DARTS Astro

total 998

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