sources. The 11 AGN only have severely underexposed Swift XRT coverage below 10 keV whereas the remaining sources have either Suzaku or XMM coverage. The Suzaku data have the additional advantage of sensitivity above 10 keV that helps to mitigate the long time-baseline of the BAT spectra. The new observations will create a significantly enhanced legacy data set that will provide value for years to come. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TAHIR YAQOOB | USA | 8 | AO8 | ROBUST CHARACTERIZATION OF ABSORPTION AND REFLECTION IN A LOCAL FLUX-LIMITED AGN POPULATION FROM THE SWIFT BAT SURVEY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708033010/ | Quick Look | ![]() |
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748 | PMN J1603-4904 | 240.9652 | -49.0681 | 240.045662 | -48.930987 | 248.937832 | -27.726173 | 332.15292306 | 2.57171396 | 292.7209 | 56547.6621643518 | 2013-09-12 15:53:31 | 56548.4842013889 | 2013-09-13 11:37:15 | 708035010 | 50.9129 | 50 | 50.9252 | 50.9129 | 0 | 50.9172 | 3 | 2 | 0 | 3 | 1 | 0 | 0 | 49.2803 | 49.2803 | 70.99 | 0 | PROCESSED | 57612.626875 | 2016-08-12 15:02:42 | 56956 | 2014-10-26 00:00:00 | 56588.7813657407 | 2013-10-23 18:45:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081432 | We propose a 50ksec Suzaku observation of the gamma-ray emitting compact symmetric radio source PMN J1603-4904 as a crucial part of the first simultaneous radio to gamma-ray campaign on this object. Constraining the X-ray spectrum of the compact radio source is needed to properly model the broadband spectral energy distribution (SED), which is essential for understanding the physical nature of this unusual object. The Swift detection allows no spectral modeling of its very faint X-ray counterpart, hence, precise spectral investigations with Suzaku are strongly required. PMN J1603-4904 is one of the few young radio galaxy candidates associated with a bright Fermi gamma-ray source, thus it plays a key role in investigating the underlying emission mechanism of newly born active galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ROOPESH OJHA | USA | 8 | AO8 | CONSTRAINING THE NATURE OF PMN J1603-4904: IS IT A GAMMA-LOUD YOUNG RADIO GALAXY? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708035010/ | Quick Look | ![]() |
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749 | WR140 | 305.1374 | 43.8475 | 304.71526 | 43.688126 | 327.381123 | 60.483368 | 80.93293792 | 4.16074264 | 212.5272 | 56283.3528356482 | 2012-12-22 08:28:05 | 56284.2085300926 | 2012-12-23 05:00:17 | 407041010 | 54.7802 | 50 | 54.7962 | 54.7802 | 0 | 54.8042 | 3 | 2 | 0 | 3 | 1 | 0 | 0 | 52.3811 | 52.3811 | 73.92 | 0 | PROCESSED | 57608.3396990741 | 2016-08-08 08:09:10 | 56710 | 2014-02-22 00:00:00 | 56344.6961689815 | 2013-02-21 16:42:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071203 | In the campaign observations of the prototypical colliding wind binary system WR 140 at its last periastron passage in 2009, Suzaku discovered an extremely hard and variable X-ray component. The current best explanation of its origin is inverse-Compton cooling of particles accelerated in the wind-wind collision shock, and if so this would be the first detection of non-thermal X-ray emission from any Wolf-Rayet system. However, other mechanisms cannot be excluded because the observed intensity was stronger than expected from the observed radio luminosity. We propose to re-observe WR 140 near apastron in 2012 with Suzaku to identify the emission mechanism which produces the hard component. | GALACTIC POINT SOURCES | 4 | C | KENJI HAMAGUCHI | USA | 7 | AO7 | MEASURING EXTREMELY HARD X-RAY EMISSION FROM WR140 AT APASTRON | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407041010/ | Quick Look | ![]() |
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750 | HOLMBERG IX X-1 | 149.4599 | 69.05 | 148.442008 | 69.288451 | 119.782652 | 51.677007 | 141.95121201 | 41.07533054 | 294.5528 | 56780.1586111111 | 2014-05-03 03:48:24 | 56780.8752546296 | 2014-05-03 21:00:22 | 709015010 | 31.886 | 30 | 31.886 | 31.886 | 0 | 31.886 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.8618 | 30.8618 | 61.9159 | 0 | PROCESSED | 57615.0271990741 | 2016-08-15 00:39:10 | 57218 | 2015-07-15 00:00:00 | 56852.5963194444 | 2014-07-14 14:18:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091251 | Broadband X-ray spectroscopy of ultraluminous X-ray sources (ULXs) with NuSTAR and Suzaku has begun to provide important information regarding the nature of these enigmatic sources. Recent NuSTAR observations of the extreme ULX Holmberg IX X-1 revealed unusual spectral variability, and different competing evolutionary scenarios can explain the available data. Resolving this degeneracy is critical to determining the nature of the accretion onto this source, and requires multi-epoch broadband spectroscopy probing a more diverse range of fluxes. We propose to undertake 4x30 ks coordinated Suzaku+NuSTAR observations of Holmberg IX X-1 to provide the additional spectra needed to robustly determine the nature of the observed evolution, providing a vital step in our understanding of extreme ULXs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | DOMINIC WALTON | USA | 9 | AO9 | MULTI-EPOCH BROADBAND X-RAY SPECTROSCOPY OF HOLMBERG IX X-1 WITH SUZAKU AND NUSTAR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709015010/ | Quick Look | ![]() |
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751 | Q0142-100 | 26.3171 | -9.7556 | 25.697719 | -10.005838 | 20.677718 | -19.226515 | 161.63610788 | -68.48152364 | 68.9469 | 56854.9601041667 | 2014-07-16 23:02:33 | 56856.4794328704 | 2014-07-18 11:30:23 | 709019010 | 60.9751 | 55 | 60.9831 | 60.9831 | 0 | 60.9751 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.53 | 10.53 | 22.736 | 0 | PROCESSED | 57615.4077083333 | 2016-08-15 09:47:06 | 57261 | 2015-08-27 00:00:00 | 56895.341412037 | 2014-08-26 08:11:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091431 | The origin of AGN iron K alpha emission has been debated for two decades. We propose to constrain iron line emission sizes using quasar X-ray microlensing. Our Chandra Cycle 11 observations have shown that the iron line equivalent widths (EWs) in six lensed systems are significantly higher than those measured in local AGNs. This implies that the iron line emission is microlensed more strongly than the X-ray continuum and originates from very compact regions. We propose to confirm the high iron line EWs in lensed quasars by monitoring two more lenses, Q0142-100 and HE0512+3329 using Suzaku, with a total exposure time 115 kilo-seconds. This will provide independent constraints for settling the debate on the origin of the iron line emission. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | BIN CHEN | USA | 9 | AO9 | CONSTRAINING QUASAR IRON LINE EMISSION USING MICROLENSING | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709019010/ | Quick Look | ![]() |
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752 | HE0512-3329 | 78.54 | -33.4465 | 78.079714 | -33.502938 | 72.667363 | -56.201883 | 236.6358247 | -33.85842065 | 104.8837 | 56933.2970833333 | 2014-10-03 07:07:48 | 56934.0071180556 | 2014-10-04 00:10:15 | 709020020 | 27.5086 | 60 | 27.5086 | 27.5166 | 0 | 27.5166 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6104976852 | 2016-08-16 14:39:07 | 57345 | 2015-11-19 00:00:00 | 56979.4110300926 | 2014-11-18 09:51:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091431 | The origin of AGN iron K alpha emission has been debated for two decades. We propose to constrain iron line emission sizes using quasar X-ray microlensing. Our Chandra Cycle 11 observations have shown that the iron line equivalent widths (EWs) in six lensed systems are significantly higher than those measured in local AGNs. This implies that the iron line emission is microlensed more strongly than the X-ray continuum and originates from very compact regions. We propose to confirm the high iron line EWs in lensed quasars by monitoring two more lenses, Q0142-100 and HE0512+3329 using Suzaku, with a total exposure time 115 kilo-seconds. This will provide independent constraints for settling the debate on the origin of the iron line emission. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | BIN CHEN | USA | 9 | AO9 | CONSTRAINING QUASAR IRON LINE EMISSION USING MICROLENSING | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709020020/ | Quick Look | ![]() |
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753 | SCT X-1 | 278.8604 | -7.62 | 278.182699 | -7.661262 | 279.107683 | 15.540839 | 24.33197703 | 0.06047842 | 260.9601 | 56940.5300810185 | 2014-10-10 12:43:19 | 56940.854375 | 2014-10-10 20:30:18 | 409033010 | 15.1616 | 50 | 15.1789 | 15.1776 | 0 | 15.1616 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6415625 | 2016-08-16 15:23:51 | 57373 | 2015-12-17 00:00:00 | 56979.4099421296 | 2014-11-18 09:50:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091222 | We propose to observe the accreting 112s pulsar Scutum X-1 with Suzaku for 50ks. The optical companion is a late type giant or supergiant, making this a rare, persistent, non-OB-type wind accreting, Symbiotic X-ray Binary (SyXB). After initial flaring in the 1970s, the source generally exhibited low flux levels and has only rarely been observed. We will constrain the broadband spectrum, check for signs of wind accretion (variable absorption, log-normal count rate distribution), search for an iron fluorescence line, update the pulse period evolution, and compare to other Suzaku observations of SyXBs, especially to a quiescent observation of the prototype SyXB 4U 1954+31. | GALACTIC POINT SOURCES | 4 | A | KATJA POTTSCHMIDT | USA | 9 | AO9 | THE SYMBIOTIC X-RAY BINARY SCUTUM X-1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409033010/ | Quick Look | ![]() |
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754 | NGC5548 | 214.4931 | 25.1284 | 213.926191 | 25.358593 | 201.994041 | 36.406695 | 31.93341942 | 70.49864062 | 309.3821 | 54269.9362847222 | 2007-06-18 22:28:15 | 54270.6389814815 | 2007-06-19 15:20:08 | 702042010 | 31.1188 | 30 | 31.1188 | 31.1188 | 0 | 31.1188 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.1759 | 27.1759 | 60.7059 | 0 | PROCESSED | 57538.9803703704 | 2016-05-30 23:31:44 | 54695 | 2008-08-17 00:00:00 | 54319.4659953704 | 2007-08-07 11:11:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021307 | We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARTIN ELVIS | USA | 2 | AO2 | NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702042010/ | Quick Look | ![]() |
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755 | ABELL 3364 | 87.0888 | -31.8215 | 86.620794 | -31.836795 | 85.667368 | -55.219752 | 236.92588426 | -26.48475311 | 295.0036 | 55670.3589699074 | 2011-04-19 08:36:55 | 55670.9259027778 | 2011-04-19 22:13:18 | 806067020 | 29.9913 | 29.5 | 29.9993 | 29.9913 | 0 | 30.0073 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 26.718 | 26.718 | 48.9759 | 0 | PROCESSED | 57601.5361689815 | 2016-08-01 12:52:05 | 56067 | 2012-05-20 00:00:00 | 55691.2162037037 | 2011-05-10 05:11:20 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061524 | Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but none was studied for non-cool core clusters. We propose a 118 ks Suzaku observation of a regular non-cool core cluster (for the first time) Abell 3364. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KA-WAH WONG | USA | 6 | AO6 | THE FIRST REGULAR NON-COOL CORE GALAXY CLUSTER TO BE STUDIED NEAR THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806067020/ | Quick Look | ![]() |
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756 | 73P/SW3 | 17.8996 | -9.1693 | 17.272719 | -9.434717 | 12.886588 | -15.48163 | 138.7272506 | -71.42013328 | 59.3998 | 53893.8025 | 2006-06-07 19:15:36 | 53893.8689699074 | 2006-06-07 20:51:19 | 500014030 | 3.2361 | 35 | 3.2361 | 3.2361 | 3.2361 | 3.2361 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.4331 | 2.4331 | 5.7359 | 0 | PROCESSED | 57534.5821875 | 2016-05-26 13:58:21 | 54267 | 2007-06-16 00:00:00 | 54052.5088310185 | 2006-11-13 12:12:43 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014030/ | Quick Look | ![]() |
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757 | 73P/SW3 | 18.2084 | -9.2837 | 17.581929 | -9.54866 | 13.13101 | -15.70655 | 139.744498 | -71.45365551 | 59.3985 | 53894.2087384259 | 2006-06-08 05:00:35 | 53894.2689467593 | 2006-06-08 06:27:17 | 500014090 | 1.5089 | 35 | 1.5089 | 1.5089 | 1.5089 | 1.5089 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1.6552 | 1.6552 | 5.202 | 0 | PROCESSED | 57534.5937037037 | 2016-05-26 14:14:56 | 54267 | 2007-06-16 00:00:00 | 54052.5382986111 | 2006-11-13 12:55:09 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014090/ | Quick Look | ![]() |
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758 | CYGNUS LOOP NE1 | 314.1885 | 31.738 | 313.671289 | 31.544868 | 329.414773 | 46.489683 | 75.60815027 | -8.84073861 | 223.0005 | 53697.7354282407 | 2005-11-23 17:39:01 | 53698.2051388889 | 2005-11-24 04:55:24 | 500020010 | 20.3437 | 20 | 20.3517 | 20.3517 | 20.3517 | 20.3437 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 17.992 | 17.992 | 40.5759 | 0 | PROCESSED | 57528.0684837963 | 2016-05-20 01:38:37 | 54247 | 2007-05-27 00:00:00 | 54037.9167476852 | 2006-10-29 22:00:07 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001093 | We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 0 | SWG | CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500020010/ | Quick Look | ![]() |
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759 | CYGNUS LOOP NE2 | 313.9681 | 31.9542 | 313.452396 | 31.761838 | 329.292075 | 46.763002 | 75.65570239 | -8.55863001 | 223.0005 | 53698.2056134259 | 2005-11-24 04:56:05 | 53698.6766666667 | 2005-11-24 16:14:24 | 500021010 | 21.4135 | 20 | 21.4455 | 21.4375 | 21.4295 | 21.4135 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 21.6541 | 21.6541 | 40.6939 | 0 | PROCESSED | 57528.0693518518 | 2016-05-20 01:39:52 | 54247 | 2007-05-27 00:00:00 | 54038.4014351852 | 2006-10-30 09:38:04 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001093 | We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 0 | SWG | CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500021010/ | Quick Look | ![]() |
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760 | ABELL 3364 | 86.7248 | -31.9341 | 86.257494 | -31.951159 | 85.117761 | -55.320671 | 236.9466602 | -26.81319905 | 295.0042 | 55670.9264699074 | 2011-04-19 22:14:07 | 55671.5940162037 | 2011-04-20 14:15:23 | 806067030 | 30.7802 | 29.5 | 30.7802 | 30.7802 | 0 | 30.7802 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.2762 | 30.2762 | 57.6639 | 1 | PROCESSED | 57601.5516782407 | 2016-08-01 13:14:25 | 56059 | 2012-05-12 00:00:00 | 55692.1831018518 | 2011-05-11 04:23:40 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061524 | Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but none was studied for non-cool core clusters. We propose a 118 ks Suzaku observation of a regular non-cool core cluster (for the first time) Abell 3364. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KA-WAH WONG | USA | 6 | AO6 | THE FIRST REGULAR NON-COOL CORE GALAXY CLUSTER TO BE STUDIED NEAR THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806067030/ | Quick Look | ![]() |
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761 | LMC X-3 OFF FIELD 1 | 85.5246 | -64.555 | 85.467763 | -64.576889 | 45.273362 | -87.277293 | 274.10794908 | -31.71433471 | 145.4977 | 54039.3159722222 | 2006-10-31 07:35:00 | 54039.7509722222 | 2006-10-31 18:01:24 | 501097020 | 15.3749 | 10 | 15.3749 | 15.3829 | 15.3829 | 15.3829 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 14.9263 | 14.9263 | 37.58 | 0 | PROCESSED | 57536.0002314815 | 2016-05-28 00:00:20 | 54526 | 2008-03-01 00:00:00 | 54088.8072222222 | 2006-12-19 19:22:24 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011256 | The Galactic corona is believed to play an essential role in the ``eco-system'' of the Galaxy. But the extent as well as the physical properties of the corona are yet to be determined. We request deep Suzaku XIS observations of the soft X-ray background in the vicinity of LMC X-3, toward which we have already conducted far-UV and X-ray absorption line spectroscopy. We have developed a software tool for a joint model fit to the absorption and emission data, allowing for statistical tests of various models and constraints on such parameters as hot gas temperature, density, and scale. The results will provide a unique calibration of our understanding of the corona. | GALACTIC DIFFUSE EMISSION | 5 | A | Q. DANIEL WANG | USA | 1 | AO1 | A JOINT EMISSION AND ABSORPTION STUDY OF THE GALACTIC CORONA | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501097020/ | Quick Look | ![]() |
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762 | COMET_8P_TUTTLE-P2_18 | 40.6547 | -37.9803 | 40.155519 | -38.192358 | 20.729743 | -50.258243 | 244.9394556 | -64.31314542 | 254.1595 | 54492.2963773148 | 2008-01-27 07:06:47 | 54492.4293287037 | 2008-01-27 10:18:14 | 502063180 | 6.1505 | 6 | 6.1505 | 6.1505 | 0 | 6.1505 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6.6133 | 6.6133 | 11.4799 | 0 | PROCESSED | 57541.4227083333 | 2016-06-02 10:08:42 | 54912 | 2009-03-22 00:00:00 | 54546.2369675926 | 2008-03-21 05:41:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063180/ | Quick Look | ![]() |
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763 | ARC2 | 39.9365 | -39.101 | 39.440937 | -39.3153 | 19.107499 | -50.973986 | 247.81076012 | -64.49485898 | 35.5401 | 54256.3120486111 | 2007-06-05 07:29:21 | 54258.149525463 | 2007-06-07 03:35:19 | 502071010 | 105.7271 | 100 | 105.7351 | 105.7351 | 0 | 105.7271 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82.9236 | 82.9236 | 158.7418 | 1 | PROCESSED | 57538.8944097222 | 2016-05-30 21:27:57 | 54702 | 2008-08-24 00:00:00 | 54264.533275463 | 2007-06-13 12:47:55 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021222 | Outside of the largest loops in the northern sky, few X-ray bright regions in the Galactic halo are understood. Here, we propose to study of a medium sized (~10 degree) bright feature in the southern sky. The feature is arc-shaped, suspiciously like the edge of a hot bubble. We propose to make three Suzaku observations along a radial line through the arc. With them, we will be able to determine the thermal properties of the region and whether or not the plasma temperature decreases with radius from the projected center, as expected for middle aged supernova remnants. | GALACTIC DIFFUSE EMISSION | 5 | B | ROBIN SHELTON | USA | 2 | AO2 | A CLOSER LOOK AT HOT HALO GAS: AN EXAMINATION OF AN X-RAY BRIGHT ARC | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502071010/ | Quick Look | ![]() |
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764 | VELA FRAGMENT E | 119.9016 | -44.3755 | 119.497107 | -44.237549 | 140.837519 | -62.635644 | 259.34445053 | -7.61175769 | 281.1138 | 54582.309224537 | 2008-04-26 07:25:17 | 54583.7849421296 | 2008-04-27 18:50:19 | 503096010 | 79.2004 | 70 | 79.2189 | 79.2004 | 0 | 79.2324 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 84.2529 | 84.2529 | 127.4899 | 1 | PROCESSED | 57542.4144212963 | 2016-06-03 09:56:46 | 54960 | 2009-05-09 00:00:00 | 54594.2098842593 | 2008-05-08 05:02:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031212 | Ejecta fragments projecting from the nearby Vela supernova remnant provide a unique opportunity to examine supernova ejecta as they shock and finally merge into the interstellar medium (ISM). Fragments "A" and "D", observed with Chandra and XMM, and Fragment "B", observed with Suzaku, show strongly enhanced (but very different) abundances. These fragments are indeed ejecta, but originating in different layers of the precursor. We propose to observe two of the remaining ejecta fragments. In combination with the existing observations of Fragments A, B, and D, these data will provide a much more complete picture of the variation in ejecta fragment abundances and their interactions with the remnant shell and the surrounding ISM. | GALACTIC DIFFUSE EMISSION | 5 | B | TERRANCE GAETZ | USA | 3 | AO3 | SEARCHING FOR EJECTA IN THE VELA SUPERNOVA REMNANT FRAGMENTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503096010/ | Quick Look | ![]() |
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765 | NGC 6888 | 303.111 | 38.3992 | 302.65502 | 38.248061 | 320.307714 | 56.205556 | 75.54872423 | 2.39562358 | 36.3096 | 54999.0718981482 | 2009-06-17 01:43:32 | 55001.1793287037 | 2009-06-19 04:18:14 | 504084010 | 88.8468 | 75 | 88.8548 | 88.8468 | 0 | 88.8548 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82.4052 | 82.4052 | 182.0679 | 2 | PROCESSED | 57547.6754976852 | 2016-06-08 16:12:43 | 55378 | 2010-07-01 00:00:00 | 55012.4221180556 | 2009-06-30 10:07:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041321 | Fast winds from massive stars create large cavities in the surrounding interstellar medium filled with hot gas, known as Wind-Blown Bubbles (WBB). We propose to obtain XIS imaging spectroscopy of the prototype WBB NGC 6888. Thanks to the XIS excellent sensitivity and energy resolution in the soft X-ray band, we will: (i) obtain a high quality CCD spectrum which can be used to constrain the temperature of the hot plasma and the efficiency of thermal conduction across the bubble wall, (ii) determine the spatial distribution and properties of X-ray emitting plasma, (iii) therefore, test and refine shock physics models of bubbles by a direct confrontation of their results with observations. | GALACTIC DIFFUSE EMISSION | 5 | A | SVETOZAR ZHEKOV | USA | 4 | AO4 | X-RAYS FROM THE PROTOTYPE WIND-BLOWN BUBBLE NGC 6888 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504084010/ | Quick Look | ![]() |
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766 | 3C111 | 64.5838 | 38.0364 | 63.747621 | 37.915108 | 69.36876 | 16.399466 | 161.66578558 | -8.81556542 | 79.7358 | 55441.1593055556 | 2010-09-02 03:49:24 | 55442.8995138889 | 2010-09-03 21:35:18 | 705040010 | 80.683 | 80 | 80.691 | 80.683 | 0 | 80.691 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 73.3707 | 73.3707 | 150.3079 | 1 | PROCESSED | 57553.2986458333 | 2016-06-14 07:10:03 | 55822 | 2011-09-18 00:00:00 | 55456.2202430556 | 2010-09-17 05:17:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051412 | Using our Suzaku observations we discovered ultra-fast outflows (UFOs) in radio-loud Broad-Line Radio Galaxies, with velocities v/c~0.04--0.15 and carrying a mass of the same order as the accretion mass. The bright BLRG 3C~111 was selected for an in-depth study of its UFO through its predicted variability on timescales of approximately one week. We propose 3 Suzaku pointings of 80~ks each separated by one week to determine the gas geometrical, physical, and dynamical characteristics and start addressing its role for the jet-disk connection in radio-loud AGN. Additionally, we will obtain a simultaneous radio-to-GeV Spectral Energy Distribution and model the relative contributions of the accretion and non-thermal components. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RITA SAMBRUNA | USA | 5 | AO5 | PROBING THE ULTRA-FAST OUTFLOW IN 3C 111 WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705040010/ | Quick Look | ![]() |
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767 | 3C111 | 64.5838 | 38.0341 | 63.747638 | 37.912808 | 69.368333 | 16.397202 | 161.66743119 | -8.81719194 | 77.8463 | 55448.0268865741 | 2010-09-09 00:38:43 | 55449.7585416667 | 2010-09-10 18:12:18 | 705040020 | 79.4198 | 80 | 79.4198 | 79.4198 | 0 | 79.4198 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71.809 | 71.809 | 149.6058 | 0 | PROCESSED | 57553.3942592593 | 2016-06-14 09:27:44 | 55827 | 2011-09-23 00:00:00 | 55461.3122106482 | 2010-09-22 07:29:35 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051412 | Using our Suzaku observations we discovered ultra-fast outflows (UFOs) in radio-loud Broad-Line Radio Galaxies, with velocities v/c~0.04--0.15 and carrying a mass of the same order as the accretion mass. The bright BLRG 3C~111 was selected for an in-depth study of its UFO through its predicted variability on timescales of approximately one week. We propose 3 Suzaku pointings of 80~ks each separated by one week to determine the gas geometrical, physical, and dynamical characteristics and start addressing its role for the jet-disk connection in radio-loud AGN. Additionally, we will obtain a simultaneous radio-to-GeV Spectral Energy Distribution and model the relative contributions of the accretion and non-thermal components. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RITA SAMBRUNA | USA | 5 | AO5 | PROBING THE ULTRA-FAST OUTFLOW IN 3C 111 WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705040020/ | Quick Look | ![]() |
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768 | IC 5157 | 330.8663 | -34.934 | 330.129358 | -35.176355 | 320.316602 | -21.507496 | 10.02196464 | -53.45455848 | 251.1985 | 56250.3323611111 | 2012-11-19 07:58:36 | 56251.6043287037 | 2012-11-20 14:30:14 | 807048010 | 65.5411 | 150 | 65.5411 | 65.5411 | 0 | 65.5411 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 67.764 | 67.764 | 109.8861 | 1 | PROCESSED | 57608.0722222222 | 2016-08-08 01:44:00 | 56018 | 2012-04-01 00:00:00 | 56275.5333333333 | 2012-12-14 12:48:00 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071503 | The mass profiles of elliptical galaxies are important probes of galaxy formation and cosmology. Only a few elliptical galaxies have detailed mass measurements from X-rays because of the lack of suitable targets in terms of total mass (< ~10^{13} m_sun) and relaxed dynamical states appropriate for hydrostatic analysis. We have identified a sample of (hot) gas-rich isolated elliptical galaxies, most of which were discovered from previously awarded XMM and Chandra snapshot programs to search for optimal targets for X-ray studies of mass profiles on the galaxy scale. We request Suzaku observations to map the detailed profiles of stars, dark matter, and hot gas in two of these galaxies which have (scheduled) complementary Chandra observations. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | DAVID BUOTE | USA | 7 | AO7 | THE MASS PROFILES OF ISOLATED ELLIPTICAL GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807048010/ | Quick Look | ![]() |
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769 | FG30 | 259.5133 | 56.677 | 259.289115 | 56.728173 | 238.479728 | 78.961901 | 84.88085465 | 35.08331599 | 38.7622 | 56049.4885532407 | 2012-05-02 11:43:31 | 56049.7980671296 | 2012-05-02 19:09:13 | 807051010 | 13.9787 | 10 | 13.9867 | 13.9947 | 0 | 13.9787 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.579 | 15.579 | 26.7259 | 0 | PROCESSED | 57605.3190856482 | 2016-08-05 07:39:29 | 56465 | 2013-06-22 00:00:00 | 56099.2218171296 | 2012-06-21 05:19:25 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071511 | Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ELENA D'ONGHIA | USA | 7 | AO7 | SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807051010/ | Quick Look | ![]() |
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770 | SNR G304.6+0.1 | 196.4463 | -62.6951 | 195.657347 | -62.427468 | 227.041423 | -49.777353 | 304.57643925 | 0.13082789 | 321.0575 | 55442.9126736111 | 2010-09-03 21:54:15 | 55445.5356828704 | 2010-09-06 12:51:23 | 505074010 | 99.5817 | 100 | 99.6217 | 99.5817 | 0 | 99.6297 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 90.5653 | 90.5653 | 226.5319 | 1 | PROCESSED | 57553.3505555556 | 2016-06-14 08:24:48 | 55827 | 2011-09-23 00:00:00 | 55461.4231712963 | 2010-09-22 10:09:22 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051306 | Galactic supernova remnants are believed to be the primary source of cosmic rays below 10^15.5 eV even though the exact acceleration mechanism remains unknown. This uncertainty results from the lack of remnants with synchrotron X-ray and GeV emission, needed to distinguish accelerated electrons from protons using broadband spectral modeling. An analysis of recent XMM and Fermi data suggests SNR G304.6+0.1 is just the third remnant with both, but the observed hard X-ray excess is also consistent with bremsstrahlung emission. We request a deep Suzaku observation of this source to determine the nature of its hard X-ray emission - critical for identifying the underlying acceleration mechanism. | GALACTIC DIFFUSE EMISSION | 5 | B | JOSEPH GELFAND | USA | 5 | AO5 | THE ORIGIN OF THE HARD X-RAY AND GEV GAMMA-RAY EMISSION OF SNR G304.6+0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505074010/ | Quick Look | ![]() |
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771 | FG15 | 177.008 | 56.8964 | 176.342479 | 57.174256 | 146.620123 | 49.215769 | 139.35969999 | 58.16359998 | 300.5727 | 56073.7490856482 | 2012-05-26 17:58:41 | 56074.0586226852 | 2012-05-27 01:24:25 | 807057010 | 14.0757 | 15 | 14.0757 | 14.0757 | 0 | 14.0757 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.603 | 15.603 | 26.7399 | 1 | PROCESSED | 57605.5125578704 | 2016-08-05 12:18:05 | 56470 | 2013-06-27 00:00:00 | 56103.1467013889 | 2012-06-25 03:31:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071511 | Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ELENA D'ONGHIA | USA | 7 | AO7 | SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807057010/ | Quick Look | ![]() |
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772 | FG24 | 233.4334 | 3.6096 | 232.807042 | 3.776669 | 230.06319 | 22.123365 | 8.88650115 | 44.69822064 | 290.4245 | 56136.3403935185 | 2012-07-28 08:10:10 | 56136.7487152778 | 2012-07-28 17:58:09 | 807058010 | 15.8231 | 15 | 15.8231 | 15.8231 | 0 | 15.8231 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.191 | 13.191 | 35.2759 | 0 | PROCESSED | 57606.6653819444 | 2016-08-06 15:58:09 | 56527 | 2013-08-23 00:00:00 | 56161.2328240741 | 2012-08-22 05:35:16 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071511 | Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ELENA D'ONGHIA | USA | 7 | AO7 | SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807058010/ | Quick Look | ![]() |
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773 | RXJ1159+5531 | 179.9812 | 55.4402 | 179.338152 | 55.71852 | 149.981877 | 49.065325 | 137.66567163 | 60.1900448 | 115.1582 | 56268.8799768518 | 2012-12-07 21:07:10 | 56269.4140162037 | 2012-12-08 09:56:11 | 807064020 | 21.1432 | 20 | 21.1432 | 21.1512 | 0 | 21.1512 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.6001 | 22.6001 | 46.14 | 0 | PROCESSED | 57608.2013310185 | 2016-08-08 04:49:55 | 56646 | 2013-12-20 00:00:00 | 56279.6625925926 | 2012-12-18 15:54:08 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071513 | With Chandra and Suzaku we recently constrained the hot gas and dark matter out to the virial radius (rvir=R108) in the fossil group/cluster RXJ1159+5531. Unlike some recent observations of cluster outskirts, the gas fraction is consistent with the cosmic value, and the entropy profile at rvir is consistent with gravity-only structure formation simulations. As a fossil group, RXJ1159+5531 may be unusually relaxed at large scales. If so, the gas properties should not vary much azimuthally. We propose a complementary Suzaku observation to explore this by measuring the gas in a different azimuthal region, more than doubling the current (~27%) azimuthal coverage. Our results will help determine if gas clumping, invoked to explain the outskirts of some clusters, is ubiquitous. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | PHILIP HUMPHREY | USA | 7 | AO7 | RELAXED GAS AT THE VIRIAL RADIUS IN A FOSSIL GROUP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807064020/ | Quick Look | ![]() |
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774 | MRK 841 | 226.0057 | 10.444 | 225.402057 | 10.638407 | 220.18036 | 26.59752 | 11.21871304 | 54.63485497 | 108.0015 | 55944.7625347222 | 2012-01-18 18:18:03 | 55947.3599305556 | 2012-01-21 08:38:18 | 706029020 | 110.289 | 350 | 110.2915 | 110.289 | 0 | 110.2915 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92.2182 | 92.2182 | 224.404 | 1 | PROCESSED | 57604.469224537 | 2016-08-04 11:15:41 | 55652 | 2011-04-01 00:00:00 | 55985.3097337963 | 2012-02-28 07:26:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061119 | We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | CHRISTOPHER REYNOLDS | USA | 6 | AO6-LP | A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706029020/ | Quick Look | ![]() |
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775 | RXJ1416.4+2315 | 214.0491 | 23.1704 | 213.474982 | 23.401811 | 202.508805 | 34.45187 | 25.95253376 | 70.44078356 | 293.1179 | 56125.9101736111 | 2012-07-17 21:50:39 | 56128.5008796296 | 2012-07-20 12:01:16 | 807065020 | 101.6938 | 100 | 101.7018 | 101.6938 | 0 | 101.7018 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 99.6763 | 99.6763 | 223.8209 | 2 | PROCESSED | 57606.7012037037 | 2016-08-06 16:49:44 | 56598 | 2013-11-02 00:00:00 | 56232.6190740741 | 2012-11-01 14:51:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071514 | Our study of the fossil group RXJ 1159+5531 does not find the gas clumping invoked to explain unexpectedly flat entropy profiles and large gas fractions near r_vir in some clusters. Instead its ICM properties at r_vir are consistent with adiabatic cluster formation, which may reflect that hydrostatic equilibrium is very accurate in this highly evolved fossil group. To examine whether these results extend to other fossils and to more massive systems, we propose to observe the fossil cluster RXJ 1416.4+2315 (M_vir ~3 x 10^14 M_sun) to constrain its entropy and gas fraction out to r_vir (r_112). Since it is located at a redshift of 0.137, this target provides an efficient means to explore the outer ICM, where a large azimuthal portion (~80%) of r_vir can be observed in a single Suzaku field. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | DAVID BUOTE | USA | 7 | AO7 | RXJ1416.4+2315: A MASSIVE FOSSIL CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807065020/ | Quick Look | ![]() |
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776 | ANTLIA E3 | 158.6143 | -35.3303 | 158.046217 | -35.07153 | 176.766294 | -40.455458 | 273.75347644 | 19.66467309 | 278.5008 | 56093.5404166667 | 2012-06-15 12:58:12 | 56094.1877546296 | 2012-06-16 04:30:22 | 807068010 | 23.4861 | 23 | 23.5021 | 23.4861 | 0 | 23.5021 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.6862 | 20.6862 | 55.926 | 1 | PROCESSED | 57605.6943287037 | 2016-08-05 16:39:50 | 56476 | 2013-07-03 00:00:00 | 56110.5216550926 | 2012-07-02 12:31:11 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071521 | We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KA-WAH WONG | USA | 7 | AO7 | MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807068010/ | Quick Look | ![]() |
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777 | ABELL 665 | 127.933 | 65.6581 | 126.801514 | 65.827031 | 110.986153 | 44.956941 | 149.97935617 | 34.81341699 | 289.9968 | 56028.5599537037 | 2012-04-11 13:26:20 | 56029.4036226852 | 2012-04-12 09:41:13 | 807072040 | 52.791 | 50 | 52.791 | 52.799 | 0 | 52.799 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.6671 | 51.6671 | 72.8859 | 0 | PROCESSED | 57605.1597569444 | 2016-08-05 03:50:03 | 56018 | 2012-04-01 00:00:00 | 56044.1843518518 | 2012-04-27 04:25:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071522 | We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 7 | AO7 | COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807072040/ | Quick Look | ![]() |
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778 | G18.8+0.3 | 275.9435 | -12.3781 | 275.241856 | -12.405238 | 275.902948 | 10.940788 | 18.78460262 | 0.39706413 | 83.4994 | 55994.9180324074 | 2012-03-08 22:01:58 | 55996.1598958333 | 2012-03-10 03:50:15 | 506051010 | 52.0205 | 50 | 52.0205 | 52.0285 | 0 | 52.0365 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.882 | 44.882 | 107.2639 | 1 | PROCESSED | 57604.8541435185 | 2016-08-04 20:29:58 | 56382 | 2013-03-31 00:00:00 | 56016.6717708333 | 2012-03-30 16:07:21 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061311 | We propose a 50 ks exploratory observation of an interesting first-quadrant supernova remnant, G18.8+0.3, for which radio-continuum and CO data indicate interaction with a molecular cloud. Prior X-ray studies are limited to a 14 ks ROSAT PSPC observation producing about 500 counts. We expect about 12,000 counts with Suzaku, which should permit basic characterization of the spectrum and morphology of X-rays: shell-type, mixed-morphology (central thermal emission) or even composite (central PWN). Spectral analysis will allow us to determine or estimate shock speed, age, ambient density, and swept-up mass. As more middle-aged remnants are found to have unusual properties such as GeV-TeV emission, the study of objects like G18.8+0.3 assumes greater importance. | GALACTIC DIFFUSE EMISSION | 5 | C | STEPHEN REYNOLDS | USA | 6 | AO6 | G18.8+0.3: A SUPERNOVA REMNANT WITH STRONG MOLECULAR INTERACTION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506051010/ | Quick Look | ![]() |
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779 | RCS110104-0351.3 | 165.266 | -3.8543 | 164.630074 | -3.585449 | 167.943149 | -9.357953 | 257.98650762 | 49.14106345 | 115.7008 | 56286.1353587963 | 2012-12-25 03:14:55 | 56287.8716898148 | 2012-12-26 20:55:14 | 807076010 | 76.1379 | 75 | 76.1539 | 76.1379 | 0 | 76.1539 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 67.4411 | 67.4411 | 150.0018 | 0 | PROCESSED | 57608.3704050926 | 2016-08-08 08:53:23 | 56690 | 2014-02-02 00:00:00 | 56324.5102314815 | 2013-02-01 12:14:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071525 | Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 24 optically-selected clusters of galaxies out to z~1. Here we propose 5 additional observations in order to uniformly span our total mass-redshift space over the range 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 7 | AO7 | AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES II | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807076010/ | Quick Look | ![]() |
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780 | SWCL J1403+3212 | 210.8847 | 32.2142 | 210.333728 | 32.453758 | 194.392634 | 41.437605 | 55.27159844 | 73.55798506 | 128.2493 | 56289.1009837963 | 2012-12-28 02:25:25 | 56290.2578587963 | 2012-12-29 06:11:19 | 807081010 | 52.1374 | 45 | 52.1374 | 52.143 | 0 | 52.1454 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.9868 | 42.9868 | 99.9358 | 0 | PROCESSED | 57608.4054050926 | 2016-08-08 09:43:47 | 56690 | 2014-02-02 00:00:00 | 56324.4837152778 | 2013-02-01 11:36:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071526 | The evolution of X-ray properties of galaxy clusters with redshift provides important constraints on the formation and evolution of the hot gaseous halos. The scaling relations and their deviations from self-similar model predictions due to non-gravitational processes are also important for modeling the cluster selection function for cosmology. We propose to observe a uniform sample of z~0.6 galaxy clusters, selected from the Swift archival data and confirmed by multi-band optical data, using Suzaku to better characterize their X-ray properties such the X-ray luminosity and temperature. With this sample, we are able to model the selection functions relatively easily and place cleaner and tighter constraints on the evolution of X-ray properties of galaxy clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | XINYU DAI | USA | 7 | AO7 | X-RAY PROPERTIES OF A UNIFORMLY SELECTED SAMPLE OF Z ~ 0.6 CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807081010/ | Quick Look | ![]() |
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781 | OT+081 | 267.8906 | 9.6366 | 267.297097 | 9.648276 | 267.507831 | 33.058606 | 34.9082961 | 17.63584745 | 268.2827 | 55830.0996759259 | 2011-09-26 02:23:32 | 55830.3911921296 | 2011-09-26 09:23:19 | 706047010 | 10.774 | 10 | 10.774 | 10.774 | 0 | 10.774 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.036 | 11.036 | 25.1519 | 1 | PROCESSED | 57603.2492708333 | 2016-08-03 05:58:57 | 56225 | 2012-10-25 00:00:00 | 55875.6247569444 | 2011-11-10 14:59:39 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061601 | We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | SVETLANA JORSTAD | USA | 6 | AO6 | EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706047010/ | Quick Look | ![]() |
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782 | 0827+243 | 127.7155 | 24.1863 | 126.975126 | 24.355162 | 124.074961 | 5.096162 | 200.01763935 | 31.87561316 | 105.3936 | 56213.3893287037 | 2012-10-13 09:20:38 | 56213.5959837963 | 2012-10-13 14:18:13 | 707041010 | 8.0392 | 10 | 8.0472 | 8.0392 | 0 | 8.0472 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.737 | 7.737 | 17.8479 | 0 | PROCESSED | 57607.7474652778 | 2016-08-07 17:56:21 | 56598 | 2013-11-02 00:00:00 | 56232.4327199074 | 2012-11-01 10:23:07 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071601 | We propose to perform two 2-week multi-frequency campaigns of observations of a sample of gamma-ray blazars during Fermi Cycle 5. The campaigns will involve: (1) gamma-ray monitoring with the Fermi LAT, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B, V, R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku and Swift; (6) mid-IR measurements with IRTF; and (7) near-IR photometric J, H, and K observations. The research aims i) to search for correlated variability on short timescales; ii) to compile SEDs at different states of gamma-ray and radio jet activitiy; and iii) to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | SVETLANA JORSTAD | USA | 7 | AO7 | MULTI-FREQUENCY CAMPAIGNS TO STUDY RAPID VARIABILITY IN GAMMA_RAY BLAZARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707041010/ | Quick Look | ![]() |
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783 | COMA CLUSTER | 194.3893 | 26.9261 | 193.783242 | 27.196084 | 181.532075 | 30.236179 | 24.84225016 | 88.62234831 | 316.4746 | 55348.2119907407 | 2010-06-01 05:05:16 | 55350.6877199074 | 2010-06-03 16:30:19 | 805079010 | 101.7805 | 100 | 101.7805 | 101.7805 | 0 | 101.7805 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 77.4308 | 77.4308 | 213.8639 | 1 | PROCESSED | 57553.0722685185 | 2016-06-14 01:44:04 | 55731 | 2011-06-19 00:00:00 | 55365.54125 | 2010-06-18 12:59:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051523 | The metal-enrichment mechanism of the hot gas in clusters of galaxies is still not completely understood, particularly at large (~virial) radii where current metallicity measurements are virtually non-existent. Yet a determinaton of elemental abundances of the gas at this radius will allow us to determine which enrichment mechanism (ram pressure stripping or galactic winds) is prevalant in the outskirts of clusters. We propose a 100 kec Suzaku observation of Coma at the virial radius to determine the Fe and S abundances at this location. The ratio of these two elements will allow us to discriminate among competing models for chemical enrichment. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | JIMMY IRWIN | USA | 5 | AO5 | THE DETERMINATION OF THE METALLICITY OF COMA AT THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805079010/ | Quick Look | ![]() |
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784 | MKN 6 | 103.0685 | 74.413 | 101.450971 | 74.472117 | 95.572656 | 51.225087 | 140.3435691 | 26.1094153 | 254.4482 | 57133.5883333333 | 2015-04-21 14:07:12 | 57134.7015046296 | 2015-04-22 16:50:10 | 710001010 | 50.6541 | 50 | 50.6541 | 51.3396 | 0 | 51.3396 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.0317476852 | 2016-08-18 00:45:43 | 57548 | 2016-06-09 00:00:00 | 57154.4415162037 | 2015-05-12 10:35:47 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 101730 | We request two quasi-simultaneous NuSTAR + Suzaku-XIS pointings of the radio-loud Sy 1.5 Mkn 6 to understand the complexity of its accreting circumnuclear gas structures. A series of high-quality, broadband X-ray spectra, including coverage above 10 keV, are needed to properly quantify the variable and complex line of sight absorbers. These new observations, in conjunction with radio and previous X-ray observations, will be a unique opportunity to understand accretion modes in the innermost regions of a radio-loud AGN that has recently undergone a merger. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ALEX MARKOWITZ | USA | 10 | AO10 | COMPLEX CIRCUMNUCLEAR ABSORPTION IN RADIO-LOUD AGN: VARIABLE ABSORPTION IN MKN 6 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710001010/ | Quick Look | ![]() |
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785 | MKW4-W2 | 181.7129 | 1.8545 | 181.072483 | 2.132812 | 180.830723 | 2.382546 | 278.14148217 | 62.56052834 | 136.8029 | 56652.6158217593 | 2013-12-26 14:46:47 | 56655.3919097222 | 2013-12-29 09:24:21 | 808065010 | 102.6011 | 100 | 102.6011 | 102.6011 | 0 | 102.6011 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 88.6977 | 88.6977 | 239.8258 | 1 | PROCESSED | 57613.7424421296 | 2016-08-13 17:49:07 | 57079 | 2015-02-26 00:00:00 | 56700.7408449074 | 2014-02-12 17:46:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081512 | We propose to observe the MKW4 group by leveraging existing observations to provide coverage from its center to its virial radius in two orthogonal directions. Three additional pointings, totaling 230 ksec, combined with two existing pointings, will allow us to determine radial profiles of gas temperature, density, entropy, pressure, and gas mass fraction, as well as their azimuthal variations. Comparing these properties to those of clusters will allow us to probe the role played by baryonic physics and assess the imprints of hierarchical structure formation. The stable and low background of the Suzaku XIS is crucial for the study of galaxy groups to their virial radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUANYUAN SU | USA | 8 | AO8 | PROBING A TYPICAL GALAXY GROUP TO ITS VIRAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808065010/ | Quick Look | ![]() |
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786 | A133_FIELD_1 | 15.9453 | -21.6335 | 15.33461 | -21.90164 | 5.595502 | -26.095488 | 150.67449532 | -83.82895318 | 231.9994 | 56645.5063078704 | 2013-12-19 12:09:05 | 56646.6683449074 | 2013-12-20 16:02:25 | 808081010 | 53.6483 | 50 | 53.6643 | 53.6483 | 0 | 53.6643 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52.6512 | 52.6512 | 100.3879 | 1 | PROCESSED | 57613.6155439815 | 2016-08-13 14:46:23 | 57061 | 2015-02-08 00:00:00 | 56695.6487152778 | 2014-02-07 15:34:09 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081525 | We propose observations of the outskirts of Abell 133, a relaxed galaxy cluster that is the target of a Chandra X-ray Visionary Project. These modest Suzaku observations will leverage the 2.4 Msec of Chandra time spent deeply imaging the region beyond r_500 to search for ICM clumping. Such clumping has been invoked to explain the flat entropy profiles and excess inferred gas fraction beyond r_500 in several clusters observed recently with Suzaku. The proposed Suzaku observations combined with the unprecedented Chandra depth will create a fiducial dataset to compare to the existing Suzaku cluster outskirts data, and they will definitely determine whether the excess inferred gas fractions seen with Suzaku arise from gas clumping. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | ERIC MILLER | USA | 8 | AO8 | A DEFINITIVE STUDY OF GALAXY CLUSTER OUTSKIRTS WITH SUZAKU AND CHANDRA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808081010/ | Quick Look | ![]() |
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787 | COMA E2 | 195.5294 | 27.8966 | 194.927658 | 28.165178 | 182.080007 | 31.557077 | 51.52244118 | 87.51055859 | 279.9995 | 55729.2687268518 | 2011-06-17 06:26:58 | 55729.4890856482 | 2011-06-17 11:44:17 | 806031010 | 9.1256 | 10 | 9.1336 | 9.1256 | 0 | 9.1416 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.9108 | 8.9108 | 19.0319 | 0 | PROCESSED | 57602.3188194444 | 2016-08-02 07:39:06 | 55652 | 2011-04-01 00:00:00 | 55770.1098958333 | 2011-07-28 02:38:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806031010/ | Quick Look | ![]() |
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788 | FORNAX CLUSTER NORTH | 54.7043 | -35.2294 | 54.224181 | -35.391259 | 39.001136 | -52.608154 | 236.34117402 | -53.57224789 | 244.9993 | 53749.1506134259 | 2006-01-14 03:36:53 | 53750.3265509259 | 2006-01-15 07:50:14 | 800002030 | 45.575 | 80 | 45.583 | 45.579 | 45.575 | 45.587 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 42.5713 | 42.5713 | 101.6 | 1 | PROCESSED | 57532.6714236111 | 2016-05-24 16:06:51 | 54247 | 2007-05-27 00:00:00 | 54039.9702777778 | 2006-10-31 23:17:12 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001018 | The center of the Fornax cluster was observed with Suzaku with a 80 ks exposure. We have detected excess hard-emission and derived O abundances of the ISM of NGC 1399 and NGC 1404, and the intracluster medium (ICM). Here, we propose to observe two offset pointings of the Fornax cluster for 160 ks (80 ks times 2) to study the distribution of the hard emission and the abundance distribution of O, Mg, Si, S and Fe. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | JAP | 0 | SWG | MAPPING HARD EXCESS EMISSION AND OXYGEN IN THE INTRACLUSTER MEDIUM OF THE FORNAX CLUSTER | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800002030/ | Quick Look | ![]() |
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789 | CIZASOUTHPE | 340.7756 | 52.9173 | 340.257126 | 52.654896 | 13.355059 | 54.189252 | 104.17197619 | -5.21572392 | 71.9989 | 56461.8747800926 | 2013-06-18 20:59:41 | 56464.2467361111 | 2013-06-21 05:55:18 | 808092010 | 92.9595 | 99 | 92.9675 | 92.9675 | 0 | 92.9595 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 96.3125 | 96.3125 | 204.9216 | 2 | PROCESSED | 57611.5762268518 | 2016-08-11 13:49:46 | 56848 | 2014-07-10 00:00:00 | 56481.818287037 | 2013-07-08 19:38:20 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081530 | The Sausage Cluster is a violent merging galaxy cluster that offers unique opportunities to study the physics of particle acceleration and shocks in the ICM. We propose Suzaku observations of the southern part of the Sausage Cluster to (i) measure the Mach number of a merger related shock and (ii) determine the temperature distribution in the entire cluster outskirts. These observations will provide the first complete view of a system of merger-induced radio shocks and therefore play a crucial role in (1) understanding the impacts of such shocks on the evolution of galaxy clusters, (2) determining the physics of particle acceleration at low Mach number shocks, and (3) providing vital input for modeling the merger event in detail. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | REINOUT VAN WEEREN | USA | 8 | AO8 | SHOCK AND AWE: PARTICLE ACCELERATION IN THE SAUSAGE CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808092010/ | Quick Look | ![]() |
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790 | ABELL 3364 | 86.9739 | -32.0342 | 86.50731 | -32.050049 | 85.482586 | -55.428799 | 237.12200328 | -26.63960547 | 295.0051 | 55671.5944444444 | 2011-04-20 14:16:00 | 55672.2917939815 | 2011-04-21 07:00:11 | 806067040 | 31.8869 | 29.5 | 31.8949 | 31.8949 | 0 | 31.8869 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29.6154 | 29.6154 | 60.2459 | 0 | PROCESSED | 57601.5617939815 | 2016-08-01 13:28:59 | 56067 | 2012-05-20 00:00:00 | 55692.2490277778 | 2011-05-11 05:58:36 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061524 | Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but none was studied for non-cool core clusters. We propose a 118 ks Suzaku observation of a regular non-cool core cluster (for the first time) Abell 3364. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KA-WAH WONG | USA | 6 | AO6 | THE FIRST REGULAR NON-COOL CORE GALAXY CLUSTER TO BE STUDIED NEAR THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806067040/ | Quick Look | ![]() |
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791 | IIZW108 | 318.5228 | 2.5728 | 317.890055 | 2.365228 | 321.781705 | 17.722745 | 53.56011975 | -29.86052353 | 77.7227 | 53864.5319791667 | 2006-05-09 12:46:03 | 53864.7883680556 | 2006-05-09 18:55:15 | 801075010 | 11.6052 | 11 | 11.6052 | 11.6052 | 11.6052 | 11.6052 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 9.632 | 9.632 | 22.1499 | 1 | PROCESSED | 57534.2579398148 | 2016-05-26 06:11:26 | 54401 | 2007-10-28 00:00:00 | 53913.9958564815 | 2006-06-27 23:54:02 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801075010/ | Quick Look | ![]() |
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792 | CIZASOUTHPW | 340.5329 | 52.9469 | 340.016017 | 52.68489 | 13.195696 | 54.305912 | 104.05697228 | -5.12002469 | 72.9252 | 56464.2477662037 | 2013-06-21 05:56:47 | 56466.5627777778 | 2013-06-23 13:30:24 | 808093010 | 98.4207 | 99 | 98.4287 | 98.4207 | 0 | 98.4287 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 99.1006 | 99.1006 | 200.0056 | 0 | PROCESSED | 57611.6015277778 | 2016-08-11 14:26:12 | 56848 | 2014-07-10 00:00:00 | 56481.8295486111 | 2013-07-08 19:54:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081530 | The Sausage Cluster is a violent merging galaxy cluster that offers unique opportunities to study the physics of particle acceleration and shocks in the ICM. We propose Suzaku observations of the southern part of the Sausage Cluster to (i) measure the Mach number of a merger related shock and (ii) determine the temperature distribution in the entire cluster outskirts. These observations will provide the first complete view of a system of merger-induced radio shocks and therefore play a crucial role in (1) understanding the impacts of such shocks on the evolution of galaxy clusters, (2) determining the physics of particle acceleration at low Mach number shocks, and (3) providing vital input for modeling the merger event in detail. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | REINOUT VAN WEEREN | USA | 8 | AO8 | SHOCK AND AWE: PARTICLE ACCELERATION IN THE SAUSAGE CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808093010/ | Quick Look | ![]() |
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793 | COMA RADIO RELIC | 193.8629 | 27.2883 | 193.256096 | 27.558895 | 180.859214 | 30.350856 | 43.32885714 | 89.09337318 | 130.9989 | 54823.8794328704 | 2008-12-23 21:06:23 | 54829.0002777778 | 2008-12-29 00:00:24 | 803051010 | 205.062 | 140 | 205.07 | 205.07 | 0 | 205.062 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 170.6222 | 170.6222 | 442.3917 | 3 | PROCESSED | 57545.2371412037 | 2016-06-06 05:41:29 | 55218 | 2010-01-22 00:00:00 | 54851.5095949074 | 2009-01-20 12:13:49 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031431 | We will observe the Coma cluster radio relic with the HXD/PIN to detect nonthermal Inverse Compton emission. This is the second brightest cluster radio relic known. The small PIN FOV will separate the Coma radio relic and halo. The PIN data will be a strong test of merger shock acceleration processes; a nondetection would be inconsistent with current theories. The data will allow the relic magnetic field, and nonthermal energy and pressure to be derived. The XIS observation of the relic will be used to detect the merger shock. The relic is associated with the merging NGC 4839 subgroup, which will also be observed. The 2 XIS observations will determine the dynamics of the merging subgroup. We will search for redshift differences between the Coma cluster, subgroup, and merger shock. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | CRAIG SARAZIN | USA | 3 | AO3 | HARD X-RAY INVERSE COMPTON EMISSION FROM THE RADIO RELIC AND THE DYNAMICS OF THE MERGING SUBGROUP IN THE COMA CLUSTER | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803051010/ | Quick Look | ![]() |
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794 | FG23 | 232.4567 | 44.1429 | 232.030206 | 44.313314 | 209.251166 | 59.914107 | 71.72776372 | 54.06523853 | 150.3369 | 57007.3108101852 | 2014-12-16 07:27:34 | 57008.1494791667 | 2014-12-17 03:35:15 | 809058010 | 38.4415 | 40 | 38.4415 | 38.4415 | 0 | 38.4415 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5220601852 | 2016-08-17 12:31:46 | 57482 | 2016-04-04 00:00:00 | 57114.5765972222 | 2015-04-02 13:50:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091512 | Optical and X-ray measurements of fossil galaxy systems (FGs) suggest that they are old and relaxed. If FGs are assembled at higher redshifts, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest group galaxy (BGG). We carry out the first systematic and multiwavelength study of a large sample of FGs, the FOssil Group Origins (FOGO) project. We propose to observe four bona fide fossil groups, most with T< 2 keV measuring Tx and Lx for objects at the mass scale of groups, which are rather unexplored. We will evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to our sample of fossil clusters completing the first X-ray selected sample of fossil systems ranging from the cluster to galaxy group scale. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | ELENA D'ONGHIA | USA | 9 | AO9 | SCALING RELATIONS OF FOSSIL GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809058010/ | Quick Look | ![]() |
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795 | CENTAURUS SE4 | 192.8602 | -42.5262 | 192.164471 | -42.254349 | 210.265844 | -33.700282 | 302.93248329 | 20.34554874 | 294.0685 | 56854.4082407407 | 2014-07-16 09:47:52 | 56854.9480092593 | 2014-07-16 22:45:08 | 809068010 | 20.659 | 20 | 20.659 | 20.659 | 0 | 20.659 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.395 | 10.395 | 22.0319 | 0 | PROCESSED | 57615.3959606482 | 2016-08-15 09:30:11 | 57250 | 2015-08-16 00:00:00 | 56883.1729050926 | 2014-08-14 04:08:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091522 | We propose here to observe the outskirts of the X-ray bright, nearby Centaurus cluster with good azimuthal coverage by adding 3 new arms with total exposure 204ks. This will extend our initial analysis in one direction to the north-west which has allowed our team to obtain high spatial resolution profiles of temperature, density and entropy. The XMM temperature map of the central 30 arcmins shows a complex temperature environment and deviations from spherical symmetry, and good azimuthal coverage is important to obtain an accurate understanding of the outskirts.Observations of the Perseus cluster have shown significant azimuthal variations in the ICM temperature and entropy. Centaurus is the best target for understanding the ICM in the outskirts of a relaxed, intermediate mass cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | CHRISTOPHER REYNOLDS | USA | 9 | AO9 | OBSERVATIONS OF THE X-RAY BRIGHT, NEARBY CENTAURUS CLUSTER TO THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809068010/ | Quick Look | ![]() |
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796 | RCS1102-0319 | 165.6362 | -3.316 | 164.999495 | -3.046688 | 168.075129 | -8.718258 | 257.90567893 | 49.79184665 | 114.0911 | 54817.3259259259 | 2008-12-17 07:49:20 | 54817.9773611111 | 2008-12-17 23:27:24 | 803065010 | 26.3811 | 21 | 26.3811 | 26.3811 | 0 | 26.3811 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.9089 | 13.9089 | 56.27 | 0 | PROCESSED | 57544.9757407407 | 2016-06-05 23:25:04 | 55206 | 2010-01-10 00:00:00 | 54840.2609143518 | 2009-01-09 06:15:43 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031441 | Comparisons between moderate-z X-ray and high-z optically selected clusters indicate that the latter have lower Lx than expected for a given Tx, however it is hard to tell if such discrepancies are due to cluster evolution or selection effects. In an attempt to isolate these two variables, we propose the first detailed comparison of X-ray and optically selected clusters that are well-matched in both velocity dispersion (a quantity independent of both methods) and redshift. Our X-ray analysis of X-ray selected CNOC clusters is complete. Here we propose to determine Lx, Tx, and gas distribution/morphology for an optically selected sample, most of which already have velocity dispersion data in hand, enabling rigorous quantitative comparisons between physical characteristics of the two groups. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 3 | AO3 | COSMOLOGY WITH CLUSTERS: CONSTRAINING PHYSICAL DIFFERENCES BETWEEN X-RAY AND OPTICALLY SELECTED SAMPLES AT MODERATE-Z | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803065010/ | Quick Look | ![]() |
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797 | ABELL 98-NORTH | 11.5751 | 20.8392 | 10.913914 | 20.566164 | 18.902329 | 14.584822 | 121.31617836 | -42.01643069 | 67.4405 | 56841.1634490741 | 2014-07-03 03:55:22 | 56841.958599537 | 2014-07-03 23:00:23 | 809078020 | 23.888 | 100 | 24.68 | 23.888 | 0 | 24.9396 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3618865741 | 2016-08-15 08:41:07 | 56748 | 2014-04-01 00:00:00 | 56875.6040393518 | 2014-08-06 14:29:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091525 | We propose to observe the outskirts of the strongly merging cluster Abell 98 both along and perpendicular to the large scale structure filament implied by the orientation of its three merging subclusters. This is the only remaining one of the four bright, strongly merging "double" clusters originally identified from Einstein observations that has not been observed with Suzaku. A comparison of the extended atmosphere in the filament and off-filament pointings will allow us to test for the presence of unresolved gas clumps, which should be more abundant along the filament, invoked to explain anomalously high (above cosmic) baryon fractions observed in some other clusters. If this "unresolved clumps" hypothesis is correct, then we should find higher baryon fractions along the filament. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SCOTT RANDALL | USA | 9 | AO9 | EXPLORING THE EXTENDED ATMOSPHERE OF THE STRONGLY MERGING CLUSTER ABELL 98 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809078020/ | Quick Look | ![]() |
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798 | FG34 | 359.5671 | 15.0896 | 358.927387 | 14.811234 | 5.724886 | 13.991032 | 104.34552863 | -45.85455759 | 250.6856 | 56999.6725115741 | 2014-12-08 16:08:25 | 57000.6669328704 | 2014-12-09 16:00:23 | 809060010 | 38.5062 | 40 | 38.5062 | 38.5062 | 0 | 38.5062 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.0584 | 35.0584 | 85.8958 | 1 | PROCESSED | 57617.4968634259 | 2016-08-17 11:55:29 | 57377 | 2015-12-21 00:00:00 | 57010.1825925926 | 2014-12-19 04:22:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091512 | Optical and X-ray measurements of fossil galaxy systems (FGs) suggest that they are old and relaxed. If FGs are assembled at higher redshifts, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest group galaxy (BGG). We carry out the first systematic and multiwavelength study of a large sample of FGs, the FOssil Group Origins (FOGO) project. We propose to observe four bona fide fossil groups, most with T< 2 keV measuring Tx and Lx for objects at the mass scale of groups, which are rather unexplored. We will evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to our sample of fossil clusters completing the first X-ray selected sample of fossil systems ranging from the cluster to galaxy group scale. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | ELENA D'ONGHIA | USA | 9 | AO9 | SCALING RELATIONS OF FOSSIL GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809060010/ | Quick Look | ![]() |
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799 | ABELL 2667 | 357.8478 | -26.2362 | 357.201143 | -26.514394 | 347.004245 | -23.092849 | 33.32905605 | -76.56526922 | 64.8822 | 55724.4201273148 | 2011-06-12 10:04:59 | 55725.7009490741 | 2011-06-13 16:49:22 | 806029030 | 52.2862 | 50 | 52.3022 | 52.2862 | 0 | 52.3102 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 42.9697 | 42.9697 | 110.6559 | 1 | PROCESSED | 57602.2711574074 | 2016-08-02 06:30:28 | 55652 | 2011-04-01 00:00:00 | 55757.6986458333 | 2011-07-15 16:46:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061116 | We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 6 | AO6-LP | THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806029030/ | Quick Look | ![]() |
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800 | COMA E3.5 | 195.93 | 27.9076 | 195.329276 | 28.17566 | 182.445576 | 31.726119 | 49.60850486 | 87.16763542 | 128.002 | 55917.6227314815 | 2011-12-22 14:56:44 | 55917.9487384259 | 2011-12-22 22:46:11 | 806032020 | 14.769 | 15 | 14.777 | 14.785 | 0 | 14.769 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.6169 | 9.6169 | 28.1599 | 1 | PROCESSED | 57604.2057175926 | 2016-08-04 04:56:14 | 55652 | 2011-04-01 00:00:00 | 55937.7819444444 | 2012-01-11 18:46:00 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806032020/ | Quick Look | ![]() |
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801 | COMA E7 | 197.1143 | 27.885 | 196.516478 | 28.15145 | 183.559395 | 32.176347 | 45.24852034 | 86.15126123 | 280.0002 | 55732.0582291667 | 2011-06-20 01:23:51 | 55732.4446990741 | 2011-06-20 10:40:22 | 806038010 | 15.1175 | 15 | 15.1335 | 15.1175 | 0 | 15.1415 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.3295 | 16.3295 | 33.3039 | 0 | PROCESSED | 57602.3596643518 | 2016-08-02 08:37:55 | 55652 | 2011-04-01 00:00:00 | 55770.1779398148 | 2011-07-28 04:16:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806038010/ | Quick Look | ![]() |
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802 | COMA NW1 | 194.8094 | 28.1686 | 194.206284 | 28.438076 | 181.270608 | 31.513632 | 64.44263169 | 87.98368038 | 319.9994 | 55732.4516550926 | 2011-06-20 10:50:23 | 55732.6453935185 | 2011-06-20 15:29:22 | 806039010 | 9.633 | 10 | 9.633 | 9.633 | 0 | 9.633 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.038 | 8.038 | 16.7279 | 0 | PROCESSED | 57602.3588310185 | 2016-08-02 08:36:43 | 55652 | 2011-04-01 00:00:00 | 55768.2335416667 | 2011-07-26 05:36:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806039010/ | Quick Look | ![]() |
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803 | COMA NW5.5 | 194.2342 | 29.281 | 193.631324 | 29.551161 | 180.146914 | 32.276161 | 93.88493667 | 87.52983745 | 319.9944 | 55734.0685763889 | 2011-06-22 01:38:45 | 55734.4155439815 | 2011-06-22 09:58:23 | 806043010 | 15.6631 | 15 | 15.6631 | 15.6631 | 0 | 15.6631 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.384 | 16.384 | 29.9559 | 1 | PROCESSED | 57602.3741203704 | 2016-08-02 08:58:44 | 55652 | 2011-04-01 00:00:00 | 55768.2836458333 | 2011-07-26 06:48:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806043010/ | Quick Look | ![]() |
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804 | SPT-CL J2337-5942 | 354.3472 | -59.706 | 353.656399 | -59.982964 | 322.211454 | -50.57498 | 319.15808948 | -55.0279039 | 35.9387 | 55674.1154282407 | 2011-04-23 02:46:13 | 55674.9342592593 | 2011-04-23 22:25:20 | 806073010 | 38.8415 | 35 | 38.8415 | 38.8415 | 0 | 38.8415 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33.8423 | 33.8423 | 70.74 | 0 | PROCESSED | 57601.5793402778 | 2016-08-01 13:54:15 | 56067 | 2012-05-20 00:00:00 | 55692.2710069445 | 2011-05-11 06:30:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061531 | We propose observations of four high-redshift galaxy clusters to constrain the metal enrichment history of the intra-cluster medium (ICM). The clusters, two at z ~ 1.0 and two at z ~ 0.75, are chosen from an initial mass-limited sample identified by the South Pole Telescope (SPT) cluster project, and they are among the most massive high-redshift clusters known. Chandra observations have verified the absence of point sources in these targets. The proposed Suzaku observations will increase the X-ray cluster counts by a factor of four, they will yield the most precise ICM abundance measurements at these redshifts to date, and they will provide a path-finder for future Suzaku studies of large, representative samples of high-redshift clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ERIC MILLER | USA | 6 | AO6 | THE METAL ABUNDANCE OF HIGH-REDSHIFT GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806073010/ | Quick Look | ![]() |
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805 | ABELL 3364 | 86.8402 | -31.7251 | 86.371508 | -31.741602 | 85.303796 | -55.115651 | 236.7542178 | -26.65907095 | 295.0034 | 55669.7134722222 | 2011-04-18 17:07:24 | 55670.3585416667 | 2011-04-19 08:36:18 | 806067010 | 30.0737 | 29.5 | 30.0897 | 30.0737 | 0 | 30.0897 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.5437 | 28.5437 | 55.7279 | 1 | PROCESSED | 57601.535787037 | 2016-08-01 12:51:32 | 56067 | 2012-05-20 00:00:00 | 55691.1662962963 | 2011-05-10 03:59:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061524 | Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but none was studied for non-cool core clusters. We propose a 118 ks Suzaku observation of a regular non-cool core cluster (for the first time) Abell 3364. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KA-WAH WONG | USA | 6 | AO6 | THE FIRST REGULAR NON-COOL CORE GALAXY CLUSTER TO BE STUDIED NEAR THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806067010/ | Quick Look | ![]() |
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806 | SPT-CL J0546-5345 | 86.64 | -53.7518 | 86.378624 | -53.768776 | 81.098351 | -77.090454 | 261.46331102 | -30.97881567 | 53.9016 | 55781.3261805556 | 2011-08-08 07:49:42 | 55782.8335763889 | 2011-08-09 20:00:21 | 806071010 | 99.7366 | 110 | 99.7366 | 99.7366 | 0 | 99.7366 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 78.9114 | 78.9114 | 130.2079 | 3 | PROCESSED | 57602.7921180556 | 2016-08-02 19:00:39 | 56169 | 2012-08-30 00:00:00 | 55802.4644907407 | 2011-08-29 11:08:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061531 | We propose observations of four high-redshift galaxy clusters to constrain the metal enrichment history of the intra-cluster medium (ICM). The clusters, two at z ~ 1.0 and two at z ~ 0.75, are chosen from an initial mass-limited sample identified by the South Pole Telescope (SPT) cluster project, and they are among the most massive high-redshift clusters known. Chandra observations have verified the absence of point sources in these targets. The proposed Suzaku observations will increase the X-ray cluster counts by a factor of four, they will yield the most precise ICM abundance measurements at these redshifts to date, and they will provide a path-finder for future Suzaku studies of large, representative samples of high-redshift clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ERIC MILLER | USA | 6 | AO6 | THE METAL ABUNDANCE OF HIGH-REDSHIFT GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806071010/ | Quick Look | ![]() |
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807 | NGC 7796 | 359.7407 | -55.4558 | 359.095869 | -55.734273 | 329.790591 | -49.001607 | 317.90399943 | -60.12089491 | 60.4505 | 56078.2927430556 | 2012-05-31 07:01:33 | 56080.5001851852 | 2012-06-02 12:00:16 | 807047010 | 161.6136 | 150 | 161.6216 | 161.6216 | 0 | 161.6136 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 134.0432 | 134.0432 | 190.7118 | 0 | PROCESSED | 57605.6269328704 | 2016-08-05 15:02:47 | 56018 | 2012-04-01 00:00:00 | 56090.2424537037 | 2012-06-12 05:49:08 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071503 | The mass profiles of elliptical galaxies are important probes of galaxy formation and cosmology. Only a few elliptical galaxies have detailed mass measurements from X-rays because of the lack of suitable targets in terms of total mass (< ~10^{13} m_sun) and relaxed dynamical states appropriate for hydrostatic analysis. We have identified a sample of (hot) gas-rich isolated elliptical galaxies, most of which were discovered from previously awarded XMM and Chandra snapshot programs to search for optimal targets for X-ray studies of mass profiles on the galaxy scale. We request Suzaku observations to map the detailed profiles of stars, dark matter, and hot gas in two of these galaxies which have (scheduled) complementary Chandra observations. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | DAVID BUOTE | USA | 7 | AO7 | THE MASS PROFILES OF ISOLATED ELLIPTICAL GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807047010/ | Quick Look | ![]() |
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808 | FG27 | 243.6269 | 26.7212 | 243.111772 | 26.845958 | 234.444811 | 46.957031 | 44.57695273 | 45.05698279 | 293.3995 | 56144.3018055556 | 2012-08-05 07:14:36 | 56144.5557638889 | 2012-08-05 13:20:18 | 807056010 | 11.2194 | 15 | 11.235 | 11.2194 | 0 | 11.235 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.9114 | 10.9114 | 21.9359 | 1 | PROCESSED | 57606.7546643518 | 2016-08-06 18:06:43 | 56533 | 2013-08-29 00:00:00 | 56167.1527893518 | 2012-08-28 03:40:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071511 | Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ELENA D'ONGHIA | USA | 7 | AO7 | SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807056010/ | Quick Look | ![]() |
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809 | SDSS J0837+4414 | 129.4975 | 44.2566 | 128.645697 | 44.432041 | 120.139652 | 24.860483 | 176.37698799 | 37.1577345 | 110.1912 | 56213.8277083333 | 2012-10-13 19:51:54 | 56214.3515393518 | 2012-10-14 08:26:13 | 807061010 | 20.6219 | 20 | 20.6219 | 20.6219 | 0 | 20.6219 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20.958 | 20.958 | 45.2399 | 0 | PROCESSED | 57607.7583796296 | 2016-08-07 18:12:04 | 56598 | 2013-11-02 00:00:00 | 56232.4985185185 | 2012-11-01 11:57:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071512 | Fossil groups (FGs) are systems dominated by a single large galaxy with a cluster-scale X-ray halo. They are thought to be old, isolated galaxy groups in which the large galaxies have coalesced through dynamical friction, but recent studies reveal a more complicated picture. We propose Suzaku observations of 5 optically selected FG candidates. These targets will extend our previous survey, which identified 12 FGs; when combined with 5 FG candidates approved for the current Chandra cycle, this will create the largest uniformly-selected sample of real FGs. The L_X and T_X measured will be used with optical spectroscopy to extend FG scaling relations to low mass, and to plan deeper X-ray spectroscopic follow-up to constrain the formation epoch and evolution of these puzzling systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ERIC MILLER | USA | 7 | AO7 | FINDING FOSSIL GROUPS WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807061010/ | Quick Look | ![]() |
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810 | ABELL 85 S2 | 10.6249 | -9.681 | 9.992851 | -9.954936 | 5.880188 | -13.097469 | 115.61862408 | -72.42570917 | 230.5003 | 56295.6322106482 | 2013-01-03 15:10:23 | 56296.8696064815 | 2013-01-04 20:52:14 | 807136010 | 53.603 | 50 | 53.611 | 53.611 | 0 | 53.603 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.8426 | 51.8426 | 106.8957 | 2 | PROCESSED | 57608.4325347222 | 2016-08-08 10:22:51 | 56702 | 2014-02-14 00:00:00 | 56336.5803240741 | 2013-02-13 13:55:40 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071791 | We propose exposures with CHandra and Suzaku in Abell 85 to trace the impact of a galaxy group merging with a galaxy cluster at multiple scales. Existing observations of Abell 85 reveal an infalling galaxy group ~300 kpc to the south of the main cluster moving supersonically through the ICM. Stripped gas is observed trailing behind this group to distances of 2 Mpc. We will investigate interactions between this group and the main cluster by observing the shocks associated with the group's motion and the properties of stripped gas. We will be able to measure the properties of the stripped gas from the group's current location out to the virial radius by combining the data from both telescopes. These observations will provide key insights into how the largest structures form. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | S | STEVEN ALLEN | USA | 7 | AO7 | TRACING A MERGER FROM START TO FINISH IN ABELL 85 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807136010/ | Quick Look | ![]() |
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811 | SHAPLEY B | 201.6375 | -31.8605 | 200.934316 | -31.601045 | 212.201419 | -21.080247 | 311.5766773 | 30.42117615 | 110.7883 | 56315.4877893518 | 2013-01-23 11:42:25 | 56316.3245138889 | 2013-01-24 07:47:18 | 807137010 | 30.5052 | 30 | 30.5132 | 30.5052 | 0 | 30.5203 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.1395 | 26.1395 | 72.2919 | 2 | PROCESSED | 57608.5939814815 | 2016-08-08 14:15:20 | 56709 | 2014-02-21 00:00:00 | 56342.5463888889 | 2013-02-19 13:06:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071848 | 29% of the baryon density measured at high redshift are unaccounted for at the present epoch. Since a persistent deficit would challenge our current understanding of the thermodynamics of structure formation and the effects of shocks and galactic outflows on the surrounding gas, resolving this deficit is critical for understanding low-redshift cosmology and galaxy formation. Simulations suggest these baryons emit soft X-rays and should reside along low density filaments in the cosmic web, the WHIM. We propose to combine Chandra ACIS-I with Suzaku XIS observations for 3 large scale filaments in the Shapley Supercluster, the largest overdensity of galaxies and clusters in the z<0.1 Universe, to identify galaxy groups in these filaments and search for X-ray emission from the WHIM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | S | MARIE MACHACEK | USA | 7 | AO7 | MAPPING GALAXY GROUPS AND THE HOT WHIM IN SHAPLEY SUPERCLUSTER FILAMENTS WITH CHANDRA AND SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807137010/ | Quick Look | ![]() |
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812 | SHAPLEY C | 202.085 | -31.0332 | 201.382602 | -30.774544 | 212.227549 | -20.169518 | 312.17140577 | 31.17563268 | 109.0374 | 56330.7851273148 | 2013-02-07 18:50:35 | 56331.4147453704 | 2013-02-08 09:57:14 | 807138010 | 30.8744 | 30 | 30.8904 | 30.8744 | 0 | 30.8904 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31.966 | 31.966 | 54.392 | 0 | PROCESSED | 57610.5475694444 | 2016-08-10 13:08:30 | 56715 | 2014-02-27 00:00:00 | 56349.523287037 | 2013-02-26 12:33:32 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071848 | 29% of the baryon density measured at high redshift are unaccounted for at the present epoch. Since a persistent deficit would challenge our current understanding of the thermodynamics of structure formation and the effects of shocks and galactic outflows on the surrounding gas, resolving this deficit is critical for understanding low-redshift cosmology and galaxy formation. Simulations suggest these baryons emit soft X-rays and should reside along low density filaments in the cosmic web, the WHIM. We propose to combine Chandra ACIS-I with Suzaku XIS observations for 3 large scale filaments in the Shapley Supercluster, the largest overdensity of galaxies and clusters in the z<0.1 Universe, to identify galaxy groups in these filaments and search for X-ray emission from the WHIM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | S | MARIE MACHACEK | USA | 7 | AO7 | MAPPING GALAXY GROUPS AND THE HOT WHIM IN SHAPLEY SUPERCLUSTER FILAMENTS WITH CHANDRA AND SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807138010/ | Quick Look | ![]() |
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813 | NGC 891 | 35.645 | 42.3416 | 34.858537 | 42.114299 | 47.830156 | 26.528514 | 140.39047988 | -17.41940889 | 243.1772 | 57072.5035300926 | 2015-02-19 12:05:05 | 57073.2222916667 | 2015-02-20 05:20:06 | 809054010 | 28.8738 | 100 | 28.8738 | 28.8738 | 0 | 28.8738 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6291550926 | 2016-08-17 15:05:59 | 57626 | 2016-08-26 00:00:00 | 57087.4767013889 | 2015-03-06 11:26:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091502 | The metallicity of the hot gas in the halos of isolated galaxies distinguishes between two models of galaxy formation, but few galaxies have bright enough halos to make this measurement. Metallicities measured in these systems are applied broadly and used in models, so it is important to understand the limits of the measurement. We address two ilimitations: we estimate the systematic error in the metallicity by comparing Suzaku and XMM-Newton observations, and we determine whether the bright, metal-enriched gas around starburst galaxies represents most of their mass. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | EDMUND HODGES-KLUCK | USA | 9 | AO9 | MEASURING SYSTEMATIC UNCERTAINTY IN THE HALO METALLICITY OF NGC 891 AND NGC 4631 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809054010/ | Quick Look | ![]() |
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814 | RXJ1159+5531 W | 179.7493 | 55.5442 | 179.104587 | 55.822511 | 149.726184 | 49.068198 | 137.82331154 | 60.04203639 | 299.9575 | 56808.2513657407 | 2014-05-31 06:01:58 | 56809.8959490741 | 2014-06-01 21:30:10 | 809064010 | 95.109 | 100 | 95.109 | 96.041 | 0 | 96.033 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.1837731482 | 2016-08-15 04:24:38 | 57194 | 2015-06-21 00:00:00 | 56828.5942592593 | 2014-06-20 14:15:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091521 | In contrast to some recent observations of cluster outskirts, for RXJ1159+5531, we obtain measurements of the gas fraction and entropy at the virial radius that are fully consistent with gravity-only structure formation simulations. Our preliminary Suzaku analysis of an opposite direction shows similar results. This encouraging consistency suggests that we may see little azimuthal variation in the gas properties for this unusually relaxed system. To verify and also benefit from the relaxed state of this benchmark system, we propose complementary Suzaku observations of RXJ1159+5531 in the other two directions. Simultaneously fitting these pointings would provide us the metal abundance ratios at large radii in order to place broad constrains on the enrichment history of group scale systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | YUANYUAN SU | USA | 9 | AO9 | MAPPING A BENCHMARK RELAXED POOR CLUSTER OUT TO ITS VIRIAL RADIUS WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809064010/ | Quick Look | ![]() |
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815 | ABELL 98-NORTH | 11.5755 | 20.8389 | 10.914314 | 20.565865 | 18.902557 | 14.584397 | 121.31667052 | -42.01674062 | 67.4405 | 56840.5909259259 | 2014-07-02 14:10:56 | 56841.1634375 | 2014-07-03 03:55:21 | 809078010 | 25.0582 | 100 | 0 | 0 | 0 | 25.0582 | 0 | 0 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3531481482 | 2016-08-15 08:28:32 | 56748 | 2014-04-01 00:00:00 | 56855.7487268518 | 2014-07-17 17:58:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091525 | We propose to observe the outskirts of the strongly merging cluster Abell 98 both along and perpendicular to the large scale structure filament implied by the orientation of its three merging subclusters. This is the only remaining one of the four bright, strongly merging "double" clusters originally identified from Einstein observations that has not been observed with Suzaku. A comparison of the extended atmosphere in the filament and off-filament pointings will allow us to test for the presence of unresolved gas clumps, which should be more abundant along the filament, invoked to explain anomalously high (above cosmic) baryon fractions observed in some other clusters. If this "unresolved clumps" hypothesis is correct, then we should find higher baryon fractions along the filament. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SCOTT RANDALL | USA | 9 | AO9 | EXPLORING THE EXTENDED ATMOSPHERE OF THE STRONGLY MERGING CLUSTER ABELL 98 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809078010/ | Quick Look | ![]() |
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816 | ABELL 98-NORTH | 11.5799 | 20.8287 | 10.918717 | 20.555669 | 18.902203 | 14.573403 | 121.32183614 | -42.02704716 | 251.2557 | 57012.9175231482 | 2014-12-21 22:01:14 | 57014.2377430556 | 2014-12-23 05:42:21 | 809078030 | 49.5381 | 50 | 49.5381 | 51.7925 | 0 | 51.8085 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5690509259 | 2016-08-17 13:39:26 | 56748 | 2014-04-01 00:00:00 | 57107.4424305556 | 2015-03-26 10:37:06 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091525 | We propose to observe the outskirts of the strongly merging cluster Abell 98 both along and perpendicular to the large scale structure filament implied by the orientation of its three merging subclusters. This is the only remaining one of the four bright, strongly merging "double" clusters originally identified from Einstein observations that has not been observed with Suzaku. A comparison of the extended atmosphere in the filament and off-filament pointings will allow us to test for the presence of unresolved gas clumps, which should be more abundant along the filament, invoked to explain anomalously high (above cosmic) baryon fractions observed in some other clusters. If this "unresolved clumps" hypothesis is correct, then we should find higher baryon fractions along the filament. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SCOTT RANDALL | USA | 9 | AO9 | EXPLORING THE EXTENDED ATMOSPHERE OF THE STRONGLY MERGING CLUSTER ABELL 98 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809078030/ | Quick Look | ![]() |
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817 | SWCL1313+0802 | 198.2492 | 8.0414 | 197.620834 | 8.306256 | 193.672615 | 14.576147 | 318.90135946 | 70.24184099 | 291.5304 | 56850.0041435185 | 2014-07-12 00:05:58 | 56850.5002199074 | 2014-07-12 12:00:19 | 809087010 | 20.2705 | 20 | 20.2705 | 20.2705 | 0 | 20.2705 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3782986111 | 2016-08-15 09:04:45 | 57229 | 2015-07-26 00:00:00 | 56861.6452083333 | 2014-07-23 15:29:06 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091531 | The evolution of X-ray properties of galaxy clusters with redshift provides important constraints on the self-similar models of cluster evolution. The scaling relations and their deviations from self-similar models due to non-gravitational processes are important for modeling the cluster selection function for cosmology. We propose to observe a uniform sample of z ~ 0.6 galaxy clusters, selected from Swift archival data and confirmed by multi-band optical data, using Suzaku to better characterize their X-ray properties such as the X-ray luminosity and temperature. With this uniformly selected sample from a narrow redshift bin, we are able to independently constrain the self-similar evolution of cluster properties with redshift. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | XINYU DAI | USA | 9 | AO9 | X-RAY PROPERTIES OF A UNIFORMLY SELECTED SAMPLE OF Z ~ 0.6 CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809087010/ | Quick Look | ![]() |
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818 | SWCL1330+4206 | 202.7226 | 42.119 | 202.178472 | 42.376237 | 179.66908 | 46.823596 | 97.20252966 | 72.98152353 | 144.6477 | 56984.0225347222 | 2014-11-23 00:32:27 | 56985.3840740741 | 2014-11-24 09:13:04 | 809088010 | 15.8612 | 49 | 15.8612 | 15.8776 | 0 | 15.8692 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8069212963 | 2016-08-16 19:21:58 | 57548 | 2016-06-09 00:00:00 | 57009.4143981482 | 2014-12-18 09:56:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091531 | The evolution of X-ray properties of galaxy clusters with redshift provides important constraints on the self-similar models of cluster evolution. The scaling relations and their deviations from self-similar models due to non-gravitational processes are important for modeling the cluster selection function for cosmology. We propose to observe a uniform sample of z ~ 0.6 galaxy clusters, selected from Swift archival data and confirmed by multi-band optical data, using Suzaku to better characterize their X-ray properties such as the X-ray luminosity and temperature. With this uniformly selected sample from a narrow redshift bin, we are able to independently constrain the self-similar evolution of cluster properties with redshift. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | XINYU DAI | USA | 9 | AO9 | X-RAY PROPERTIES OF A UNIFORMLY SELECTED SAMPLE OF Z ~ 0.6 CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809088010/ | Quick Look | ![]() |
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819 | 4U1700-37 | 255.9894 | -37.8441 | 255.139416 | -37.774677 | 258.577099 | -14.956185 | 347.75582102 | 2.17172645 | 269.6945 | 53991.447662037 | 2006-09-13 10:44:38 | 53992.918912037 | 2006-09-14 22:03:14 | 401058010 | 81.4425 | 80 | 81.4569 | 81.4704 | 81.4425 | 81.4544 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 82.1093 | 82.1093 | 127.109 | 1 | PROCESSED | 57535.6097916667 | 2016-05-27 14:38:06 | 54526 | 2008-03-01 00:00:00 | 54053.5428240741 | 2006-11-14 13:01:40 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011135 | The compact object in the massive X-ray binary 4U1700-37/HD153919 has been inferred to be a neutron star based on its spectral shape, but no pulsations have been observed. One possible explanation for the absence of observed pulsations is that the pulsed signal is beamed in directions other than our line of sight. This can be tested using Suzaku by searching for pulsations in the iron K line. This line is formed efficiently under almost all conditions of ionization and temperature, and so represents an X-ray bolometer which should respond to pulsed X-rays no matter where they are pointed. We plan to make such a search, and to probe the other properties of the wind and compact object in this system by observing with Suzaku for 80 ks away from eclipse. | GALACTIC POINT SOURCES | 4 | A | TIMOTHY KALLMAN | USA | 1 | AO1 | IRON LINE VARIABILITY IN 4U1700-37 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401058010/ | Quick Look | ![]() |
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820 | SERPENS X-1 | 279.9934 | 5.0285 | 279.376671 | 4.981655 | 281.288405 | 28.078275 | 36.11311789 | 4.83561165 | 256.1423 | 54032.2853819444 | 2006-10-24 06:50:57 | 54033.2259143518 | 2006-10-25 05:25:19 | 401048010 | 37.1578 | 37 | 37.1578 | 37.2698 | 37.2058 | 37.1658 | 2 | 1 | 2 | 2 | 1 | 0 | 0 | 31.0695 | 31.0695 | 81.2399 | 2 | PROCESSED | 57535.9734722222 | 2016-05-27 23:21:48 | 54526 | 2008-03-01 00:00:00 | 54056.4719328704 | 2006-11-17 11:19:35 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011113 | The potential well around low-magnetic field neutron stars is very similar to that around Schwarzschild black holes. Doppler shifts expected at the inner disk around such neutron stars should be very similar, and should produce relativistic FeK-alpha emission lines like those observed in some black hole systems. To date, however, relativistically broadened FeK-alpha emission lines have not been clearly detected in neutron star systems, in part because their lines are generally weaker than those found in black hole systems. We propose to observe the neutron star binaries 4U 1820-30, Cygnus X-2, and Serpens X-1 for 37 ksec each in Suzaku Cycle 1, to confirm possible evidence of relativistic broadening. Relativistic phenomena and accretion studies are central to NASA's ``SEU'' theme. | GALACTIC POINT SOURCES | 4 | B | JON MILLER | USA | 1 | AO1 | A SUZAKU STUDY OF BROAD IRON LINES IN NEUTRON STAR BINARIES | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401048010/ | Quick Look | ![]() |
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821 | 4U 1636-536 | 250.2273 | -53.7542 | 249.230886 | -53.657708 | 256.461437 | -31.236858 | 332.91122007 | -4.81806999 | 91.2447 | 54153.2955787037 | 2007-02-22 07:05:38 | 54154.3544560185 | 2007-02-23 08:30:25 | 401050020 | 40.096 | 38 | 40.096 | 40.104 | 0 | 40.096 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 35.55 | 35.55 | 91.4779 | 0 | PROCESSED | 57537.4821990741 | 2016-05-29 11:34:22 | 54525 | 2008-02-29 00:00:00 | 54158.392037037 | 2007-02-27 09:24:32 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011117 | Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. | GALACTIC POINT SOURCES | 4 | A | JEROEN HOMAN | USA | 1 | AO1 | THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401050020/ | Quick Look | ![]() |
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822 | IGRJ16493-4348 | 252.3173 | -43.8652 | 251.422595 | -43.77854 | 256.400238 | -21.254215 | 341.31911758 | 0.57823277 | 287.444 | 54013.8822916667 | 2006-10-05 21:10:30 | 54014.4204166667 | 2006-10-06 10:05:24 | 401054010 | 21.1998 | 20 | 21.2158 | 21.2158 | 21.1998 | 21.2078 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 20.2197 | 20.2197 | 46.4639 | 1 | PROCESSED | 57535.7818634259 | 2016-05-27 18:45:53 | 54695 | 2008-08-17 00:00:00 | 54025.4796412037 | 2006-10-17 11:30:41 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011132 | INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. | GALACTIC POINT SOURCES | 4 | A | RANDALL SMITH | USA | 1 | AO1 | HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401054010/ | Quick Look | ![]() |
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823 | OJ 287 | 133.7046 | 20.1043 | 132.989527 | 20.295378 | 130.505611 | 2.596765 | 206.8173824 | 35.82032681 | 285.8742 | 57145.5508449074 | 2015-05-03 13:13:13 | 57148.4467592593 | 2015-05-06 10:43:20 | 710011010 | 111.6388 | 323 | 111.6388 | 111.6388 | 0 | 111.6388 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.1122800926 | 2016-08-18 02:41:41 | 57113 | 2015-04-01 00:00:00 | 57164.5257523148 | 2015-05-22 12:37:05 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 101431 | Kepler will observe OJ 287 with 1 min sampling and >90% duty cycle for ~75 days in 2015, providing an unprecedented opportunity to quantitatively compare optical and X-ray variations in one of the brightest and most active blazars in the sky. We request continuous Suzaku coverage for 128 orbits (323 ks) in a simultaneous campaign including XMM, Swift, radio and multi-color optical monitoring. Suzaku samples key intermediate timescales of hours-days, allowing measurement of CCFs and PSDs spanning a wide range of temporal frequencies. These will be used to test models and determine source parameters e.g. if the X-rays are due to synchrotron-self Compton the optical should lead the X-rays by ~1 day, but if they are "synchrotron flashes" the bands should vary nearly simultaneously. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | RICK EDELSON | USA | 10 | AO10 | SIMULTANEOUS SUZAKU/KEPLER/MULTIWAVELENGTH MONITORING OF OJ 287 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710011010/ | Quick Look | ![]() |
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824 | CYG X-1 | 299.5792 | 35.2719 | 299.109639 | 35.135474 | 313.688752 | 54.318748 | 71.39034122 | 3.11120593 | 84.3565 | 54220.8163657407 | 2007-04-30 19:35:34 | 54221.783587963 | 2007-05-01 18:48:22 | 402072010 | 45.3204 | 30 | 45.3204 | 45.3284 | 0 | 45.3204 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 40.1873 | 40.1873 | 83.566 | 2 | PROCESSED | 57538.518275463 | 2016-05-30 12:26:19 | 54773 | 2008-11-03 00:00:00 | 54228.1718518518 | 2007-05-08 04:07:28 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021133 | We request two additional 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku will bring three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 200-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history. | GALACTIC POINT SOURCES | 4 | A | MICHAEL NOWAK | USA | 2 | AO2 | CONTINUING TO ENHANCE THE LONG TERM MONITORING CAMPAIGN OF CYGNUS X-1 IN THE SUZAKU ERA | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402072010/ | Quick Look | ![]() |
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825 | SWIFT J1753.5-0127 | 268.3714 | -1.4588 | 267.723576 | -1.449322 | 268.234398 | 21.971701 | 24.89300861 | 12.1795145 | 261.3846 | 54362.8585185185 | 2007-09-19 20:36:16 | 54365.4377777778 | 2007-09-22 10:30:24 | 402088010 | 94.6005 | 93 | 94.6085 | 94.6165 | 0 | 94.6005 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81.739 | 81.739 | 222.836 | 3 | PROCESSED | 57540.1123842593 | 2016-06-01 02:41:50 | 54743 | 2008-10-04 00:00:00 | 54371.6366319444 | 2007-09-28 15:16:45 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021147 | While the spectrally hard state represents the most common mode of accretion in black hole X-ray binaries, the nature of its accretion flow is poorly understood. We recently discovered cool accretion disks extending close to the innermost stable circular orbit in the hard states of two black hole transients. Such disks could give rise to strong reflection features, but instead these are weak or not detected. We propose a 70 ks Suzaku observation of Swift J1753.5-0127 (one of the two transients), which is currently in a prolonged hard state. Our goal is to put tight constraints on the strength of the reflection features and increase our understanding of the geometry of the spectrally hard component. Understanding accretion onto compact objects is fundamental to NASA's "SEU" theme. | GALACTIC POINT SOURCES | 4 | A | JEROEN HOMAN | USA | 2 | AO2 | CONSTRAINING REFLECTION FEATURES IN THE HARD STATE OF BLACK HOLE X-RAY BINARIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402088010/ | Quick Look | ![]() |
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826 | TAU SCO | 248.9733 | -28.218 | 248.193759 | -28.116325 | 251.450612 | -6.120226 | 351.53478934 | 12.80506422 | 280.0312 | 54729.4179398148 | 2008-09-20 10:01:50 | 54729.7578009259 | 2008-09-20 18:11:14 | 403034040 | 13.9711 | 10 | 13.9711 | 13.9711 | 0 | 13.9711 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.8912 | 12.8912 | 29.35 | 0 | PROCESSED | 57543.857974537 | 2016-06-04 20:35:29 | 55148 | 2009-11-13 00:00:00 | 54780.4954050926 | 2008-11-10 11:53:23 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031121 | We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars. | GALACTIC POINT SOURCES | 4 | A | RICHARD IGNACE | USA | 3 | AO3 | X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403034040/ | Quick Look | ![]() |
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827 | TAU SCO | 248.9731 | -28.2173 | 248.193563 | -28.115624 | 251.450335 | -6.119558 | 351.53521528 | 12.80565459 | 288.7028 | 54717.0750115741 | 2008-09-08 01:48:01 | 54717.3752777778 | 2008-09-08 09:00:24 | 403034020 | 14.5215 | 10 | 14.5295 | 14.5215 | 0 | 14.5375 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.6524 | 9.6524 | 25.9359 | 1 | PROCESSED | 57543.7784606482 | 2016-06-04 18:40:59 | 55148 | 2009-11-13 00:00:00 | 54780.6118171296 | 2008-11-10 14:41:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031121 | We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars. | GALACTIC POINT SOURCES | 4 | A | RICHARD IGNACE | USA | 3 | AO3 | X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403034020/ | Quick Look | ![]() |
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828 | M101 | 210.8841 | 54.3679 | 210.442342 | 54.607302 | 174.405989 | 59.838606 | 101.97854462 | 59.72940376 | 150.2959 | 54062.5790625 | 2006-11-23 13:53:51 | 54064.7182175926 | 2006-11-25 17:14:14 | 801063010 | 98.8522 | 100 | 98.8762 | 98.8522 | 0 | 98.8762 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89.6125 | 89.6125 | 184.802 | 2 | PROCESSED | 57536.2145486111 | 2016-05-28 05:08:57 | 54455 | 2007-12-21 00:00:00 | 54088.707650463 | 2006-12-19 16:59:01 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011402 | We wish to obtain a Suzaku spectrum of the diffuse X-ray emission in a typical galactic disk. The spectral resolution obtainable with Chandra/XMM does not allow the decomposition of the spectrum into more than two thermal components. The higher spectral resolution, better soft response, and lower instrumental background of Suzaku will allow the decomposition into at least three thermal components, and will place constraints on the number of thermal components and the distribution of temperatures and emission measures. The more refined fitting allowed by Suzaku spectra will allow a greater understanding of the sources of the X-ray emission. Given the Suzaku spatial resolution and detector size, M101 is the best observable example of a "typical" galactic disk. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | K. KUNTZ | USA | 1 | AO1 | SOFT DIFFUSE X-RAY EMISSION FROM M101 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801063010/ | Quick Look | ![]() |
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829 | YY MEN | 74.6207 | -75.281 | 75.005816 | -75.353979 | 292.803657 | -80.004198 | 287.41045099 | -33.23069192 | 7.2587 | 54996.0772916667 | 2009-06-14 01:51:18 | 54998.5606365741 | 2009-06-16 13:27:19 | 404036010 | 106.9498 | 100 | 106.9578 | 106.9578 | 0 | 106.9498 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 104.0902 | 104.0902 | 214.5398 | 0 | PROCESSED | 57547.6240393518 | 2016-06-08 14:58:37 | 55378 | 2010-07-01 00:00:00 | 55008.2997106482 | 2009-06-26 07:11:35 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041202 | The single K giant YY Men is one of the most active stars within 300 pc of the Sun, having produced 2 of the most powerful radio flares and 1 of the most powerful and long-duration optical flares ever detected. Its corona is one of the hottest and brightest known, with a *typical* X-ray luminosity of 32.0-32.5 (log erg/s) which most other cool stars only reach during major flares. We propose to obtain a 100-ksec observation of this hyperactive star to get a high S/N XIS exposure of its spectrum, particularly in the 5-10 keV region in which the XIS excels. We will study the He- and H-like Fe lines, search for 6.4 keV fluorescent emission, search for the presence of ultrahigh temperature and nonthermal spectral components, and look for correlations with simultaneous ATCA radio observations. | GALACTIC POINT SOURCES | 4 | B | STEPHEN DRAKE | USA | 4 | AO4 | THE EXTREME CORONAL PROPERTIES OF THE HYPERACTIVE K GIANT YY MEN | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404036010/ | Quick Look | ![]() |
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830 | T PYXIDIS | 136.1704 | -32.3688 | 135.652133 | -32.168809 | 152.023797 | -46.371088 | 257.19727302 | 9.71237496 | 121.9943 | 56266.272662037 | 2012-12-05 06:32:38 | 56268.8695486111 | 2012-12-07 20:52:09 | 407048010 | 86.676 | 100 | 86.676 | 86.676 | 0 | 86.676 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 73.6118 | 73.6118 | 224.3579 | 4 | PROCESSED | 57608.249525463 | 2016-08-08 05:59:19 | 56660 | 2014-01-03 00:00:00 | 56291.8230787037 | 2012-12-30 19:45:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071213 | We propose a 100 ks observation of the classical nova remnant in the accreting binary system T Pyxidis using Suzaku. T Pyxidis is a system which causes a cycle of classical nova outbursts in a decade time scale. Shocks might occur in the ejecta, and X-rays were detected from its spatially-resolved expanding shell like a miniature supernova remnant. The immediate purposes of this program are (1) to derive the X-ray flux and luminosity after its last outburst in 2011, (2) to diagnose plasma temperature deeply, and (3) to obtain the second sample of non-thermal X-ray emission from classical nova remnants. The target is a remarkable newly discovered candidate of cosmic-ray acceleration sites, and a successful detection of non-thermal X-rays provides a new view of cosmic-ray origins. | GALACTIC POINT SOURCES | 4 | C | DAI TAKEI | USA | 7 | AO7 | COSMIC-RAYS FROM MINIATURE SUPERNOVA REMNANTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407048010/ | Quick Look | ![]() |
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831 | HERCULES X-1 | 254.4605 | 35.3288 | 254.009904 | 35.404408 | 245.996246 | 57.479663 | 58.13264186 | 37.51848299 | 268.3999 | 56192.1811342593 | 2012-09-22 04:20:50 | 56192.781412037 | 2012-09-22 18:45:14 | 407051020 | 22.6094 | 20 | 22.6094 | 22.6094 | 0 | 22.6094 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 20.1787 | 20.1787 | 51.836 | 1 | PROCESSED | 57607.16 | 2016-08-07 03:50:24 | 56590 | 2013-10-25 00:00:00 | 56218.5726967593 | 2012-10-18 13:44:41 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071224 | This proposal is for the continuation of successful Suzaku observations of Her X-1. The proposal is led by the NuSTAR team, extended with experts on X-ray binary pulsars with cyclotron lines. We propose three 20 ks simultaneous Suzaku and NuSTAR observations of Her X-1. Joint observations will substantial increase the science that can be addressed, allowing a systematic study of the fundamental cyclotron line (~40 keV) as a function of time, X-ray flux, 35 day phase, and 1.24 s pulse phase. The combined data will probe fundamental physics in this system, including the structure of the magnetic field in the polar caps, the physics of sub-Eddington accretion, and physical processes inside the neutron star. | GALACTIC POINT SOURCES | 4 | B | BRIAN GREFENSTETTE | USA | 7 | AO7 | STUDY OF THE CYCLOTRON LINE FEATURE IN HERCULES X-1: THE PROFILE AND THE SHORT- AND LONG-TERM VARIABILITY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407051020/ | Quick Look | ![]() |
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832 | NGC 1553 | 64.0253 | -55.7788 | 63.753175 | -55.901382 | 28.715493 | -73.694617 | 265.63371114 | -43.7014546 | 176.9406 | 54429.7042939815 | 2007-11-25 16:54:11 | 54431.9029976852 | 2007-11-27 21:40:19 | 802050010 | 98.7222 | 95 | 98.7222 | 98.7222 | 0 | 98.7222 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 87.7903 | 87.7903 | 189.9159 | 2 | PROCESSED | 57540.6454976852 | 2016-06-01 15:29:31 | 54806 | 2008-12-06 00:00:00 | 54438.4258101852 | 2007-12-04 10:13:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021401 | As driving engines of metal enrichment, early-type galaxies provide vital laboratories to investigate how it operates. In our Chandra survey of galaxies, we found solar ISM abundances (Zfe), similar to the stars and implying enrichment homology from clusters to moderate-Lx galaxies. The only outlier was NGC1553, for which we found a tantalizing hint of very subsolar Zfe, inconsistent with simple models. Unlike other galaxies with recent reports of low Zfe, NGC1553 has a bright gas halo, so the results are insensitive to the modelling of unresolved LMXB. We propose an 80ks observation of NGC1553 to measure definitively the ISM abundances of Fe and other crucial diagnostic elements. These data will either confirm enrichment bimodality or provide a vital low-Lx data-point to anchor models. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | PHILIP HUMPHREY | USA | 2 | AO2 | NGC 1553: PROOF OF BIMODAL METAL ENRICHMENT? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802050010/ | Quick Look | ![]() |
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833 | BOOTES GROUP 7 | 217.7796 | 35.0938 | 217.258508 | 35.314562 | 199.66622 | 46.620571 | 59.62119131 | 67.30227758 | 316.719 | 54266.3117592593 | 2007-06-15 07:28:56 | 54267.3863310185 | 2007-06-16 09:16:19 | 802053010 | 42.1244 | 38 | 42.1324 | 42.1244 | 0 | 42.1324 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.3384 | 37.3384 | 92.8238 | 0 | PROCESSED | 57538.9915509259 | 2016-05-30 23:47:50 | 54695 | 2008-08-17 00:00:00 | 54322.4630324074 | 2007-08-10 11:06:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021424 | We propose four 30 ksec Suzaku pointings (120 ksec total) to obtain Lx and Tx for 4 distant (0.15 < z < 0.35) galaxy groups discovered in a contiguous, 9.3 sq. deg Chandra survey in Bootes. Our targets are spatially resolved by Chandra and are chosen to minimize point-source contamination of the Suzaku group spectra. The XIS data will significantly expand the sample of groups with known temperature in this redshift range, and so will improve constraints on group evolution mechanisms. We will use the existing, deep multicolor imaging and 20,000-object spectroscopic catalog for Bootes to study the effect of local environment on group properties, as well as the relationship between optically-selected and X-ray selected groups, for the first time in this redshift range. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MARSHALL BAUTZ | USA | 2 | AO2 | SUZAKU SPECTROSCOPY OF DISTANT GALAXY GROUPS IN BOOTES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802053010/ | Quick Look | ![]() |
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834 | ABELL 2029 | 227.4644 | 6.0238 | 226.845557 | 6.213105 | 223.157402 | 22.814931 | 6.57368779 | 50.92713703 | 112.4532 | 54473.6848958333 | 2008-01-08 16:26:15 | 54478.0211226852 | 2008-01-13 00:30:25 | 802060010 | 169.2861 | 160 | 169.2861 | 169.2861 | 0 | 169.2861 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 150.7661 | 150.7661 | 374.6201 | 4 | PROCESSED | 57541.3859953704 | 2016-06-02 09:15:50 | 54860 | 2009-01-29 00:00:00 | 54490.7163657407 | 2008-01-25 17:11:34 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021433 | The properties of clusters of galaxies in very distant regions encompassing the virial radius (r_vir) are poorly understood yet these regions are sites of very important processes for the cluster formation and evolution. The recent generation of X-ray satellites (Chandra and XMM) thanks to their fine spatial resolution and high sensitivity have provided so far detailed spectral information mainly in the inner bright regions but they have not been very helpful in background dominated regimes typical of cluster outskirts' observations because of their high background. Suzaku has the capabilities to target those regions. We propose to observe the outskirts of the very relaxed cluster of galaxies A2029 with XIS to measure for the first time temperature and metallicity of the ICM up to r_vir. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | LUCA ZAPPACOSTA | USA | 2 | AO2 | EXPLORING THE OUTSKIRTS OF THE RELAXED CLUSTER ABELL 2029 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802060010/ | Quick Look | ![]() |
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835 | ABEL 754 | 137.2113 | -9.6361 | 136.602656 | -9.432794 | 142.867226 | -24.832228 | 239.25284371 | 24.7578079 | 295.1878 | 54249.7445833333 | 2007-05-29 17:52:12 | 54252.4495949074 | 2007-06-01 10:47:25 | 802063010 | 108.9779 | 100 | 108.9859 | 108.9859 | 0 | 108.9779 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 97.904 | 97.904 | 233.6958 | 2 | PROCESSED | 57538.8549537037 | 2016-05-30 20:31:08 | 54773 | 2008-11-03 00:00:00 | 54257.5596759259 | 2007-06-06 13:25:56 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021445 | We propose a 100 ksec observation of Abell 754 and a 50 ksec observation of Triangulum Australis, in order to measure the spectral shape and flux of possible nonthermal emission from clusters of galaxies. They are bright clusters of galaxies in the BAT all sky survey sample, which is crucial for making good spectral measurements by the HXD. And their spectra have a significant hard excess (power-law component). We intend to constrain the power-law photon index of the nonthermal emission for the first time and to determine the size of hard X-ray emitting region by using both of the HXD and Swift BAT data. We are aiming to test the origin of the hard flux and see whether it originates from either diffuse inverse Compton scattering by relativistic cosmic-ray electrons or an AGN. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TAKASHI OKAJIMA | USA | 2 | AO2 | OBSERVATIONS OF NONTHERMAL EMISSION FROM CLUSTERS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802063010/ | Quick Look | ![]() |
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836 | RCS 1122+2423 | 170.6071 | 24.3899 | 169.945012 | 24.664262 | 161.499487 | 18.645294 | 215.72830536 | 69.79971375 | 120.0624 | 54421.3268518518 | 2007-11-17 07:50:40 | 54421.8891087963 | 2007-11-17 21:20:19 | 802070010 | 20.9729 | 18 | 20.9809 | 20.9809 | 0 | 20.9729 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.022 | 19.022 | 48.5679 | 0 | PROCESSED | 57540.5406828704 | 2016-06-01 12:58:35 | 54797 | 2008-11-27 00:00:00 | 54430.3244097222 | 2007-11-26 07:47:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021451 | We propose Suzaku observations of a sample of 10 galaxy clusters at redshifts between 0.6 and 0.95 from the RCS-1 cluster survey. These objects represent the optically richest clusters at these redshifts from the 100 square degree survey using the red-sequence method of cluster detection. As such, they form a critical sample for calibrating the mass-richness relationship for high redshift cluster surveys. Our proposed observations will allow us to determine their X-ray luminosities, as a first guide to estimating their masses, and enable future studies to determine accurate masses from their X-ray properties. These studies are complimentary to mass calibration programs we are carrying out using estimates based on lensing, IR stellar mass and galaxy dynamics. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 2 | AO2 | A SUZAKU SNAPSHOT SURVEY OF HIGH-REDSHIFT GALAXY CLUSTERS FROM THE RCS SURVEY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802070010/ | Quick Look | ![]() |
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837 | RCW86 SW | 220.2761 | -62.6782 | 219.292066 | -62.464185 | 240.754321 | -44.190898 | 315.14426109 | -2.43598628 | 109.6929 | 53778.0961689815 | 2006-02-12 02:18:29 | 53780.2814699074 | 2006-02-14 06:45:19 | 500004010 | 100.7659 | 100 | 100.7819 | 100.7659 | 100.7819 | 100.7819 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 90.6819 | 90.6819 | 188.7918 | 2 | PROCESSED | 57533.035787037 | 2016-05-25 00:51:32 | 54247 | 2007-05-27 00:00:00 | 54041.2835648148 | 2006-11-02 06:48:20 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001019 | The supernova remnants (SNRs) are most convincing candidates for the acceleration of cosmic-rays. Together with the TeV gamma-ray detection by CANGAROO and HESS, it is now confirmed that at least some of the SNRs can actually accelerate electrons up to > 10 TeV. However, such studies have not provided direct information on ``protons'', which is the major component of cosmic-rays. Here we propose to measure spatial distribution of accelerated protons in the shell of RCW 86, and its association with the high energy (>10 TeV) electrons which emit synchrotron X-rays up to 50 keV. Large effective area and the good detection capability of Suzaku will be ideal tools for our scientific goal. | GALACTIC DIFFUSE EMISSION | 5 | A | JUN KATAOKA | JAP | 0 | SWG | THE FIRST DIRECT MAPPING OF ACCELERATED PROTONS IN THE SW SHELL OF RCW 86 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500004010/ | Quick Look | ![]() |
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838 | 73P/SW3 | 279.2884 | 33.5067 | 278.829487 | 33.462856 | 284.096243 | 56.493773 | 62.26395264 | 17.33399104 | 47.3721 | 53862.3946875 | 2006-05-07 09:28:21 | 53862.4794444444 | 2006-05-07 11:30:24 | 500012010 | 3.25 | 5 | 3.25 | 3.25 | 3.25 | 3.25 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.3139 | 2.3139 | 7.304 | 0 | PROCESSED | 57533.6418402778 | 2016-05-25 15:24:15 | 54256 | 2007-06-05 00:00:00 | 54042.1755671296 | 2006-11-03 04:12:49 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500012010/ | Quick Look | ![]() |
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839 | N154 SB | 84.0182 | -69.641 | 84.124614 | -69.669786 | 303.069824 | -86.201105 | 280.12884425 | -31.83619967 | 313.3253 | 54583.7906944444 | 2008-04-27 18:58:36 | 54584.7849305556 | 2008-04-28 18:50:18 | 803037010 | 50.404 | 40 | 50.404 | 50.404 | 0 | 50.404 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 56.6171 | 56.6171 | 85.8878 | 1 | PROCESSED | 57542.411724537 | 2016-06-03 09:52:53 | 54964 | 2009-05-13 00:00:00 | 54598.4914699074 | 2008-05-12 11:47:43 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031238 | Clusters of massive stars, through their stellar winds and supernovae, form large diffuse structures known as superbubbles (SBs), which play an essential role in shaping the local interstellar medium. Most SB models indicate that these objects should be dominated by thermal plasma processes. However, observations of 3 SBs have detected significant nonthermal contributions to their X-ray emission, which raises many questions. Is it generated by synchrotron, inverse-Compton, or nonthermal Bremsstrahlung processes? Are colliding stellar winds or internal supernova remnants responsible? We therefore propose to examine the X-ray emission from 3 X-ray bright SBs, to search for nonthermal X-ray emission, and if possible place strong constraints on the source of this emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | LARRY MADDOX | USA | 3 | AO3 | A SEARCH FOR NONTHERMAL X-RAY EMISSION FROM SUPERBUBBLES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803037010/ | Quick Look | ![]() |
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840 | NGC 5846 | 226.6234 | 1.6025 | 225.988646 | 1.794814 | 223.667836 | 18.340527 | 0.42380195 | 48.79350498 | 287.2336 | 54675.6192939815 | 2008-07-28 14:51:47 | 54679.0008564815 | 2008-08-01 00:01:14 | 803042010 | 155.9331 | 150 | 155.9331 | 155.9331 | 0 | 155.9331 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 145.4704 | 145.4704 | 292.1519 | 2 | PROCESSED | 57543.2487152778 | 2016-06-04 05:58:09 | 55059 | 2009-08-16 00:00:00 | 54693.5527546296 | 2008-08-15 13:15:58 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031404 | We propose Suzaku observations of three elliptical galaxies, selected on brightness and the availability of XMM-Newton RGS data, as part of a program to investigate their star formation history and chemical evolution via abundance studies of the hot interstellar medium. The low-energy sensitivity, spectral resolution, and low background of the Suzaku XIS enables the first accurate model-independent measurements of the abundance pattern while expanding the number of measurable temperature diagnostic features. Analysis of XIS spectra (critically, with SCI on), exclusively and in combination with RGS data, demonstrates the unique power of Suzaku to contribute to our understanding of the thermal and chemical properties of these systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MICHAEL LOEWENSTEIN | USA | 3 | AO3 | UNCOVERING THE TRUE ABUNDANCES OF ELLIPTICAL GALAXIES WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803042010/ | Quick Look | ![]() |
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841 | A496 P-OUT | 68.2513 | -13.0087 | 67.67058 | -13.113188 | 64.018052 | -34.510238 | 209.22191803 | -36.52315476 | 62.0525 | 54674.5225347222 | 2008-07-27 12:32:27 | 54675.6050231482 | 2008-07-28 14:31:14 | 803048010 | 37.5516 | 35 | 37.5516 | 37.5596 | 0 | 37.5596 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33.1599 | 33.1599 | 93.4939 | 1 | PROCESSED | 57543.1577314815 | 2016-06-04 03:47:08 | 55055 | 2009-08-12 00:00:00 | 54689.4360416667 | 2008-08-11 10:27:54 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031424 | A496 is a "normal" nearby cluster that has been the testbed for metal enrichment models in clusters and, more recently, of different mechanisms to generate cold fronts. Suzaku's excellent spectral resolution, low background and high effective area, combined with the moderate temperatures of this cluster allows us to probe, with two short exposures, into the large scale metal enrichment processes through determination of elemental abundance ratios out to half the virial radius for the first time. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | RENATO DUPKE | USA | 3 | AO3 | LARGE SCALE METAL ENRICHMENT MECHANISMS IN ABELL 496 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803048010/ | Quick Look | ![]() |
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842 | SNR G106.3+2.7 P2 | 336.9121 | 60.9439 | 336.468568 | 60.688281 | 21.166616 | 61.378787 | 106.34649405 | 2.79001657 | 12.2687 | 55423.4230787037 | 2010-08-15 10:09:14 | 55424.0209837963 | 2010-08-16 00:30:13 | 505072010 | 24.5562 | 50 | 24.5722 | 24.5562 | 0 | 24.5722 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 26.6147 | 26.6147 | 51.6559 | 1 | PROCESSED | 57553.084212963 | 2016-06-14 02:01:16 | 55807 | 2011-09-03 00:00:00 | 55441.2685069444 | 2010-09-02 06:26:39 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051305 | After two decades searching for the origin of the GeV emission from 3EG J2227+6122, it is now identified with PSR J2229+6114 and its PWN.~This highly energetic young pulsar lies within the arcmin diameter Boomerang radio nebula. Now, recently discovered nearby extended TeV emission suggest a second Vela-like "cocoon" feed by relic electrons from the PWN, blowing out the vast degree-scale radio feature.~Interactions of the SNR shock front with overlapping molecular cloud material can also contribute in the gamma-ray production.~An XIS mosaic will allow us to search for soft and hard X-ray emission similar to Vela's "Cocoon" and resolve the nature of the TeV emission and its connection to the Boomerang and the radio feature. | GALACTIC DIFFUSE EMISSION | 5 | C | ESTER ALIU | USA | 5 | AO5 | ORIGIN OF THE VHE GAMMA-RAY EMISSION FROM SNR G106.3+2.7 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505072010/ | Quick Look | ![]() |
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843 | CARINA SW | 160.2531 | -60.104 | 159.777159 | -59.842292 | 202.080754 | -59.579426 | 287.34811018 | -1.23919183 | 109.6766 | 55542.7308333333 | 2010-12-12 17:32:24 | 55543.4438888889 | 2010-12-13 10:39:12 | 505075010 | 47.0039 | 45 | 47.0039 | 47.0119 | 0 | 47.0119 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 42.4341 | 42.4341 | 61.5999 | 0 | PROCESSED | 57554.3916435185 | 2016-06-15 09:23:58 | 55960 | 2012-02-03 00:00:00 | 55592.9230324074 | 2011-01-31 22:09:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051312 | X-ray nebulae with kT =0.1-0.8 keV, log Lx up to 35 ergs/s, and size of 1-1000 pc accompany a number of giant HII region. The Carinae Nebula is the best region to study their origin with 10-100 times more luminous soft X-rays than any other giant HII regions in our Galaxy. X-ray observations especially with Suzaku revealed that a part, or all, of the diffuse plasma would heat up by earlier supernova explosions, but it is unknown when these explosions occurred and how they made the current X-ray nebula. The Chandra Carina Complex Project displayed that the southern part of the nebula emits strong hydrogen-like oxygen line. We will measure helium-like oxygen line with Suzaku to measure its plasma temperature and abundance to help understand relation with plasma in the nebula center. | GALACTIC DIFFUSE EMISSION | 5 | C | KENJI HAMAGUCHI | USA | 5 | AO5 | SOUTHERN PART OF DIFFUSE PLASMA IN THE CARINA NEBULA - RICH IN OXYGEN? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505075010/ | Quick Look | ![]() |
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844 | RCS2347-3535 | 356.9535 | -35.5892 | 356.30102 | -35.867184 | 341.527794 | -31.116965 | 357.03141214 | -74.03003146 | 61.6856 | 54617.4612384259 | 2008-05-31 11:04:11 | 54617.8890509259 | 2008-05-31 21:20:14 | 803057010 | 15.4812 | 11 | 15.4892 | 15.4892 | 0 | 15.4812 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.6376 | 14.6376 | 36.9599 | 0 | PROCESSED | 57542.6853703704 | 2016-06-03 16:26:56 | 54999 | 2009-06-17 00:00:00 | 54633.6966087963 | 2008-06-16 16:43:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031441 | Comparisons between moderate-z X-ray and high-z optically selected clusters indicate that the latter have lower Lx than expected for a given Tx, however it is hard to tell if such discrepancies are due to cluster evolution or selection effects. In an attempt to isolate these two variables, we propose the first detailed comparison of X-ray and optically selected clusters that are well-matched in both velocity dispersion (a quantity independent of both methods) and redshift. Our X-ray analysis of X-ray selected CNOC clusters is complete. Here we propose to determine Lx, Tx, and gas distribution/morphology for an optically selected sample, most of which already have velocity dispersion data in hand, enabling rigorous quantitative comparisons between physical characteristics of the two groups. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 3 | AO3 | COSMOLOGY WITH CLUSTERS: CONSTRAINING PHYSICAL DIFFERENCES BETWEEN X-RAY AND OPTICALLY SELECTED SAMPLES AT MODERATE-Z | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803057010/ | Quick Look | ![]() |
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845 | RCS1102-0340 | 165.6613 | -3.6697 | 165.025025 | -3.400357 | 168.238102 | -9.034138 | 258.27932815 | 49.53254853 | 114.238 | 54817.9779282407 | 2008-12-17 23:28:13 | 54818.8987731482 | 2008-12-18 21:34:14 | 803064010 | 37.789 | 28 | 37.797 | 37.797 | 0 | 37.789 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.621 | 27.621 | 79.55 | 1 | PROCESSED | 57545.0002893518 | 2016-06-06 00:00:25 | 55206 | 2010-01-10 00:00:00 | 54840.5080439815 | 2009-01-09 12:11:35 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031441 | Comparisons between moderate-z X-ray and high-z optically selected clusters indicate that the latter have lower Lx than expected for a given Tx, however it is hard to tell if such discrepancies are due to cluster evolution or selection effects. In an attempt to isolate these two variables, we propose the first detailed comparison of X-ray and optically selected clusters that are well-matched in both velocity dispersion (a quantity independent of both methods) and redshift. Our X-ray analysis of X-ray selected CNOC clusters is complete. Here we propose to determine Lx, Tx, and gas distribution/morphology for an optically selected sample, most of which already have velocity dispersion data in hand, enabling rigorous quantitative comparisons between physical characteristics of the two groups. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 3 | AO3 | COSMOLOGY WITH CLUSTERS: CONSTRAINING PHYSICAL DIFFERENCES BETWEEN X-RAY AND OPTICALLY SELECTED SAMPLES AT MODERATE-Z | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803064010/ | Quick Look | ![]() |
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846 | VELA PWN E4 | 130.4202 | -45.4045 | 129.99462 | -45.224746 | 155.536956 | -59.986634 | 264.40968594 | -2.03918199 | 304.5026 | 55712.4105902778 | 2011-05-31 09:51:15 | 55712.7362268518 | 2011-05-31 17:40:10 | 506047010 | 17.0314 | 15 | 17.0354 | 17.0549 | 0 | 17.0314 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.1078 | 15.1078 | 28.128 | 0 | PROCESSED | 57602.173900463 | 2016-08-02 04:10:25 | 56093 | 2012-06-15 00:00:00 | 55726.0290046296 | 2011-06-14 00:41:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | B | SATORU KATSUDA | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506047010/ | Quick Look | ![]() |
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847 | NGC741MOSAICE_P3 | 29.6423 | 5.6966 | 28.988354 | 5.453848 | 29.583767 | -6.010817 | 151.72656453 | -53.38013742 | 71.7748 | 55054.3340509259 | 2009-08-11 08:01:02 | 55054.5765393518 | 2009-08-11 13:50:13 | 804052030 | 9.8918 | 10 | 9.8918 | 9.8918 | 0 | 9.9078 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.9599 | 7.9599 | 20.9439 | 1 | PROCESSED | 57548.1180555556 | 2016-06-09 02:50:00 | 55448 | 2010-09-09 00:00:00 | 55081.2008101852 | 2009-09-07 04:49:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JOEL BREGMAN | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804052030/ | Quick Look | ![]() |
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848 | NGC741MOSAICS_P2 | 29.298 | 4.8125 | 28.646295 | 4.568934 | 28.95035 | -6.72009 | 151.84866444 | -54.32564909 | 71.7104 | 55052.6950925926 | 2009-08-09 16:40:56 | 55052.9238310185 | 2009-08-09 22:10:19 | 804054020 | 11.4289 | 10 | 11.4529 | 11.4289 | 0 | 11.4529 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6.3123 | 6.3123 | 19.7439 | 0 | PROCESSED | 57548.0884953704 | 2016-06-09 02:07:26 | 55451 | 2010-09-12 00:00:00 | 55085.0388425926 | 2009-09-11 00:55:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JOEL BREGMAN | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804054020/ | Quick Look | ![]() |
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849 | N63A | 83.9019 | -66.0368 | 83.884731 | -66.066447 | 9.218584 | -87.500527 | 275.90835505 | -32.28360929 | 166.1398 | 56628.8025347222 | 2013-12-02 19:15:39 | 56629.9556828704 | 2013-12-03 22:56:11 | 508071010 | 82.0387 | 80 | 82.0467 | 82.0387 | 0 | 82.0467 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.8129 | 70.8129 | 99.6119 | 3 | PROCESSED | 57613.5008680556 | 2016-08-13 12:01:15 | 56383 | 2013-04-01 00:00:00 | 56639.6281365741 | 2013-12-13 15:04:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081315 | We propose deep observations of the LMC SNRs N63A and 0509-67.5. The Chandra observation of N63A showed possible signatures of He-like Fe emission and radiative recombination continua of Si and S. With the new observation by Suzaku, we will determine the plasma state of this SNR. The remarkable characteristic of 0509-67.5 is its extremely-low ionization age. This SNR, therefore, provides us a unique opportunity to explore detailed emission features of lowly-ionized atoms. The immediate objective of this observation is to accurately measure the Fe K-beta to K-alpha flux ratio to constrain the dominant charge state of the Fe ejecta. Both observations will provide us crucial datasets useful to improve our knowledge of SNR plasma and atomic physics. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROYA YAMAGUCHI | USA | 8 | AO8 | LEAVING A LEGACY OF SUZAKU: HIGH-QUALITY SPECTRAL DATASET ON IMPORTANT SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508071010/ | Quick Look | ![]() |
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850 | ABELL 426 E4 | 51.4246 | 41.5162 | 50.593046 | 41.341069 | 59.755665 | 22.042042 | 151.51141512 | -12.63936589 | 90 | 55042.2912847222 | 2009-07-30 06:59:27 | 55042.7466898148 | 2009-07-30 17:55:14 | 804059010 | 21.8613 | 20 | 21.8613 | 21.8613 | 0 | 21.8613 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19.707 | 19.707 | 39.336 | 0 | PROCESSED | 57547.9976736111 | 2016-06-08 23:56:39 | 55427 | 2010-08-19 00:00:00 | 55060.7938425926 | 2009-08-17 19:03:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804059010/ | Quick Look | ![]() |
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851 | ABELL 426 E6 | 52.1705 | 41.5044 | 51.337024 | 41.332096 | 60.333006 | 21.882473 | 151.98723888 | -12.32905015 | 86.9996 | 55043.2937847222 | 2009-07-31 07:03:03 | 55043.9501736111 | 2009-07-31 22:48:15 | 804061010 | 31.9431 | 30 | 31.9431 | 31.9431 | 0 | 31.9431 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29.9436 | 29.9436 | 56.702 | 1 | PROCESSED | 57548.0213657407 | 2016-06-09 00:30:46 | 55427 | 2010-08-19 00:00:00 | 55060.7142013889 | 2009-08-17 17:08:27 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804061010/ | Quick Look | ![]() |
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852 | ABELL 426 N1 | 49.7797 | 41.7196 | 48.951337 | 41.538337 | 58.536882 | 22.573374 | 150.34867405 | -13.15794685 | 59.9997 | 55061.841099537 | 2009-08-18 20:11:11 | 55062.1397453704 | 2009-08-19 03:21:14 | 804063010 | 14.7276 | 10 | 14.7356 | 14.7276 | 0 | 14.737 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.1724 | 13.1724 | 25.7919 | 0 | PROCESSED | 57548.2770833333 | 2016-06-09 06:39:00 | 55441 | 2010-09-02 00:00:00 | 55075.0515740741 | 2009-09-01 01:14:16 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804063010/ | Quick Look | ![]() |
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853 | G93.3+6.9 SOUTH | 313.0658 | 55.1877 | 312.717301 | 54.998248 | 351.809721 | 66.81178 | 93.13746865 | 6.81993623 | 52.2984 | 56817.2417708333 | 2014-06-09 05:48:09 | 56819.1057638889 | 2014-06-11 02:32:18 | 509041010 | 85.4695 | 80 | 85.7132 | 85.4695 | 0 | 85.7131 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.2181712963 | 2016-08-15 05:14:10 | 57201 | 2015-06-28 00:00:00 | 56835.7539236111 | 2014-06-27 18:05:39 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091316 | We propose three relatively long observations (totaling 280 ksec) of the high Galactic latitude supernova remnant G093.3+6.9, previously observed in AO-1 with a series of short exposures. This remnant is of particular interest because it is expanding in a low-density medium, appears sub-energetic, and has mixed-morphology, with central thermal X-ray emission surrounded by a radio synchrotron shell. Fits to the spectrum suggest a Type Ia SNR, but the possible presence of a pulsar wind nebula challenges that interpretation. The new pointings will significantly improve the statistics for key regions (rims and background), allowing us to type the remnant, determine its age, study its energetics, place limits on nonthermal X-ray emission, and better characterize the PWN. | GALACTIC DIFFUSE EMISSION | 5 | C | MICHAEL STAGE | USA | 9 | AO9 | G093.3+6.9: SUPERNOVA PHYSICS IN A LOW-DENSITY MEDIUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509041010/ | Quick Look | ![]() |
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854 | FERMI_JET_COCOON_1 | 324.2719 | -34.1434 | 323.519422 | -34.36838 | 315.213492 | -18.826861 | 11.0027102 | -48.00136957 | 252.0162 | 56980.9718402778 | 2014-11-19 23:19:27 | 56981.4029166667 | 2014-11-20 09:40:12 | 509047010 | 23.1647 | 20 | 23.1647 | 23.1887 | 0 | 23.1727 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.793125 | 2016-08-16 19:02:06 | 57444 | 2016-02-26 00:00:00 | 57076.4062037037 | 2015-02-23 09:44:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091322 | The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way. | GALACTIC DIFFUSE EMISSION | 5 | C | MATTHEW MILLER | USA | 9 | AO9 | OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509047010/ | Quick Look | ![]() |
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855 | DIFFUSE1CENTER | 201.5497 | 7.7363 | 200.922947 | 7.99578 | 196.916148 | 15.561038 | 327.54309857 | 68.93048937 | 123.2999 | 57014.2523842593 | 2014-12-23 06:03:26 | 57014.7820949074 | 2014-12-23 18:46:13 | 509058010 | 20.5308 | 20 | 20.5308 | 20.5308 | 0 | 20.5308 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5530555556 | 2016-08-17 13:16:24 | 57475 | 2016-03-28 00:00:00 | 57107.4252546296 | 2015-03-26 10:12:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091324 | In the course of a program to fit spatial models to the Galactic hot gas content, we discovered a few fields that were highly discrepant in the strength of their O VII and/or O VIII line strengths. These are rare emission regions, occurring in fewer than 1% of the fields and they are not due to known extended emission regions (SNR, galaxy clusters, etc.). These emission anomalies probably signify locations of unusual physics, such as shocks, conductive heating, or local heat injection. We propose observations to determine the angular extent of these unusual regions and to better define the intensities of the O VII and O VIII lines. These observations will help identify the relevant physical process and the nature of the phenomenon causing them. | GALACTIC DIFFUSE EMISSION | 5 | C | JOEL BREGMAN | USA | 9 | AO9 | UNIDENTIFIED BRIGHT X-RAY BACKGROUND REGIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509058010/ | Quick Look | ![]() |
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856 | ABELL2811-OFF | 10.1781 | -28.7333 | 9.563743 | -29.007637 | 356.740152 | -30.181509 | 358.19144602 | -87.13859798 | 232.6526 | 53702.8821296296 | 2005-11-28 21:10:16 | 53703.731412037 | 2005-11-29 17:33:14 | 800006010 | 33.9494 | 25 | 33.9574 | 33.9654 | 33.9494 | 33.9498 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 30.9056 | 30.9056 | 73.3659 | 1 | PROCESSED | 57528.1125115741 | 2016-05-20 02:42:01 | 54247 | 2007-05-27 00:00:00 | 54038.6719560185 | 2006-10-30 16:07:37 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001025 | We propose to observe the central region of the Sculptor supercluster at z=0.11, in a search for the theoretically predicted Warm/Hot Intergalactic Medium (WHIM). The WHIM has been 'missing' observationally, until recent detection of the X-ray absorption due to the ionized light elements in the background quasar spectra. Still there is no confident detection of the expected soft X-ray emission. This is mainly because that the X-ray brightness is very low, compared to the Galactic diffuse emission in the soft X-ray band and/or the spectral sensitivity of previous experiments are limited. To separate the expected X-ray lines of the WHIM (mainly O VII) from the Galactic emission, we select an unique supercluster at z>0.1. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | TAKAYUKI TAMURA | JAP | 0 | SWG | THE SCULPTOR SUPERCLUSTER: SEARCH FOR THE WARM/HOT INTERGALACTIC MEDIUM | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800006010/ | Quick Look | ![]() |
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857 | NGC 2992 | 146.4592 | -14.2821 | 145.857736 | -14.050853 | 154.047551 | -26.059819 | 249.69438343 | 28.83515423 | 128.4959 | 53717.4275462963 | 2005-12-13 10:15:40 | 53718.506412037 | 2005-12-14 12:09:14 | 700005030 | 46.8361 | 120 | 46.8441 | 46.8681 | 46.8361 | 46.8601 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 44.2983 | 44.2983 | 93.2079 | 1 | PROCESSED | 57532.4690046296 | 2016-05-24 11:15:22 | 54247 | 2007-05-27 00:00:00 | 54039.2254861111 | 2006-10-31 05:24:42 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001013 | NGC 2992 is a nearby Seyfert 1.9 galaxy showing long-term (20 yrs) large amplitude (factor of 20) variability. This object showed switching between Compton-thick and -thin. Recent RXTE monitoring has shown that this object is highly variable on shorter time scales (2 weeks). We propose three Suzaku observations to monitor the variability of absorption column, broad band continuum shape, and Fe line intensity to understand the cause of the remarkable variability. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YUICHI TERASHIMA | JAP | 0 | SWG | THE SPECTRAL VARIABILITY IN NGC 2992: FE-LINE, REFLECTION, AND COMPTON-THIN/THICK SWITCHING | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700005030/ | Quick Look | ![]() |
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858 | NGC 5506 | 213.3095 | -3.2029 | 212.660624 | -2.969373 | 212.1852 | 9.604154 | 339.1508826 | 53.81542712 | 91.2728 | 54131.0918055556 | 2007-01-31 02:12:12 | 54132.6279513889 | 2007-02-01 15:04:15 | 701030030 | 57.4063 | 150 | 57.4143 | 57.4063 | 0 | 57.4143 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.7027 | 47.7027 | 132.6858 | 0 | PROCESSED | 57536.9491666667 | 2016-05-28 22:46:48 | 54695 | 2008-08-17 00:00:00 | 54139.3642361111 | 2007-02-08 08:44:30 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011312 | NGC 5506 is one of the brightest Seyferts in the X-ray sky, the second brightest in the PIN bandpass. Obscuring gas has kept the true nature of this AGN secret until recent optical and infrared studies have unmasked the narrow-line-seyfert 1 nucleus. With this knowledge, NGC 5506 is the perfect candidate for confirming the generality of a new result based on a recent XMM observation of Mkn 766, ie that the ionized component of Fe K emission originates from the inner accretion disk and closely tracks the hard X-ray continuum flux. This immediately gives us the ionization-state and size-scale of the inner disk. We request a 150 ks Suzaku observation to see whether a similar result holds for NGC 5506 and, by extension, may be a property of NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TRACEY TURNER | USA | 1 | AO1 | SUZAKU STUDY OF THE BRIGHTEST NARROW LINE SEYFERT 1: NGC 5506 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701030030/ | Quick Look | ![]() |
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859 | CIRCINUS GALAXY | 213.2971 | -65.3336 | 212.329588 | -65.099539 | 238.600438 | -47.951762 | 311.32997737 | -3.80345965 | 276.4798 | 53937.5207986111 | 2006-07-21 12:29:57 | 53939.0475 | 2006-07-23 01:08:24 | 701036010 | 108.0217 | 100 | 108.0457 | 108.0217 | 108.0457 | 108.0297 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 94.272 | 94.272 | 131.8879 | 1 | PROCESSED | 57535.0550578704 | 2016-05-27 01:19:17 | 54401 | 2007-10-28 00:00:00 | 53943.5986574074 | 2006-07-27 14:22:04 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011331 | The light of AGN dominates the hard cosmic X-ray background. However, the contribution of Compton thick objects is poorly constrained because they emit chiefly above the energy range where Chandra and XMM are sensitive. Here we propose to observe the Circinus galaxy, one of the two brightest AGN reflection sources below 10 keV and with a known high column density. Our observations below 10 keV will provide CCD spectra of the rich emission line and continuum spectra, allowing limited photoionization modelling and searches for variability, possibly seen in Circinus. In the range 10 - 60 keV, we shall obtain a spectrum of the directly viewed continuum with unprecedented S/N in the key band for the HCXB. Above 60 keV, we will detect Circinus and check whether the spectrum has a rollover. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | ANDREW WILSON | USA | 1 | AO1 | THE HARD X-RAY BACKGROUND, COMPTON-THICK AGN AND WATER VAPOR MEGAMASERS | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701036010/ | Quick Look | ![]() |
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860 | APM 08279+5255 | 127.9195 | 52.7471 | 126.987464 | 52.916366 | 116.240703 | 32.704357 | 165.76446097 | 36.2381521 | 299.485 | 54183.9301041667 | 2007-03-24 22:19:21 | 54186.4654513889 | 2007-03-27 11:10:15 | 701057030 | 117.1433 | 125 | 117.1433 | 117.1513 | 0 | 117.1433 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 110.9324 | 110.9324 | 219.0418 | 3 | PROCESSED | 57538.0464467593 | 2016-05-30 01:06:53 | 54702 | 2008-08-24 00:00:00 | 54209.5933680556 | 2007-04-19 14:14:27 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011353 | Motivated by the detection of a relativistic outflow of highly ionized gas in previous XMM-Newton and Chandra observations of the lensed quasar APM08279+5255 we propose to monitor this object with three 100ks observations with the aim of improving our understanding of the significance of such outflows in regulating black hole growth and in influencing structure formation. The main scientific goals are : (a) verify the present interpretations of Fe line features in this quasar, (b) monitor the time variability of the Fe absorption features and thus constrain the acceleration mechanism, (c) constrain the kinematic, ionization and absorbing properties of the outflow, and (d) show whether the low-energy ionized absorber is part of the relativistic outflow. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GEORGE CHARTAS | USA | 1 | AO1 | VIEWS OF RELATIVISTIC WINDS THROUGH NATURAL LENSES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701057030/ | Quick Look | ![]() |
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861 | 1ES 1553+113 | 238.8999 | 11.1305 | 238.306227 | 11.275519 | 233.852477 | 30.750337 | 21.81691499 | 43.96274027 | 296.7536 | 53940.6127777778 | 2006-07-24 14:42:24 | 53941.8036342593 | 2006-07-25 19:17:14 | 701070010 | 55.6355 | 55 | 55.6435 | 55.6515 | 55.6515 | 55.6355 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 53.2015 | 53.2015 | 102.8819 | 0 | PROCESSED | 57535.0418171296 | 2016-05-27 01:00:13 | 54401 | 2007-10-28 00:00:00 | 53955.6133680556 | 2006-08-08 14:43:15 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011376 | Detecting absorption effects in TeV blazar spectra from TeV photon collisions on the extragalactic IR background (EBL) is a powerful tool to probe the EBL. It requires a thorough understanding of the intrinsic blazar spectra. We propose XIS and HXD observations, with emphasis on the hard X-rays, for the 3 most distant HESS blazars, coordinated with HESS observations. Thanks to Suzaku's sensitivity in a broad energy range, we expect to set tight limits on the models' parameter space, and constrain emission and acceleration scenarios by studying the shape and evolution of the particle distribution, most sensitively conducted in the important hard X-ray energy range. In coordination with TeV observations, it allows us to disentangle EBL absorption effects from the blazar intrinsic spectra. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ANITA REIMER | USA | 1 | AO1 | CHALLENGING JET MODELS OF THE MOST DISTANT TEV-BLAZARS | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701070010/ | Quick Look | ![]() |
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862 | N206 SB | 82.6396 | -71.0391 | 82.803839 | -71.074403 | 297.258629 | -84.798656 | 281.83986558 | -32.08582418 | 315.5807 | 54584.7862384259 | 2008-04-28 18:52:11 | 54585.7640509259 | 2008-04-29 18:20:14 | 803038010 | 48.8345 | 40 | 48.8345 | 48.8345 | 0 | 48.8345 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54.7297 | 54.7297 | 84.4678 | 1 | PROCESSED | 57542.434837963 | 2016-06-03 10:26:10 | 54964 | 2009-05-13 00:00:00 | 54598.4969444445 | 2008-05-12 11:55:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031238 | Clusters of massive stars, through their stellar winds and supernovae, form large diffuse structures known as superbubbles (SBs), which play an essential role in shaping the local interstellar medium. Most SB models indicate that these objects should be dominated by thermal plasma processes. However, observations of 3 SBs have detected significant nonthermal contributions to their X-ray emission, which raises many questions. Is it generated by synchrotron, inverse-Compton, or nonthermal Bremsstrahlung processes? Are colliding stellar winds or internal supernova remnants responsible? We therefore propose to examine the X-ray emission from 3 X-ray bright SBs, to search for nonthermal X-ray emission, and if possible place strong constraints on the source of this emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | LARRY MADDOX | USA | 3 | AO3 | A SEARCH FOR NONTHERMAL X-RAY EMISSION FROM SUPERBUBBLES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803038010/ | Quick Look | ![]() |
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863 | NGC741S2_P1 | 29.0961 | 5.1589 | 28.443649 | 4.91486 | 28.882528 | -6.325199 | 151.28423043 | -54.09870829 | 71.6444 | 55053.3762962963 | 2009-08-10 09:01:52 | 55053.6078587963 | 2009-08-10 14:35:19 | 804055010 | 8.6016 | 10 | 8.6176 | 8.6016 | 0 | 8.6256 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.748 | 8.748 | 19.984 | 1 | PROCESSED | 57548.1032291667 | 2016-06-09 02:28:39 | 55465 | 2010-09-26 00:00:00 | 55098.1609375 | 2009-09-24 03:51:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JOEL BREGMAN | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804055010/ | Quick Look | ![]() |
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864 | ABELL 426 E7 | 52.5439 | 41.4965 | 51.709488 | 41.325623 | 60.621576 | 21.801638 | 152.22519414 | -12.17349332 | 85.5 | 55043.9514814815 | 2009-07-31 22:50:08 | 55044.6843055556 | 2009-08-01 16:25:24 | 804062010 | 30.9516 | 30 | 30.9516 | 31.2216 | 0 | 31.2056 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 28.5449 | 28.5449 | 63.314 | 0 | PROCESSED | 57548.0327083333 | 2016-06-09 00:47:06 | 55427 | 2010-08-19 00:00:00 | 55060.8353703704 | 2009-08-17 20:02:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804062010/ | Quick Look | ![]() |
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865 | A2204_FIELD_3 | 248.3129 | 5.7152 | 247.698224 | 5.819454 | 245.539745 | 27.332187 | 21.30307351 | 33.20188623 | 261.0004 | 55436.6750347222 | 2010-08-28 16:12:03 | 55437.758587963 | 2010-08-29 18:12:22 | 805058010 | 36.2307 | 40 | 36.2387 | 36.2307 | 0 | 36.2467 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31.6564 | 31.6564 | 93.6018 | 2 | PROCESSED | 57553.2217361111 | 2016-06-14 05:19:18 | 55287 | 2010-04-01 00:00:00 | 55449.3168634259 | 2010-09-10 07:36:17 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805058010/ | Quick Look | ![]() |
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866 | A1413_FIELD_2 | 178.6363 | 23.4218 | 177.992083 | 23.700041 | 169.007568 | 20.85313 | 225.87600909 | 76.62442609 | 303.0004 | 55346.1403240741 | 2010-05-30 03:22:04 | 55347.1856828704 | 2010-05-31 04:27:23 | 805060010 | 40.9512 | 40 | 40.9592 | 40.9512 | 0 | 40.9512 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 34.5464 | 34.5464 | 90.2959 | 0 | PROCESSED | 57551.669837963 | 2016-06-12 16:04:34 | 55287 | 2010-04-01 00:00:00 | 55365.258912037 | 2010-06-18 06:12:50 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805060010/ | Quick Look | ![]() |
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867 | A383_FIELD_1 | 42.1211 | -3.4616 | 41.492043 | -3.669137 | 38.559838 | -18.768369 | 177.79816007 | -53.37318565 | 60.9988 | 55388.2747337963 | 2010-07-11 06:35:37 | 55389.1376388889 | 2010-07-12 03:18:12 | 805062010 | 40.3915 | 40 | 40.4155 | 40.3915 | 0 | 40.4155 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 35.3721 | 35.3721 | 74.52 | 1 | PROCESSED | 57552.5965046296 | 2016-06-13 14:18:58 | 55287 | 2010-04-01 00:00:00 | 55411.2489467593 | 2010-08-03 05:58:29 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805062010/ | Quick Look | ![]() |
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868 | A383_FIELD_3 | 41.9643 | -3.6473 | 41.33581 | -3.855343 | 38.341492 | -18.895957 | 177.84591826 | -53.61436812 | 60.9989 | 55390.0630902778 | 2010-07-13 01:30:51 | 55390.9764930556 | 2010-07-13 23:26:09 | 805064010 | 43.1968 | 40 | 43.1968 | 43.1968 | 0 | 43.1968 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.5929 | 39.5929 | 78.8959 | 1 | PROCESSED | 57552.6323842593 | 2016-06-13 15:10:38 | 55287 | 2010-04-01 00:00:00 | 55411.2967592593 | 2010-08-03 07:07:20 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805064010/ | Quick Look | ![]() |
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869 | COMA E1 | 195.2288 | 27.9019 | 194.626316 | 28.170859 | 181.798966 | 31.442311 | 53.6887936 | 87.76083997 | 279.9992 | 55728.9920601852 | 2011-06-16 23:48:34 | 55729.2682523148 | 2011-06-17 06:26:17 | 806030010 | 9.184 | 10 | 9.2 | 9.184 | 0 | 9.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.2038 | 10.2038 | 23.858 | 0 | PROCESSED | 57602.3046296296 | 2016-08-02 07:18:40 | 55652 | 2011-04-01 00:00:00 | 55770.1007407407 | 2011-07-28 02:25:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806030010/ | Quick Look | ![]() |
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870 | ABELL 426 N2 | 49.5875 | 41.9633 | 48.758073 | 41.781328 | 58.461538 | 22.847366 | 150.08864093 | -13.03246307 | 59.9939 | 55062.1402662037 | 2009-08-19 03:21:59 | 55062.4716898148 | 2009-08-19 11:19:14 | 804064010 | 13.166 | 10 | 13.166 | 13.166 | 0 | 13.166 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.647 | 9.647 | 28.6239 | 0 | PROCESSED | 57548.2750578704 | 2016-06-09 06:36:05 | 55441 | 2010-09-02 00:00:00 | 55075.0035416667 | 2009-09-01 00:05:06 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804064010/ | Quick Look | ![]() |
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871 | ABELL 426 N4 | 49.2103 | 42.4455 | 48.378755 | 42.262141 | 58.317611 | 23.388756 | 149.57911953 | -12.77962749 | 59.999 | 55062.754837963 | 2009-08-19 18:06:58 | 55063.2460532407 | 2009-08-20 05:54:19 | 804066010 | 25.3046 | 20 | 25.3046 | 25.3065 | 0 | 25.3086 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.6295 | 21.6295 | 42.44 | 0 | PROCESSED | 57548.2829282407 | 2016-06-09 06:47:25 | 55441 | 2010-09-02 00:00:00 | 55075.0762384259 | 2009-09-01 01:49:47 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804066010/ | Quick Look | ![]() |
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872 | ABELL 1068 | 160.4236 | 39.9791 | 159.703028 | 40.240763 | 145.773983 | 29.164286 | 178.96037586 | 60.29153459 | 130.001 | 55861.8826273148 | 2011-10-27 21:10:59 | 55863.1258564815 | 2011-10-29 03:01:14 | 806028020 | 52.0056 | 50 | 52.0136 | 52.0056 | 0 | 52.0196 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.2759 | 43.2759 | 107.4038 | 1 | PROCESSED | 57603.6533333333 | 2016-08-03 15:40:48 | 55652 | 2011-04-01 00:00:00 | 55874.1687615741 | 2011-11-09 04:03:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061116 | We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 6 | AO6-LP | THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806028020/ | Quick Look | ![]() |
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873 | AB DOR | 82.2881 | -65.4658 | 82.252574 | -65.503277 | 15.679222 | -86.688003 | 275.31538375 | -33.00189818 | 204.2849 | 54108.0647569444 | 2007-01-08 01:33:15 | 54109.4724421296 | 2007-01-09 11:20:19 | 401031020 | 49.0965 | 45 | 49.0965 | 49.0965 | 0 | 49.0965 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.9611 | 44.9611 | 121.6199 | 2 | PROCESSED | 57536.5000578704 | 2016-05-28 12:00:05 | 54502 | 2008-02-06 00:00:00 | 54133.0127083333 | 2007-02-02 00:18:18 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011021 | We propose to observe the rapidly rotating star AB Doradus for 80 ks with Suzaku Our main goals are to detect non-thermal hard X-rays and fluorescent Fe at 6.4 keV with the HXD and the XIS during a stellar flare. Such a spectral feature can be induced by non-thermal electrons in the impulsive flare phase, or by X-rays of the very hot flare plasma. The hard X-ray detectors will be used to detect non-thermal bremsstrahlung expected when a beam of non-thermal electrons (typically observed in the radio) impacts the dense chromosphere. We will also study the coronal element composition and its temporal evolution during the flare. Finally, we will attempt coordination with the Australian Telescope to monitor the non-thermal electron population, without any timing constraint for Suzaku. | GALACTIC POINT SOURCES | 4 | B | MARC AUDARD | USA | 1 | AO1 | NON-THERMAL HARD X-RAYS AND FLUORESCENT FE IN STELLAR FLARES | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401031020/ | Quick Look | ![]() |
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874 | 1RXS J213344.1+51072 | 323.4354 | 51.1973 | 323.001109 | 50.974362 | 356.300054 | 59.716219 | 94.50909334 | -0.42447705 | 94.0452 | 53854.2853009259 | 2006-04-29 06:50:50 | 53856.2501736111 | 2006-05-01 06:00:15 | 401038010 | 81.9241 | 80 | 81.9241 | 81.9241 | 81.9241 | 81.9241 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 62.8881 | 62.8881 | 169.7261 | 3 | PROCESSED | 57533.6330671296 | 2016-05-25 15:11:37 | 54391 | 2007-10-18 00:00:00 | 53908.1887962963 | 2006-06-22 04:31:52 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011102 | Intermediate Polars (IPs) are strong soft and hard X-ray sources and Suzaku is therefore ideally suited to their study. We have selected three IPs that are of particularly high priority. They have all been detected as hard (E>10 keV) X-ray sources; they all have a hot (kT~100 eV), blackbody-like component; none have been studied simultaneously over a wide band-pass. We therefore propose 80 ksec observations each of V2400 Oph, 1RXS J154814.5-452845, and 1RXS J213344.1+510725, with an additional 40 ksec background observation for V2400 Oph. We plan to analyze the average and phase-resolved spectra to determine the strength of the reflection continuum; the highest temperature present in the plasma; and the details of the complex absorber. | GALACTIC POINT SOURCES | 4 | A | KOJI MUKAI | USA | 1 | AO1 | BROAD-BAND SPECTROSCOPY OF INTERMEDIATE POLARS: FROM THE SOFT COMPONENT TO REFLECTION | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401038010/ | Quick Look | ![]() |
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875 | V893 SCO | 243.8144 | -28.6275 | 243.038085 | -28.502934 | 247.008203 | -7.251726 | 348.06577336 | 15.88028883 | 274.6746 | 53973.4024189815 | 2006-08-26 09:39:29 | 53974.056412037 | 2006-08-27 01:21:14 | 401041010 | 18.4978 | 20 | 18.4978 | 18.4978 | 18.4978 | 18.4978 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 16.1403 | 16.1403 | 56.482 | 0 | PROCESSED | 57535.3695601852 | 2016-05-27 08:52:10 | 54526 | 2008-03-01 00:00:00 | 54053.4763888889 | 2006-11-14 11:26:00 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011103 | The RXTE All-Sky Slew Survey (XSS) catalog, containing 294 objects detected in the 3-20 keV sky, is of great potential use for a variety of purposes. Included in this catalog are two sources identified with lesser known dwarf novae, V893 Sco and SS Aur. Although these are known to be soft X-ray sources from the ROSAT All-sky Survey, there has never been a pointed observation with an imaging X-ray telescope of either object. Here I propose short Suzaku observations of V893 Sco and SS Aur to check the reliability of XSS fluxes, hence that of the luminosity functions derived from the XSS catalog. In addition, such observations serve as a pilot study to determine if these individual dwarf novae may merit further in-depth X-ray studies. | GALACTIC POINT SOURCES | 4 | B | KOJI MUKAI | USA | 1 | AO1 | CONFIRMING THE IDENTIFICATION OF RXTE ALL-SKY SLEW SURVEY SOURCES WITH DWARF NOVAE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401041010/ | Quick Look | ![]() |
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876 | 4U 1636-536 | 250.2277 | -53.7538 | 249.23129 | -53.65731 | 256.461636 | -31.236425 | 332.91167841 | -4.81798429 | 93.2445 | 54186.4802777778 | 2007-03-27 11:31:36 | 54187.3043287037 | 2007-03-28 07:18:14 | 401050040 | 32.1304 | 38 | 32.1304 | 32.1384 | 0 | 32.1304 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 27.7842 | 27.7842 | 71.1779 | 1 | PROCESSED | 57538.0141782407 | 2016-05-30 00:20:25 | 54695 | 2008-08-17 00:00:00 | 54209.541412037 | 2007-04-19 12:59:38 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011117 | Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. | GALACTIC POINT SOURCES | 4 | A | JEROEN HOMAN | USA | 1 | AO1 | THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401050040/ | Quick Look | ![]() |
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877 | 4U 1822-37 | 276.4461 | -37.1042 | 275.595774 | -37.133404 | 275.279951 | -13.781506 | 356.85149319 | -11.29112534 | 258.4537 | 54010.4563888889 | 2006-10-02 10:57:12 | 54011.5189699074 | 2006-10-03 12:27:19 | 401051010 | 37.7434 | 40 | 37.7682 | 37.7682 | 37.7434 | 37.7434 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 33.1785 | 33.1785 | 91.8059 | 0 | PROCESSED | 57535.7615393518 | 2016-05-27 18:16:37 | 54695 | 2008-08-17 00:00:00 | 54024.6539814815 | 2006-10-16 15:41:44 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011121 | We propose a 40 ks observation of the accretion disk corona source 4U 1822-37. Despite repeated observations over the years and even excellent high-resolution data from the Chandra Observatory, the nature and origin of the corona and even the source of the Fe K fluorescence emission remains controversial. The spectral resolution of the XIS and the broad-band coverage provided by the combined XIS and HXD instruments make Suzaku uniquely suited to a definitive measurement. Determining the physical conditions in this source is particularly interesting. Because of its geometry 4U 1822-37 is a link between x-ray binaries and AGN, and an therefore serve as a laboratory for studying accretion processes throughout the universe. | GALACTIC POINT SOURCES | 4 | B | JEAN COTTAM | USA | 1 | AO1 | ACCRETION PHYSICS IN THE ADC SOURCE 4U 1822-37 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401051010/ | Quick Look | ![]() |
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878 | HD432 | 2.3072 | 59.1394 | 1.650501 | 58.861236 | 35.115755 | 51.206006 | 117.5327944 | -3.28915956 | 247.7181 | 54469.7038310185 | 2008-01-04 16:53:31 | 54470.5154513889 | 2008-01-05 12:22:15 | 402034010 | 38.2406 | 40 | 38.2486 | 38.2406 | 0 | 38.2486 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.0503 | 35.0503 | 70.12 | 1 | PROCESSED | 57540.9911574074 | 2016-06-01 23:47:16 | 54908 | 2009-03-18 00:00:00 | 54483.4635532407 | 2008-01-18 11:07:31 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021016 | Suzaku XIS spectra of three "X-ray deficient" Hertzsprung gap giants will explore why they display anomalous coronal behavior compared with cooler giants only slightly further advanced in their evolution. The apparent sharp transition in coronal properties on the way to helium flash might be caused by disruption of a "fossil" magnetosphere by a newly born solar-like dynamo. A key discriminator is the coronal energy distribution, especially enhanced and sporadic hard emission associated with flaring. The proposed targets are the brightest not previously observed in X-rays at CCD resolution; all three have supporting high resolution UV spectra. Expanding the sample of high quality, high energy information on this key class of objects is essential for probing their odd behavior. | GALACTIC POINT SOURCES | 4 | C | THOMAS AYRES | USA | 2 | AO2 | ANOMALOUS CORONAE OF HERTZSPRUNG GAP GIANTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402034010/ | Quick Look | ![]() |
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879 | SW UMA | 129.1769 | 53.4845 | 128.242011 | 53.658568 | 116.840982 | 33.632115 | 164.80593722 | 36.96002764 | 98.2716 | 54410.2367708333 | 2007-11-06 05:40:57 | 54410.6252199074 | 2007-11-06 15:00:19 | 402044010 | 16.8991 | 20 | 16.9071 | 16.8991 | 0 | 16.9071 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.8969 | 13.8969 | 33.5519 | 1 | PROCESSED | 57540.4388194444 | 2016-06-01 10:31:54 | 54784 | 2008-11-14 00:00:00 | 54417.2697569444 | 2007-11-13 06:28:27 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021105 | Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose short Suzaku observations of dwarf novae with secure, parallax-based distance estimates that have not been the subject of pointed, imaging, X-ray observations in the 0.5-10 keV band. This will be an important check of potential biases in earlier studies. | GALACTIC POINT SOURCES | 4 | C | KOJI MUKAI | USA | 2 | AO2 | BUILDING UP AN UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A PARALLAX SELECTED SAMPLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402044010/ | Quick Look | ![]() |
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880 | GX17+2 | 274.0098 | -14.0991 | 273.299204 | -14.116851 | 273.930842 | 9.286846 | 16.37876929 | 1.24433559 | 268.3778 | 54370.5988078704 | 2007-09-27 14:22:17 | 54371.2502199074 | 2007-09-28 06:00:19 | 402050020 | 23.0117 | 20 | 23.0197 | 23.0258 | 0 | 23.0117 | 3 | 2 | 0 | 3 | 1 | 0 | 0 | 19.0488 | 19.0488 | 56.276 | 0 | PROCESSED | 57540.1139351852 | 2016-06-01 02:44:04 | 54769 | 2008-10-30 00:00:00 | 54402.3511921296 | 2007-10-29 08:25:43 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021111 | Z sources are bright low-mass X-ray binaries with variable spectra that describe a characteristic "Z" shape in an X-ray color-color plot. The forces driving the spectral shape and variability of the Z sources are not well understood, as there are few detectors with the necessary capabilities. GX17+2 is a Sco-type Z sources with an unusual time-varying hard X-ray tail whose origin is uncertain. Bright X-ray sources also illuminate the interstellar medium. Highly absorbed X-ray sources show halos due to dust scattering as well as absorption features. These will allow us to place constraints on interstellar dust and gas models. Suzaku can address all of these issues with simultaneous observations of the hard X-ray continuum and the dust-scattered X-ray halo. | GALACTIC POINT SOURCES | 4 | A | RANDALL SMITH | USA | 2 | AO2 | OBSERVING THE SPECTRUM AND HALO OF GX17+2 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402050020/ | Quick Look | ![]() |
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881 | 2S 0921-630 | 140.6643 | -63.2995 | 140.374106 | -63.084565 | 195.141929 | -68.892072 | 281.84516955 | -9.33669084 | 18.1705 | 54342.4079166667 | 2007-08-30 09:47:24 | 54343.5134722222 | 2007-08-31 12:19:24 | 402058010 | 45.6937 | 40 | 45.6937 | 45.6937 | 0 | 45.6937 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.3463 | 43.3463 | 95.4998 | 2 | PROCESSED | 57539.9018981482 | 2016-05-31 21:38:44 | 54724 | 2008-09-15 00:00:00 | 54356.2760763889 | 2007-09-13 06:37:33 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021118 | 2S 0921-630 is a bright, long-period LMXB that is thought to contain an accretion disk corona. Observations with both the Chandra HETGS and XMM-Newton spectrometers revealed line emission from a photoionized plasma. The spectral features are consistent with the predictions for emission from an accretion disk corona. However, with the present data it is impossible to determine whether the emission originates in the corona or in a localized region of the disk. We propose to observer 2S 0921-630 with Suzaku at four orbital phases in order to localize and identify the emitting plasma. The simultaneous HXD coverage will also allow us to constrain the underlying continuum and allow more sensitive study of the high energy region of the spectrum. | GALACTIC POINT SOURCES | 4 | A | JEAN COTTAM | USA | 2 | AO2 | PHASE-RESOLVED SPECTROSCOPY OF 2S 0921-630 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402058010/ | Quick Look | ![]() |
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882 | IGR J00370+6122 | 9.2836 | 61.3722 | 8.564252 | 61.097243 | 41.619526 | 50.769336 | 121.21895683 | -1.4519667 | 87.6081 | 54273.499849537 | 2007-06-22 11:59:47 | 54274.230775463 | 2007-06-23 05:32:19 | 402064010 | 34.9089 | 30 | 35.3844 | 35.4004 | 0 | 34.9089 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33.7926 | 33.7926 | 63.1419 | 2 | PROCESSED | 57637.5249652778 | 2016-09-06 12:35:57 | 54695 | 2008-08-17 00:00:00 | 54322.4714236111 | 2007-08-10 11:18:51 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021122 | We propose to observe 3 INTEGRAL-discovered High Mass X-ray Binaries (IGR HMXBs) to search for X-ray pulsations and to study their broadband spectra. Over the past few years, INTEGRAL has found a surprising number of HMXBs, and the large number of new, locally absorbed supergiant HMXBs indicate that these wind-accretors are more common than previously thought. In addition to high column densities, some of these systems have other extreme properties such as slowly rotating neutron stars (NSs) or rapid X-ray flares. For the systems we propose to observe, detection of pulsations is important for establishing the presence of a NS and for constraining the spin period distribution for HMXB NSs. As these are strong hard X-ray emitters, we will take advantage of Suzaku's broadband capabilities. | GALACTIC POINT SOURCES | 4 | B | JOHN TOMSICK | USA | 2 | AO2 | LOOKING FOR SIGNATURES OF HIGH MAGNETIC FIELD NEUTRON STARS IN INTEGRAL HMXBS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402064010/ | Quick Look | ![]() |
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883 | 4U 1907+09 | 287.4001 | 9.8965 | 286.805564 | 9.814618 | 290.343315 | 32.116545 | 43.79892996 | 0.51344636 | 85.3836 | 54209.4191666667 | 2007-04-19 10:03:36 | 54211.2612731482 | 2007-04-21 06:16:14 | 402067010 | 80.6283 | 65 | 80.6283 | 80.6363 | 0 | 80.6363 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 73.2685 | 73.2685 | 159.1479 | 2 | PROCESSED | 57538.4515393518 | 2016-05-30 10:50:13 | 54702 | 2008-08-24 00:00:00 | 54216.2674189815 | 2007-04-26 06:25:05 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021123 | The HMXB 4U 1907+09 shows a rich phenomenology: two cyclotron lines, an uncommonly weak iron line, intermittent X-ray fading, and a recent torque reversal. Compared to other persistent supergiant X-ray pulsars it has been less well observed, although it is a prime target to study the interaction of the neutron star's X-rays with the stellar wind and the accretion column. The latter has been confirmed by our 60ks AO1 observation which allowed for the first detection of a soft excess below 2keV as well as the determination of the paramters of the fundamental cyclotron line with unprecedented accuracy. Due to an unusually low source state during the AO1 exposure, however, an additional observation of 65ks is needed to perform the first phase resolved analysis of this interesting source. | GALACTIC POINT SOURCES | 4 | B | KATJA POTTSCHMIDT | USA | 2 | AO2 | THE BROAD BAND SPECTRUM OF 4U 1907+09 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402067010/ | Quick Look | ![]() |
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884 | HD72779 | 128.8308 | 19.5933 | 128.112263 | 19.766482 | 126.214353 | 0.900748 | 205.51018209 | 31.33811175 | 104.3214 | 55141.3245949074 | 2009-11-06 07:47:25 | 55142.9515277778 | 2009-11-07 22:50:12 | 404035010 | 71.0335 | 70 | 71.0335 | 71.0335 | 0 | 71.0335 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.461 | 47.461 | 140.5559 | 0 | PROCESSED | 57549.2155902778 | 2016-06-10 05:10:27 | 55532 | 2010-12-02 00:00:00 | 55166.2074189815 | 2009-12-01 04:58:41 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041201 | Suzaku XIS spectra of two G0 III Hertzsprung gap giants will complete a multi-observatory survey of the anomalous coronal behavior of this "X-ray deficient" class. The abrupt rise in coronal luminosities from the warmer giants to their cooler cousins, only slightly further advanced in evolution, might signal disruption of a "fossil" magnetosphere by a newly born solar-like dynamo. Key discriminators are the coronal energy distribution, composition (FIP bias), and sporadic hard emission associated with flaring. The proposed targets are the brightest not previously observed in X-rays at CCD resolution, and both have supporting HST UV spectra. Expanding the high energy sample of this key class of objects is essential for probing their contrary, but perhaps deeply significant, behavior. | GALACTIC POINT SOURCES | 4 | B | THOMAS AYRES | USA | 4 | AO4 | ANOMALOUS CORONAE IN THE MIDST OF THE HERTZSPRUNG GAP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404035010/ | Quick Look | ![]() |
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885 | GX 340+0 | 251.4463 | -45.6133 | 250.537018 | -45.522593 | 255.990327 | -23.069192 | 339.58535361 | -0.07953483 | 81.21 | 54892.2765740741 | 2009-03-02 06:38:16 | 54894.8168287037 | 2009-03-04 19:36:14 | 403060010 | 107.3127 | 100 | 107.3145 | 107.3127 | 0 | 107.3145 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86.104 | 86.104 | 219.4467 | 1 | PROCESSED | 57545.7913541667 | 2016-06-06 18:59:33 | 55329 | 2010-05-13 00:00:00 | 54908.7293055556 | 2009-03-18 17:30:12 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031164 | In this proposal we request to observe accreting neutron stars sources GX 340+0, GX 3+1 and GX 13+1. The observational goal of the observations is to collect high-spectral resolution data in the region of K$_alpha$ iron line. Our scientific motivation is to put the origin of the line emission under additional theoretical scrutiny. We wish to compare the performance of the wind-reprocessing model to relativistic model in as many sources as possible. This proposal is a part of our broader effort to investigate the origin of iron emission line in Galactic X-ray binaries, which includes a parallel proposal to observe WD binaries. | GALACTIC POINT SOURCES | 4 | B | NIKOLAI SHAPOSHNIKOV | USA | 3 | AO3 | IRON KALPHA EMISSION LINE DIAGNOSTICS IN ACCRETING NEUTRON STARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403060010/ | Quick Look | ![]() |
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886 | 4U 1608-52 | 243.1847 | -52.3651 | 242.223789 | -52.237385 | 251.315712 | -30.647315 | 330.96850701 | -0.81056533 | 96.6085 | 55266.077650463 | 2010-03-11 01:51:49 | 55267.0072222222 | 2010-03-12 00:10:24 | 404044010 | 34.0101 | 30 | 34.0101 | 34.0101 | 0 | 34.0101 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.194 | 30.194 | 80.2978 | 0 | PROCESSED | 57550.8305902778 | 2016-06-11 19:56:03 | 55647 | 2011-03-27 00:00:00 | 55279.4591666667 | 2010-03-24 11:01:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041223 | The true nature of X-ray emission from neutron star X-ray binaries (NSXRBs) has not been clear for sometime and there are many possibilities for the spectral model. Recent progress has been made, but relies on RXTE data which lacks the low energy sensitivity where disk emission is most prominent. Using Suzaku we propose four 30 ksec observations of the transient 4U 1608-52 throughout an outburst. We will test how spectral parameters change with luminosity, allowing us to untangle the correct model. An essential part of this proposal is the unique ability of Suzaku to detect asymmetric broad iron emission lines in NSXRBs. We will study how the iron line varies throughout the outburst, which combined with the spectral fits will test the interaction between the accretion disk and corona. | GALACTIC POINT SOURCES | 4 | A | EDWARD CACKETT | USA | 4 | AO4-TOO | ACCRETION DISK EVOLUTION THROUGHOUT A NEUTRON STAR LMXB OUTBURST | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404044010/ | Quick Look | ![]() |
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887 | A 0535+26 | 84.7291 | 26.2457 | 83.952015 | 26.21825 | 85.269487 | 2.891446 | 181.50526016 | -2.67952465 | 272.2555 | 55292.5024074074 | 2010-04-06 12:03:28 | 55293.7029282407 | 2010-04-07 16:52:13 | 404055010 | 3.1779 | 45 | 3.1779 | 3.4604 | 0 | 3.1779 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.3928 | 34.3928 | 103.7158 | 1 | PROCESSED | 57553.0049074074 | 2016-06-14 00:07:04 | 55689 | 2011-05-08 00:00:00 | 55323.4435532407 | 2010-05-07 10:38:43 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041232 | We propose to perform Target of Opportunity Observations of one accreting neutron star in outburst during Suzaku's AO-4. The aim of the observations is to observe the source at a level of 40 and 200mCrab, to determine the properties of the cyclotron line(s) in this system and to constrain its broad band spectrum. | GALACTIC POINT SOURCES | 4 | A | KATJA POTTSCHMIDT | USA | 4 | AO4-TOO | CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404055010/ | Quick Look | ![]() |
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888 | 4U 0115+63 | 19.6209 | 63.7559 | 18.795542 | 63.493074 | 49.810072 | 49.806241 | 125.91670035 | 1.04099954 | 84.7167 | 55747.0027430556 | 2011-07-05 00:03:57 | 55748.0529976852 | 2011-07-06 01:16:19 | 406048010 | 24.279 | 50 | 24.28 | 24.279 | 0 | 24.2839 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.1272 | 45.1272 | 90.7279 | 1 | PROCESSED | 57602.5201157407 | 2016-08-02 12:28:58 | 56163 | 2012-08-24 00:00:00 | 55778.4298611111 | 2011-08-05 10:19:00 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061234 | We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | KATJA POTTSCHMIDT | USA | 6 | AO6-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406048010/ | Quick Look | ![]() |
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889 | GX 304-1 | 195.3153 | -61.5986 | 194.542717 | -61.329512 | 225.389902 | -49.202492 | 304.10001953 | 1.25086712 | 115.9338 | 55957.437037037 | 2012-01-31 10:29:20 | 55959.1669444444 | 2012-02-02 04:00:24 | 406060010 | 16.5243 | 65 | 16.6912 | 16.5243 | 0 | 16.6912 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 58.7124 | 58.7124 | 149.4321 | 3 | PROCESSED | 57604.5523148148 | 2016-08-04 13:15:20 | 56399 | 2013-04-17 00:00:00 | 56033.2695023148 | 2012-04-16 06:28:05 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061235 | We propose to perform Target of Opportunity observations of one accreting neutron star that is not yet a known or clearly confirmed cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 65 ks at a level of >~100 mCrab, in order search for cyclotron line(s) and constrain the broad band spectrum. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | KATJA POTTSCHMIDT | USA | 6 | AO6-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS II: NEW LINES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406060010/ | Quick Look | ![]() |
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890 | HD162020 | 267.6612 | -40.3294 | 266.784393 | -40.315902 | 268.126935 | -16.903295 | 350.72995016 | -6.73261971 | 268.3343 | 55816.4132291667 | 2011-09-12 09:55:03 | 55816.727962963 | 2011-09-12 17:28:16 | 406037020 | 15.0362 | 15 | 15.0442 | 15.0442 | 0 | 15.0362 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.5829 | 15.5829 | 27.1839 | 0 | PROCESSED | 57603.1194328704 | 2016-08-03 02:51:59 | 56218 | 2012-10-18 00:00:00 | 55851.4394444444 | 2011-10-17 10:32:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061202 | Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. | GALACTIC POINT SOURCES | 4 | A | IGNAZIO PILLITTERI | USA | 6 | AO6 | STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406037020/ | Quick Look | ![]() |
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891 | HD162020 | 267.6578 | -40.3138 | 266.781124 | -40.300286 | 268.12395 | -16.887741 | 350.74222411 | -6.72254511 | 106.352 | 56005.8535069444 | 2012-03-19 20:29:03 | 56006.0626157407 | 2012-03-20 01:30:10 | 406038010 | 10.4286 | 10 | 10.4373 | 10.4373 | 0 | 10.4286 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.673 | 7.673 | 18.0559 | 0 | PROCESSED | 57604.9610185185 | 2016-08-04 23:03:52 | 56435 | 2013-05-23 00:00:00 | 56068.625474537 | 2012-05-21 15:00:41 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061202 | Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. | GALACTIC POINT SOURCES | 4 | A | IGNAZIO PILLITTERI | USA | 6 | AO6 | STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406038010/ | Quick Look | ![]() |
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892 | HERCULES X-1 | 254.4605 | 35.3288 | 254.009904 | 35.404408 | 245.996246 | 57.479663 | 58.13264186 | 37.51848299 | 268.7999 | 56189.3538310185 | 2012-09-19 08:29:31 | 56190.0300231482 | 2012-09-20 00:43:14 | 407051010 | 25.5356 | 20 | 25.5436 | 25.5494 | 0 | 25.5356 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.0879 | 25.0879 | 58.4219 | 0 | PROCESSED | 57607.1017013889 | 2016-08-07 02:26:27 | 56590 | 2013-10-25 00:00:00 | 56218.5228472222 | 2012-10-18 12:32:54 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071224 | This proposal is for the continuation of successful Suzaku observations of Her X-1. The proposal is led by the NuSTAR team, extended with experts on X-ray binary pulsars with cyclotron lines. We propose three 20 ks simultaneous Suzaku and NuSTAR observations of Her X-1. Joint observations will substantial increase the science that can be addressed, allowing a systematic study of the fundamental cyclotron line (~40 keV) as a function of time, X-ray flux, 35 day phase, and 1.24 s pulse phase. The combined data will probe fundamental physics in this system, including the structure of the magnetic field in the polar caps, the physics of sub-Eddington accretion, and physical processes inside the neutron star. | GALACTIC POINT SOURCES | 4 | B | BRIAN GREFENSTETTE | USA | 7 | AO7 | STUDY OF THE CYCLOTRON LINE FEATURE IN HERCULES X-1: THE PROFILE AND THE SHORT- AND LONG-TERM VARIABILITY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407051010/ | Quick Look | ![]() |
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893 | 1FGL J1018.6-5856 | 154.7377 | -58.9433 | 154.295067 | -58.691919 | 196.56156 | -60.86748 | 284.35288518 | -1.68600623 | 306.342 | 56102.9882407407 | 2012-06-24 23:43:04 | 56103.3696875 | 2012-06-25 08:52:21 | 407070010 | 17.4473 | 20 | 17.4645 | 17.4633 | 0 | 17.4473 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.4474 | 14.4474 | 32.9499 | 2 | PROCESSED | 57606.4834722222 | 2016-08-06 11:36:12 | 56480 | 2013-07-07 00:00:00 | 56114.1719328704 | 2012-07-06 04:07:35 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071234 | We propose Suzaku observations of a newly discovered gamma-ray binary 1FGL J1018.6-5856. Recent observations by the Fermi Gamma-ray Space Telescope and follow-up observations in other wavelengths revealed that the gamma-ray source is a new member of the rare gamma-ray binary class with an orbital period of 16 days. We propose two types of observations with Suzaku. One is a continuous observation of a sharp X-ray peak found in the lightcurve by the Swift XRT. Another is a series of snap shot observations in orbital phase between the peaks. We aim to perform phase-resolved spectral analysis which is not possible with the Swift XRT data. We also compare the Swift XRT lightcurve with new lightcurves taken by Suzaku in order to test the repeatability of the X-ray orbital modulation. | GALACTIC POINT SOURCES | 4 | B | TAKAAKI TANAKA | USA | 7 | AO7 | SUZAKU OBSERVATIONS OF A NEWLY DISCOVERED GAMMA-RAY BINARY: 1FGL J1018.6-5856 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407070010/ | Quick Look | ![]() |
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894 | V1159 ORI | 82.2495 | -3.563 | 81.626179 | -3.602056 | 81.331403 | -26.771731 | 206.52568579 | -19.93854352 | 268.4348 | 56732.3915856482 | 2014-03-16 09:23:53 | 56737.0939583333 | 2014-03-21 02:15:18 | 408029010 | 200.5487 | 200 | 200.5567 | 200.5487 | 0 | 200.5567 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 188.9927 | 188.9927 | 404.0226 | 3 | PROCESSED | 57614.1201967593 | 2016-08-14 02:53:05 | 56383 | 2013-04-01 00:00:00 | 56807.8867708333 | 2014-05-30 21:16:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081211 | We propose two 200 ks Suzaku observations of the dwarf nova V1159 Ori, chosen as our target because it is a known X-ray source with an extremely short (~4 day) outburst cycle. Each proposed observation will take ~5 calendar days and cover a complete outburst cycle. The dense X-ray coverage of the early rise in particular will be unprecedented for any dwarf nova, which is essential to further our understanding of the response of the boundary layer to the increased mass flux from the Keplerian accretion disk. We will also determine whether X-ray flux increases or decreases during quiescence to test the disk instability model. We will interpret the detailed picture of V1159 Ori in the context of existing, though less complete, X-ray campaigns on several other dwarf novae. | GALACTIC POINT SOURCES | 4 | A | KOJI MUKAI | USA | 8 | AO8 | X-RAY EMISSION THROUGH COMPLETE OUTBURST CYCLES OF THE DWARF NOVA V1159 ORI | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408029010/ | Quick Look | ![]() |
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895 | SERPENS X-1 | 279.9926 | 5.0265 | 279.375861 | 4.979658 | 281.287327 | 28.076343 | 36.11096598 | 4.83541867 | 266.6732 | 56566.4312037037 | 2013-10-01 10:20:56 | 56570.3821759259 | 2013-10-05 09:10:20 | 408033010 | 1.7605 | 250 | 9.5056 | 34.8553 | 0 | 1.7605 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 130.3293 | 130.3293 | 341.2899 | 2 | PROCESSED | 57612.9481018518 | 2016-08-12 22:45:16 | 57198 | 2015-06-25 00:00:00 | 56588.8182060185 | 2013-10-23 19:38:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081222 | Much recent work has been focused on Fe K emission lines in neutron star low-mass X-ray binaries (LMXBs). Suzaku and XMM observations appear to have revealed asymmetric line profiles characteristic of relativistic effects present at the innermost accretion disk. However, the nature of these lines are still hotly debated, with recent work suggesting that pile-up can artificially broaden lines. In order to address this critical issue, we propose a 250 ks Suzaku observation of the NS LMXB, Ser X-1. The broadband capabilities of Suzaku will allow for a robust model of the continuum either side of the Fe K line, while all CCDs will be operated in fast clocking modes to achieve pile-up free spectra. This Suzaku observation will help settle the nature of broad Fe K emission lines in NS LMXBs. | GALACTIC POINT SOURCES | 4 | B | EDWARD CACKETT | USA | 8 | AO8 | THE NATURE OF BROAD FE KALPHA EMISSION LINES IN NEUTRON STAR LOW-MASS X-RAY BINARIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408033010/ | Quick Look | ![]() |
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896 | SWIFT J1753.5-0127 | 268.3654 | -1.4463 | 267.717637 | -1.436793 | 268.227765 | 21.984126 | 24.9013847 | 12.1907035 | 84.8023 | 56750.7354398148 | 2014-04-03 17:39:02 | 56752.4452777778 | 2014-04-05 10:41:12 | 409051010 | 59.7028 | 50 | 59.7028 | 59.7108 | 0 | 59.7226 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53.6812 | 53.6812 | 147.7095 | 2 | PROCESSED | 57614.197025463 | 2016-08-14 04:43:43 | 57157 | 2015-05-15 00:00:00 | 56789.6957175926 | 2014-05-12 16:41:50 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091243 | Due to the presence of a steady jet, constraining the properties of black hole systems in their hard state is important for understanding accretion disks and jets. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? This proposal includes the use of Suzaku, NuSTAR, and radio observations to address these questions. A main diagnostic of the accretion geometry is the Compton reflection component, and the combination of Suzaku and NuSTAR covers, with very good energy resolution and sensitivity, the iron emission line, the absorption edges, and the hard X-ray reflection hump. | GALACTIC POINT SOURCES | 4 | A | JOHN TOMSICK | USA | 9 | AO9-TOO | CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409051010/ | Quick Look | ![]() |
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897 | SN 1987A | 83.8361 | -69.2786 | 83.928024 | -69.308301 | 307.518784 | -86.433209 | 279.71542477 | -31.94667609 | 132.5904 | 53677.835775463 | 2005-11-03 20:03:31 | 53678.3475 | 2005-11-04 08:20:24 | 500006010 | 36.7863 | 40 | 36.7863 | 36.7863 | 36.7863 | 36.7863 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 32.9198 | 32.9198 | 44.1661 | 1 | PROCESSED | 57527.9193518518 | 2016-05-19 22:03:52 | 54247 | 2007-05-27 00:00:00 | 54037.1281481482 | 2006-10-29 03:04:32 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001028 | SN1987A is providing us with a unique opportunity to study the supernova explosion itself and the very early phase of the supernova-remnants evolution. The supernova blast wave has started to strike the inner circumstellar ring. The neutrino flash observed at the time of explosion implies the formation of a neutron star, but no evidence of this has been detected yet. We propose to observe SN1987A for 40 ksec with Suzaku HXD and XIS. Our first goal is the search for a periodic hard signal from the putative pulsar. We also want to study the collision of the supernova blast wave with the inner ring. In order to follow the temporal evolution of the shock, we propose to observe the source with Suzaku in the early phase of the SWG PV-phase as a reference for further studies. | GALACTIC DIFFUSE EMISSION | 5 | A | GUENTHER HASINGER | JAP | 0 | SWG | SUZAKU OBSERVATION OF SN1987A : SEARCH FOR PULSAR EMISSION AND STUDY OF A NEWBORN SNR | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500006010/ | Quick Look | ![]() |
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898 | GALACTIC RIDGE | 281.0049 | -4.0776 | 280.344509 | -4.129178 | 281.602156 | 18.920781 | 28.45801897 | -0.21166151 | 265.5297 | 53671.1112037037 | 2005-10-28 02:40:08 | 53673.8960069445 | 2005-10-30 21:30:15 | 500009010 | 93.3276 | 100 | 93.3436 | 93.3596 | 93.3436 | 93.3276 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 77.5364 | 77.5364 | 240.5759 | 0 | PROCESSED | 57527.7330439815 | 2016-05-19 17:35:35 | 54247 | 2007-05-27 00:00:00 | 54037.6929513889 | 2006-10-29 16:37:51 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001042 | We propose to observe the blank Galactic plane field at (l,b)=(28.6,0.0) for 200 ksec to study energy spectra of Galactic Ridge X-ray Emission. This is a Chandra deep field where we have spent 100 ksec. We will carry out plasma diagnostics of the Galactic ridge emission using primarily iron lines, and also Kalpha and Kbeta lines of Ne, Mg, Si, and S. The 200 ksec Ridge observation by Suzaku enables us to compare Galactic center and ridge emission lines directly. We believe the Galactic Ridge X-ray emission is truely diffuse, based on our Chandra study. However, there is a claim that the ridge emission is preimaly composed of dim sources down to 10^-16 cgs in 2-10 keV. To end the controversy, we plan to carry out a 1Msec Chandra observation on this Chandra-Suzaku field. | GALACTIC DIFFUSE EMISSION | 5 | A | KEN EBISAWA | JAP | 0 | SWG | ORIGIN OF THE GALACTIC RIDGE X-RAY EMISSION | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500009010/ | Quick Look | ![]() |
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899 | 73P/SW3 | 318.3252 | 23.9905 | 317.766876 | 23.78347 | 329.890581 | 37.931404 | 71.97868305 | -16.64134569 | 72.7093 | 53868.4091666667 | 2006-05-13 09:49:12 | 53868.4752199074 | 2006-05-13 11:24:19 | 500013050 | 3.225 | 20 | 3.225 | 3.225 | 3.225 | 3.225 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.584 | 2.584 | 5.7039 | 0 | PROCESSED | 57534.2992476852 | 2016-05-26 07:10:55 | 54256 | 2007-06-05 00:00:00 | 54089.4348611111 | 2006-12-20 10:26:12 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013050/ | Quick Look | ![]() |
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900 | 73P/SW3 | 318.7382 | 23.8104 | 318.178519 | 23.602036 | 330.247137 | 37.622205 | 72.09504522 | -17.04458663 | 72.7096 | 53868.4758333333 | 2006-05-13 11:25:12 | 53868.5418865741 | 2006-05-13 13:00:19 | 500013060 | 3.218 | 20 | 3.218 | 3.218 | 3.218 | 3.218 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.539 | 2.539 | 5.6959 | 0 | PROCESSED | 57534.3046759259 | 2016-05-26 07:18:44 | 54256 | 2007-06-05 00:00:00 | 54042.3000462963 | 2006-11-03 07:12:04 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013060/ | Quick Look | ![]() |
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901 | 73P/SW3 | 319.575 | 23.4516 | 319.012619 | 23.240566 | 330.968775 | 37.00001 | 72.3420597 | -17.8575616 | 72.7092 | 53868.609212963 | 2006-05-13 14:37:16 | 53868.6738310185 | 2006-05-13 16:10:19 | 500013080 | 3.1644 | 20 | 3.1644 | 3.1644 | 3.1644 | 3.1644 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.986 | 2.986 | 5.5519 | 0 | PROCESSED | 57534.3120601852 | 2016-05-26 07:29:22 | 54256 | 2007-06-05 00:00:00 | 54042.3213657407 | 2006-11-03 07:42:46 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013080/ | Quick Look | ![]() |
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902 | CAR-D1 | 162.0244 | -59.5887 | 161.531362 | -59.324189 | 202.52434 | -58.576902 | 287.89332648 | -0.36746291 | 282.973 | 53891.5567361111 | 2006-06-05 13:21:42 | 53892.6343055556 | 2006-06-06 15:13:24 | 501099010 | 76.9074 | 75 | 76.924 | 76.932 | 76.9314 | 76.9074 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 64.2576 | 64.2576 | 93.0899 | 0 | PROCESSED | 57534.5127430556 | 2016-05-26 12:18:21 | 54401 | 2007-10-28 00:00:00 | 53926.947974537 | 2006-07-10 22:45:05 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011257 | Soft X-ray emission nebulae with kT =0.1-0.8 keV, log Lx =33-35 ergs/s, and the size of 1-1000 pc accompany a number of giant HII region, but the origin is not understood yet. The Carinae Nebula is 10-100 times more luminous than any other giant HII region in our Galaxy in soft X-rays. From an XMM-Newton observation of the eastern tip of the nebula called Car-D1, we found marginal CVI, CV and OVII lines. If it is real, the carbon abundance should be more than >6 solar, and the OVII line requires more than 2-temperature components. To detect those emission lines clearly and address the origin and environment of the diffuse plasma, we propose a Suzaku observation of the Car-D1 region, optimized for the XIS BI chip. | GALACTIC DIFFUSE EMISSION | 5 | B | KENJI HAMAGUCHI | USA | 1 | AO1 | ORIGIN OF THE DIFFUSE X-RAY EMISSION AROUND THE CARINA NEBULA, A MASSIVE STAR FORMING REGION | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501099010/ | Quick Look | ![]() |
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903 | GALACTIC PLANE 111 | 347.9369 | 61.9538 | 347.407091 | 61.681886 | 29.574403 | 58.088255 | 111.50111702 | 1.31488521 | 81.8498 | 53892.6499652778 | 2006-06-06 15:35:57 | 53893.680775463 | 2006-06-07 16:20:19 | 501100010 | 72.1409 | 75 | 72.1649 | 72.1649 | 72.1649 | 72.1409 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 61.025 | 61.025 | 89.0349 | 1 | PROCESSED | 57534.5221064815 | 2016-05-26 12:31:50 | 54401 | 2007-10-28 00:00:00 | 53927.3325115741 | 2006-07-11 07:58:49 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011258 | We propose to observe the line of sight towards (l,b)=(111.5,1.3). This line of sight was observed by XMM because the line of sight is particularly simple, allowing the isolation of the spectrum of the Local Hot Bubble (LHB). The XMM observation did not isolate the LHB, but did reveal the existance of a cool (kT~0.18 keV) X-ray emitting component between 200 and 2000 pcs away that was morphologically unidentifiable in the ROSAT All-Sky Survey. This component may represent the gas responsible for the 3/4 keV "infill problem", and may represent a previously overlooked high filling factor component of the hot ISM. Suzaku observations along this line of sight, coupled with the Suzaku observation towards MBM12, will allow the isolation of this component. | GALACTIC DIFFUSE EMISSION | 5 | B | K. KUNTZ | USA | 1 | AO1 | BEYOND THE LOCAL HOT BUBBLE TOWARDS L=111 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501100010/ | Quick Look | ![]() |
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904 | DRACO ENHANCEMENT | 239.3128 | 61.2868 | 239.109888 | 61.42925 | 187.011559 | 75.692319 | 93.98685674 | 43.98646489 | 194.9053 | 54048.1213888889 | 2006-11-09 02:54:48 | 54049.8515509259 | 2006-11-10 20:26:14 | 501101010 | 43.8628 | 75 | 79.4274 | 79.4274 | 43.8628 | 79.4194 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 75.8741 | 75.8741 | 149.474 | 1 | PROCESSED | 57536.1016319444 | 2016-05-28 02:26:21 | 54455 | 2007-12-21 00:00:00 | 54088.7470486111 | 2006-12-19 17:55:45 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011259 | We propose to observe the Draco Enhancement, a region of very bright 1/4 keV emission in the northern Galactic halo that is only 15 degrees from the Suzaku observation of the North Ecliptic Pole. A decomposition of the spectrum of the Galactic halo by Kuntz & Snowden showed that, to within the uncertainties of the ROSAT All-Sky Survey, the halo emission was composed of two thermal components; a uniform hot component with kT~0.25 keV, and a very patchy soft component with kT~0.1 keV. The soft component is found in only a few isolated regions of the sky, of which the Draco Enhancement is the brightest. This emission is too soft to be studied with XMM. Suzaku will allow us to determine the temperature of the soft component or place very strict upper limits on its temperature. | GALACTIC DIFFUSE EMISSION | 5 | C | K. KUNTZ | USA | 1 | AO1 | THE SOFT COMPONENT OF THE GALACTIC HALO | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501101010/ | Quick Look | ![]() |
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905 | COMET_8P_TUTTLE-P1-2 | 27.9946 | 7.7582 | 27.33663 | 7.511628 | 28.768937 | -3.5069 | 147.87340904 | -52.1573456 | 248.4994 | 54470.5826041667 | 2008-01-05 13:58:57 | 54470.6488310185 | 2008-01-05 15:34:19 | 502062020 | 2.2193 | 2 | 2.2193 | 2.2193 | 0 | 2.2193 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2.164 | 2.164 | 5.718 | 0 | PROCESSED | 57540.985162037 | 2016-06-01 23:38:38 | 54908 | 2009-03-18 00:00:00 | 54542.2129166667 | 2008-03-17 05:06:36 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062020/ | Quick Look | ![]() |
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906 | COMET_8P_TUTTLE-P1-4 | 28.0997 | 7.2516 | 27.442835 | 7.005266 | 28.688048 | -4.017818 | 148.34803657 | -52.5857522 | 248.4989 | 54470.7159143518 | 2008-01-05 17:10:55 | 54470.7821527778 | 2008-01-05 18:46:18 | 502062040 | 1.7233 | 2 | 1.7233 | 1.7233 | 0 | 1.7233 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1.4567 | 1.4567 | 5.722 | 0 | PROCESSED | 57540.9953125 | 2016-06-01 23:53:15 | 54908 | 2009-03-18 00:00:00 | 54542.2187847222 | 2008-03-17 05:15:03 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062040/ | Quick Look | ![]() |
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907 | NEP #1 | 270.0492 | 66.5597 | 270.050416 | 66.559437 | 358.096328 | 89.986108 | 96.38280784 | 29.79186901 | 217.1802 | 55150.229212963 | 2009-11-15 05:30:04 | 55151.1953587963 | 2009-11-16 04:41:19 | 504070010 | 56.3367 | 50 | 56.3367 | 56.3447 | 0 | 56.3447 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 41.4345 | 41.4345 | 83.4719 | 2 | PROCESSED | 57549.3863657407 | 2016-06-10 09:16:22 | 54922 | 2009-04-01 00:00:00 | 55162.2062268518 | 2009-11-27 04:56:58 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | STEVEN SNOWDEN | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504070010/ | Quick Look | ![]() |
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908 | SEP #2 | 89.966 | -66.5714 | 89.96805 | -66.571581 | 300.397678 | -89.984546 | 276.39630454 | -29.82495373 | 163.7813 | 55170.9454166667 | 2009-12-05 22:41:24 | 55172.4863194444 | 2009-12-07 11:40:18 | 504071010 | 57.9991 | 50 | 58.0071 | 57.9991 | 0 | 58.0071 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.4152 | 35.4152 | 133.112 | 1 | PROCESSED | 57549.7252546296 | 2016-06-10 17:24:22 | 54922 | 2009-04-01 00:00:00 | 55187.4854398148 | 2009-12-22 11:39:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | STEVEN SNOWDEN | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504071010/ | Quick Look | ![]() |
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909 | SEP #4 | 89.9798 | -66.5683 | 89.981754 | -66.568414 | 282.855223 | -89.989511 | 276.39272547 | -29.81946932 | 185.1981 | 55192.0059490741 | 2009-12-27 00:08:34 | 55193.3995833333 | 2009-12-28 09:35:24 | 504075010 | 49.9566 | 50 | 49.9566 | 49.9566 | 0 | 49.9566 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.143 | 45.143 | 120.3939 | 1 | PROCESSED | 57549.980474537 | 2016-06-10 23:31:53 | 54922 | 2009-04-01 00:00:00 | 55225.3094907407 | 2010-01-29 07:25:40 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | STEVEN SNOWDEN | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504075010/ | Quick Look | ![]() |
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910 | VELA PWN NE1 | 129.3684 | -44.9817 | 128.942936 | -44.80588 | 153.830902 | -60.001311 | 263.62243766 | -2.36980886 | 142.6395 | 55916.6230439815 | 2011-12-21 14:57:11 | 55917.0070601852 | 2011-12-22 00:10:10 | 506041010 | 15.408 | 15 | 15.424 | 15.408 | 0 | 15.424 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.5681 | 11.5681 | 33.1759 | 1 | PROCESSED | 57604.1925347222 | 2016-08-04 04:37:15 | 56305 | 2013-01-13 00:00:00 | 55937.7788310185 | 2012-01-11 18:41:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | C | SATORU KATSUDA | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506041010/ | Quick Look | ![]() |
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911 | VELA PWN E2 | 129.5733 | -45.3227 | 129.149771 | -45.146105 | 154.428094 | -60.221749 | 263.98172095 | -2.46094632 | 304.5019 | 55711.9038773148 | 2011-05-30 21:41:35 | 55712.1328935185 | 2011-05-31 03:11:22 | 506045010 | 13.904 | 15 | 13.92 | 13.904 | 0 | 13.92 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.404 | 8.404 | 19.7759 | 0 | PROCESSED | 57602.1624074074 | 2016-08-02 03:53:52 | 56092 | 2012-06-14 00:00:00 | 55725.2563888889 | 2011-06-13 06:09:12 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | B | SATORU KATSUDA | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506045010/ | Quick Look | ![]() |
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912 | NGC5129 OFF-CENTER1 | 201.3141 | 14.0346 | 200.698603 | 14.294472 | 194.098163 | 21.268391 | 335.68408417 | 74.71314923 | 124.7585 | 55548.0427314815 | 2010-12-18 01:01:32 | 55548.7883101852 | 2010-12-18 18:55:10 | 805072010 | 30.2512 | 30 | 30.2512 | 30.2512 | 0 | 30.2512 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24.4611 | 24.4611 | 64.4119 | 0 | PROCESSED | 57554.4566203704 | 2016-06-15 10:57:32 | 55960 | 2012-02-03 00:00:00 | 55592.9994444444 | 2011-01-31 23:59:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051512 | Using the composite data from dwarf galaxies to rich clusters, we find that the baryon fraction is mainly set by the system's potential well depth. The small scatter of baryon fractions as a function of the gravitational potential well depth indicates a universal baryon loss mechanism for these systems. However, the relation is most poorly constrained in the poor galaxy group regime below 1keV, where few individual measurements exists. Since most galaxies reside in these groups, it is also important to test whether the missing baryons from the galaxies are actually in these poor groups. We propose deep, off-center observations of two such groups, doubling the sample, to better delineate and understand the transition of the baryon loss from clusters to galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | XINYU DAI | USA | 5 | AO5 | BARYON LOSS IN POOR GALAXY GROUPS: DISTINGUISHING PRE-HEATING AND FEEDBACK MODELS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805072010/ | Quick Look | ![]() |
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913 | MKW 4-OFFSET2 | 181.4291 | 1.9058 | 180.78864 | 2.184142 | 180.549883 | 2.316727 | 277.53009765 | 62.50090006 | 114.4199 | 55530.2508101852 | 2010-11-30 06:01:10 | 55532.2286805556 | 2010-12-02 05:29:18 | 805082010 | 82.9361 | 80 | 82.9401 | 82.9361 | 0 | 82.9441 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.0619 | 70.0619 | 170.8541 | 2 | PROCESSED | 57554.329525463 | 2016-06-15 07:54:31 | 55910 | 2011-12-15 00:00:00 | 55544.2869328704 | 2010-12-14 06:53:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051525 | We propose a set of two 19 arcmin offset observations for the galaxy groups MKW 4 to measure spatially resolved density, temperature and iron abundance out to r_{500}. These measurements are crucial for an accurate determination of the gas mass profile and gas fraction, for probing the entropy profile near the region where the accretion shocks start to be important, and for exploring the chemical enrichment at a spatial scale which retains information of early SNII and SNIa enrichment. Due to its brightness, regularity and low temperature, the object is an ideal candidate for an offset observation of its peripheral gas by Suzaku, making an excellent use of its low background and soft X-ray sensitivity. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | FABIO GASTALDELLO | USA | 5 | AO5 | THE OUTSKIRTS OF MKW 4 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805082010/ | Quick Look | ![]() |
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914 | PKS 0745-191 | 117.0925 | -18.8008 | 116.536214 | -18.67521 | 123.761788 | -39.117935 | 236.11480248 | 3.4506494 | 113.9994 | 55514.1140625 | 2010-11-14 02:44:15 | 55515.1105324074 | 2010-11-15 02:39:10 | 805083010 | 37.2084 | 35 | 37.2164 | 37.2084 | 0 | 37.2164 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 31.5228 | 31.5228 | 86.0879 | 1 | PROCESSED | 57554.0728703704 | 2016-06-15 01:44:56 | 55903 | 2011-12-08 00:00:00 | 55537.2095486111 | 2010-12-07 05:01:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051526 | Suzaku has enabled us to make the first measurement of the temperature profile beyond the virial radius of any cluster. The gas in the outskirts of galaxy clusters presents information of astrophysical and cosmological importance. Measurements at the virial radius, where the dominant gas behavior switches from infall to equilibrium, can improve cluster mass estimates. Temperature and entropy profiles in the outskirts describe the accretion history and energy balance of clusters, near where they must match the background properties of the Universe. But these observations are just beginning. How do clusters grow? Are there large scale accretion shocks? To what extent are clusters relaxed? Here we propose to continue our study of PKS 0745-191 using Suzaku's unique capability to map this area. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MATTHEW GEORGE | USA | 5 | AO5 | BEYOND THE VIRIAL RADIUS OF PKS 0745-191, THE BRIGHTEST CLUSTER PAST Z=0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805083010/ | Quick Look | ![]() |
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915 | PKS 0745-191 | 116.6522 | -19.7838 | 116.101042 | -19.660112 | 123.535239 | -40.170782 | 236.7569882 | 2.59757333 | 114.0013 | 55515.1115162037 | 2010-11-15 02:40:35 | 55516.1335416667 | 2010-11-16 03:12:18 | 805087010 | 37.9286 | 35 | 37.9526 | 37.9446 | 0 | 37.9286 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.1037 | 32.1037 | 88.2858 | 2 | PROCESSED | 57554.1054976852 | 2016-06-15 02:31:55 | 55895 | 2011-11-30 00:00:00 | 55526.1606018518 | 2010-11-26 03:51:16 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051526 | Suzaku has enabled us to make the first measurement of the temperature profile beyond the virial radius of any cluster. The gas in the outskirts of galaxy clusters presents information of astrophysical and cosmological importance. Measurements at the virial radius, where the dominant gas behavior switches from infall to equilibrium, can improve cluster mass estimates. Temperature and entropy profiles in the outskirts describe the accretion history and energy balance of clusters, near where they must match the background properties of the Universe. But these observations are just beginning. How do clusters grow? Are there large scale accretion shocks? To what extent are clusters relaxed? Here we propose to continue our study of PKS 0745-191 using Suzaku's unique capability to map this area. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MATTHEW GEORGE | USA | 5 | AO5 | BEYOND THE VIRIAL RADIUS OF PKS 0745-191, THE BRIGHTEST CLUSTER PAST Z=0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805087010/ | Quick Look | ![]() |
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916 | SNR 0519-69.0 | 79.8865 | -69.038 | 79.962501 | -69.086742 | 322.357221 | -85.457085 | 279.70295655 | -33.37204199 | 53.6181 | 55782.8380324074 | 2011-08-09 20:06:46 | 55789.4030555556 | 2011-08-16 09:40:24 | 806026010 | 347.5681 | 350 | 347.5681 | 347.5761 | 0 | 347.5761 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 355.0724 | 355.0724 | 395.8115 | 7 | PROCESSED | 57602.9665740741 | 2016-08-02 23:11:52 | 55652 | 2011-04-01 00:00:00 | 55802.468900463 | 2011-08-29 11:15:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061102 | We propose two relatively deep observations of the young ejecta-dominated supernova remnants 0509-67.5 and 0519-69.0 in the Large Magellanic Cloud. Our goal is to seek line emission from the trace elements Mn and Cr in these remnants of Type Ia supernovae, and to measure the corresponding abundances using calculated atomic data. The relative masses of Mn and Cr produced in Type Ia supernovae are a diagnostic of the initial metallicity of the progenitor system. Of the supernovae that produced these two remnants, one had a normal luminosity, while the other was over-luminous. Together with existing data for another LMC Ia remnant, N103B, which shows evidence for circumstellar interactions, these observations will provide a broad sample of the variety seen in Ia events. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | UNA HWANG | USA | 6 | AO6-LP | ABUNDANCES OF CR AND MN AND THE PROGENITOR METALLICITY IN TWO TYPE IA MAGELLANIC CLOUD SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806026010/ | Quick Look | ![]() |
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917 | ABELL 773 | 139.6885 | 51.8172 | 138.816003 | 52.028068 | 124.747961 | 34.198508 | 165.93230971 | 43.4884399 | 276.9986 | 55682.3638888889 | 2011-05-01 08:44:00 | 55683.2105902778 | 2011-05-02 05:03:15 | 806027010 | 42.5779 | 50 | 42.5859 | 42.5859 | 0 | 42.5779 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 32.7052 | 32.7052 | 73.1439 | 0 | PROCESSED | 57601.9080555556 | 2016-08-01 21:47:36 | 55652 | 2011-04-01 00:00:00 | 55697.2644560185 | 2011-05-16 06:20:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061116 | We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 6 | AO6-LP | THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806027010/ | Quick Look | ![]() |
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918 | ABELL 1068 | 159.9611 | 39.9499 | 159.238834 | 40.210787 | 145.421786 | 28.986121 | 179.20513519 | 59.95740225 | 130.001 | 55864.5464583333 | 2011-10-30 13:06:54 | 55865.764849537 | 2011-10-31 18:21:23 | 806028040 | 51.1493 | 50 | 51.1573 | 51.1493 | 0 | 51.1653 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.5701 | 46.5701 | 105.2498 | 0 | PROCESSED | 57603.6525810185 | 2016-08-03 15:39:43 | 55652 | 2011-04-01 00:00:00 | 55879.1651967593 | 2011-11-14 03:57:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061116 | We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 6 | AO6-LP | THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806028040/ | Quick Look | ![]() |
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919 | COMA E5 | 196.4286 | 27.8904 | 195.829087 | 28.157796 | 182.91784 | 31.908863 | 47.28907584 | 86.74411283 | 279.9981 | 55730.3360416667 | 2011-06-18 08:03:54 | 55730.7848726852 | 2011-06-18 18:50:13 | 806034010 | 18.2706 | 20 | 18.2706 | 18.2946 | 0 | 18.2786 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15.0751 | 15.0751 | 38.7599 | 0 | PROCESSED | 57602.3384259259 | 2016-08-02 08:07:20 | 55652 | 2011-04-01 00:00:00 | 55770.1405324074 | 2011-07-28 03:22:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806034010/ | Quick Look | ![]() |
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920 | COMA NW4 | 194.43 | 28.912 | 193.827069 | 29.181931 | 180.525216 | 32.025522 | 85.44172027 | 87.7408795 | 319.999 | 55732.9798611111 | 2011-06-20 23:31:00 | 55733.468912037 | 2011-06-21 11:15:14 | 806041010 | 21.1196 | 20 | 21.1236 | 21.1434 | 0 | 21.1196 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.5915 | 21.5915 | 42.246 | 0 | PROCESSED | 57602.3778819444 | 2016-08-02 09:04:09 | 55652 | 2011-04-01 00:00:00 | 55768.2688888889 | 2011-07-26 06:27:12 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806041010/ | Quick Look | ![]() |
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921 | NGC5866 | 226.5977 | 55.7554 | 226.254302 | 55.947234 | 186.820283 | 67.076445 | 92.03719886 | 52.50531538 | 352.5583 | 55701.1230092593 | 2011-05-20 02:57:08 | 55703.3466898148 | 2011-05-22 08:19:14 | 806053010 | 101.8346 | 100 | 101.8426 | 101.8346 | 0 | 101.8426 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 94.7812 | 94.7812 | 192.0718 | 2 | PROCESSED | 57602.140787037 | 2016-08-02 03:22:44 | 56102 | 2012-06-24 00:00:00 | 55735.3197800926 | 2011-06-23 07:40:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061502 | An existing Chandra observation indicates hot gas in the S0 galaxy NGC5866 has a supersolar iron abundance and an unusually low O/Fe ratio. The galaxy is also rich in molecular gas and shows distinct vertical dusty filaments, which most likely represent cold gas blown out by SNe from the disk. We herein propose a 100ks Suzaku observation of it to better measure the hot gas properties and its spatial distribution. The energy resolution and counting statistics of the observation will enable us to greatly improve the measurement of the abundances. By further comparing such measurements among galaxies of different cold gas contents, we will investigate the effect of cold/hot gas interaction on the dynamics of the hot gas, as well as its thermal and chemical properties. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JIANG-TAO LI | USA | 6 | AO6 | X-RAY SPECTROSCOPY OF STELLAR FEEDBACK PROCESSES IN A COOL GAS-RICH S0 GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806053010/ | Quick Look | ![]() |
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922 | SPT-CL J2341-5119 | 355.3013 | -51.333 | 354.629905 | -51.610408 | 330.126015 | -44.109465 | 326.93544545 | -62.39708341 | 56.9213 | 55703.3602662037 | 2011-05-22 08:38:47 | 55706.0800810185 | 2011-05-25 01:55:19 | 806072010 | 100.2347 | 100 | 100.2427 | 100.2347 | 0 | 100.2507 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 88.2081 | 88.2081 | 234.9799 | 3 | PROCESSED | 57602.1463310185 | 2016-08-02 03:30:43 | 56092 | 2012-06-14 00:00:00 | 55725.3016550926 | 2011-06-13 07:14:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061531 | We propose observations of four high-redshift galaxy clusters to constrain the metal enrichment history of the intra-cluster medium (ICM). The clusters, two at z ~ 1.0 and two at z ~ 0.75, are chosen from an initial mass-limited sample identified by the South Pole Telescope (SPT) cluster project, and they are among the most massive high-redshift clusters known. Chandra observations have verified the absence of point sources in these targets. The proposed Suzaku observations will increase the X-ray cluster counts by a factor of four, they will yield the most precise ICM abundance measurements at these redshifts to date, and they will provide a path-finder for future Suzaku studies of large, representative samples of high-redshift clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ERIC MILLER | USA | 6 | AO6 | THE METAL ABUNDANCE OF HIGH-REDSHIFT GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806072010/ | Quick Look | ![]() |
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923 | RCS044406-2820.4 | 71.0221 | -28.343 | 70.523595 | -28.434713 | 63.530115 | -50.056858 | 228.67801491 | -39.02616141 | 99.3268 | 55827.6316319444 | 2011-09-23 15:09:33 | 55828.8751736111 | 2011-09-24 21:00:15 | 806080010 | 50.6723 | 50 | 50.6723 | 50.6723 | 0 | 50.6723 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.9027 | 41.9027 | 107.4318 | 3 | PROCESSED | 57603.2531134259 | 2016-08-03 06:04:29 | 56222 | 2012-10-22 00:00:00 | 55854.3160300926 | 2011-10-20 07:35:05 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061533 | Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 19 optically-selected clusters of galaxies, half at z~0.3 and half at z~0.8. Here we propose 6 additional observations in order to uniformly span a total redshift range of 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | AMALIA HICKS | USA | 6 | AO6 | AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806080010/ | Quick Look | ![]() |
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924 | SDSS J0906+0301 | 136.6571 | 3.0284 | 136.006 | 3.229773 | 138.178094 | -12.954149 | 226.89088068 | 31.22930355 | 109.9836 | 56253.2318981482 | 2012-11-22 05:33:56 | 56253.846099537 | 2012-11-22 20:18:23 | 807059010 | 21.7148 | 20 | 21.7228 | 21.7148 | 0 | 21.7228 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.632 | 20.632 | 53.066 | 0 | PROCESSED | 57608.0815972222 | 2016-08-08 01:57:30 | 56702 | 2014-02-14 00:00:00 | 56336.4694328704 | 2013-02-13 11:15:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071512 | Fossil groups (FGs) are systems dominated by a single large galaxy with a cluster-scale X-ray halo. They are thought to be old, isolated galaxy groups in which the large galaxies have coalesced through dynamical friction, but recent studies reveal a more complicated picture. We propose Suzaku observations of 5 optically selected FG candidates. These targets will extend our previous survey, which identified 12 FGs; when combined with 5 FG candidates approved for the current Chandra cycle, this will create the largest uniformly-selected sample of real FGs. The L_X and T_X measured will be used with optical spectroscopy to extend FG scaling relations to low mass, and to plan deeper X-ray spectroscopic follow-up to constrain the formation epoch and evolution of these puzzling systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ERIC MILLER | USA | 7 | AO7 | FINDING FOSSIL GROUPS WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807059010/ | Quick Look | ![]() |
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925 | SDSS J1431+0047 | 217.7608 | 0.788 | 217.122744 | 1.009037 | 215.129123 | 14.8431 | 349.30444711 | 54.43383912 | 287.7594 | 56140.9857291667 | 2012-08-01 23:39:27 | 56141.454375 | 2012-08-02 10:54:18 | 807062010 | 22.3553 | 20 | 22.371 | 22.3553 | 0 | 22.363 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.5809 | 16.5809 | 40.4799 | 1 | PROCESSED | 57606.7190740741 | 2016-08-06 17:15:28 | 56528 | 2013-08-24 00:00:00 | 56162.1265972222 | 2012-08-23 03:02:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071512 | Fossil groups (FGs) are systems dominated by a single large galaxy with a cluster-scale X-ray halo. They are thought to be old, isolated galaxy groups in which the large galaxies have coalesced through dynamical friction, but recent studies reveal a more complicated picture. We propose Suzaku observations of 5 optically selected FG candidates. These targets will extend our previous survey, which identified 12 FGs; when combined with 5 FG candidates approved for the current Chandra cycle, this will create the largest uniformly-selected sample of real FGs. The L_X and T_X measured will be used with optical spectroscopy to extend FG scaling relations to low mass, and to plan deeper X-ray spectroscopic follow-up to constrain the formation epoch and evolution of these puzzling systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ERIC MILLER | USA | 7 | AO7 | FINDING FOSSIL GROUPS WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807062010/ | Quick Look | ![]() |
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926 | ABELL 2597 | 351.4175 | -11.9496 | 350.767566 | -12.224675 | 347.389222 | -7.579212 | 65.78537526 | -64.80325971 | 249.1017 | 56261.057650463 | 2012-11-30 01:23:01 | 56262.3299768518 | 2012-12-01 07:55:10 | 807073010 | 51.0526 | 50 | 51.0566 | 51.0674 | 0 | 51.0526 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.3613 | 46.3613 | 109.9139 | 1 | PROCESSED | 57608.180462963 | 2016-08-08 04:19:52 | 56018 | 2012-04-01 00:00:00 | 56278.743587963 | 2012-12-17 17:50:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071522 | We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 7 | AO7 | COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807073010/ | Quick Look | ![]() |
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927 | RXJ1159+5531 E | 180.1946 | 55.5211 | 179.553068 | 55.799424 | 150.053445 | 49.203071 | 137.37799324 | 60.16358606 | 301.575 | 56806.5416550926 | 2014-05-29 12:59:59 | 56808.2502430556 | 2014-05-31 06:00:21 | 809063010 | 99.1618 | 100 | 99.1778 | 99.1618 | 0 | 99.1778 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.1713657407 | 2016-08-15 04:06:46 | 57234 | 2015-07-31 00:00:00 | 56866.7150925926 | 2014-07-28 17:09:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091521 | In contrast to some recent observations of cluster outskirts, for RXJ1159+5531, we obtain measurements of the gas fraction and entropy at the virial radius that are fully consistent with gravity-only structure formation simulations. Our preliminary Suzaku analysis of an opposite direction shows similar results. This encouraging consistency suggests that we may see little azimuthal variation in the gas properties for this unusually relaxed system. To verify and also benefit from the relaxed state of this benchmark system, we propose complementary Suzaku observations of RXJ1159+5531 in the other two directions. Simultaneously fitting these pointings would provide us the metal abundance ratios at large radii in order to place broad constrains on the enrichment history of group scale systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | YUANYUAN SU | USA | 9 | AO9 | MAPPING A BENCHMARK RELAXED POOR CLUSTER OUT TO ITS VIRIAL RADIUS WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809063010/ | Quick Look | ![]() |
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928 | ABELL 98-CENTER | 11.6247 | 20.5572 | 10.963731 | 20.284211 | 18.829002 | 14.307964 | 121.3687084 | -42.29955696 | 80.8972 | 56837.6648726852 | 2014-06-29 15:57:25 | 56839.2014236111 | 2014-07-01 04:50:03 | 809077010 | 60.781 | 60 | 60.781 | 60.917 | 0 | 60.925 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3554282407 | 2016-08-15 08:31:49 | 56748 | 2014-04-01 00:00:00 | 56854.7844212963 | 2014-07-16 18:49:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091525 | We propose to observe the outskirts of the strongly merging cluster Abell 98 both along and perpendicular to the large scale structure filament implied by the orientation of its three merging subclusters. This is the only remaining one of the four bright, strongly merging "double" clusters originally identified from Einstein observations that has not been observed with Suzaku. A comparison of the extended atmosphere in the filament and off-filament pointings will allow us to test for the presence of unresolved gas clumps, which should be more abundant along the filament, invoked to explain anomalously high (above cosmic) baryon fractions observed in some other clusters. If this "unresolved clumps" hypothesis is correct, then we should find higher baryon fractions along the filament. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SCOTT RANDALL | USA | 9 | AO9 | EXPLORING THE EXTENDED ATMOSPHERE OF THE STRONGLY MERGING CLUSTER ABELL 98 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809077010/ | Quick Look | ![]() |
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929 | ABELL 98-WEST | 11.3131 | 20.6695 | 10.652564 | 20.396219 | 18.599995 | 14.528185 | 120.97936172 | -42.17879703 | 80.8359 | 56841.9624537037 | 2014-07-03 23:05:56 | 56844.7606712963 | 2014-07-06 18:15:22 | 809079010 | 96.6924 | 100 | 96.6924 | 100.6438 | 0 | 100.6598 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3882638889 | 2016-08-15 09:19:06 | 56748 | 2014-04-01 00:00:00 | 56881.441724537 | 2014-08-12 10:36:05 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091525 | We propose to observe the outskirts of the strongly merging cluster Abell 98 both along and perpendicular to the large scale structure filament implied by the orientation of its three merging subclusters. This is the only remaining one of the four bright, strongly merging "double" clusters originally identified from Einstein observations that has not been observed with Suzaku. A comparison of the extended atmosphere in the filament and off-filament pointings will allow us to test for the presence of unresolved gas clumps, which should be more abundant along the filament, invoked to explain anomalously high (above cosmic) baryon fractions observed in some other clusters. If this "unresolved clumps" hypothesis is correct, then we should find higher baryon fractions along the filament. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SCOTT RANDALL | USA | 9 | AO9 | EXPLORING THE EXTENDED ATMOSPHERE OF THE STRONGLY MERGING CLUSTER ABELL 98 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809079010/ | Quick Look | ![]() |
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930 | MONOGEM RING WEST | 118.3557 | 8.2507 | 117.679197 | 8.381467 | 118.769502 | -12.402687 | 212.50229712 | 17.5030797 | 287.8334 | 53865.545462963 | 2006-05-10 13:05:28 | 53867.1127199074 | 2006-05-12 02:42:19 | 501084010 | 54.2685 | 50 | 54.2685 | 54.2685 | 54.2685 | 54.2685 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 43.2312 | 43.2312 | 135.3899 | 2 | PROCESSED | 57534.3136689815 | 2016-05-26 07:31:41 | 54401 | 2007-10-28 00:00:00 | 53914.2479282407 | 2006-06-28 05:57:01 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011243 | We propose to acquire the first high-quality, CCD resolution spectrum of the Monogem Ring SNR. The Monogem Ring is a large (D~25 degrees), old (t~10^5 yr) SNR with a soft X-ray spectrum. A 50 ks observation with Suzaku will detect and measure the OVII Triplet and OVIII Lyman-alpha line fluxes. We will use the ratio of these two line complexes to constrain the temperature and ionization timescale of the plasma in this region of the Monogem Ring. Determing the plasma conditions in such evolved SNRs is important for understanding how these remnants merge with and affect the interstellar medium. | GALACTIC DIFFUSE EMISSION | 5 | B | PAUL PLUCINSKY | USA | 1 | AO1 | THE MONOGEM RING: MEASURING THE O LINE EMISSION WITH SUZAKU | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501084010/ | Quick Look | ![]() |
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931 | 3C 390.3 | 280.629 | 79.7686 | 281.497615 | 79.715169 | 81.957835 | 76.491681 | 111.4356997 | 27.05756334 | 197.286 | 54083.1426851852 | 2006-12-14 03:25:28 | 54085.1384722222 | 2006-12-16 03:19:24 | 701060010 | 0.024 | 100 | 99.3678 | 99.3678 | 0.024 | 99.3678 | 2 | 2 | 1 | 2 | 1 | 0 | 0 | 97.8813 | 97.8813 | 172.4199 | 3 | PROCESSED | 57536.3784722222 | 2016-05-28 09:05:00 | 54702 | 2008-08-24 00:00:00 | 54132.9968055556 | 2007-02-01 23:55:24 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011363 | We propose Suzaku observations of the X-ray bright Broad-Line Radio Galaxies 3C382 and 3C390.3 to study their complex broad-band X-ray spectra. The HXD will constrain the continuum above 10 keV, discriminating between competing physically-different models, while at the same time the XIS will determine the parameters of the FeKalpha line and the shape of the soft X-rays. The proposed observations will allow us to shed light on the origin of reflection features in radio-loud AGN, ultimately determining the structure and ionization state of the accretion flow in these objects. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | RITA SAMBRUNA | USA | 1 | AO1 | THE BROAD-BAND X-RAY SPECTRUM OF BROAD-LINE RADIO GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701060010/ | Quick Look | ![]() |
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932 | Q1158-1843 | 180.1895 | -18.9957 | 179.549068 | -18.717273 | 187.964658 | -17.299195 | 286.65628264 | 42.26876142 | 291.8577 | 54636.8208912037 | 2008-06-19 19:42:05 | 54637.4202314815 | 2008-06-20 10:05:08 | 703039010 | 24.085 | 22 | 24.101 | 24.085 | 0 | 24.101 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.4309 | 22.4309 | 51.7819 | 1 | PROCESSED | 57542.8567361111 | 2016-06-03 20:33:42 | 55014 | 2009-07-02 00:00:00 | 54648.3349305556 | 2008-07-01 08:02:18 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031334 | Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GEORGE CHARTAS | USA | 3 | AO3 | A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703039010/ | Quick Look | ![]() |
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933 | W63 | 304.8117 | 45.7821 | 304.405742 | 45.623994 | 328.881818 | 62.294552 | 82.4091518 | 5.43831098 | 57.9996 | 57171.5134837963 | 2015-05-29 12:19:25 | 57172.616712963 | 2015-05-30 14:48:04 | 510025010 | 42.7003 | 150 | 44.302 | 44.606 | 0 | 42.7003 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.7747 | 13.7747 | 92.7739 | 0 | PROCESSED | 57618.8028703704 | 2016-08-18 19:16:08 | 57636 | 2016-09-05 00:00:00 | 57260.7216898148 | 2015-08-26 17:19:14 | 3.0.22.44 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 101315 | We propose to conduct a deep Suzaku observation of the X-ray bright central portion of the Galactic supernova remnant (SNR) W63 (G82.2+5.3). This SNR belongs to a class of objects known as mixed-morphology SNRs (MMSNRs) that feature a shell-like radio morphology with a center-filled thermal X-ray morphology: the origin of these contrasting morphologies for these SNRs remains unknown. Our proposed Suzaku observation of this SNR will investigate the putative overabundances of such elements as magnesium, silicon and sulfur (as reported in a previous analysis of an ASCA observation of W63) as well as search for evidence of over-ionization conditions in the X-ray emitting plasma, as has been reported for other MMSNRs. | GALACTIC DIFFUSE EMISSION | 5 | C | THOMAS PANNUTI | USA | 10 | AO10 | A SUZAKU OBSERVATION OF THE GALACTIC SUPERNOVA REMNANT W63 (G82.2+5.3) | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/510025010/ | Quick Look | ![]() |
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934 | MCG-6-30-15 | 203.9706 | -34.2946 | 203.254215 | -34.039458 | 215.17105 | -22.544253 | 313.28931603 | 27.68170589 | 107.0204 | 53744.9738310185 | 2006-01-09 23:22:19 | 53749.1390277778 | 2006-01-14 03:20:12 | 700007010 | 143.1965 | 300 | 143.1965 | 143.3162 | 143.2685 | 143.2445 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 126.2903 | 126.2903 | 359.8399 | 4 | PROCESSED | 57532.7604398148 | 2016-05-24 18:15:02 | 54247 | 2007-05-27 00:00:00 | 54040.4060416667 | 2006-11-01 09:44:42 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001035 | The broad iron line in the Seyfert 1 galaxy MCG-6-30-15 shows that most of the power is released at 2--4 gravitational radii enabling the strong gravity, accretion flow and energy release in that exciting regime to be studied. The spectral variability of the source decomposes into a highly variable power law and a reflection-dominated component, containing the iron line and Compton hump, which varies significantly but with much less amplitude. This can be explained by the extreme gravitational light bending occuring in this region. We propose to observe MCG--6-30-15 for 4 x 50~ks in order to determine for the first time the variability of the reflection over a wide range of energies from below 1 keV to above 40 keV and timescales . | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ANDREW FABIAN | JAP | 0 | SWG | REFLECTION, ABSORPTION AND STRONG GRAVITY AROUND THE SPINNING BLACK HOLE IN MCG--6-30-15 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700007010/ | Quick Look | ![]() |
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935 | NGC 7213 | 332.316 | -47.1629 | 331.53332 | -47.408605 | 315.985734 | -33.170959 | 349.59497628 | -52.58020545 | 231.3714 | 54030.2323611111 | 2006-10-22 05:34:36 | 54032.2759722222 | 2006-10-24 06:37:24 | 701029010 | 90.736 | 100 | 90.76 | 90.744 | 90.736 | 90.752 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 90.3418 | 90.3418 | 176.5358 | 0 | PROCESSED | 57535.9564814815 | 2016-05-27 22:57:20 | 54695 | 2008-08-17 00:00:00 | 54056.3665162037 | 2006-11-17 08:47:47 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011305 | We propose a 100ks Suzaku observation of the low luminosity AGN, NGC 7213. Previous observations show a complex iron line and weak or no Compton reflection. However the iron line and reflection hump are poorly constrained, so the line emitting matter could arise from a truncated disk, BLR or a Compton-thin torus. A high quality Suzaku observation will constrain the iron line profile, resolve the ionized emission and unambiguously determine its origin. Using the unique broad bandpass of Suzaku above 10 keV we will place tight constraints on any reflection hump, enabling us to determine if the iron line originates from a truncated disk. This could provide a direct test of the paradigm that the X-ray emission in low accretion rate AGN occurs in a truncated disk system such as an ADAF. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | JAMES REEVES | USA | 1 | AO1 | DOES THE LOW LUMINOSITY AGN NGC7213 CONTAIN A TRUNCATED ACCRETION DISK? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701029010/ | Quick Look | ![]() |
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936 | IRAS 19254-7245 | 292.8508 | -72.6492 | 291.381636 | -72.754038 | 280.373528 | -50.031737 | 322.5078751 | -28.76929596 | 279.8892 | 54041.9830208333 | 2006-11-02 23:35:33 | 54044.5967476852 | 2006-11-05 14:19:19 | 701052010 | 113.5123 | 120 | 113.5203 | 113.5203 | 113.5123 | 113.5203 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 151.9778 | 151.9778 | 225.8099 | 1 | PROCESSED | 57536.068125 | 2016-05-28 01:38:06 | 54455 | 2007-12-21 00:00:00 | 54088.8285185185 | 2006-12-19 19:53:04 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011342 | We propose a 120 ksec Suzaku exposure of the ULIRG IRAS19254-7245. A previous XMM-Newton observation revealed the presence of a strong iron emission line and a flat continuum, both suggesting that this source hosts a Compton-thick AGN. In this scenario, the 2-10 keV luminosity of IRAS19254-7245 could be greater than 10e44 erg/s. However since no direct continuum is visible in the XMM bandpass, a direct measure of the absorbing column density was not feasible, thus the intrinsic X-ray luminosity of this source was derived only through indirect arguments. The unique bandpass and sensititvity of Suzaku above 10 keV will allow us to confirm the Compton-thick nature of this source and to measure for the first time the intrinsic X-ray luminosity of the AGN hosted in IRAS 19254-7245. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | VALENTINA BRAITO | USA | 1 | AO1 | ASSESSING THE ENERGETIC BUDGET IN THE SUPERANTENNAE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701052010/ | Quick Look | ![]() |
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937 | COMET_8P_TUTTLE-P1-7 | 28.2572 | 6.4878 | 27.602012 | 6.241824 | 28.565429 | -4.78789 | 149.08057764 | -53.2281425 | 248.4991 | 54470.9158333333 | 2008-01-05 21:58:48 | 54470.9820717593 | 2008-01-05 23:34:11 | 502062070 | 3.219 | 2 | 3.219 | 3.219 | 0 | 3.219 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3.459 | 3.459 | 5.664 | 0 | PROCESSED | 57541.0036805556 | 2016-06-02 00:05:18 | 54908 | 2009-03-18 00:00:00 | 54542.2385532407 | 2008-03-17 05:43:31 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062070/ | Quick Look | ![]() |
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938 | NGC3227 | 155.8772 | 19.8688 | 155.194637 | 20.122177 | 150.387911 | 9.14334 | 216.98506904 | 55.4463804 | 114.6051 | 54774.1503587963 | 2008-11-04 03:36:31 | 54775.6780555556 | 2008-11-05 16:16:24 | 703022020 | 53.6995 | 50 | 53.6995 | 53.6995 | 0 | 53.6995 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50.2891 | 50.2891 | 131.9718 | 3 | PROCESSED | 57544.3625810185 | 2016-06-05 08:42:07 | 54557 | 2008-04-01 00:00:00 | 54788.4371643518 | 2008-11-18 10:29:31 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031013 | We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARTIN ELVIS | USA | 3 | AO3 | NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703022020/ | Quick Look | ![]() |
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939 | IC 4329A | 207.3331 | -30.3096 | 206.618942 | -30.061447 | 216.346028 | -17.776613 | 317.49896941 | 30.91923491 | 296.2 | 56152.0924652778 | 2012-08-13 02:13:09 | 56154.6425578704 | 2012-08-15 15:25:17 | 707025010 | 117.5938 | 120 | 117.5938 | 117.5938 | 0 | 117.5938 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 112.9986 | 112.9986 | 220.2637 | 2 | PROCESSED | 57606.8955208333 | 2016-08-06 21:29:33 | 56540 | 2013-09-05 00:00:00 | 56170.1592824074 | 2012-08-31 03:49:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071417 | We propose simultaneous NuSTAR/Suzaku observations of NGC 4151 and IC 4329A. These pointings will achieve three goals: (1) They will provide the best-ever broad-band X-ray spectra of two of the brightest Seyfert galaxies in the 0.5-80 keV band; (2) They will enable broad-band, time-resolved X-ray spectroscopy of these fascinating and variable sources; (3) They will serve as invaluable calibration targets for the two observatories. The spectral coverage and sensitivity will enable the continuum, absorption and reflection components of each spectrum to be conclusively disentangled, allowing us to determine whether inner disk reflection signatures are present. We will also be able to break the degeneracy between the coronal temperature and optical depth in both AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | LAURA BRENNEMAN | USA | 7 | AO7 | SHEDDING NEW LIGHT ON THE BROAD-BAND X-RAY SPECTRA OF NGC 4151 AND IC 4329A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707025010/ | Quick Look | ![]() |
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940 | NGC 4138 | 182.4434 | 43.7345 | 181.812692 | 44.012643 | 161.129219 | 40.276316 | 147.09151655 | 71.38668226 | 137.6226 | 55137.5331365741 | 2009-11-02 12:47:43 | 55138.8849305556 | 2009-11-03 21:14:18 | 704047010 | 60.7716 | 60 | 60.8436 | 60.7716 | 0 | 60.8436 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.8724 | 35.8724 | 116.7818 | 2 | PROCESSED | 57549.0852893518 | 2016-06-10 02:02:49 | 55517 | 2010-11-17 00:00:00 | 55151.1923263889 | 2009-11-16 04:36:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041415 | The SWIFT BAT hard (14-195 KeV) survey is performing the first unbiased hard X-ray survey of the entire sky with follow-up observations with the Swift XRT to fully identify the sample. In this survey we have found two very low luminosity nearby hard X-ray sources which show little, if any, evidence for nuclear activity in the optical or UV band, and have very low apparent Eddington ratios. We propose Suzaku observations of these objects to determine whether there is an X-ray spectral signature of a low Eddington ratio, as predicted if these objects are indeed in a radiatively inefficient accretion flow. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RICHARD MUSHOTZKY | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF NGC4138 AND NGC3718 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704047010/ | Quick Look | ![]() |
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941 | HE0512-3329 | 78.5402 | -33.4449 | 78.079903 | -33.501337 | 72.668068 | -56.200323 | 236.63398617 | -33.8579138 | 105.1284 | 56932.4291435185 | 2014-10-02 10:17:58 | 56932.6252083333 | 2014-10-02 15:00:18 | 709020010 | 6.8649 | 60 | 6.873 | 6.8729 | 0 | 6.8649 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.600474537 | 2016-08-16 14:24:41 | 57345 | 2015-11-19 00:00:00 | 56979.403125 | 2014-11-18 09:40:30 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091431 | The origin of AGN iron K alpha emission has been debated for two decades. We propose to constrain iron line emission sizes using quasar X-ray microlensing. Our Chandra Cycle 11 observations have shown that the iron line equivalent widths (EWs) in six lensed systems are significantly higher than those measured in local AGNs. This implies that the iron line emission is microlensed more strongly than the X-ray continuum and originates from very compact regions. We propose to confirm the high iron line EWs in lensed quasars by monitoring two more lenses, Q0142-100 and HE0512+3329 using Suzaku, with a total exposure time 115 kilo-seconds. This will provide independent constraints for settling the debate on the origin of the iron line emission. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | BIN CHEN | USA | 9 | AO9 | CONSTRAINING QUASAR IRON LINE EMISSION USING MICROLENSING | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709020010/ | Quick Look | ![]() |
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942 | HOLMBERG II X-1 | 124.8826 | 70.7169 | 123.581394 | 70.873481 | 106.843254 | 49.308296 | 144.27185866 | 32.72527495 | 119.959 | 56562.4955555556 | 2013-09-27 11:53:36 | 56563.5730324074 | 2013-09-28 13:45:10 | 708015020 | 49.283 | 50 | 49.283 | 49.283 | 0 | 49.283 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.206 | 48.206 | 93.0879 | 0 | PROCESSED | 57612.7832986111 | 2016-08-12 18:47:57 | 56954 | 2014-10-24 00:00:00 | 56588.5225462963 | 2013-10-23 12:32:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081251 | Recent X-ray observations have produced evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in an unusual super-Eddington state. Current data are unable to deliver a clear answer, as attempts to model the 0.5-10keV spectra have been plagued by degeneracies resulting from the limited bandpass, owing to the previous lack of focusing hard X-ray telescopes. Combined, Suzaku and NuSTAR will obtain high-quality spectra covering 0.5-30keV, providing powerful probes for understanding the accretion modes and nature of the central BHs. A definitive statement on the existence of either 100-1000Msun black holes or extreme accretion states will be an important legacy of both missions. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | DOMINIC WALTON | USA | 8 | AO8 | COORDINATED SUZAKU AND NUSTAR OBSERVATIONS OF HOLMBERG II X-1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708015020/ | Quick Look | ![]() |
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943 | ARP220 | 233.7664 | 23.5658 | 233.223657 | 23.731386 | 223.777121 | 41.366844 | 36.73879852 | 53.01919685 | 114.8377 | 53742.3490856482 | 2006-01-07 08:22:41 | 53744.9654398148 | 2006-01-09 23:10:14 | 700006010 | 98.5506 | 100 | 98.5586 | 98.5506 | 98.5586 | 98.5586 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 93.3623 | 93.3623 | 226.0419 | 2 | PROCESSED | 57532.6850925926 | 2016-05-24 16:26:32 | 54247 | 2007-05-27 00:00:00 | 54040.0356597222 | 2006-11-01 00:51:21 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001033 | We propose a 100 ks observation of the nearest ultraluminous infrared galaxy (ULIG) Arp220. The major objective is to search for evidence of heavily obscured nuclei. First detection of a Compton-thick source may be possible with the HXD's sensitivity, if a powerful nucleus is present, leading to a major discovery. The good quality XIS spectrum can be decisive for the origin of the strong Fe K line, barely detected with the previous XMM-Newton observation. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KAZUSHI IWASAWA | JAP | 0 | SWG | HARD X-RAY EMISSION FROM THE NEAREST ULTRALUMINOUS INFRARED GALAXY ARP220 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700006010/ | Quick Look | ![]() |
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944 | EN2-109 | 248.6774 | 40.3802 | 248.257276 | 40.482344 | 234.834061 | 61.240527 | 64.11782178 | 42.55568423 | 145.2754 | 55927.5063425926 | 2012-01-01 12:09:08 | 55929.8577314815 | 2012-01-03 20:35:08 | 806075010 | 108.616 | 100 | 108.632 | 108.616 | 0 | 108.64 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 0.571 | 0.571 | 0.5729 | 0 | PROCESSED | 57604.2767592593 | 2016-08-04 06:38:32 | 56065 | 2012-05-18 00:00:00 | 55946.1449537037 | 2012-01-20 03:28:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061532 | We propose Suzaku XIS observations of a sample of three high redshift galaxy clusters with 0.87 < z < 1.20 discovered by the 42 square degree Spitzer Adaptation of the Red Sequence Survey (SpARCS). This survey is currently the largest optical/IR survey for high redshift clusters, and includes significant multi-wavelength follow-up. Extensive Gemini spectroscopic observations have confirmed that all of our targets are rich, massive clusters with velocity dispersions ranging from 550-800 km/sec. Our Suzaku observations are designed to detect the extended intra-cluster medium in the cluster cores, provide first estimates of cluster X-ray luminosities, and broadly investigate the core gas densities of our targets. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 6 | AO6 | OBSERVING DISTANT GALAXY CLUSTERS FROM THE SPITZER SPARCS SURVEY WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806075010/ | Quick Look | ![]() |
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945 | ES1-230 | 9.1906 | -44.1805 | 8.591944 | -44.455632 | 346.325718 | -43.236883 | 311.80619624 | -72.69400023 | 239.5046 | 55907.020787037 | 2011-12-12 00:29:56 | 55907.8925694444 | 2011-12-12 21:25:18 | 806076010 | 44.8024 | 40 | 44.8024 | 44.8024 | 0 | 44.8024 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52.0193 | 52.0193 | 75.3199 | 0 | PROCESSED | 57604.1212037037 | 2016-08-04 02:54:32 | 56065 | 2012-05-18 00:00:00 | 55920.9678587963 | 2011-12-25 23:13:43 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061532 | We propose Suzaku XIS observations of a sample of three high redshift galaxy clusters with 0.87 < z < 1.20 discovered by the 42 square degree Spitzer Adaptation of the Red Sequence Survey (SpARCS). This survey is currently the largest optical/IR survey for high redshift clusters, and includes significant multi-wavelength follow-up. Extensive Gemini spectroscopic observations have confirmed that all of our targets are rich, massive clusters with velocity dispersions ranging from 550-800 km/sec. Our Suzaku observations are designed to detect the extended intra-cluster medium in the cluster cores, provide first estimates of cluster X-ray luminosities, and broadly investigate the core gas densities of our targets. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 6 | AO6 | OBSERVING DISTANT GALAXY CLUSTERS FROM THE SPITZER SPARCS SURVEY WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806076010/ | Quick Look | ![]() |
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946 | FORNAX CLUSTER NORTH | 54.7022 | -35.2276 | 54.222066 | -35.389468 | 38.999643 | -52.605839 | 236.33819165 | -53.57399329 | 245.0013 | 53740.3046990741 | 2006-01-05 07:18:46 | 53740.493275463 | 2006-01-05 11:50:19 | 800002010 | 7.7635 | 80 | 7.7635 | 7.7635 | 7.7635 | 7.7635 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 8.2708 | 8.2708 | 16.2719 | 0 | PROCESSED | 57532.6205324074 | 2016-05-24 14:53:34 | 54247 | 2007-05-27 00:00:00 | 54039.6718518518 | 2006-10-31 16:07:28 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001018 | The center of the Fornax cluster was observed with Suzaku with a 80 ks exposure. We have detected excess hard-emission and derived O abundances of the ISM of NGC 1399 and NGC 1404, and the intracluster medium (ICM). Here, we propose to observe two offset pointings of the Fornax cluster for 160 ks (80 ks times 2) to study the distribution of the hard emission and the abundance distribution of O, Mg, Si, S and Fe. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | JAP | 0 | SWG | MAPPING HARD EXCESS EMISSION AND OXYGEN IN THE INTRACLUSTER MEDIUM OF THE FORNAX CLUSTER | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800002010/ | Quick Look | ![]() |
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947 | A1060 OFFSET | 159.5124 | -27.532 | 158.922997 | -27.271679 | 173.074389 | -33.196781 | 269.88117164 | 26.64663217 | 96.4857 | 53694.9817708333 | 2005-11-20 23:33:45 | 53696.6231365741 | 2005-11-22 14:57:19 | 800004010 | 52.4025 | 60 | 52.4025 | 53.2025 | 52.4185 | 52.5385 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 46.2039 | 46.2039 | 141.8018 | 1 | PROCESSED | 57528.0764583333 | 2016-05-20 01:50:06 | 54247 | 2007-05-27 00:00:00 | 54038.1216666667 | 2006-10-30 02:55:12 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001021 | A1060 is a bright non cD cluster and gives us a unique opportunity to study injection process of metals in the intracluster space. Reliable measurement of oxygen distribution with XIS will tell us whether the metals produced by Type-II supernova (mainly oxygen) ditributes over a different scale compared with the SN-Ia product (Fe). A1060 is the best cluster where we can directly observe distribution of metals produced by general cluster galaxies. Also, central increase of temperature by 20%, probably connected with motions of bright central galaxies, suggests that non-thermal X-rays may be produced. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | TAKAYA OHASHI | JAP | 0 | SWG | OXYGEN DISTRIBUTION AND CENTRAL GAS FEATURES OF A1060 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800004010/ | Quick Look | ![]() |
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948 | A426VIR E | 49.1256 | 42.621 | 48.293128 | 42.437331 | 58.306623 | 23.574763 | 149.42807458 | -12.66566367 | 271.4976 | 56709.0457986111 | 2014-02-21 01:05:57 | 56709.5683101852 | 2014-02-21 13:38:22 | 808086010 | 25.3703 | 25 | 25.3823 | 25.3703 | 0 | 25.3703 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24.322 | 24.322 | 45.14 | 1 | PROCESSED | 57613.8778935185 | 2016-08-13 21:04:10 | 57141 | 2015-04-29 00:00:00 | 56764.7643171296 | 2014-04-17 18:20:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081526 | Our analysis of Suzaku Key Project data of the Perseus Cluster of galaxies has uncovered a significant drop in temperature, density and derived thermodynamic properties of the intra-cluster medium in the NW direction at the cluster's virial radius, suggesting the presence of a strong shock. In order to firmly confirm and further explore this feature we propose to expand upon the observation of this region. Confirmation of a shock at the virial radius will provide the first ever direct observation of the formation of a galaxy cluster and virialization of the in-falling hot gas. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ONDREJ URBAN | USA | 8 | AO8 | SHOCK FRONT AT THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808086010/ | Quick Look | ![]() |
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949 | ABELL 115 OFFSET | 13.7779 | 26.1853 | 13.1056 | 25.914555 | 23.090334 | 18.655077 | 123.95957255 | -36.67911837 | 45.0019 | 55399.3766666667 | 2010-07-22 09:02:24 | 55401.6050115741 | 2010-07-24 14:31:13 | 805078010 | 101.8065 | 100 | 101.8065 | 101.8065 | 0 | 101.8065 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91.1134 | 91.1134 | 192.5058 | 3 | PROCESSED | 57552.7084259259 | 2016-06-13 17:00:08 | 55779 | 2011-08-06 00:00:00 | 55413.4333449074 | 2010-08-05 10:24:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051521 | We propose central and offset pointed observations of the strongly merging ``double'' cluster A115 to study the properties of the intracluster gas at the virial radius. Ultimately, the results can be compared with results from both relaxed and other merging systems to determine the effects of mergers on the extended gas halos of clusters (e.g., departures from hydrostatic equilibrium, and the level of non-thermal pressure support). Additionally, we will verify the presence of hard X-ray emission between the subclusters, marginally detected in Chandra observations, accurately measure its temperature, and determine its origin by confirming it as hot thermal (shock heated gas) or non-thermal (shock or turbulent accelerated particles) emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SCOTT RANDALL | USA | 5 | AO5 | THE EXTENDED ATMOSPHERES OF STRONGLY MERGING GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805078010/ | Quick Look | ![]() |
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950 | ANTLIA EB | 160.0852 | -35.3304 | 159.51241 | -35.06908 | 178.137624 | -39.871032 | 274.84198608 | 20.29194272 | 279.6006 | 56096.5981828704 | 2012-06-18 14:21:23 | 56097.8197106482 | 2012-06-19 19:40:23 | 807071010 | 45.7475 | 45 | 45.7635 | 45.7475 | 0 | 45.7635 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.3619 | 40.3619 | 105.536 | 1 | PROCESSED | 57605.7231481482 | 2016-08-05 17:21:20 | 56477 | 2013-07-04 00:00:00 | 56111.1019328704 | 2012-07-03 02:26:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071521 | We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KA-WAH WONG | USA | 7 | AO7 | MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807071010/ | Quick Look | ![]() |
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951 | ABELL 3112 | 49.4972 | -44.2507 | 49.062824 | -44.43238 | 25.520697 | -58.972198 | 252.95338075 | -56.0704995 | 43.5006 | 56468.5418171296 | 2013-06-25 13:00:13 | 56469.5834259259 | 2013-06-26 14:00:08 | 808068020 | 65.3977 | 200 | 65.4057 | 65.4057 | 0 | 65.3977 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54.0744 | 54.0744 | 89.9838 | 1 | PROCESSED | 57611.633912037 | 2016-08-11 15:12:50 | 56848 | 2014-07-10 00:00:00 | 56481.7677083333 | 2013-07-08 18:25:30 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081522 | The hot X-ray emitting gas in clusters of galaxies is a very large repository of metals produced by stars and galaxies. These metals enter the intra-cluster medium (ICM) via strong galactic winds, supernovae explosions, and ram-pressure stripping. However, the details of the mechanisms that transport metals to the ICM and the origin of these metals remain still unclear. We aim to accurately measure the temperature and abundance patterns of a bright nearby galaxy cluster A3112 out to the virial radius and compare these data with metal abundance yields produced by supernovae. Our proposed observation will provide information about how these metals are created, as well as how and when the metals were transported to the ICM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ESRA BULBUL | USA | 8 | AO8 | CHEMICAL EVOLUTION HISTORY OF A COOL CORE CLUSTER A3112 OUT TO THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808068020/ | Quick Look | ![]() |
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952 | CENCL OFFSET1 | 192.2015 | -41.4461 | 191.510562 | -41.173577 | 209.146138 | -32.971575 | 302.40210867 | 21.42294125 | 106.2765 | 53732.1811689815 | 2005-12-28 04:20:53 | 53733.2502199074 | 2005-12-29 06:00:19 | 800015010 | 44.8802 | 40 | 44.8962 | 44.9042 | 44.8802 | 44.9196 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 37.2267 | 37.2267 | 92.3478 | 2 | PROCESSED | 57532.5827893518 | 2016-05-24 13:59:13 | 54247 | 2007-05-27 00:00:00 | 54039.5403472222 | 2006-10-31 12:58:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001070 | A dramatic central concentration of iron and silicon is present in the Centaurus cluster. Apart from this well-recognized contribution from Type Ia supernova, enrichment process due to Type II supernova is poorly understood. Centaurus cluster is most suited for the study of large-scale oxygen distribution, for which XIS is most sensitive. The XIS data will give us a key knowledge about how past Type II supernova have affected the enrichment process. The data would also confirm that the central gas is a mixture of hot and cool components with much better sensitivity than before. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YASUSHI FUKAZAWA | JAP | 0 | SWG | OXYGEN DISTRIBUTION AND MIXTURE OF HOT AND COOL GAS IN THE CENTAURUS CLUSTER | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800015010/ | Quick Look | ![]() |
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953 | AQL X-1 | 287.8171 | 0.5794 | 287.178828 | 0.495683 | 289.378182 | 22.829317 | 35.71359616 | -4.14591745 | 272.6027 | 54388.3395833333 | 2007-10-15 08:09:00 | 54388.7225 | 2007-10-15 17:20:24 | 402053040 | 17.9157 | 15 | 17.9157 | 17.9157 | 0 | 17.9157 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.6682 | 17.6682 | 33.08 | 0 | PROCESSED | 57540.2752893518 | 2016-06-01 06:36:25 | 54769 | 2008-10-30 00:00:00 | 54402.4060648148 | 2007-10-29 09:44:44 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021114 | We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. | GALACTIC POINT SOURCES | 4 | A | RONALD REMILLARD | USA | 2 | AO2-TOO | X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402053040/ | Quick Look | ![]() |
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954 | G189 NORTH | 94.8937 | 22.8595 | 94.136063 | 22.881413 | 94.510579 | -0.50482 | 189.05453502 | 3.64004382 | 92.0693 | 56941.8561458333 | 2014-10-11 20:32:51 | 56944.6669328704 | 2014-10-14 16:00:23 | 509035010 | 100.65 | 100 | 100.65 | 102.898 | 0 | 102.922 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.652337963 | 2016-08-16 15:39:22 | 57362 | 2015-12-06 00:00:00 | 56996.4204282407 | 2014-12-05 10:05:25 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091314 | We propose observations of G189.6+3.3, a large candidate supernova remnant (SNR) that overlaps with the much better studied remnant IC 443. Little is known about G189; ROSAT images show a shell-like structure about 1.5$^{circ}$ in diameter, but it has never been observed with modern X-ray telescopes. Its association, or lack thereof, with IC 443 is unknown. It may not be a supernova remnant at all; a superbubble origin for the X-ray emission also provides an intriguing possibility. Spatially-resolved spectroscopy with Suzaku will allow the detailed measurement of the plasma properties, illuminating the nature of this object. Determining the nature of G189 will help to probe the evolution of the ISM driven by the deaths of massive stars. | GALACTIC DIFFUSE EMISSION | 5 | B | BRIAN WILLIAMS | USA | 9 | AO9 | OBSERVATIONS OF G189.6+3.3: AN SNR COMPANION TO IC 443? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509035010/ | Quick Look | ![]() |
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955 | NGC 1550-OFFSET1 | 65.1493 | 2.6086 | 64.497489 | 2.490158 | 63.709607 | -18.593747 | 190.9426677 | -31.53770965 | 265.5852 | 54901.8171875 | 2009-03-11 19:36:45 | 54903.699525463 | 2009-03-13 16:47:19 | 803046010 | 66.8274 | 62 | 66.8274 | 66.8274 | 0 | 66.8274 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 60.9307 | 60.9307 | 162.6001 | 2 | PROCESSED | 57545.8588541667 | 2016-06-06 20:36:45 | 55329 | 2010-05-13 00:00:00 | 54917.3952314815 | 2009-03-27 09:29:08 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031422 | We propose a set of two 19 arcmin offset observations of the galaxy groups NGC 1550 and MKW 4 to measure spatially resolved densities, temperatures and iron abundances out to r_500. These measurements are crucial for an accurate determination of the gas mass profile and gas fraction, for probing the entropy profile near the region where the accretion shocks start to be important, and for exploring the chemical enrichment at a spatial scale which retains information of early SNII and SNIa enrichment. Due to their brightness, regularity and low temperature, the two objects are ideal candidates for an offset observation of their peripheral gas by Suzaku, making an excellent use of its low background and soft X-ray sensitivity. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | FABIO GASTALDELLO | USA | 3 | AO3 | THE OUTSKIRTS OF NGC 1550 AND MKW 4 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803046010/ | Quick Look | ![]() |
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956 | NGC741MOSAICE_P2 | 29.9595 | 5.5362 | 29.305812 | 5.294206 | 29.82553 | -6.270862 | 152.32010482 | -53.38732445 | 71.7775 | 55054.083912037 | 2009-08-11 02:00:50 | 55054.3334837963 | 2009-08-11 08:00:13 | 804052020 | 12.7341 | 10 | 12.7341 | 12.7421 | 0 | 12.7421 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.0159 | 12.0159 | 21.5599 | 0 | PROCESSED | 57548.1149884259 | 2016-06-09 02:45:35 | 55448 | 2010-09-09 00:00:00 | 55081.2532060185 | 2009-09-07 06:04:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JOEL BREGMAN | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804052020/ | Quick Look | ![]() |
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957 | VELA X-1 | 135.5377 | -40.5514 | 135.064105 | -40.353478 | 157.048654 | -53.915556 | 263.06039339 | 3.93722667 | 314.5441 | 54634.1981134259 | 2008-06-17 04:45:17 | 54635.9043287037 | 2008-06-18 21:42:14 | 403045010 | 104.7096 | 100 | 104.7234 | 104.7096 | 0 | 104.7154 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 96.0089 | 96.0089 | 147.3899 | 1 | PROCESSED | 57542.8859375 | 2016-06-03 21:15:45 | 55010 | 2009-06-28 00:00:00 | 54644.4687847222 | 2008-06-27 11:15:03 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031153 | We propose to observe the well-known X-ray pulsar Vela X-1 (4U0900-40) using Suzaku in order to test models for the circumstellar environment by measuring teh spectrum and searching for variability in the iron line. The line is expected to exhibit changes in intensity and centroid energy as the X-ray beam sweeps around the wind an illuminates material with varying column density, ionization state, and vleocity. In addition we will study the variability in the cyclotron feature. We will compare our observations with detailed hydrodynamical simulations of the stellar wind and its interaction with the compact object. | GALACTIC POINT SOURCES | 4 | A | TIMOTHY KALLMAN | USA | 3 | AO3 | SPECTROSCOPY OF VELA X-1 (4U0900-40) AND SEARCHES FOR PULSE PHASE VARIABILITY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403045010/ | Quick Look | ![]() |
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958 | SNR 0103-72.6 | 16.2944 | -72.389 | 15.898915 | -72.656584 | 313.931508 | -65.2662 | 301.47055063 | -44.70024477 | 13.8765 | 53848.0156018518 | 2006-04-23 00:22:28 | 53849.3773032407 | 2006-04-24 09:03:19 | 501077010 | 49.2715 | 50 | 49.2795 | 49.2875 | 49.2875 | 49.2715 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 37.1905 | 37.1905 | 117.6299 | 3 | PROCESSED | 57533.5571296296 | 2016-05-25 13:22:16 | 54401 | 2007-10-28 00:00:00 | 53907.4220023148 | 2006-06-21 10:07:41 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011241 | We propose Suzaku observations of O-rich supernova remnants (SNRs) 0103-72.6 and 0049-73.6 in the Small Magellanic Cloud (SMC). These SMC SNRs are oldest members (18000 and 14000 yr old) of O-rich SNRs and share X-ray spectral characteristics with a young (1000 yr old) O-rich SNR 0102-7219 which is also in the SMC. While sharing similar spectral features with 0102-7219, the morphologies of 0103-72.6 and 0049-73.6 indicate more evolved phases of the SNR in a similar interstellar environment as 0102-7219. Cross-comparison studies with the high spectral resolution Suzaku/XIS observations among 0103-72.6/0049-73.6 (this proposal) and 0102-7219 (scheduled/observed for the instrument calibrations) will provide a unique opportunity for the study of a long-term evolution of an O-rich SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | SANGWOOK PARK | USA | 1 | AO1 | BACK TO THE FUTURE: LONG-TERM EVOLUTION OF OXYGET-RICH SUPERNOVA REMNANTS IN THE SMALL MAGELLANIC CLOUD | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501077010/ | Quick Look | ![]() |
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959 | ARC_BACKGROUND | 39.2055 | -35.7283 | 38.691278 | -35.944876 | 20.761341 | -47.725244 | 240.48717091 | -66.02341726 | 233.8071 | 54830.2554861111 | 2008-12-30 06:07:54 | 54835.3468055556 | 2009-01-04 08:19:24 | 503104010 | 201.8775 | 140 | 201.9575 | 201.8775 | 0 | 201.9815 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 5.5028 | 5.5028 | 14.506 | 0 | PROCESSED | 57545.0672685185 | 2016-06-06 01:36:52 | 55328 | 2010-05-12 00:00:00 | 54851.4354166667 | 2009-01-20 10:27:00 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031235 | Aside from the lengthy bright arcs in the northern sky, few X-ray bright, high latitude regions are understood. Yet, studying this gas is important for understanding the Galactic halo. Here, we propose to study a medium-sized (~7 degree) bright feature in the southern sky. The feature is arc-shaped, suspiciously like the edge of a hot bubble. We propose to make Suzaku observations of the arc and nearby background. With them and an existing Suzaku observation, we will be able to determine the thermal properties of the arc plasma and if the arc is the bright limb of a hot bubble. | GALACTIC DIFFUSE EMISSION | 5 | B | ROBIN SHELTON | USA | 3 | AO3 | A CLOSER LOOT AT HOT HALO GAS: A SUZAKU STUDY OF AN X-RAY BRIGHT ARC | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503104010/ | Quick Look | ![]() |
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960 | RXCJ0605 | 91.4958 | -35.4837 | 91.05364 | -35.477523 | 92.366503 | -58.913023 | 241.98342334 | -24.04647163 | 309.0856 | 55321.4301041667 | 2010-05-05 10:19:21 | 55322.221712963 | 2010-05-06 05:19:16 | 805065010 | 40.9762 | 40 | 40.9762 | 40.9762 | 0 | 40.9762 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.5095 | 35.5095 | 68.3681 | 0 | PROCESSED | 57551.3998032407 | 2016-06-12 09:35:43 | 55287 | 2010-04-01 00:00:00 | 55341.4983217593 | 2010-05-25 11:57:35 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805065010/ | Quick Look | ![]() |
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961 | PUP A : BEK | 125.942 | -42.9405 | 125.511174 | -42.777913 | 147.596211 | -59.401563 | 260.51799115 | -3.16426215 | 276.3687 | 53842.2933449074 | 2006-04-17 07:02:25 | 53842.5807407407 | 2006-04-17 13:56:16 | 501086010 | 16.0913 | 15 | 16.0913 | 16.0993 | 16.0913 | 16.0913 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 9.6985 | 9.6985 | 24.797 | 0 | PROCESSED | 57533.4850115741 | 2016-05-25 11:38:25 | 54401 | 2007-10-28 00:00:00 | 53906.8467708333 | 2006-06-20 20:19:21 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011246 | We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present. | GALACTIC DIFFUSE EMISSION | 5 | A | UNA HWANG | USA | 1 | AO1 | MAPPING OXYGEN IN PUPPIS A | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501086010/ | Quick Look | ![]() |
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962 | SWIFT J0918.5+0425 | 139.5114 | 4.476 | 138.856225 | 4.686688 | 140.50448 | -10.713106 | 227.10001498 | 34.41934616 | 102.3204 | 54408.8894097222 | 2007-11-04 21:20:45 | 54410.2293981482 | 2007-11-06 05:30:20 | 702076010 | 61.0185 | 53 | 61.0185 | 61.0401 | 0 | 61.0185 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 56.1565 | 56.1565 | 115.7659 | 2 | PROCESSED | 57540.4472916667 | 2016-06-01 10:44:06 | 54787 | 2008-11-17 00:00:00 | 54419.0312847222 | 2007-11-15 00:45:03 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021372 | The nature and even the existence of type II quasars is highly controversial. Due to their highly obscured nature, very hard (> 15 keV) observations are needed to probe their properties. With the 9-month SWIFT BAT all-sky AGN survey, detection of heavily obscured sources is now possible. Indeed, 6 type II quasars have been identified. Their properties, however, are a challenge to standard AGN models e.g., all but one of these sources are strong radio sources and several have optical spectra indicative of an un-absorbed source. We propose Suzaku observations of the 5 without broadband high signal to noise x-ray data to perform a detailed analysis of their x-ray properties and to understand their relationship to the lower luminosity well studied Seyfert IIs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | RICHARD MUSHOTZKY | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF SWIFT BAT TYPE II QUASARS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702076010/ | Quick Look | ![]() |
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963 | COMET_8P_TUTTLE-P1_BGD-2 | 28.5654 | 5.0072 | 27.913501 | 4.76193 | 28.330895 | -6.281929 | 150.57128999 | -54.45813442 | 248.5002 | 54471.5006018518 | 2008-01-06 12:00:52 | 54471.6876273148 | 2008-01-06 16:30:11 | 502061020 | 5.6821 | 4 | 5.6901 | 5.6821 | 0 | 5.6967 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 5.598 | 5.598 | 16.1519 | 0 | PROCESSED | 57541.2728819444 | 2016-06-02 06:32:57 | 54908 | 2009-03-18 00:00:00 | 54542.2619097222 | 2008-03-17 06:17:09 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502061020/ | Quick Look | ![]() |
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964 | COMET_8P_TUTTLE-P1_BGD-1 | 28.5142 | 5.254 | 27.861749 | 5.008612 | 28.370132 | -6.032929 | 150.31676982 | -54.25438929 | 248.4996 | 54471.3338888889 | 2008-01-06 08:00:48 | 54471.5001273148 | 2008-01-06 12:00:11 | 502061010 | 8.39 | 6 | 8.39 | 8.39 | 0 | 8.39 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.4419 | 7.4419 | 14.3439 | 0 | PROCESSED | 57541.2728935185 | 2016-06-02 06:32:58 | 54908 | 2009-03-18 00:00:00 | 54542.2616319444 | 2008-03-17 06:16:45 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502061010/ | Quick Look | ![]() |
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965 | COMET_8P_TUTTLE-P1-13 | 28.5683 | 5.0085 | 27.916397 | 4.763237 | 28.334076 | -6.281727 | 150.57488577 | -54.45575395 | 248.5007 | 54471.3158333333 | 2008-01-06 07:34:48 | 54471.3334606482 | 2008-01-06 08:00:11 | 502062130 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1.5039 | 0 | PROCESSED | 57541.2672337963 | 2016-06-02 06:24:49 | 54910 | 2009-03-20 00:00:00 | 54544.4202893518 | 2008-03-19 10:05:13 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062130/ | Quick Look | ![]() |
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966 | G296.1-0.5S | 177.6962 | -62.7172 | 177.080034 | -62.439005 | 216.307928 | -55.355417 | 296.04515802 | -0.65925146 | 111.5869 | 54482.7727662037 | 2008-01-17 18:32:47 | 54484.6668402778 | 2008-01-19 16:00:15 | 502069010 | 69.213 | 67 | 69.213 | 69.213 | 0 | 69.213 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61.0096 | 61.0096 | 163.6237 | 2 | PROCESSED | 57541.3665740741 | 2016-06-02 08:47:52 | 54929 | 2009-04-08 00:00:00 | 54563.4417824074 | 2008-04-07 10:36:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021218 | Supernova (SN) explosions within wind-blown bubbles are common among core-collapse (CC) SNe, and are expected to occur for some Type Ia SNe. We propose observations of an X-ray bright supernova remnant (SNR), G296.1-0.5, with very strong evidence for an explosion within a bubble. Spectroscopy with Suzaku will provide us with temperatures, abundances, and ionization ages of the X-ray emitting gas. If we detect SN ejecta, we will distinguish between a CC or a Type Ia progenitor. Gas temperatures will provide us with the shock speeds, while ionization ages will tell us when this gas was shocked. We will infer how progenitor winds affected the ambient medium prior to the explosion. The proposed observations will advance our knowledge of poorly understood SNR evolution in wind-blown bubbles. | GALACTIC DIFFUSE EMISSION | 5 | C | KAZIMIERZ BORKOWSKI | USA | 2 | AO2 | G296.1-0.5: A SUPERNOVA EXPLOSION WITHIN A BUBBLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502069010/ | Quick Look | ![]() |
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967 | G12.8-0.0 | 273.3975 | -17.831 | 272.667266 | -17.845732 | 273.239831 | 5.571499 | 12.81826803 | -0.01988984 | 90.5577 | 54894.8233680556 | 2009-03-04 19:45:39 | 54896.1050810185 | 2009-03-06 02:31:19 | 503087010 | 56.2026 | 50 | 56.2026 | 56.2026 | 0 | 56.2059 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.5312 | 51.5312 | 110.7278 | 1 | PROCESSED | 57545.7287962963 | 2016-06-06 17:29:28 | 55329 | 2010-05-13 00:00:00 | 54908.5701388889 | 2009-03-18 13:41:00 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031203 | By studying pulsar wind nebulae, the synchrotron nebulae powered by a neutron star's loss of rotational energy, it is possible to determine the energetics of both the progenitor supernova and central neutron star. This requires estimates of the expansion velocity and mass swept-up the pulsar wind nebulae, best obtained by analyzing the spectrum of the thermal X-rays emitting by this material. In the proposal, we request a 50ks observation of four of the most energetic pulsar wind nebulae in the Milky Way to both detect such thermal X-ray emission and use the measured spectral properties to infer the ejecta mass and kinetic energy of their progenitor supernova and the initial spin period of the central neutron star -- all currently unmeasurable using the currently available information. | GALACTIC DIFFUSE EMISSION | 5 | C | JOSEPH GELFAND | USA | 3 | AO3 | STUDYING THE PROGENITOR SUPERNOVA AND CENTRAL NEUTRON STAR OF PULSAR WIND NEBULAE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503087010/ | Quick Look | ![]() |
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968 | 1H 0419-577 | 66.5658 | -57.2343 | 66.322649 | -57.345613 | 29.362681 | -75.708089 | 267.01881665 | -41.95465908 | 226.9739 | 55212.4834259259 | 2010-01-16 11:36:08 | 55214.8224421296 | 2010-01-18 19:44:19 | 704064010 | 122.8354 | 140 | 123.1154 | 122.8354 | 0 | 123.1154 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 113.4392 | 113.4392 | 202.0668 | 4 | PROCESSED | 57550.2328472222 | 2016-06-11 05:35:18 | 55594 | 2011-02-02 00:00:00 | 55228.2152893518 | 2010-02-01 05:10:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041417 | A 'hard excess' has been detected in 2007 Suzaku PIN data for the nearby quasar 1H 0419-577 relative to models fitting below 10 keV. The excess can be accounted for with Compton-thick partial-covering gas probably part of a clumpy disk wind originating inside of the BLR. The observed Fe Ka line luminosity is consistent with an origin in an equatorial wind. Blurred reflection models cannot satisfactorily fit the source and so 1H0419-577 provides a rare distinction between two observationally-similar classes of model. We propose two 140 ks follow-up Suzaku observations separated by months to probe the properties of the Compton-thick gas via variability measurements: this is an important new science area that can only be studied using the broad bandpass available from Suzaku. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TRACEY TURNER | USA | 4 | AO4 | STUDYING THE COMPTON-THICK PARTIAL-COVERING ABSORPTION IN 1H 0419-577 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704064010/ | Quick Look | ![]() |
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969 | 0534-69.9 | 83.5094 | -69.9134 | 83.62618 | -69.94462 | 302.596953 | -85.878508 | 280.47493809 | -31.97334872 | 273.4822 | 55286.3873726852 | 2010-03-31 09:17:49 | 55289.2981597222 | 2010-04-03 07:09:21 | 505064010 | 109.2367 | 100 | 109.2687 | 109.2367 | 0 | 109.2767 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79.8262 | 79.8262 | 251.4437 | 2 | PROCESSED | 57551.1453819445 | 2016-06-12 03:29:21 | 55287 | 2010-04-01 00:00:00 | 55302.4291898148 | 2010-04-16 10:18:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051102 | Type Ia SNe play a central role in modern astrophysics, and yet we know little about their progenitors. Some of these progenitors are expected to significantly modify ambient medium around them prior to SN explosions. A standard Type Ia SNR model, a white dwarf explosion in a uniform ambient medium, fails to account for bright Fe-rich ejecta and faint blast waves seen in majority of Type Ia SNRs in the Magellanic Clouds. A promising explanation involves presence of dense circumstellar medium (CSM) around their progenitors. We propose a Suzaku study of 4 mature Type Ia SNRs in the LMC, with the goal of determining chemical abundances, temperatures and ionization ages within their ejecta. This will allow us to construct dynamical SNR models, and learn about their CSM and progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | KAZIMIERZ BORKOWSKI | USA | 5 | AO5 | TYPE IA REMNANTS IN THE LARGE MAGELLANIC CLOUD: WHAT PROGENITORS? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505064010/ | Quick Look | ![]() |
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970 | G352.7-0.1 | 261.9227 | -35.1119 | 261.088463 | -35.070764 | 263.245639 | -11.859611 | 352.75195989 | -0.12120729 | 94.0335 | 55988.8605671296 | 2012-03-02 20:39:13 | 55993.5536111111 | 2012-03-07 13:17:12 | 506052010 | 201.5474 | 200 | 201.5474 | 201.5474 | 0 | 201.5474 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 171.544 | 171.544 | 405.4396 | 4 | PROCESSED | 57604.9422569445 | 2016-08-04 22:36:51 | 56375 | 2013-03-24 00:00:00 | 56008.397337963 | 2012-03-22 09:32:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061315 | Supernova remnants showing strong Fe K emission are relatively rare, and primarily of Type Ia. We propose a long observation of one of the least well-studied Fe-rich Galactic SNRs, G352.7-0.1, with the goal of characterizing the Fe emission, confirming its likely identification as the remnant of a Type Ia supernova, and constraining the properties of ejected material and the dynamics of the explosion. Its thermal X-ray spectrum is strikingly similar to Tycho's SNR, but unexpectedly X-rays are uniformly distributed throughout the remnant. Our proposed observation will produce high-quality spectra, adequate for detailed studies with some spatial information, that will greatly aid in understanding of this very interesting young remnant. | GALACTIC DIFFUSE EMISSION | 5 | C | KAZIMIERZ BORKOWSKI | USA | 6 | AO6 | STRONG IRON EMISSION IN THE SUPERNOVA REMNANT G352.7-0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506052010/ | Quick Look | ![]() |
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971 | 3C 105 | 61.8399 | 3.6518 | 61.183972 | 3.519003 | 60.504157 | -16.952891 | 187.66746701 | -33.63397375 | 251.3728 | 54501.5363078704 | 2008-02-05 12:52:17 | 54503.0833912037 | 2008-02-07 02:00:05 | 702074010 | 38.319 | 53 | 38.319 | 38.319 | 0 | 38.319 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.8811 | 48.8811 | 133.6558 | 2 | PROCESSED | 57541.5364351852 | 2016-06-02 12:52:28 | 54883 | 2009-02-21 00:00:00 | 54515.7678819444 | 2008-02-19 18:25:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021372 | The nature and even the existence of type II quasars is highly controversial. Due to their highly obscured nature, very hard (> 15 keV) observations are needed to probe their properties. With the 9-month SWIFT BAT all-sky AGN survey, detection of heavily obscured sources is now possible. Indeed, 6 type II quasars have been identified. Their properties, however, are a challenge to standard AGN models e.g., all but one of these sources are strong radio sources and several have optical spectra indicative of an un-absorbed source. We propose Suzaku observations of the 5 without broadband high signal to noise x-ray data to perform a detailed analysis of their x-ray properties and to understand their relationship to the lower luminosity well studied Seyfert IIs. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RICHARD MUSHOTZKY | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF SWIFT BAT TYPE II QUASARS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702074010/ | Quick Look | ![]() |
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972 | NGC 7469 | 345.7842 | 8.9301 | 345.154297 | 8.660604 | 350.460681 | 13.82437 | 83.10914575 | -45.403242 | 63.4793 | 54641.7015856482 | 2008-06-24 16:50:17 | 54644.683599537 | 2008-06-27 16:24:23 | 703028010 | 112.1128 | 100 | 112.1251 | 112.1331 | 0 | 112.1128 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91.5571 | 91.5571 | 257.6126 | 2 | PROCESSED | 57542.968125 | 2016-06-03 23:14:06 | 55027 | 2009-07-15 00:00:00 | 54658.7891319444 | 2008-07-11 18:56:21 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031311 | We propose a 100 ksec observation of the X-ray bright Seyfert 1 AGN NGC 7469, a strong candidate for having ionized reflection from the accretion disk. Only the broad bandpass provided by Suzaku, including >12 keV coverage via the HXD, will allow us to deconvolve the broadband emitting components, including the strong Compton reflection hump, broad Fe K line, and soft excess. With the XIS, we will study in detail the Fe K emission complex, including the narrow 6.4 keV Fe K core and in particular the prominent ``blue wing'' near 6.9 keV. Our proposed observation will thus be an example of how broad bandpass X-ray observations can critically test blurred, ionized disk reflection model in Seyfert 1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | ALEX MARKOWITZ | USA | 3 | AO3 | IONIZED DISK REFLECTION IN THE SEYFERT AGN NGC 7469 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703028010/ | Quick Look | ![]() |
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973 | IRAS 12072-0444 | 182.4393 | -5.0116 | 181.797769 | -4.733385 | 184.228917 | -3.627834 | 283.97337665 | 56.31820605 | 111.9489 | 55534.0444328704 | 2010-12-04 01:03:59 | 55535.5169328704 | 2010-12-05 12:24:23 | 705045010 | 61.9339 | 60 | 61.9419 | 61.9419 | 0 | 61.9339 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.1596 | 28.1596 | 127.206 | 0 | PROCESSED | 57554.3475810185 | 2016-06-15 08:20:31 | 55910 | 2011-12-15 00:00:00 | 55544.3011226852 | 2010-12-14 07:13:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051441 | We propose two Suzaku-HXD observations of two ULIRGs hosting a deeply buried AGN. These two objects are expected to host a powerful AGN in the luminosity range of quasars, based on solid evidence from mid-IR Spitzer spectroscopy. However, these sources are completely buried behind a screen of dust with column density in excess of 10^24 cm^-2, so not only the primary emission below 10 keV is obscured, but the reflected emission, usually ascribed to a circumnuclear "torus", is also absent. This suggests a complete spherical coverage of the X-ray source along all directions. The unique capabilities of Suzaku at high energies will allow to confirm the existence of these objects, representing the most extreme examples of buried AGNs, both in terms of obscuration and of intrinsic luminosity. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | GUIDO RISALITI | USA | 5 | AO5 | BURIED QUASAR 2S INSIDE ULIRGS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705045010/ | Quick Look | ![]() |
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974 | NGC 6814 | 295.6733 | -10.3371 | 294.986368 | -10.456223 | 295.709061 | 10.841132 | 29.34034439 | -16.02176478 | 260.0004 | 55867.6992013889 | 2011-11-02 16:46:51 | 55868.637662037 | 2011-11-03 15:18:14 | 706032010 | 42.12 | 40 | 42.1435 | 42.136 | 0 | 42.12 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.0918 | 40.0918 | 81.0698 | 1 | PROCESSED | 57603.6893518518 | 2016-08-03 16:32:40 | 56248 | 2012-11-17 00:00:00 | 55881.0746527778 | 2011-11-16 01:47:30 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061411 | Fermi-LAT has revealed gamma-ray emission from Seyfert galaxies in its 1st catalog. Optical and X-ray spectra of Seyferts generally provide important clues to the nature of the accretion process, and thus those objects are promising targets to investigate the connection of the jet to the central source. Here, we propose Suzaku observations of three Seyfert-type AGNs from our gamma-ray candidate list: those objects are also present in the Swift-BAT catalog. Those are III Zw 2, NGC 6814 and ESO 323-G077 and we request pointings of 80 ks, 40 ks and 40 ks respectively. All three candidates appear to be associated with AGN, but show different radio or IR properties. Suzaku data will give us crucial information to investigate the origin of high-energy emission from those Seyfert objects. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MASAAKI HAYASHIDA | USA | 6 | AO6 | SUZAKU OBSERVATIONS OF SEYFERT GALAXIES AS GAMMA-RAY SOURCE CANDIDATES SELECTED FROM THE SWIFT-BAT CATALOG | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706032010/ | Quick Look | ![]() |
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975 | BOOTES_GROUP_32 | 217.4805 | 33.2976 | 216.950847 | 33.519259 | 200.513031 | 44.906456 | 55.13369931 | 67.90745799 | 91.5977 | 54868.4415740741 | 2009-02-06 10:35:52 | 54869.3619675926 | 2009-02-07 08:41:14 | 803045010 | 40.7287 | 40 | 40.7447 | 40.7287 | 0 | 40.7447 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.6563 | 34.6563 | 79.4878 | 2 | PROCESSED | 57545.4809490741 | 2016-06-06 11:32:34 | 55328 | 2010-05-12 00:00:00 | 54880.5918518518 | 2009-02-18 14:12:16 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031411 | Galaxy groups are vital to our understanding of structure formation, cluster evolution, and galaxy evolution, yet they are difficult to study at even moderate redshift. We have undertaken a project to observe a flux-limited sample of intermediate-redshift groups identified by the XBootes Chandra survey, and here we propose Suzaku/XIS observations of two targets to continue this program. With the unique multiwavelength coverage of the XBootes field, we aim to understand the physical connection between the X-ray and optical properties of groups, and to probe the evolution of group X-ray emission in order to constrain the non-gravitational physics affecting the energetics of the intragroup medium. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | ERIC MILLER | USA | 3 | AO3 | UNDERSTANDING GROUP EVOLUTION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803045010/ | Quick Look | ![]() |
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976 | BOOTES_GROUP_37 | 216.3696 | 32.9366 | 215.835617 | 33.161488 | 199.570858 | 44.168282 | 54.59315934 | 68.88543442 | 308.8196 | 54640.4539467593 | 2008-06-23 10:53:41 | 54641.6898611111 | 2008-06-24 16:33:24 | 803044010 | 52.9034 | 40 | 52.9114 | 52.9114 | 0 | 52.9034 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.6527 | 47.6527 | 106.7658 | 2 | PROCESSED | 57542.9257638889 | 2016-06-03 22:13:06 | 55020 | 2009-07-08 00:00:00 | 54651.1591319444 | 2008-07-04 03:49:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031411 | Galaxy groups are vital to our understanding of structure formation, cluster evolution, and galaxy evolution, yet they are difficult to study at even moderate redshift. We have undertaken a project to observe a flux-limited sample of intermediate-redshift groups identified by the XBootes Chandra survey, and here we propose Suzaku/XIS observations of two targets to continue this program. With the unique multiwavelength coverage of the XBootes field, we aim to understand the physical connection between the X-ray and optical properties of groups, and to probe the evolution of group X-ray emission in order to constrain the non-gravitational physics affecting the energetics of the intragroup medium. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | ERIC MILLER | USA | 3 | AO3 | UNDERSTANDING GROUP EVOLUTION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803044010/ | Quick Look | ![]() |
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977 | ABELL 2259 | 259.8931 | 27.621 | 259.395788 | 27.671022 | 255.818642 | 50.564036 | 50.28820146 | 31.27138653 | 102.8681 | 57093.1224305556 | 2015-03-12 02:56:18 | 57094.3141203704 | 2015-03-13 07:32:20 | 809081040 | 43.027 | 42.5 | 43.027 | 43.027 | 0 | 43.5266 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.7751736111 | 2016-08-17 18:36:15 | 57475 | 2016-03-28 00:00:00 | 57108.4150578704 | 2015-03-27 09:57:41 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091526 | Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but not many were studied for "regular" non-cool core clusters. We propose a 170 ks Suzaku observation of a regular non-cool core cluster Abell 2259. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KA-WAH WONG | USA | 9 | AO9 | REGULAR NON-COOL CORE GALAXY CLUSTER OUT TO THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809081040/ | Quick Look | ![]() |
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978 | ABELL 426 N5 | 49.0181 | 42.6863 | 48.185508 | 42.502238 | 58.244167 | 23.659861 | 149.32374876 | -12.65326208 | 59.9992 | 55063.2465740741 | 2009-08-20 05:55:04 | 55063.8238310185 | 2009-08-20 19:46:19 | 804067010 | 23.6074 | 20 | 23.6314 | 23.6074 | 0 | 23.6394 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.1435 | 21.1435 | 49.8659 | 1 | PROCESSED | 57548.2975115741 | 2016-06-09 07:08:25 | 55441 | 2010-09-02 00:00:00 | 55075.0347685185 | 2009-09-01 00:50:04 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804067010/ | Quick Look | ![]() |
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979 | COMA E6 | 196.7721 | 27.8867 | 196.173433 | 28.153627 | 183.239501 | 32.041991 | 46.15941504 | 86.44797144 | 279.9997 | 55731.2742013889 | 2011-06-19 06:34:51 | 55731.589837963 | 2011-06-19 14:09:22 | 806036010 | 12.4586 | 15 | 12.4666 | 12.4586 | 0 | 12.4666 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.2065 | 12.2065 | 27.2519 | 0 | PROCESSED | 57602.3498263889 | 2016-08-02 08:23:45 | 55652 | 2011-04-01 00:00:00 | 55770.1165046296 | 2011-07-28 02:47:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806036010/ | Quick Look | ![]() |
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980 | ABELL 3411 | 130.503 | -17.558 | 129.929319 | -17.378234 | 138.643901 | -34.411415 | 242.03718903 | 14.84069283 | 105.0003 | 56964.4121759259 | 2014-11-03 09:53:32 | 56967.3091898148 | 2014-11-06 07:25:14 | 809082010 | 126.6792 | 130 | 126.6792 | 131.2712 | 0 | 131.2632 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.749525463 | 2016-08-16 17:59:19 | 57358 | 2015-12-02 00:00:00 | 56982.4526273148 | 2014-11-21 10:51:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091528 | Galaxy cluster mergers trigger Mpc-scale shocks in the ICM, which can accelerate particles to relativistic energies to form arc-shaped radio relics. Last year, we discovered a spectacular radio relic in the Planck cluster A3411. The relic has a complex, fragmentary morphology, at odds with the arc-shaped shocks predicted by hydrodynamical simulations. In light of this unexpected discovery, we propose for a 169-ks Suzaku observation to characterize the ICM properties at the radio relic in A3411. The combination of high-quality X-ray and radio data will provide a unique opportunity to (1) measure the shock properties and relate them to the radio structures; (2) explore the reason for the fragmentation of the relic; (3) model the merger event; and (4) test different shock acceleration models. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | REINOUT VAN WEEREN | USA | 9 | AO9 | ABELL 3411: PARTICLE RE-ACCELERATION AND A COMPLEX SHOCK GEOMETRY? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809082010/ | Quick Look | ![]() |
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981 | ABELL2804 | 9.8968 | -28.9096 | 9.281885 | -29.184169 | 356.393467 | -30.22696 | 357.98440451 | -86.83577265 | 234.7036 | 53706.3688078704 | 2005-12-02 08:51:05 | 53707.166875 | 2005-12-03 04:00:18 | 800007010 | 31.6129 | 25 | 31.6129 | 31.6129 | 31.6129 | 31.6129 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 26.9145 | 26.9145 | 68.95 | 2 | PROCESSED | 57532.3559259259 | 2016-05-24 08:32:32 | 54247 | 2007-05-27 00:00:00 | 54038.8727893518 | 2006-10-30 20:56:49 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001025 | We propose to observe the central region of the Sculptor supercluster at z=0.11, in a search for the theoretically predicted Warm/Hot Intergalactic Medium (WHIM). The WHIM has been 'missing' observationally, until recent detection of the X-ray absorption due to the ionized light elements in the background quasar spectra. Still there is no confident detection of the expected soft X-ray emission. This is mainly because that the X-ray brightness is very low, compared to the Galactic diffuse emission in the soft X-ray band and/or the spectral sensitivity of previous experiments are limited. To separate the expected X-ray lines of the WHIM (mainly O VII) from the Galactic emission, we select an unique supercluster at z>0.1. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | TAKAYUKI TAMURA | JAP | 0 | SWG | THE SCULPTOR SUPERCLUSTER: SEARCH FOR THE WARM/HOT INTERGALACTIC MEDIUM | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800007010/ | Quick Look | ![]() |
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982 | HD432 | 2.3079 | 59.1397 | 1.651195 | 58.861536 | 35.116502 | 51.20601 | 117.53319828 | -3.2889222 | 246.0535 | 54471.6956944444 | 2008-01-06 16:41:48 | 54472.297349537 | 2008-01-07 07:08:11 | 402034020 | 26.9844 | 27 | 26.9844 | 26.9844 | 0 | 26.9844 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24.601 | 24.601 | 51.9759 | 0 | PROCESSED | 57541.2823958333 | 2016-06-02 06:46:39 | 54871 | 2009-02-09 00:00:00 | 54483.3863773148 | 2008-01-18 09:16:23 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021016 | Suzaku XIS spectra of three "X-ray deficient" Hertzsprung gap giants will explore why they display anomalous coronal behavior compared with cooler giants only slightly further advanced in their evolution. The apparent sharp transition in coronal properties on the way to helium flash might be caused by disruption of a "fossil" magnetosphere by a newly born solar-like dynamo. A key discriminator is the coronal energy distribution, especially enhanced and sporadic hard emission associated with flaring. The proposed targets are the brightest not previously observed in X-rays at CCD resolution; all three have supporting high resolution UV spectra. Expanding the sample of high quality, high energy information on this key class of objects is essential for probing their odd behavior. | GALACTIC POINT SOURCES | 4 | C | THOMAS AYRES | USA | 2 | AO2 | ANOMALOUS CORONAE OF HERTZSPRUNG GAP GIANTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402034020/ | Quick Look | ![]() |
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983 | HD162020 | 267.6611 | -40.3282 | 266.784303 | -40.314701 | 268.126834 | -16.902096 | 350.73095661 | -6.73195128 | 265.867 | 55808.0919560185 | 2011-09-04 02:12:25 | 55808.4078703704 | 2011-09-04 09:47:20 | 406037010 | 15.9229 | 15 | 15.9229 | 15.9229 | 0 | 15.9229 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15.9406 | 15.9406 | 27.2879 | 2 | PROCESSED | 57603.0570949074 | 2016-08-03 01:22:13 | 56232 | 2012-11-01 00:00:00 | 55865.1159953704 | 2011-10-31 02:47:02 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061202 | Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. | GALACTIC POINT SOURCES | 4 | A | IGNAZIO PILLITTERI | USA | 6 | AO6 | STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406037010/ | Quick Look | ![]() |
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984 | ETA CARINAE | 161.2639 | -59.6881 | 160.777388 | -59.424763 | 202.155739 | -58.924842 | 287.59810122 | -0.63296206 | 310.0122 | 55766.0329398148 | 2011-07-24 00:47:26 | 55766.9286226852 | 2011-07-24 22:17:13 | 406039010 | 42.0302 | 50 | 42.0302 | 42.0302 | 0 | 42.0302 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 49.0937 | 49.0937 | 77.3839 | 0 | PROCESSED | 57602.6625462963 | 2016-08-02 15:54:04 | 56163 | 2012-08-24 00:00:00 | 55785.0281712963 | 2011-08-12 00:40:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061205 | Eta Car is the nearest highly unstable extremely massive star and a key object for understanding how mass and angular momentum change as an extremely massive star heads towards hypernova. Periodic minima in X-rays and other wavebands show it as an extremely eccentric binary with a massive companion. A surprising change in the X-ray emission during the January 2009 X-ray minimum probably indicates a large-scale variation in the LBV primary's mass loss rate. We propose a Suzaku observation in AO6 to monitor the change of the absorption column in the line of sight and the non-thermal emission above 10 keV. The observation will help to study geometry of the binary orbit of Eta Car and the mechanism of the non-thermal emission. | GALACTIC POINT SOURCES | 4 | B | KENJI HAMAGUCHI | USA | 6 | AO6 | MONITORING DYNAMICAL MASS LOSS FROM ETA CAR WITH SUZAKU: APASTRON | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406039010/ | Quick Look | ![]() |
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985 | EK TRA | 228.5098 | -65.0893 | 227.42561 | -64.902826 | 246.763957 | -44.956932 | 317.22984637 | -6.25468419 | 278.6002 | 56149.7387152778 | 2012-08-10 17:43:45 | 56150.8473611111 | 2012-08-11 20:20:12 | 407044010 | 77.8344 | 70 | 77.8504 | 77.8344 | 0 | 77.8504 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69.8973 | 69.8973 | 95.7779 | 2 | PROCESSED | 57606.8494907407 | 2016-08-06 20:23:16 | 56540 | 2013-09-05 00:00:00 | 56170.0360532407 | 2012-08-31 00:51:55 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071212 | The mass of an accreting white dwarf is a key parameter governing its X-ray emission. We expect that the higher the mass, the higher the temperature and luminosity. Existing data appear consistent with this expectation, given the considerable uncertainties usually associated with the white dwarf masses of individual systems. Here we propose Suzaku observations of 5 dwarf novae for which very high or very low white dwarf mass estimates have been published. These targets provide the best opportunity of further establishing the mass-temperature correlation. Moreover, if the mass estimates are reliable, these targets are of interest from evolutionary considerations - how did these systems form with such high/low mass white dwarfs, and what are their ultimate fates? | GALACTIC POINT SOURCES | 4 | A | KOJI MUKAI | USA | 7 | AO7 | DWARF NOVAE WITH EXTREME WHITE DWARF MASSES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407044010/ | Quick Look | ![]() |
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986 | GALACTIC RIDGE | 281.0036 | -4.078 | 280.343207 | -4.129572 | 281.600756 | 18.920487 | 28.45707071 | -0.21069081 | 265.5303 | 54023.0938888889 | 2006-10-15 02:15:12 | 54025.8141087963 | 2006-10-17 19:32:19 | 500009020 | 98.8583 | 100 | 98.8743 | 98.8663 | 98.8583 | 98.8743 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 81.9519 | 81.9519 | 235.0139 | 1 | PROCESSED | 57535.9070023148 | 2016-05-27 21:46:05 | 54697 | 2008-08-19 00:00:00 | 54055.6082407407 | 2006-11-16 14:35:52 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001042 | We propose to observe the blank Galactic plane field at (l,b)=(28.6,0.0) for 200 ksec to study energy spectra of Galactic Ridge X-ray Emission. This is a Chandra deep field where we have spent 100 ksec. We will carry out plasma diagnostics of the Galactic ridge emission using primarily iron lines, and also Kalpha and Kbeta lines of Ne, Mg, Si, and S. The 200 ksec Ridge observation by Suzaku enables us to compare Galactic center and ridge emission lines directly. We believe the Galactic Ridge X-ray emission is truely diffuse, based on our Chandra study. However, there is a claim that the ridge emission is preimaly composed of dim sources down to 10^-16 cgs in 2-10 keV. To end the controversy, we plan to carry out a 1Msec Chandra observation on this Chandra-Suzaku field. | GALACTIC DIFFUSE EMISSION | 5 | A | KEN EBISAWA | JAP | 0 | SWG | ORIGIN OF THE GALACTIC RIDGE X-RAY EMISSION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500009020/ | Quick Look | ![]() |
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987 | DIFFUSE1C | 201.9274 | 6.8104 | 201.299196 | 7.069212 | 197.642152 | 14.849246 | 327.54723828 | 67.93166205 | 123.897 | 57015.2219560185 | 2014-12-24 05:19:37 | 57015.3450115741 | 2014-12-24 08:16:49 | 509060010 | 5.5117 | 20 | 5.5277 | 5.5197 | 0 | 5.5117 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5590393518 | 2016-08-17 13:25:01 | 57417 | 2016-01-30 00:00:00 | 57049.4528587963 | 2015-01-27 10:52:07 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091324 | In the course of a program to fit spatial models to the Galactic hot gas content, we discovered a few fields that were highly discrepant in the strength of their O VII and/or O VIII line strengths. These are rare emission regions, occurring in fewer than 1% of the fields and they are not due to known extended emission regions (SNR, galaxy clusters, etc.). These emission anomalies probably signify locations of unusual physics, such as shocks, conductive heating, or local heat injection. We propose observations to determine the angular extent of these unusual regions and to better define the intensities of the O VII and O VIII lines. These observations will help identify the relevant physical process and the nature of the phenomenon causing them. | GALACTIC DIFFUSE EMISSION | 5 | C | JOEL BREGMAN | USA | 9 | AO9 | UNIDENTIFIED BRIGHT X-RAY BACKGROUND REGIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509060010/ | Quick Look | ![]() |
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988 | PKS 0745-191 | 116.6543 | -19.2063 | 116.100315 | -19.082609 | 123.362638 | -39.608686 | 236.25768919 | 2.88874721 | 294.0002 | 54231.8221180556 | 2007-05-11 19:43:51 | 54232.5001041667 | 2007-05-12 12:00:09 | 802062020 | 31.2266 | 30 | 31.2266 | 31.2266 | 0 | 31.2266 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.967 | 25.967 | 58.5739 | 1 | PROCESSED | 57538.6330208333 | 2016-05-30 15:11:33 | 54695 | 2008-08-17 00:00:00 | 54238.8889814815 | 2007-05-18 21:20:08 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021440 | PKS 0745-191 is the X-ray brightest galaxy cluster beyond a redshift of 0.1. It has a smooth surface brightness profile and appears relaxed. Using the low background of Suzaku we will measure the temperature of the intracluster medium to the virial radius of the cluster. Its high temperature means that we will be unaffected by any loss of effective area at low energies. In addition the cluster is bright enough so that the bremsstrahlung emission will be easily detected using the PIN detector. This will allow us to search for any nonthermal component as well as accurately determining the high temperature components in the cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ANDREW YOUNG | USA | 2 | AO2 | PKS 0745-191: THE BRIGHTEST CLUSTER BEYOND Z=0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802062020/ | Quick Look | ![]() |
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989 | RCS 1104-0445 | 166.1645 | -4.748 | 165.529365 | -4.478046 | 169.133755 | -9.830173 | 259.90521833 | 48.99506028 | 108.5039 | 54420.9087037037 | 2007-11-16 21:48:32 | 54421.3210532407 | 2007-11-17 07:42:19 | 802068010 | 19.335 | 15 | 19.335 | 19.335 | 0 | 19.335 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15.1627 | 15.1627 | 35.6159 | 0 | PROCESSED | 57540.5367013889 | 2016-06-01 12:52:51 | 54797 | 2008-11-27 00:00:00 | 54430.2980787037 | 2007-11-26 07:09:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021451 | We propose Suzaku observations of a sample of 10 galaxy clusters at redshifts between 0.6 and 0.95 from the RCS-1 cluster survey. These objects represent the optically richest clusters at these redshifts from the 100 square degree survey using the red-sequence method of cluster detection. As such, they form a critical sample for calibrating the mass-richness relationship for high redshift cluster surveys. Our proposed observations will allow us to determine their X-ray luminosities, as a first guide to estimating their masses, and enable future studies to determine accurate masses from their X-ray properties. These studies are complimentary to mass calibration programs we are carrying out using estimates based on lensing, IR stellar mass and galaxy dynamics. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 2 | AO2 | A SUZAKU SNAPSHOT SURVEY OF HIGH-REDSHIFT GALAXY CLUSTERS FROM THE RCS SURVEY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802068010/ | Quick Look | ![]() |
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990 | NGC741MOSAICS_P3 | 28.9813 | 4.9712 | 28.329333 | 4.726893 | 28.70862 | -6.461023 | 151.24323938 | -54.31718683 | 71.7124 | 55052.9243981482 | 2009-08-09 22:11:08 | 55053.1529976852 | 2009-08-10 03:40:19 | 804054030 | 9.4013 | 10 | 9.4093 | 9.4013 | 0 | 9.415 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.0683 | 7.0683 | 19.72 | 0 | PROCESSED | 57548.0955671296 | 2016-06-09 02:17:37 | 55451 | 2010-09-12 00:00:00 | 55085.0001736111 | 2009-09-11 00:00:15 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JOEL BREGMAN | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804054030/ | Quick Look | ![]() |
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991 | SKY(270, +25) | 270.2558 | 25.1504 | 269.745742 | 25.150381 | 270.337589 | 48.59021 | 50.99920401 | 21.68976417 | 70.6538 | 55284.5620023148 | 2010-03-29 13:29:17 | 55285.2994791667 | 2010-03-30 07:11:15 | 404041010 | 1.7019 | 25 | 1.9266 | 2.0944 | 0 | 1.7019 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 5.6211 | 5.6211 | 63.7139 | 1 | PROCESSED | 57551.0540277778 | 2016-06-12 01:17:48 | 55284 | 2010-03-29 00:00:00 | 55301.2652314815 | 2010-04-15 06:21:56 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041222 | Suzaku has recently revealed relativistically broadened Fe Kalpha emission lines in the spectra of neutron star low-mass X-ray binaries (LMXBs). We have now seen these lines in 10 neutron star LMXBs that we have examined, allowing measurements of the inner accretion disk radius, and hence an upper limit on the neutron star radius in all these objects. Only with the sensitivity of Suzaku, its high effective area in the Fe K band, and its broad bandpass has it been possible to robustly determine the shape of the lines. With a longer-term aim of completing a census of iron lines in neutron star LMXBs, we request a total of 200 ks to observe 5 neutron star low-mass X-ray binaries to study the relativistic broadening in the Fe Kalpha emission line profiles. | GALACTIC POINT SOURCES | 4 | C | EDWARD CACKETT | USA | 4 | AO4 | AN FE KALPHA EMISSION LINE SURVEY OF NEUTRON STAR LMXBS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404041010/ | Quick Look | ![]() |
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992 | 4U 1210-64 | 183.3036 | -64.8719 | 182.632422 | -64.593786 | 222.057216 | -55.171704 | 298.88624165 | -2.30082607 | 98.4956 | 55553.1591550926 | 2010-12-23 03:49:11 | 55555.1488194444 | 2010-12-25 03:34:18 | 405045010 | 79.3476 | 80 | 79.3476 | 79.3476 | 0 | 79.3561 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.7512 | 70.7512 | 171.8799 | 0 | PROCESSED | 57554.5554398148 | 2016-06-15 13:19:50 | 55961 | 2012-02-04 00:00:00 | 55595.085474537 | 2011-02-03 02:03:05 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051236 | 4U 1210-64 is a high mass X-ray binary with a stable 6.7 day period when the long-term (RXTE ASM) light curve is analyzed. However, we observed strong aperiodic variability in a series of pointed observations with the RXTE PCA, to the point of masking this 6.7 day period. Moreover, we have not detected a spin period, even though the accretor is most likely a neutron star. The strong variability is suggestive of accretion from a clumpy wind. We propose a 2-day Suzaku observation of this object (1) to search for unequivocal evidence for a neutron star, such as the spin period and cyclotron features; and (2) to measure the spectral shapes at different flux levels, to investigate the cause of the strong aperiodic variability. | GALACTIC POINT SOURCES | 4 | C | KOJI MUKAI | USA | 5 | AO5 | 4U 1210-64: A HIGHLY VARIABLE X-RAY BINARY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405045010/ | Quick Look | ![]() |
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993 | 4U 1957+11 | 299.8426 | 11.72 | 299.251782 | 11.582704 | 304.891281 | 31.61725 | 51.31417386 | -9.31797438 | 71.6227 | 55320.4377777778 | 2010-05-04 10:30:24 | 55321.4168055556 | 2010-05-05 10:00:12 | 405057010 | 35.796 | 35 | 35.804 | 35.804 | 0 | 35.796 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.8692 | 30.8692 | 84.58 | 0 | PROCESSED | 57551.4086226852 | 2016-06-12 09:48:25 | 55741 | 2011-06-29 00:00:00 | 55375.7567013889 | 2010-06-28 18:09:39 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051254 | We propose three observations of the black hole candidate 4U 1957+11. It is one of only two persistently soft state BHC, and has the highest fitted temperature, and highest fitted spin parameter, of any observed BHC. The question arises of whether this high spin is a good estimate of the true spin, or whether this high temperature is evidence of a low level or corona or wind. The multiple Suzaku observations will allow us to track how the disk parameters change, and offer us a 40% chance of observing a state with a large coronal component. The latter might be indicative of launching of a disk wind. | GALACTIC POINT SOURCES | 4 | B | MICHAEL NOWAK | USA | 5 | AO5 | 4U1957+11: THE MOST RAPIDLY SPINNING BLACK HOLE? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405057010/ | Quick Look | ![]() |
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994 | 73P/SW3 | 317.5094 | 24.3437 | 316.953773 | 24.139336 | 329.181406 | 38.538464 | 71.75290875 | -15.84652301 | 72.7094 | 53868.2758333333 | 2006-05-13 06:37:12 | 53868.3418865741 | 2006-05-13 08:12:19 | 500013030 | 3.225 | 20 | 3.225 | 3.225 | 3.225 | 3.225 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.915 | 2.915 | 5.7039 | 0 | PROCESSED | 57534.2995023148 | 2016-05-26 07:11:17 | 54256 | 2007-06-05 00:00:00 | 54042.2712731482 | 2006-11-03 06:30:38 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013030/ | Quick Look | ![]() |
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995 | COMET_8P_TUTTLE-P1-1 | 27.7163 | 7.989 | 27.057965 | 7.741803 | 28.591929 | -3.193745 | 147.31647839 | -52.04673223 | 248.4436 | 54470.5233333333 | 2008-01-05 12:33:36 | 54470.5821759259 | 2008-01-05 13:58:20 | 502062010 | 0.6803 | 2 | 0.6803 | 0.6803 | 0 | 0.6803 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 0.632 | 0.632 | 5.08 | 0 | PROCESSED | 57540.9802199074 | 2016-06-01 23:31:31 | 54908 | 2009-03-18 00:00:00 | 54542.4502083333 | 2008-03-17 10:48:18 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062010/ | Quick Look | ![]() |
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996 | SEP #1 | 89.966 | -66.5774 | 89.968235 | -66.57758 | 292.016086 | -89.97915 | 276.40322057 | -29.82494721 | 141.7136 | 55149.1175925926 | 2009-11-14 02:49:20 | 55150.2141087963 | 2009-11-15 05:08:19 | 504069010 | 51.8621 | 50 | 51.8701 | 51.8621 | 0 | 51.8701 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.3534 | 48.3534 | 94.7259 | 2 | PROCESSED | 57549.3577546296 | 2016-06-10 08:35:10 | 54922 | 2009-04-01 00:00:00 | 55160.1496296296 | 2009-11-25 03:35:28 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | STEVEN SNOWDEN | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504069010/ | Quick Look | ![]() |
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997 | FG14 | 176.6962 | 9.8632 | 176.052451 | 10.141025 | 173.028517 | 7.733182 | 258.4262435 | 66.96745764 | 295.6185 | 56076.7125925926 | 2012-05-29 17:06:08 | 56077.2168171296 | 2012-05-30 05:12:13 | 807055010 | 12.4926 | 10 | 12.5006 | 12.495 | 0 | 12.4926 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.535 | 13.535 | 43.5539 | 1 | PROCESSED | 57605.5555671296 | 2016-08-05 13:20:01 | 56452 | 2013-06-09 00:00:00 | 56086.1554861111 | 2012-06-08 03:43:54 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071511 | Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ELENA D'ONGHIA | USA | 7 | AO7 | SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807055010/ | Quick Look | ![]() |
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998 | SWCL0759+3244 | 119.7517 | 32.7514 | 118.954635 | 32.88785 | 115.246831 | 11.881047 | 188.23731341 | 27.65711067 | 99.0622 | 56961.3067708333 | 2014-10-31 07:21:45 | 56962.2286574074 | 2014-11-01 05:29:16 | 809085010 | 42.3039 | 41 | 42.3039 | 42.3039 | 0 | 42.3039 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7390277778 | 2016-08-16 17:44:12 | 57345 | 2015-11-19 00:00:00 | 56979.4492708333 | 2014-11-18 10:46:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091531 | The evolution of X-ray properties of galaxy clusters with redshift provides important constraints on the self-similar models of cluster evolution. The scaling relations and their deviations from self-similar models due to non-gravitational processes are important for modeling the cluster selection function for cosmology. We propose to observe a uniform sample of z ~ 0.6 galaxy clusters, selected from Swift archival data and confirmed by multi-band optical data, using Suzaku to better characterize their X-ray properties such as the X-ray luminosity and temperature. With this uniformly selected sample from a narrow redshift bin, we are able to independently constrain the self-similar evolution of cluster properties with redshift. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | XINYU DAI | USA | 9 | AO9 | X-RAY PROPERTIES OF A UNIFORMLY SELECTED SAMPLE OF Z ~ 0.6 CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809085010/ | Quick Look | ![]() |
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