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173 results on '"Kohmura, T."'

2. Sub-pixel Response of Double-SOI Pixel Sensors for X-ray Astronomy

Author

Hagino, K., Negishi, K., Oono, K., Yarita, K., Kohmura, T., Tsuru, T. G., Tanaka, T., Harada, S., Kayama, K., Matsumura, H., Mori, K., Takeda, A., Nishioka, Y., Yukumoto, M., Fukuda, K., Hida, T., Arai, Y., Kurachi, I., and Kishimoto, S.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We have been developing the X-ray silicon-on-insulator (SOI) pixel sensor called XRPIX for future astrophysical satellites. XRPIX is a monolithic active pixel sensor consisting of a high-resistivity Si sensor, thin SiO$_2$ insulator, and CMOS pixel circuits that utilize SOI technology. Since XRPIX is capable of event-driven readouts, it can achieve high timing resolution greater than $\sim 10{\rm ~\mu s}$, which enables low background observation by adopting the anti-coincidence technique. One of the major issues in the development of XRPIX is the electrical interference between the sensor layer and circuit layer, which causes nonuniform detection efficiency at the pixel boundaries. In order to reduce the interference, we introduce a Double-SOI (D-SOI) structure, in which a thin Si layer (middle Si) is added to the insulator layer of the SOI structure. In this structure, the middle Si layer works as an electrical shield to decouple the sensor layer and circuit layer. We measured the detector response of the XRPIX with D-SOI structure at KEK. We irradiated the X-ray beam collimated with $4{\rm ~\mu m\phi}$ pinhole, and scanned the device with $6{\rm ~\mu m}$ pitch, which is 1/6 of the pixel size. In this paper, we present the improvement in the uniformity of the detection efficiency in D-SOI sensors, and discuss the detailed X-ray response and its physical origins., Comment: 12 pages, 9 figures, accepted for publication in Journal of Instrumentation

Published
2019
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3. Development of a 32-channel ASIC for an X-ray APD Detector onboard the ISS

Author

Arimoto, M., Harita, S., Sugita, S., Yatsu, Y., Kawai, N., Ikeda, H., Tomida, H., Isobe, N., Ueno, S., Mihara, T., Serino, M., Kohmura, T., Sakamoto, T., Yoshida, A., Tsunemi, H., Hatori, S., Kume, K., and Hasegawa, T.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Instrumentation and Detectors
Abstract

We report on the design and performance of a mixed-signal application specific integrated circuit (ASIC) dedicated to avalanche photodiodes (APDs) in order to detect hard X-ray emissions in a wide energy band onboard the International Space Station. To realize wide-band detection from 20 keV to 1 MeV, we use Ce:GAGG scintillators, each coupled to an APD, with low-noise front-end electronics capable of achieving a minimum energy detection threshold of 20 keV. The developed ASIC has the ability to read out 32-channel APD signals using 0.35 $\mu$m CMOS technology, and an analog amplifier at the input stage is designed to suppress the capacitive noise primarily arising from the large detector capacitance of the APDs. The ASIC achieves a performance of 2099 e$^{-}$ + 1.5 e$^{-}$/pF at root mean square (RMS) with a wide 300 fC dynamic range. Coupling a reverse-type APD with a Ce:GAGG scintillator, we obtain an energy resolution of 6.7% (FWHM) at 662 keV and a minimum detectable energy of 20 keV at room temperature (20 $^{\circ}$C). Furthermore, we examine the radiation tolerance for space applications by using a 90 MeV proton beam, confirming that the ASIC is free of single-event effects and can operate properly without serious degradation in analog and digital processing., Comment: Accepted for publication in NIMA

Published
2017
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4. In-orbit performance of the soft X-ray imaging system aboard Hitomi (ASTRO-H)

Author

Nakajima, H., Maeda, Y., Uchida, H., Tanaka, T., Tsunemi, H., Hayashida, K., Tsuru, T. G., Dotani, T., Nagino, R., Inoue, S., Ozaki, M., Tomida, H., Natsukari, C., Ueda, S., Mori, K., Yamauchi, M., Hatsukade, I., Nishioka, Y., Sakata, M., Beppu, T., Honda, D., Nobukawa, M., Hiraga, J. S., Kohmura, T., Murakami, H., Nobukawa, K. K., Bamba, A., Doty, J. P., Iizuka, R., Sato, T., Kurashima, S., Nakaniwa, N., Asai, R., Ishida, M., Mori, H., Soong, Y., Okajima, T., Serlemitsos, P., Tawara, Y., Mitsuishi, I., Ishibashi, K., Tamura, K., Hayashi, T., Furuzawa, A., Sugita, S., Miyazawa, T., Awaki, H., Miller, E. D., and Yamaguchi, H.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We describe the in-orbit performance of the soft X-ray imaging system consisting of the Soft X-ray Telescope and the Soft X-ray Imager aboard Hitomi. Verification and calibration of imaging and spectroscopic performance are carried out making the best use of the limited data of less than three weeks. Basic performance including a large field of view of 38'x38' is verified with the first light image of the Perseus cluster of galaxies. Amongst the small number of observed targets, the on-minus-off pulse image for the out-of-time events of the Crab pulsar enables us to measure a half power diameter of the telescope as about 1.3'. The average energy resolution measured with the onboard calibration source events at 5.89 keV is 179 pm 3 eV in full width at half maximum. Light leak and cross talk issues affected the effective exposure time and the effective area, respectively, because all the observations were performed before optimizing an observation schedule and parameters for the dark level calculation. Screening the data affected by these two issues, we measure the background level to be 5.6x10^{-6} counts s^{-1} arcmin^{-2} cm^{-2} in the energy band of 5-12 keV, which is seven times lower than that of the Suzaku XIS-BI., Comment: Accepted for publication in PASJ. 17 pages, 18 figures

Published
2017
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5. ASTRO-H White Paper - Accreting Pulsars, Magnetars, and Related Sources

Author

Kitamoto, S., Enoto, T., Safi-Harb, S., Pottschmidt, K., Ferrigno, C., Chernyakova, M., Hayashi, T., Hell, N., Kaneko, K., Khangulyan, D., Kohmura, T., Krimm, H., Makishima, K., Nakano, T., Odaka, H., Ohno, M., Sasano, M., Sugita, S., Terada, Y., Yasuda, T., and Yuasa, T.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

As the endpoints of massive star evolution, neutron stars are enigmatic celestial objects characterized by extremely dense and exotic nuclear matter, magnetospheres with positrons (antimatter), rapid rotation and ultra-strong magnetic fields. Such an extreme environment has provided an accessible astrophysical laboratory to study physics under conditions unattainable on Earth and to tackle a range of fundamental questions related to: the aftermath of stellar evolution and the powerful explosions of massive stars, the equation of state and physics of some of the most exotic and magnetic stars in the Universe, the workings of the most powerful particle accelerators in our Galaxy and beyond, and the sources of gravitational waves that are yet to be detected. Recent observations revealed a great diversity of neutron stars, including ultra-strongly magnetized pulsars, referred to as "magnetars", and unusual types of accreting X-ray pulsars. In this white paper, we highlight the prospects of the upcoming X-ray mission, ASTRO-H, in studying these highly magnetized neutron stars., Comment: 40 pages, 28 figures, ASTRO-H White Paper

Published
2014

6. ASTRO-H White Paper - Low-mass X-ray Binaries

Author

Done, C., Tsujimoto, M., Cackett, E., Herder, J. W. den, Dotani, T., Enoto, T., Ferrigno, C., Kallman, T., Kohmura, T., Laurent, P., Miller, J., Mineshige, S., Mori, H., Nakazawa, K., Paerels, F., Sakurai, S., Soong, Y., Sugita, S., Takahashi, H., Tamagawa, T., Tanaka, Y., Terada, Y., and Uno, S.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

There is still 10-20% uncertainty on the neutron star (NS) mass-radius relation. These uncertainties could be reduced by an order of magnitude through an unambiguous measure of M/R from the surface redshift of a narrow line, greatly constraining the Equation of State for ultra-dense material. It is possible that the SXS on ASTRO-H can detect this from an accreting neutron star with low surface velocity in the line of sight i.e. either low inclination or low spin. Currently there is only one known low inclination LMXB, Ser X-1, and one known slow spin LMXB, J17480-2446 in Terzan 5. Ser X-1 is a persistent source which is always in the soft state (banana branch), where the accreting material should form a equatorial belt around the neutron star. A pole-on view should then allow the NS surface to be seen directly. A 100 ks observation should allow us to measure M/R if there are any heavy elements in the photosphere at the poles. Conversely, J17480-2446 in Terzan 5 is a transient accretion powered millisecond pulsar, where the accreting material is collimated onto the magnetic pole in the hard (island) state (L_x < 0.1 L_Edd). The hotspot where the shock illuminates the NS surface is clearly seen in this state. A 100 ks ToO observation of this (or any other similarly slow spin system) in this state, may again allow the surface redshift to be directly measured. (abstract continues), Comment: 19 pages, 7 figures, ASTRO-H White Paper

Published
2014

7. The first back-side illuminated types of Kyoto's X-ray astronomy SOIPIX

Author

Itou, M, Tsuru, TG, Tanaka, T, Takeda, A, Matsumura, H, Ohmura, S, Uchida, H, Nakashima, S, Arai, Y, Kurachi, I, Mori, K, Takenaka, R, Nishioka, Y, Kohmura, T, Tamasawa, K, and Tindall, C

Subjects
Nuclear & Particles Physics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Other Physical Sciences
Abstract

We have been developing Kyoto's X-ray astronomy SOI pixel sensors, called “XRPIX”, aiming to extend the frontiers of X-ray astronomy with the wide-band imaging spectroscopy in the 0.5–40 keV band. A dead layer on the X-ray incident surface should ideally be as thin as possible to achieve a high sensitivity below 1 keV, and the depletion layer is required to be thick enough to detect 40 keV X-rays. Thus, we have started developing fully-depleted back-side illuminated (BI) types of XRPIXs. This paper reports on our first two BI devices and their X-ray evaluation (2.6–12 keV). The device named “XRPIX2b-FZ-LA” successfully reaches a full depletion with a thickness of 500 μm. On the other hand, it has a dead layer with a thickness of 1.1–1.5 μm and struggles to achieve the requirement of 1.0 μm. The other device named “XRPIX2b-CZ-PZ”, which is applied with a thin Si sensor-layer and an improved back-side process, is found to satisfy the requirement with its thickness of 0.9–1.0 μm, including Al optical blocking filter of 0.2 μm, although the Si sensor-layer is rather thin with 62 μm. We also describe in this paper the X-ray calibration system that we have built for the X-ray evaluation of XRPIXs.

Published
2016

9. Development of large area SOI pixel sensor "XRPIX-X" with pinned depleted diode structure

Author

Uenomachi, M., primary, Tsuru, T. G., additional, Uchida, H., additional, Ikeda, T., additional, Matsuda, M., additional, Narita, T., additional, Izumi, D., additional, Magata, K., additional, Iwakiri, U., additional, Yukumoto, M., additional, Takeda, A., additional, Mori, K., additional, Ishida, T., additional, Nishioka, Y., additional, Shimazoe, K., additional, Takahashi, H., additional, Hagino, K., additional, Kurachi, I., additional, Arai, Y., additional, Kohmura, T., additional, Uchida, Y., additional, Tanaka, T., additional, and Suzuki, H., additional

Published
2023
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10. Property of LCP-GEM in Pure Dimethyl Ether at Low Pressure

Author

Takeuchi, Y., Tamagawa, T., Kitaguchi, T., Yamada, S., Iwakiri, W., Asami, F., Yoshikawa, A., Kaneko, K., Enoto, T., Hayato, A., Kohmura, T., and team, the GEMS/XACT

Subjects
Physics - Instrumentation and Detectors
Abstract

We present a systematic investigation of the gain properties of a gas electron multiplier (GEM) foil in pure dimethyl ether (DME) at low pressures. The GEM is made from copper- clad liquid crystal polymer insulator (LCP-GEM) designed for space use, and is applied to a time projection chamber filled with low-pressure DME gas to observe the linear polarization of cosmic X-rays. We have measured gains of a 100 um-thick LCP-GEM as a function of the voltage between GEM electrodes at various gas pressures ranging from 10 to 190 Torr with 6.4 keV X-rays. The highest gain at 190 Torr is about 2x10^4, while that at 20 Torr is about 500. We find that the pressure and electric-field dependence of the GEM gain is described by the first Townsend coefficient. The energy scale from 4.5 to 8.0 keV is linear with non-linearity of less than 1.4% above 30 Torr., Comment: 3rd International Conference on Micro Pattern Gaseous Detectors (MPGD2013)

Published
2013
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11. Broad-Band Spectrum of The Black Hole Candidate IGR J17497-2821 Studied with Suzaku

Author

Paizis, A., Ebisawa, K., Takahashi, H., Dotani, T., Kohmura, T., Kokubun, M., Rodriguez, J., Ueda, Y., Walter, R., Yamada, S., Yamaoka, K., and Yuasa, T.

Subjects
Astrophysics
Abstract

The broad-band 1-300 keV Suzaku spectrum of IGR J17497-2821, the X-ray transient discovered by INTEGRAL in September 2006, is presented. Suzaku observed IGR J17497-2821 on September 25, eight days after its discovery, for a net exposure of about 53 ksec. During the Suzaku observation, IGR J17497-2821 is very bright, 2 x 10^37 erg/s at 8 kpc in the 1-300 keV range, and shows a hard spectrum, typical of black hole candidates in the low-hard state. Despite the multi-mission X-ray monitoring of the source, only with Suzaku is it possible to obtain a broad-band spectrum in the 1-300 keV range with a very high signal to noise ratio. A sum of a multi-color disc (DISKBB) and a thermal Comptonization component (COMPPS) with mild reflection is a good representation of our IGR J17497-2821 Suzaku spectrum. The spectral properties of the accretion disc as well as the cut-off energy in the spectrum at about 150 keV are clearly detected and constrained. We discuss the implications on the physical model used to interpret the data and the comparison with previous results., Comment: 7 pages, 6 figures, Accepted for publication in PASJ, Suzaku Special Issue

Published
2008

12. Suzaku Observation of AXP 1E 1841-045 in SNR Kes 73

Author

Morii, M., Kitamoto, S., Shibazaki, N., Takei, D., Kawai, N., Arimoto, M., Ueno, M., Terada, Y., Kohmura, T., and Yamauchi, S.

Subjects
Astrophysics
Abstract

Anomalous X-ray pulsars (AXPs) are thought to be magnetars, which are neutron stars with ultra strong magnetic field of $10^{14}$-- $10^{15}$ G. Their energy spectra below $\sim$10 keV are modeled well by two components consisting of a blackbody (BB) ($\sim$0.4 keV) and rather steep power-law (POW) function (photon index $\sim$2-4). Kuiper et al.(2004) discovered hard X-ray component above $\sim$10 keV from some AXPs. Here, we present the Suzaku observation of the AXP 1E 1841-045 at the center of supernova remnant Kes 73. By this observation, we could analyze the spectrum from 0.4 to 50 keV at the same time. Then, we could test whether the spectral model above was valid or not in this wide energy range. We found that there were residual in the spectral fits when fit by the model of BB + POW. Fits were improved by adding another BB or POW component. But the meaning of each component became ambiguous in the phase-resolved spectroscopy. Alternatively we found that NPEX model fit well for both phase-averaged spectrum and phase-resolved spectra. In this case, the photon indices were constant during all phase, and spectral variation seemed to be very clear. This fact suggests somewhat fundamental meaning for the emission from magnetars., Comment: To appear in the proceedings of the "40 Years of Pulsars: Millisecond Pulsars, Magnetars and More" conference, held 12-17 August 2007, in Montreal QC (AIP, in press, eds: C. Bassa, Z. Wang, A. Cumming, V. Kaspi)

Published
2007
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13. Swift and Suzaku Observations of the X-Ray Afterglow from the GRB 060105

Author

Tashiro, M. S., Abe, K., Angelini, L., Barthelmy, S., Gehrels, N., Ishikawa, N., Kaluzienski, L. J., Kawai, N., Kelley, R. L., Kinugasa, K., Kodaira, H., Kohmura, T., Kubota, K., Maeda, Y., Maeno, S., Murakami, H., Murakami, T., Nakagawa, Y. E., Nakazawa, K., Nousek, J., Okuno, S., Onda, K., Reeves, J. N., Ricker, G., Sato, G., Sonoda, E., Suzuki, M., Takahashi, T., Tamagawa, T., Torii, K., Ueda, Y., Urata, Y., Yamaoka, K., Yamauchi, M., Yonetoku, D., Yoshida, A., and Yoshinari, S.

Subjects
Astrophysics
Abstract

Results are presented of early X-ray afterglow observations of GRB 060105 by Swift and Suzaku. The bright, long gamma-ray burst GRB 060105 triggered the Swift Burst Alert Telescope (BAT) at 06:49:28 on 5 January 2006. The Suzaku team commenced a pre-planned target of opportunity observation at 19 ks (5.3 hr) after the Swift trigger. Following the prompt emission and successive very steep decay, a shallow decay was observed from T_0+187 s to T_0+1287 s. After an observation gap during T_0 +(1.5-3) ks, an extremely early steep decay was observed in T_0+(4-30) ks. The lightcurve flattened again at T_0+30 ks, and another steep decay followed from T_0+50 ks to the end of observations. Both steep decays exhibited decay indices of 2.3 - 2.4. This very early break, if it is a jet break, is the earliest case among X-ray afterglow observations, suggesting a very narrow jet whose opening angle is well below 1 degree. The unique Suzaku/XIS data allow us to set very tight upper limits on line emission or absorption in this GRB. For the reported pseudo-redshift of z=4.0+/-1.3 the upper limit on the iron line equivalent width is 50 eV., Comment: 8 pages, 5 figures, Accepted for publication in PASJ Suzaku Special Issue (vol. 58)

Published
2006
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14. Cyclotron resonance energies at a low X-ray luminosity: A0535+262 observed with Suzaku

Author

Terada, Y., Mihara, T., Nakajima, M., Suzuki, M., Isobe, N., Makishima, K., Takahashi, H., Enoto, T., Kokubun, M., Kitaguchi, T., Naik, S., Dotani, T., Nagase, F., Tanaka, T., Watanabe, S., Kitamoto, S., Sudoh, K., Yoshida, A., Nakagawa, Y., Sugita, S., Kohmura, T., Kotani, T., Yonetoku, D., Angelini, L., Cottam, J., Mukai, K., Kelley, R., Soong, Y., Bautz, M., Kissel, S., and Doty, J.

Subjects
Astrophysics
Abstract

The binary X-ray pulsar A0535+262 was observed with the Suzaku X-ray observatory, on 2005 September 14 for a net exposure of 22 ksec. The source was in a declining phase of a minor outburst, exhibiting 3--50 keV luminosity of about $3.7 \times 10^{35}$ ergs s$^{-1}$ at an assumed distance of 2 kpc. In spite of the very low source intensity (about 30 mCrab at 20 keV), its electron cyclotron resonance was detected clearly with the Suzaku Hard X-ray Detector, in absorption at about 45 keV. The resonance energy is found to be essentially the same as those measured when the source is almost two orders of magnitude more luminous. These results are compared with the luminosity-dependent changes in the cyclotron resonance energy, observed from 4U 0115+63 and X 0331+53., Comment: 12 pages, 4 figures, accepted to ApJL, high resolution version is available from http://cosmic.riken.jp/terada/01work/paper/a0535_suzaku2006.pdf

Published
2006
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15. Nuclear collective tunneling transitions between Hartree states deformed in quadrupole symmetry

Author

Maruyama, M., Kohmura, T., and Hashimoto, Y.

Subjects
Nuclear Theory
Abstract

In a nucleus which has two Hartree states deformed in quadrupole symmetry, i.e., prolate state and oblate state, the nuclear residual interaction derived in the present theory beyond the Hartree approximation acts as the restoring force for the spherical symmetry of the nuclear system to be recovered so that the deformed nucleus makes collective tunneling transitions between prolate states and oblate states. We derive the Hamiltonian that is effective not only for the Hartree states but also for the collective tunneling transitions between the Hartree states. Solving the secular equation for the effective Hamiltonian on the basis states expressed in terms of SU(5) algebra, we analyze the nuclear collective tunneling transitions between a prolate state and an oblate state in the real-time description. The collective tunneling transitions are discussed to proceed through tri-axially asymmetric deformed states., Comment: LaTex, 12 pages, 7 postscript figures

Published
2005

16. Wide band X-ray Imager (WXI) and Soft Gamma-ray Detector (SGD) for the NeXT Mission

Author

Takahashi, T., Awaki, A., Dotani, T., Fukazawa, Y., Hayashida, K., Kamae, T., Kataoka, J., Kawai, N., Kitamoto, S., Kohmura, T., Kokubun, M., Koyama, K., Makishima, K., Matsumoto, H., Miyata, E., Murakami, T., Nakazawa, K., Momachi, M., Ozaki, M., Tajima, H., Tashiro, M., Tamagawa, T., Terada, Y., Tsunemi, H., Tsuru, T., Yamaoka, K., Yonetoku, D., and Yoshida, A.

Subjects
Astrophysics
Abstract

The NeXT mission has been proposed to study high-energy non-thermal phenomena in the universe. The high-energy response of the super mirror will enable us to perform the first sensitive imaging observations up to 80 keV. The focal plane detector, which combines a fully depleted X-ray CCD and a pixellated CdTe detector, will provide spectra and images in the wide energy range from 0.5 keV to 80 keV. In the soft gamma-ray band up to ~1 MeV, a narrow field-of-view Compton gamma-ray telescope utilizing several tens of layers of thin Si or CdTe detector will provide precise spectra with much higher sensitivity than present instruments. The continuum sensitivity will reach several times 10^(-8) photons/s/keV/cm^(2) in the hard X-ray region and a few times10^(-7) photons/s/keV/cm^(2) in the soft gamma-ray region., Comment: 12 pages, 13 figures, to be published in the SPIE proceedings 5488, typo corrected in sec.3

Published
2004
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17. The Earliest Optical Observations of GRB 030329

Author

Torii, K., Kato, T., Yamaoka, H., Kohmura, T., Okamoto, Y., Ohnishi, K., Kadota, K., Yoshida, S., Kinugasa, K., Kohama, M., Oribe, T., and Kawabata, T.

Subjects
Astrophysics
Abstract

We present the earliest optical imaging observations of GRB 030329 related to SN 2003dh. The burst was detected by the HETE-2 satellite at 2003 March 29, 11:37:14.67 UT. Our wide-field monitoring started 97 minutes before the trigger and the burst position was continuously observed. We found no precursor or contemporaneous flare brighter than $V=5.1$ ($V=5.5$) in 32 s (64 s) timescale between 10:00 and 13:00 UT. Follow-up time series photometries started at 12:51:39 UT (75 s after position notice through the GCN) and continued for more than 5 hours. The afterglow was $Rc= 12.35\pm0.07$ at $t=74$ min after burst. Its fading between 1.2 and 6.3 hours is well characterized by a single power-law of the form $f{\rm(mJy)} = (1.99\pm0.02{\rm (statistic)}\pm0.14{\rm (systematic)}) \times (t/1 {\rm day})^{-0.890\pm 0.006 {\rm (statistic)}\pm 0.010 {\rm (systematic)}}$ in $Rc$-band. No significant flux variation was detected and upper limits are derived as $(\Delta f/f)_{\rm RMS} = 3-5$% in minutes to hours timescales and $(\Delta f/f)_{\rm RMS} = 35-5$% in seconds to minutes timescales. Such a featureless lightcurve is explained by the smooth distribution of circumburst medium. Another explanation is that the optical band was above the synchrotron cooling frequency where emergent flux is insensitive to the ambient density contrasts. Extrapolation of the afterglow lightcurve to the burst epoch excludes the presence of an additional flare component at $t<10$ minutes as seen in GRB 990123 and GRB 021211., Comment: ApJL, in press

Published
2003
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18. Metal Rich Plasma at the Center Portion of the Cygnus Loop

Author

Miyata, Emi, Tsunemi, H., Kohmura, T., Suzuki, S., and Kumagai, S.

Subjects
Astrophysics
Abstract

We observed the center portion of the Cygnus Loop supernova remnant with the ASCA observatory. The X-ray spectrum of the center portion was significantly different from that obtained at the North-East (NE) limb. The emission lines from Si and S were quite strong while those of O and the continuum emission were similar to those obtained at the NE limb. Based on the spectral analysis, Si and S emission lines originated from a high-kTe and low ionization plasma whereas O and most of the continuum emission arose from a low-kTe and high ionization plasma. We suppose that Si and S emitting gas are present at the interior of the Loop while O lines and continuum emission mainly arise from the shell region. Therefore, we subtracted the spectrum of the NE limb from that of the center. Obtained abundances of Si, S, and Fe were 4 $\pm$ 1, 6 $\pm$ 2, and ${1.3}^{+0.6}_{-0.3}$ times higher than those of the cosmic abundances, respectively, and are $\sim$40 times richer than those obtained at the NE limb. These facts strongly support that some of the crude ejecta must be left at the center portion of the Cygnus Loop. The low abundance of Fe relative to Si and S suggests a type II SN with a massive progenitor star as the origin of the Cygnus Loop., Comment: Accepted for Publications of the Astronomical Society of Japan, 40 pages, 12 Postscript figures, uses PASJ95.sty, PASJadd.sty, and psbox.sty

Published
1998
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19. Spectroscopic performance improvement of SOI pixel detector for X-ray astronomy by introducing Double-SOI structure

Author

Takeda, A., primary, Mori, K., additional, Nishioka, Y., additional, Fukuda, K., additional, Yukumoto, M., additional, Hida, T., additional, Tsuru, T.G., additional, Tanaka, T., additional, Uchida, H., additional, Hayashi, H., additional, Harada, S., additional, Okuno, T., additional, Kayama, K., additional, Arai, Y., additional, Kurachi, I., additional, Kohmura, T., additional, Hagino, K., additional, Negishi, K., additional, Oono, K., additional, Yarita, K., additional, Matsumura, H., additional, Kawahito, S., additional, Kagawa, K., additional, Yasutomi, K., additional, Shrestha, S., additional, Nakanishi, S., additional, and Kamehama, H., additional

Published
2020
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21. Sub-pixel response of double-SOI pixel sensors for X-ray astronomy

Author

Hagino, K., primary, Negishi, K., additional, Oono, K., additional, Yarita, K., additional, Kohmura, T., additional, Tsuru, T.G., additional, Tanaka, T., additional, Harada, S., additional, Kayama, K., additional, Matsumura, H., additional, Mori, K., additional, Takeda, A., additional, Nishioka, Y., additional, Yukumoto, M., additional, Fukuda, K., additional, Hida, T., additional, Arai, Y., additional, Kurachi, I., additional, and Kishimoto, S., additional

Published
2019
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23. X-ray imaging spectrometers (XIS) of Astro-E2

Author

Matsumoto, H., Koyama, K., Tsuru, T.G., Nakajima, H., Yamaguchi, H., Tsunemi, H., Hayashida, K., Miyata, E., Torii, K., Namiki, M., Dotani, T., Ozaki, M., Murakami, H., Anabuki, N., Kitamoto, S., Awaki, H., Kohmura, T., Katayama, H., Bamba, A., Bautz, M.W., Doty, J.P., Ricker, G.R., Foster, R.F., Prigozhin, G.Y., Kissel, S.E., Burke, B.E., Pillsbury, A.D., and LaMarr, B.

Published
2005
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24. Atmospheric gas dynamics in the Perseus cluster observed with Hitomi*

Author

Aharonia, F., Aharonian, F., Akamatsu, H., Akimoto, F., Allen, S. W., Angelini, L., Audard, M., Awaki, H., Axelsson, M., Bamba, A., Bautz, M. W., Blandford, R., Brenneman, L. W., Brown, G. V., Bulbul, E., Cackett, E. M., Canning, R. E. A., Chernyakova, M., Chiao, M. P., Coppi, P. S., Costantini, E., Plaa, J., Vries, C. P., Den Herder, J. -W, Done, C., Dotani, T., Ebisawa, K., Eckart, M. E., Enoto, T., Ezoe, Y., Fabian, A. C., Ferrigno, C., Foster, A. R., Fujimoto, R., Fukazawa, Y., Furuzawa, A., Galeazzi, M., Gallo, L. C., Gandhi, P., Giustini, M., Goldwurm, A., Gu, L., Guainazzi, M., Haba, Y., Hagino, K., Hamaguchi, K., Harrus, I. M., Hatsukade, I., Hayashi, K., Hayashi, T., Hayashida, K., Hiraga, J. S., Hornschemeier, A., Hoshino, A., Hughes, J. P., Ichinohe, Y., Iizuka, R., Inoue, H., Inoue, S., Inoue, Y., Ishida, M., Ishikawa, K., Ishisaki, Y., Iwai, M., Kaastra, J., Kallman, T., Kamae, T., Kataoka, J., Katsuda, S., Kawai, N., Kelley, R. L., Kilbourne, C. A., Kitaguchi, T., Kitamoto, S., Kitayama, T., Kohmura, T., Kokubun, M., Koyama, K., Koyama, S., Kretschmar, P., Krimm, H. A., Kubota, A., Kunieda, H., Laurent, P., Lee, S. -H, Leutenegger, M. A., Limousin, O., Loewenstein, M., Long, K. S., Lumb, D., Madejski, G., Maeda, Y., Maier, D., Makishima, K., Markevitch, M., Matsumoto, H., Kyoko Matsushita, Mccammon, D., Mcnamara, B. R., Mehdipour, M., Miller, E. D., Miller, J. M., Mineshige, S., Mitsuda, K., Mitsuishi, I., Miyazawa, T., Mizuno, T., Mori, H., Mori, K., Mukai, K., Murakami, H., Mushotzky, R. F., Nakagawa, T., Nakajima, H., Nakamori, T., Nakashima, S., Nakazawa, K., Nobukawa, K. K., Nobukawa, M., Noda, H., Odaka, H., Ohashi, T., Ohno, M., Okajima, T., Ota, N., Ozaki, M., Paerels, F., Paltani, S., Petre, R., Pinto, C., Porter, F. S., Pottschmidt, K., Reynolds, C. S., Safi-Harb, S., Saito, S., Sakai, K., Sasaki, T., Sato, G., Sato, K., Sato, R., Sawada, M., Schartel, N., Serlemtsos, P. J., Seta, H., Shidatsu, M., Simionescu, A., Smith, R. K., Soong, Y., Stawarz, Ł., Sugawara, Y., Sugita, S., Szymkowiak, A., Tajima, H., Takahashi, H., Takahashi, T., Takeda, S., Takei, Y., Amagawa, T. T., Tamura, T., Tanaka, K., Tanaka, T., Tanaka, Y., Tanaka, Y. T., Tashiro, M. S., Tawara, Y., Terada, Y., Erashima, Y. T., Tombesi, F., Tomida, H., Tsuboi, Y., Tsujimoto, M., Tsunemi, H., Tsuru, T. G., Uchida, H., Uchiyama, H., Uchiyama, Y., Ueda, S., Ueda, Y., Uno, S., Urry, C. M., Ursino, E., Wang, Q. H. S., Watanabe, S., Werner, N., Wilkins, D. R., Williams, B. J., Yamada, S., Yamaguchi, H., Yamaoka, K., Yamasaki, N. Y., Yamauchi, M., Yamauchi, S., Yaqoob, T., Yatsu, Y., Yonetoku, D., Zhuravleva, I., Zoghbi, A., AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Hitomi, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), and Commissariat à l'énergie atomique et aux énergies alternatives ( CEA )

Subjects
galaxies: clusters: individual, galaxies: clusters: intracluster medium, Active galactic nucleus, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], individual (NGC 1275) [galaxies], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, galaxies: individual, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, clusters: individual (Perseus) [galaxies], 01 natural sciences, Intracluster medium, 0103 physical sciences, Emission spectrum, Brightest cluster galaxy, 010303 astronomy & astrophysics, STFC, Astrophysics::Galaxy Astrophysics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Settore FIS/05, 010308 nuclear & particles physics, Velocity gradient, RCUK, Velocity dispersion, Astronomy and Astrophysics, Redshift, ST/J003697/2, clusters: intracluster medium [galaxies], Space and Planetary Science, X-rays: galaxies: clusters, Electron temperature, galaxies: clusters [X-rays], ST/L00075X/1, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

著者人数: Hitomi Collaboration 197名（所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 堂谷, 忠靖; 海老沢, 研; 林, 克洋; 林, 佑; 飯塚, 亮; 井上, 芳幸; 石田, 学; 石川, 久美; 岩井, 将親; 国分, 紀秀; 小山, 志勇; 前田, 良知; 満田, 和久; 中川, 貴雄; 尾崎, 正伸; 佐藤, 悟郎; 佐藤, 理江; Simionescu, Aurora; 菅原, 泰晴; 高橋, 忠幸; 竹井, 洋; 田村, 隆幸; 田中, 靖郎; 冨田, 洋; 辻本, 匡弘; 上田, 周太朗; 渡辺, 伸; 山崎, 典子）, Number of authors: Hitomi Collaboration 197 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS): Dotani, Tadayasu; Ebisawa, Ken; Hayashi, Katsuhiro; Hayashi, Tasuku; Iizuka, Ryo; Inoue, Yoshiyuki; Ishida, Manabu; Ishikawa, Kumi; Iwai, Masachika; Kokubun, Motohide; Koyama, Shu; Maeda, Yoshitomo; Mitsuda, Kazuhisa; Nakagawa, Takao; Ozaki, Masanobu; Sato, Goro; Sato, Rie; Simionescu, Aurora; Sugawara, Yasuharu; Takahashi, Tadayuki; Takei, Yoh; Tamura, Takayuki; Tanaka, Yasuo; Tomida, Hiroshi; Tsujimoto, Masahiro; Ueda, Shutaro; Watanabe, Shin; Yamasaki, Noriko Y.), Accepted: 201710-31, 資料番号: SA1170334000

Published
2018

25. Atomic data and spectral modeling constraints from high-resolution X-ray observations of the Perseus cluster with Hitomi

Author

Hitomi, C, Aharonian, F, Akamatsu, H, Akimoto, F, Allen, Sw, Angelini, L, Audard, M, Awaki, H, Axelsson, M, Bamba, A, Bautz, Mw, Blandford, R, Brenneman, Lw, Brown, Gv, Bulbul, E, Cackett, Em, Chernyakova, M, Chiao, Mp, Coppi, Ps, Costantini, E, de Plaa, J, de Vries, Cp, den Herder, J, Done, C, Dotani, T, Ebisawa, K, Eckart, Me, Enoto, T, Ezoe, Y, Fabian, Ac, Ferrigno, C, Foster, Ar, Fujimoto, R, Fukazawa, Y, Furuzawa, A, Galeazzi, M, Gallo, Lc, Gandhi, P, Giustini, M, Goldwurm, A, Liyi, G, Guainazzi, M, Haba, Y, Hagino, K, Hamaguchi, K, Harrus, Im, Hatsukade, I, Hayashi, K, Hayashi, T, Hayashida, K, Hell, N, Hiraga, Js, Hornschemeier, A, Hoshino, A, Hughes, Jp, Ichinohe, Y, Iizuka, R, Inoue, H, Inoue, Y, Ishida, M, Ishikawa, K, Ishisaki, Y, Iwai, M, Kaastra, J, Kallman, T, Kamae, T, Kataoka, J, Katsuda, S, Kawai, N, Kelley, Rl, Kilbourne, Ca, Kitaguchi, T, Kitamoto, S, Kitayama, T, Kohmura, T, Kokubun, M, Koyama, K, Koyama, S, Kretschmar, P, Krimm, Ha, Kubota, A, Kunieda, H, Laurent, P, Lee, S, Leutenegger, Ma, Limousin, O, Loewenstein, M, Long, Ks, Lumb, D, Madejski, G, Maeda, Y, Maier, D, Makishima, K, Markevitch, M, Matsumoto, H, Matsushita, K, Mccammon, D, Mcnamara, Br, Mehdipour, M, Miller, Ed, Miller, Jm, Mineshige, S, Mitsuda, K, Mitsuishi, I, Miyazawa, T, Mizuno, T, Mori, H, Mori, K, Mukai, K, Murakami, H, Mushotzky, Rf, Nakagawa, T, Nakajima, H, Nakamori, T, Nakashima, S, Nakazawa, K, Nobukawa, Kk, Nobukawa, M, Noda, H, Odaka, H, Ohashi, T, Ohno, M, Okajima, T, Ota, N, Ozaki, M, Paerels, F, Paltani, S, Petre, R, Pinto, C, Porter, Fs, Pottschmidt, K, Reynolds, Cs, Safi-Harb, S, Saito, S, Sakai, K, Sasaki, T, Sato, G, Sato, K, Sato, R, Sawada, M, Schartel, N, Serlemtsos, Pj, Seta, H, Shidatsu, M, Simionescu, A, Smith, Rk, Soong, Y, Stawarz, Ł, Sugawara, Y, Sugita, S, Szymkowiak, A, Tajima, H, Takahashi, H, Takahashi, T, Takeda, S, Takei, Y, Tamagawa, T, Tamura, T, Tanaka, T, Tanaka, Y, Tanaka, Yt, Tashiro, Ms, Tawara, Y, Terada, Y, Terashima, Y, Tombesi, F, Tomida, H, Tsuboi, Y, Tsujimoto, M, Tsunemi, H, Tsuru, Tg, Uchida, H, Uchiyama, H, Uchiyama, Y, Ueda, S, Ueda, Y, Uno, S, Urry, Cm, Ursino, E, Watanabe, S, Werner, N, Wilkins, Dr, Williams, Bj, Yamada, S, Yamaguchi, H, Yamaoka, K, Yamasaki, Ny, Yamauchi, M, Yamauchi, S, Yaqoob, T, Yatsu, Y, Yonetoku, D, Zhuravleva, I, Zoghbi, A, Raassen, Ajj, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Hitomi, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
FOS: Physical sciences, Astrophysics, X-rays: general, 01 natural sciences, Measure (mathematics), X-ray, nickel, benchmark, iron, Settore FIS/05 - Astronomia e Astrofisica, general [X-rays], excited state, 0103 physical sciences, data analysis [methods], Calibration, Emission spectrum, Sensitivity (control systems), cluster, dielectric, 010306 general physics, 010303 astronomy & astrophysics, Collisional excitation, plasma, instrumentation: spectrographs, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Resolution (electron density), temperature, resolution, Astronomy and Astrophysics, Plasma, calibration, sensitivity, methods: data analysis, recombination, 13. Climate action, Space and Planetary Science, spectral, data management, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], statistical, spectrographs [instrumentation]
Abstract

著者人数: Hitomi Collaboration 194名（所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 堂谷, 忠靖; 海老沢, 研; 林, 克洋; 飯塚, 亮; 井上, 芳幸; 石田, 学; 石川, 久美; 岩井, 将親; 国分, 紀秀; 小山, 志勇; 前田, 良知; 満田, 和久; 中川, 貴雄; 尾崎, 正伸; 佐藤, 悟郎; 佐藤, 理江; Simionescu, Aurora; 菅原, 泰晴; 高橋, 忠幸; 竹井, 洋; 田村, 隆幸; 田中, 靖郎; 冨田, 洋; 辻本, 匡弘; 上田, 周太朗; 渡辺, 伸; 山崎, 典子）, Number of authors: Hitomi Collaboration 194 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS): Dotani, Tadayasu; Ebisawa, Ken; Hayashi, Katsuhiro; Iizuka, Ryo; Inoue, Yoshiyuki; Ishida, Manabu; Ishikawa, Kumi; Iwai, Masachika; Kokubun, Motohide; Koyama, Shu; Maeda, Yoshitomo; Mitsuda, Kazuhisa; Nakagawa, Takao; Ozaki, Masanobu; Sato, Goro; Sato, Rie; Simionescu, Aurora; Sugawara, Yasuharu; Takahashi, Tadayuki; Takei, Yoh; Tamura, Takayuki; Tanaka, Yasuo; Tomida, Hiroshi; Tsujimoto, Masahiro; Ueda, Shutaro; Watanabe, Shin; Yamasaki, Noriko Y.), Accepted: 2017-12-13, 資料番号: SA1170337000

Published
2018

26. Hitomi observations of the LMC SNR N 132 D: Highly redshifted X-ray emission from iron ejecta

Author

Aharonian, Hitomi, C, Felix, Akamatsu, H, Akimoto, F, Allen, Sw, Angelini, L, Audard, M, Awaki, H, Axelsson, M, Bamba, A, Bautz, Mw, Blandford, R, Brenneman, Lw, Brown, Gv, Bulbul, E, Cackett, Em, Chernyakova, M, Chiao, Mp, Coppi, Ps, Costantini, E, de Plaa, J, de Vries, Cp, den Herder, J, Done, C, Dotani, T, Ebisawa, K, Eckart, Me, Enoto, T, Ezoe, Y, Fabian, Ac, Ferrigno, C, Foster, Ar, Fujimoto, R, Fukazawa, Y, Furuzawa, A, Galeazzi, M, Gallo, Lc, Gandhi, P, Giustini, M, Goldwurm, A, Liyi, G, Guainazzi, M, Haba, Y, Hagino, K, Hamaguchi, K, Harrus, Im, Hatsukade, I, Hayashi, K, Hayashi, T, Hayashida, K, Hiraga, Js, Hornschemeier, A, Hoshino, A, Hughes, Jp, Ichinohe, Y, Iizuka, R, Inoue, H, Inoue, Y, Ishida, M, Ishikawa, K, Ishisaki, Y, Iwai, M, Kaastra, J, Kallman, T, Kamae, T, Kataoka, J, Katsuda, S, Kawai, N, Kelley, Rl, Kilbourne, Ca, Kitaguchi, T, Kitamoto, S, Kitayama, T, Kohmura, T, Kokubun, M, Koyama, K, Koyama, S, Kretschmar, P, Krimm, Ha, Kubota, A, Kunieda, H, Laurent, P, Lee, S, Leutenegger, Ma, Limousin, O, Loewenstein, M, Long, Ks, Lumb, D, Madejski, G, Maeda, Y, Maier, D, Makishima, K, Markevitch, M, Matsumoto, H, Matsushita, K, Mccammon, D, Mcnamara, Br, Mehdipour, M, Miller, Ed, Miller, Jm, Mineshige, S, Mitsuda, K, Mitsuishi, I, Miyazawa, T, Mizuno, T, Mori, H, Mori, K, Mukai, K, Murakami, H, Mushotzky, Rf, Nakagawa, T, Nakajima, H, Nakamori, T, Nakashima, S, Nakazawa, K, Nobukawa, Kk, Nobukawa, M, Noda, H, Odaka, H, Ohashi, T, Ohno, M, Okajima, T, Ota, N, Ozaki, M, Paerels, F, Paltani, S, Petre, R, Pinto, C, Porter, Fs, Pottschmidt, K, Reynolds, Cs, Safi-Harb, S, Saito, S, Sakai, K, Sasaki, T, Sato, G, Sato, K, Sato, R, Sato, T, Sawada, M, Schartel, N, Serlemtsos, Pj, Seta, H, Shidatsu, M, Simionescu, A, Smith, Rk, Soong, Y, Stawarz, Ł, Sugawara, Y, Sugita, S, Szymkowiak, A, Tajima, H, Takahashi, H, Takahashi, T, Takeda, S, Takei, Y, Tamagawa, T, Tamura, T, Tanaka, T, Tanaka, Y, Tanaka, Yt, Tashiro, Ms, Tawara, Y, Terada, Y, Terashima, Y, Tombesi, F, Tomida, H, Tsuboi, Y, Tsujimoto, M, Tsunemi, H, Tsuru, Tg, Uchida, H, Uchiyama, H, Uchiyama, Y, Ueda, S, Ueda, Y, Uno, S, Urry, Cm, Ursino, E, Watanabe, S, Werner, N, Wilkins, Dr, Williams, Bj, Yamada, S, Yamaguchi, H, Yamaoka, K, Yamasaki, Ny, Yamauchi, M, Yamauchi, S, Yaqoob, T, Yatsu, Y, Yonetoku, D, Zhuravleva, I, Zoghbi, A, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Hitomi, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], observational [methods], FOS: Physical sciences, Astrophysics, 01 natural sciences, individual objects (N 132 D) [ISM], Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Spectral resolution, 010306 general physics, Large Magellanic Cloud, Ejecta, Supernova remnant, 010303 astronomy & astrophysics, Line (formation), ISM: supernova remnants, instrumentation: spectrographs, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), supernova remnants [ISM], individual (N 132 D) [X-rays], Astronomy and Astrophysics, X-rays: individual (N 132 D), Redshift, Interstellar medium, Supernova, ISM: individual object (N 132 D), 13. Climate action, Space and Planetary Science, methods: observational, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], spectrographs [instrumentation]
Abstract

著者人数: Hitomi Collaboration 193名（所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 堂谷, 忠靖; 海老沢, 研; 林, 克洋; 飯塚, 亮; 井上, 芳幸; 石田, 学; 石川, 久美; 岩井, 将親; 国分, 紀秀; 小山, 志勇; 前田, 良知; 満田, 和久; 中川, 貴雄; 尾崎, 正伸; 佐藤, 悟郎; 佐藤, 理江; Simionescu, Aurora; 菅原, 泰晴; 高橋, 忠幸; 竹井, 洋; 田村, 隆幸; 田中, 靖郎; 冨田, 洋; 辻本, 匡弘; 上田, 周太朗; 渡辺, 伸; 山崎, 典子）, Number of authors: Hitomi Collaboration 193 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS): Dotani, Tadayasu; Ebisawa, Ken; Hayashi, Katsuhiro; Iizuka, Ryo; Inoue, Yoshiyuki; Ishida, Manabu; Ishikawa, Kumi; Iwai, Masachika; Kokubun, Motohide; Koyama, Shu; Maeda, Yoshitomo; Mitsuda, Kazuhisa; Nakagawa, Takao; Ozaki, Masanobu; Sato, Goro; Sato, Rie; Simionescu, Aurora; Sugawara, Yasuharu; Takahashi, Tadayuki; Takei, Yoh; Tamura, Takayuki; Tanaka, Yasuo; Tomida, Hiroshi; Tsujimoto, Masahiro; Ueda, Shutaro; Watanabe, Shin; Yamasaki, Noriko Y.), Masahiro; Ueda, Shutaro; Watanabe, Shin; Yamasaki, Noriko Y.), Accepted: 2017-12-06, 資料番号: SA1170341000

Published
2018

27. Hitomi X-ray studies of giant radio pulses from the Crab pulsar

Author

Aharonian, Hitomi, C, Felix, Akamatsu, H, Akimoto, F, Allen, Sw, Angelini, L, Audard, M, Awaki, H, Axelsson, M, Bamba, A, Bautz, Mw, Blandford, R, Brenneman, Lw, Brown, Gv, Bulbul, E, Cackett, Em, Chernyakova, M, Chiao, Mp, Coppi, Ps, Costantini, E, de Plaa, J, de Vries, Cp, den Herder, J, Done, C, Dotani, T, Ebisawa, K, Eckart, Me, Enoto, T, Ezoe, Y, Fabian, Ac, Ferrigno, C, Foster, Ar, Fujimoto, R, Fukazawa, Y, Furuzawa, A, Galeazzi, M, Gallo, Lc, Gandhi, P, Giustini, M, Goldwurm, A, Liyi, G, Guainazzi, M, Haba, Y, Hagino, K, Hamaguchi, K, Harrus, Im, Hatsukade, I, Hayashi, K, Hayashi, T, Hayashida, K, Hiraga, Js, Hornschemeier, A, Hoshino, A, Hughes, Jp, Ichinohe, Y, Iizuka, R, Inoue, H, Inoue, Y, Ishida, M, Ishikawa, K, Ishisaki, Y, Iwai, M, Kaastra, J, Kallman, T, Kamae, T, Kataoka, J, Katsuda, S, Kawai, N, Kelley, Rl, Kilbourne, Ca, Kitaguchi, T, Kitamoto, S, Kitayama, T, Kohmura, T, Kokubun, M, Koyama, K, Koyama, S, Kretschmar, P, Krimm, Ha, Kubota, A, Kunieda, H, Laurent, P, Lee, S, Leutenegger, Ma, Limousin, Oo, Loewenstein, M, Long, Ks, Lumb, D, Madejski, G, Maeda, Y, Maier, D, Makishima, K, Markevitch, M, Matsumoto, H, Matsushita, K, Mccammon, D, Mcnamara, Br, Mehdipour, M, Miller, Ed, Miller, Jm, Mineshige, S, Mitsuda, K, Mitsuishi, I, Miyazawa, T, Mizuno, T, Mori, H, Mori, K, Mukai, K, Murakami, H, Mushotzky, Rf, Nakagawa, T, Nakajima, H, Nakamori, T, Nakashima, S, Nakazawa, K, Nobukawa, Kk, Nobukawa, M, Noda, H, Odaka, H, Ohashi, T, Ohno, M, Okajima, T, Oshimizu, K, Ota, N, Ozaki, M, Paerels, F, Paltani, S, Petre, R, Pinto, C, Porter, Fs, Pottschmidt, K, Reynolds, Cs, Safi-Harb, S, Saito, S, Sakai, K, Sasaki, T, Sato, G, Sato, K, Sato, R, Sawada, M, Schartel, N, Serlemtsos, Pj, Seta, H, Shidatsu, M, Simionescu, A, Smith, Rk, Soong, Y, Stawarz, Ł, Sugawara, Y, Sugita, S, Szymkowiak, A, Tajima, H, Takahashi, H, Takahashi, T, Takeda, S, Takei, Y, Tamagawa, T, Tamura, T, Tanaka, T, Tanaka, Y, Tanaka, Yt, Tashiro, Ms, Tawara, Y, Terada, Y, Terashima, Y, Tombesi, F, Tomida, H, Tsuboi, Y, Tsujimoto, M, Tsunemi, H, Tsuru, Tg, Uchida, H, Uchiyama, H, Uchiyama, Y, Ueda, S, Ueda, Y, Uno, S, Urry, Cm, Ursino, E, Watanabe, S, Werner, N, Wilkins, Dr, Williams, Bj, Yamada, S, Yamaguchi, H, Yamaoka, K, Yamasaki, Ny, Yamauchi, M, Yamauchi, S, Yaqoob, T, Yatsu, Y, Yonetoku, D, Zhuravleva, I, Zoghbi, A, Terasawa, T, Sekido, M, Takefuji, K, Kawai, E, Misawa, H, Tsuchiya, F, Yamazaki, R, Kobayashi, E, Kisaka, S, Aoki, T, AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Hitomi, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Magnetosphere, X-rays: stars, Astrophysics, 01 natural sciences, Article, Radio observatory, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, pulsars: individual (B0531+21), 010306 general physics, 010303 astronomy & astrophysics, stars [radio continuum], stars [X-rays], High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Crab Pulsar, X-ray, Astronomy and Astrophysics, Pulse (physics), Space and Planetary Science, individual (B0531+21) [pulsars], Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], radio continuum: stars, Phase width
Abstract

著者人数: Hitomi Collaboration 203名（所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 堂谷, 忠靖; 海老沢, 研; 萩野, 浩一; 林, 克洋; 飯塚, 亮; 井上, 芳幸; 石田, 学; 石川, 久美; 岩井, 将親; 国分, 紀秀; 小山, 志勇; 前田, 良知; 満田, 和久; 中川, 貴雄; 尾崎, 正伸; 佐藤, 悟郎; 佐藤, 理江; Simionescu, Aurora; 菅原, 泰晴; 高橋, 忠幸; 竹井, 洋; 田村, 隆幸; 冨田, 洋; 辻本, 匡弘; 上田, 周太朗; 渡辺, 伸; 山崎, 典子）, Number of authors: Hitomi Collaboration 203 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS): Dotani, Tadayasu; Ebisawa, Ken; Hagino, Kouichi; Hayashi, Katsuhiro; Iizuka, Ryo; Inoue, Yoshiyuki; Ishida, Manabu; Ishikawa, Kumi; Iwai, Masachika; Kokubun, Motohide; Koyama, Shu; Maeda, Yoshitomo; Mitsuda, Kazuhisa; Nakagawa, Takao; Ozaki, Masanobu; Sato, Goro; Sato, Rie; Simionescu, Aurora; Sugawara, Yasuharu; Takahashi, Tadayuki; Takei, Yoh; Tamura, Takayuki; Tomida, Hiroshi; Tsujimoto, Masahiro; Ueda, Shutaro; Watanabe, Shin; Yamasaki, Noriko Y.), Masahiro; Ueda, Shutaro; Watanabe, Shin; Yamasaki, Noriko Y.), Accepted: 2017-07-27, 資料番号: SA1170340000

Published
2018

28. Subpixel response of SOI pixel sensor for X-ray astronomy with pinned depleted diode: first result from mesh experiment

Author

Kayama, K., primary, Tsuru, T. G., additional, Tanaka, T., additional, Uchida, H., additional, Harada, S., additional, Okuno, T., additional, Amano, Y., additional, Hiraga, J. S., additional, Yoshida, M., additional, Kamata, Y., additional, Sakuma, S., additional, Yuhi, D., additional, Urabe, Y., additional, Tsunemi, H., additional, Matsumura, H., additional, Kawahito, S., additional, Kagawa, K., additional, Yasutomi, K., additional, Shrestha, S., additional, Nakanishi, S., additional, Kamehama, H., additional, Arai, Y., additional, Kurachi, I., additional, Takeda, A., additional, Mori, K., additional, Nishioka, Y., additional, Fukuda, K., additional, Hida, T., additional, Yukumoto, M., additional, Kohmura, T., additional, Hagino, K., additional, Oono, K., additional, Negishi, K., additional, and Yarita, K., additional

Published
2019
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29. Radiation hardness of a p-channel notch CCD developed for the X-ray CCD camera onboard the XRISM satellite

Author

Kanemaru, Y., primary, Sato, J., additional, Mori, K., additional, Nakajima, H., additional, Nishioka, Y., additional, Takeda, A., additional, Hayashida, K., additional, Matsumoto, H., additional, Iwagaki, J., additional, Okazaki, K., additional, Asakura, K., additional, Yoneyama, T., additional, Uchida, H., additional, Okon, H., additional, Tanaka, T., additional, Tsuru, T.G., additional, Tomida, H., additional, Shimoi, T., additional, Kohmura, T., additional, Hagino, K., additional, Murakami, H., additional, Kobayashi, S.B., additional, Yamauchi, M., additional, Hatsukade, I., additional, Nobukawa, M., additional, Nobukawa, K.K., additional, Hiraga, J.S., additional, Uchiyama, H., additional, Yamaoka, K., additional, Ozaki, M., additional, Dotani, T., additional, Tsunemi, H., additional, and Hamano, T., additional

Published
2019
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31. Hitomi Constraints on the 3.5 keV Line in the Perseus Galaxy Cluster

Author

Aharonian, FA, Akamatsu, H, Akimoto, F, Allen, SW, Angelini, L, Arnaud, KA, Audard, M, Awaki, H, Axelsson, M, Bamba, A, Bautz, MW, Blandford, RD, Bulbul, E, Brenneman, LW, Brown, GV, Cackett, EM, Chernyakova, M, Chiao, MP, Coppi, P, Costantini, E, Plaa, JD, Herder, JWD, Done, C, Dotani, T, Ebisawa, K, Eckart, ME, Enoto, T, Ezoe, Y, Fabian, AC, Ferrigno, C, Foster, AR, Fujimoto, R, Fukazawa, Y, Furuzawa, A, Galeazzi, M, Gallo, LC, Gandhi, P, Giustini, M, Goldwurm, A, Gu, L, Guainazzi, M, Haba, Y, Hagino, K, Hamaguchi, K, Harrus, I, Hatsukade, I, Hayashi, K, Hayashi, T, Hayashida, K, Hiraga, J, Hornschemeier, AE, Hoshino, A, Hughes, JP, Ichinohe, Y, Iizuka, R, Inoue, H, Inoue, S, Inoue, Y, Ishibashi, K, Ishida, M, Ishikawa, K, Ishisaki, Y, Itoh, M, Iwai, M, Iyomoto, N, Kaastra, JS, Kallman, T, Kamae, T, Kara, E, Kataoka, J, Katsuda, S, Katsuta, J, Kawaharada, M, Kawai, N, Kelley, RL, Khangulyan, D, Kilbourne, CA, King, AL, Kitaguchi, T, Kitamoto, S, Kitayama, T, Kohmura, T, Kokubun, M, Koyama, S, Koyama, K, Kretschmar, P, Krimm, HA, Kubota, A, Kunieda, H, Laurent, P, Lebrun, F, Lee, SH, Leutenegger, MA, Limousin, O, Loewenstein, M, Long, KS, Lumb, DH, Madejski, GM, Maeda, Y, Maier, D, Fabian, Andrew [0000-0002-9378-4072], and Apollo - University of Cambridge Repository

Subjects
galaxies: clusters: intracluster medium, Astrophysics::High Energy Astrophysical Phenomena, X-rays: galaxies: clusters, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: clusters: individual (A426), Astrophysics::Galaxy Astrophysics, dark matter
Abstract

© 2017. The American Astronomical Society. All rights reserved. High-resolution X-ray spectroscopy with Hitomi was expected to resolve the origin of the faint unidentified E ≈ 3.5 keV emission line reported in several low-resolution studies of various massive systems, such as galaxies and clusters, including the Perseus cluster. We have analyzed the Hitomi first-light observation of the Perseus cluster. The emission line expected for Perseus based on the XMM-Newton signal from the large cluster sample under the dark matter decay scenario is too faint to be detectable in the Hitomi data. However, the previously reported 3.5 keV flux from Perseus was anomalously high compared to the sample-based prediction. We find no unidentified line at the reported high flux level. Taking into account the XMM measurement uncertainties for this region, the inconsistency with Hitomi is at a 99% significance for a broad dark matter line and at 99.7% for a narrow line from the gas. We do not find anomalously high fluxes of the nearby faint K line or the Ar satellite line that were proposed as explanations for the earlier 3.5 keV detections. We do find a hint of a broad excess near the energies of high-n transitions of S xvi (E ≃ 3.44 keV rest-frame) - a possible signature of charge exchange in the molecular nebula and another proposed explanation for the unidentified line. While its energy is consistent with XMM pn detections, it is unlikely to explain the MOS signal. A confirmation of this interesting feature has to wait for a more sensitive observation with a future calorimeter experiment.

Published
2017

34. The quiescent intracluster medium in the core of the Perseus cluster

Author

Aharonian, F, Akamatsu, H, Akimoto, F, Allen, SW, Anabuki, N, Angelini, L, Arnaud, K, Audard, M, Awaki, H, Axelsson, M, Bamba, A, Bautz, M, Blandford, R, Brenneman, L, Brown, GV, Bulbul, E, Cackett, E, Chernyakova, M, Chiao, M, Coppi, P, Costantini, E, De Plaa, J, Den Herder, JW, Done, C, Dotani, T, Ebisawa, K, Eckart, M, Enoto, T, Ezoe, Y, Fabian, AC, Ferrigno, C, Foster, A, Fujimoto, R, Fukazawa, Y, Furuzawa, A, Galeazzi, M, Gallo, L, Gandhi, P, Giustini, M, Goldwurm, A, Gu, L, Guainazzi, M, Haba, Y, Hagino, K, Hamaguchi, K, Harrus, I, Hatsukade, I, Hayashi, K, Hayashi, T, Hayashida, K, Hiraga, J, Hornschemeier, A, Hoshino, A, Hughes, J, Iizuka, R, Inoue, H, Inoue, Y, Ishibashi, K, Ishida, M, Ishikawa, K, Ishisaki, Y, Itoh, M, Iyomoto, N, Kaastra, J, Kallman, T, Kamae, T, Kara, E, Kataoka, J, Katsuda, S, Katsuta, J, Kawaharada, M, Kawai, N, Kelley, R, Khangulyan, D, Kilbourne, C, King, A, Kitaguchi, T, Kitamoto, S, Kitayama, T, Kohmura, T, Kokubun, M, Koyama, S, Koyama, K, Kretschmar, P, Krimm, H, Kubota, A, Kunieda, H, Laurent, P, Fabian, Andrew [0000-0002-9378-4072], and Apollo - University of Cambridge Repository

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Hitomi Collaboration, Astrophysics::Galaxy Astrophysics
Abstract

Clusters of galaxies are the most massive gravitationally bound objects in the Universe and are still forming. They are thus important probes of cosmological parameters and many astrophysical processes. However, knowledge of the dynamics of the pervasive hot gas, the mass of which is much larger than the combined mass of all the stars in the cluster, is lacking. Such knowledge would enable insights into the injection of mechanical energy by the central supermassive black hole and the use of hydrostatic equilibrium for determining cluster masses. X-rays from the core of the Perseus cluster are emitted by the 50-million-kelvin diffuse hot plasma filling its gravitational potential well. The active galactic nucleus of the central galaxy NGC 1275 is pumping jetted energy into the surrounding intracluster medium, creating buoyant bubbles filled with relativistic plasma. These bubbles probably induce motions in the intracluster medium and heat the inner gas, preventing runaway radiative cooling - a process known as active galactic nucleus feedback. Here we report X-ray observations of the core of the Perseus cluster, which reveal a remarkably quiescent atmosphere in which the gas has a line-of-sight velocity dispersion of 164 ± 10 kilometres per second in the region 30-60 kiloparsecs from the central nucleus. A gradient in the line-of-sight velocity of 150 ± 70 kilometres per second is found across the 60-kiloparsec image of the cluster core. Turbulent pressure support in the gas is four per cent of the thermodynamic pressure, with large-scale shear at most doubling this estimate. We infer that a total cluster mass determined from hydrostatic equilibrium in a central region would require little correction for turbulent pressure., Please visit the publisher's website for funding information.

Published
2016

38. Improvement of spectroscopic performance using a charge-sensitive amplifier circuit for an X-ray astronomical SOI pixel detector

Author

Takeda, A., primary, Tsuru, T.G., additional, Tanaka, T., additional, Uchida, H., additional, Matsumura, H., additional, Arai, Y., additional, Mori, K., additional, Nishioka, Y., additional, Takenaka, R., additional, Kohmura, T., additional, Nakashima, S., additional, Kawahito, S., additional, Kagawa, K., additional, Yasutomi, K., additional, Kamehama, H., additional, and Shrestha, S., additional

Published
2015
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39. Suzaku Discovery of Absorption Lines from the Black Hole Transient 4U1630-472

Author

Kubota, A., Dotani, T., Cottam, J., Kotani, Takayuki, Done, Chris, Ueda, Yoshihiro, Fabian, Andy C., Yasuda, T., Takahashi, Hirotaka, Fukazawa, Y., Yamaoka, Kazutaka, Makishima, K., Yamada, S., Kohmura, T., Angelini, L., Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Astronomie du LESIA, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience

Published
2007

40. Property of LCP-GEM in pure dimethyl ether at low pressure

Author

Takeuchi, Y, primary, Tamagawa, T, additional, Kitaguchi, T, additional, Yamada, S, additional, Iwakiri, W, additional, Asami, F, additional, Yoshikawa, A, additional, Kaneko, K, additional, Enoto, T, additional, Hayato, A, additional, Kohmura, T, additional, and team, the GEMS/XACT, additional

Published
2014
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42. Suzaku Observation of AXP 1E 1841-045 in SNR Kes 73

Author

Morii, M., primary, Kitamoto, S., additional, Shibazaki, N., additional, Takei, D., additional, Kawai, N., additional, Arimoto, M., additional, Ueno, M., additional, Terada, Y., additional, Kohmura, T., additional, Yamauchi, S., additional, Bassa, C., additional, Wang, Z., additional, Cumming, A., additional, and Kaspi, V. M., additional

Published
2008
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43. In-flight status of the X-ray observatory Suzaku

Author

Dotani, T., primary, Mitsuda, K., additional, Bautz, M., additional, Inoue, H., additional, Kelley, R. L., additional, Koyama, K., additional, Kunieda, H., additional, Makishima, K., additional, Ogawara, Y., additional, Petre, R., additional, Takahashi, T., additional, Tsunemi, H., additional, White, N. E., additional, Anabuki, N., additional, Angelini, L., additional, Arnaud, K., additional, Awaki, H., additional, Bamba, A., additional, Boyce, K., additional, Brown, G. V., additional, Chan, K.-W., additional, Cottam, J., additional, Doty, J., additional, Ebisawa, K., additional, Ezoe, Y., additional, Fabian, A. C., additional, Figueroa, E., additional, Fujimoto, R., additional, Fukazawa, Y., additional, Furusho, T., additional, Furuzawa, A., additional, Gendreau, K., additional, Griffiths, R. E., additional, Haba, Y., additional, Hamaguchi, K., additional, Harrus, I., additional, Hasinger, G., additional, Hatsukade, I., additional, Hayashida, K., additional, Henry, P. J., additional, Hiraga, J. S., additional, Holt, S. S., additional, Hornschemeier, A., additional, Hughes, J. P., additional, Hwang, U., additional, Ishida, M., additional, Ishisaki, Y., additional, Isobe, N., additional, Itoh, M., additional, Iyomoto, N., additional, Kahn, S. M., additional, Kamae, T., additional, Katagiri, H., additional, Kataoka, J., additional, Katayama, H., additional, Kawai, N., additional, Kawaharada, M., additional, Kilbourne, C., additional, Kinugasa, K., additional, Kissel, S., additional, Kitamoto, S., additional, Kohama, M., additional, Kohmura, T., additional, Kokubun, M., additional, Kotani, T., additional, Kotoku, J., additional, Kubota, A., additional, Madejski, G. M., additional, Maeda, Y., additional, Makino, F., additional, Markowitz, A., additional, Matsumoto, C., additional, Matsumoto, H., additional, Matsuoka, M., additional, Matsushita, K., additional, McCammon, D., additional, Mihara, T., additional, Misaki, K., additional, Miyata, E., additional, Mizuno, T., additional, Mori, K., additional, Mori, H., additional, Morii, M., additional, Moseley, H., additional, Mukai, K., additional, Murakami, H., additional, Murakami, T., additional, Mushotzky, R., additional, Nagase, F., additional, Namiki, M., additional, Negoro, H., additional, Nakazawa, K., additional, Nousek, J. A., additional, Okajima, T., additional, Ogasaka, Y., additional, Ohashi, T., additional, Oshima, T., additional, Ota, N., additional, Ozaki, M., additional, Ozawa, H., additional, Parmar, A. N., additional, Pence, W. D., additional, Porter, F. Scott, additional, Reeves, J. N., additional, Ricker, G. R., additional, Sakurai, I., additional, Sanders, W. T., additional, Senda, A., additional, Serlemitsos, P., additional, Shibata, R., additional, Shinozaki, K., additional, Soong, Y., additional, Smith, R., additional, Suzuki, M., additional, Szymkowiak, A. E., additional, Takahashi, H., additional, Takei, Y., additional, Tamagawa, T., additional, Tamura, K., additional, Tamura, T., additional, Tanaka, Y., additional, Tashiro, M., additional, Tawara, Y., additional, Terada, Y., additional, Terashima, Y., additional, Tomida, H., additional, Torii, K., additional, Tsuboi, Y., additional, Tsujimoto, Y., additional, Tsuru, T., additional, Turner, M. J. L., additional, Uchiyama, Y., additional, Ueda, Y., additional, Ueno, S., additional, Ueno, M., additional, Uno, S., additional, Urata, Y., additional, Watanabe, S., additional, Yamamoto, N., additional, Yamaoka, K., additional, Yamasaki, N. Y., additional, Yamashita, K., additional, Yamauchi, M., additional, Yamauchi, S., additional, Yaqoob, T., additional, Yonetoku, D., additional, and Yoshida, A., additional

Published
2007
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44. Suzaku observations of cyclotron resonances in binary X-ray pulsars

Author

Terada, Y., primary, Mihara, T., additional, Nagase, F., additional, Angelini, L., additional, Dotani, T., additional, Enoto, T., additional, Kitamoto, S., additional, Kohmura, T., additional, Kokubun, M., additional, Kotani, T., additional, Makishima, K., additional, Naik, S., additional, Nakajima, M., additional, Sugita, S., additional, Sudoh, K., additional, Suzuki, M., additional, Takahashi, H., additional, Yonetoku, D., additional, and Yoshida, A., additional

Published
2007
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45. Strategy of the Suzaku gamma-ray burst observations

Author

Tashiro, M.S., primary, Abe, K., additional, Angelini, L., additional, Endo, Y., additional, Enoto, T., additional, Fukazawa, Y., additional, Hong, S., additional, Ishikawa, N., additional, Kaluzienski, L.J., additional, Kawai, N., additional, Kelley, R.L., additional, Kinugasa, K., additional, Kodaira, H., additional, Kohmura, T., additional, Kokubun, M., additional, Kubota, K., additional, Maeno, S., additional, Makishima, K., additional, Miyawaki, R., additional, Murakami, T., additional, Nakagawa, Y.E., additional, Nakazawa, K., additional, Nousek, J.A., additional, Ohno, M., additional, Okuno, S., additional, Onda, K., additional, Reeves, J.N., additional, Ricker, G., additional, Sato, G., additional, Sonoda, E., additional, Sugita, S., additional, Suzuki, M., additional, Takahashi, T., additional, Tamagawa, T., additional, Terada, Y., additional, Torii, K., additional, Ueda, Y., additional, Urata, Y., additional, Yamaoka, K., additional, Yamauchi, M., additional, Yoshida, A., additional, Yoshinari, S., additional, and Yonetoku, D., additional

Published
2007
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46. Cyclotron Resonance Energies at a Low X-Ray Luminosity: A0535+262 Observed with Suzaku

Author

Terada, Y., primary, Mihara, T., additional, Nakajima, M., additional, Suzuki, M., additional, Isobe, N., additional, Makishima, K., additional, Takahashi, H., additional, Enoto, T., additional, Kokubun, M., additional, Kitaguchi, T., additional, Naik, S., additional, Dotani, T., additional, Nagase, F., additional, Tanaka, T., additional, Watanabe, S., additional, Kitamoto, S., additional, Sudoh, K., additional, Yoshida, A., additional, Nakagawa, Y., additional, Sugita, S., additional, Kohmura, T., additional, Kotani, T., additional, Yonetoku, D., additional, Angelini, L., additional, Cottam, J., additional, Mukai, K., additional, Kelley, R., additional, Soong, Y., additional, Bautz, M., additional, Kissel, S., additional, and Doty, J., additional

Published
2006
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47. The Earliest Optical Observations of GRB 030329

Author

Torii, K., primary, Kato, T., additional, Yamaoka, H., additional, Kohmura, T., additional, Okamoto, Y., additional, Ohnishi, K., additional, Kadota, K., additional, Yoshida, S., additional, Kinugasa, K., additional, Kohama, M., additional, Oribe, T., additional, and Kawabata, T., additional

Published
2003
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