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645 results on '"Iizuka, R."'

1. Inorbit Performance of the Hard X-ray Telescope (HXT) on board the Hitomi (ASTRO-H) satellite

Author

Matsumoto, H., Awaki, H., Ishida, M., Furuzawa, A., Yamauchi, S., Maeda, Y., Mitsuishi, I., Haba, Y., Hayashi, T., Iizuka, R., Ishibashi, K., Itoh, M., Kunieda, H., Miyazawa, T., Mori, H., Okajima, T., Sugita, S., Tamura., K., and Tawara, Y.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Hitomi (ASTRO-H) carries two Hard X-ray Telescopes (HXTs) that can focus X-rays up to 80 keV. Combined with the Hard X-ray Imagers (HXIs) that detect the focused X-rays, imaging spectroscopy in the high-energy band from 5 keV to 80 keV is made possible. We studied characteristics of HXTs after the launch such as the encircled energy function (EEF) and the effective area using the data of a Crab observation. The half power diameters (HPDs) in the 5--80 keV band evaluated from the EEFs are 1.59 arcmin for HXT-1 and 1.65 arcmin for HXT-2. Those are consistent with the HPDs measured with ground experiments when uncertainties are taken into account. We can conclude that there is no significant change in the characteristics of the HXTs before and after the launch. The off-axis angle of the aim point from the optical axis is evaluated to be less than 0.5 arcmin for both HXT-1 and HXT-2. The best-fit parameters for the Crab spectrum obtained with the HXT-HXI system are consistent with the canonical values., Comment: 13 pages, 5 figures; the acknowledgment was modified

Published
2018
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2. 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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3. ASTRO-H White Paper - High Resolution Spectroscopy of Interstellar and Circumgalactic Gas in the Milky Way and Other Galaxies

Author

Paerels, F., Yamasaki, N., Anabuki, N., Costantini, E., de Vries, C., Fujimoto, R., Hornschemeier, A., Iizuka, R., Kilbourne, C., Konami, S., LaMassa, S., Loewenstein, M., McCammon, D., Matsushita, K., McNamara, B., Mitsuishi, I., Nagino, R., Nakagawa, T., Porter, S., Sakai, K., Smith, R. K., Takei, Y., Tsuru, T., Uchiyama, H., Yamaguchi, H., and Yamauchi, S.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We describe the potential of high resolution imaging spectroscopy with the SXS on ASTRO-H to advance our understanding of the interstellar- and circumgalactic media of our own Galaxy, and other galaxies. Topics to be addressed range from absorption spectroscopy of dust in the Galactic interstellar medium, to observations to constrain the total mass-, metal-, and energy flow out of starburst galaxies., Comment: 21 pages, 13 figures, ASTRO-H White Paper

Published
2014

4. Gas bulk motion in the Perseus cluster measured with SUZAKU

Author

Tamura, Takayuki, Yamasaki, N., Iizuka, R., Fukazawa, Y., Hayashida, K., Ueda, S., Matsushita, K., Sato, K., Nakazawa, K., Ota, N., and Takizawa, M.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the results from Suzaku observations of the Perseus galaxy cluster, which is relatively close, the brightest in the X-ray sky and a relaxed object with a cool core. A number of exposures of central regions and offset pointing with the X-ray Imaging Spectrometer cover a region within radii of 20'-30'. The central data are used to evaluate the instrumental energy-scale calibration with accuracy confirmed to within around 300 km/s, by the spatial and temporal variation of the instruments. These deep and well-calibrated data are used to measure X-ray redshifts of the intracluster medium. A hint of gas bulk motion, with radial velocity of about -(150-300) km/s, relative to the main system was found at 2-4 arcmin (45-90kpc) west of the cluster center, where an X-ray excess and a cold front were found previously. No other velocity structure was discovered. Over spatial scales of 50-100kpc and within 200kpc radii of the center, the gas-radial-velocity variation is below 300 km/s, while over scales of 400 kpc within 600 kpc radii, the variation is below 600 km/s. These X-ray redshift distributions are compared spatially with those of optical member galaxies for the first time in galaxy clusters. Based on X-ray line widths gas turbulent velocities within these regions are also constrained within 1000-3000 km/s. These results of gas dynamics in the core and larger scales in association with cluster merger activities are discussed and future potential of high-energy resolution spectroscopy with ASTRO-H is considered., Comment: Accepted to ApJ

Published
2013
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5. X-ray Spectroscopy of the Core of the Perseus Cluster with Suzaku: Elemental Abundances in the Intracluster Medium

Author

Tamura, Takayuki, Maeda, Y., Mitsuda, K., Fabian, A. C., Sanders, J. S., Furuzawa, A., Hughes, J. P., Iizuka, R., Matsushita, K., and Tamagawa, T.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The results from Suzaku observations of the central region of the Perseus cluster are presented. Deep exposures with the X-ray Imaging Spectrometer provide high quality X-ray spectra from the intracluster medium. X-ray lines from helium-like Cr and Mn have been detected significantly for the first time in clusters. In addition, elemental abundances of Ne, Mg, Si, S, Ar, Ca, Fe, and Ni are accurately measured within 10' (or 220 kpc) from the cluster center. The relative abundance ratios are found to be within a range of 0.8-1.5 times the solar value. These abundance ratios are compared with previous measurements, those in extremely metal-poor stars in the Galaxy, and theoretical models., Comment: 10 pages, 3 figures, accepted for ApJL

Published
2009
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6. Observation of the first gravitational microlensing event in a sparse stellar field : the Tago event

Author

Fukui, A., Abe, F., Ayani, K., Fujii, M., Iizuka, R., Itow, Y., Kabumoto, K., Kamiya, K., Kawabata, T., Kawanomoto, S., Kinugasa, K., Koff, R. A., Krajci, T., Naito, H., Nogami, D., Narusawa, S., Ohishi, N., Ohnishi, K., Sumi, T., and Tsumuraya, F.

Subjects
Astrophysics
Abstract

We report the observation of the first gravitational microlensing event in a sparse stellar field, involving the brightest (V=11.4 mag) andclosest (~ 1 kpc) source star to date. This event was discovered by an amateurastronomer, A. Tago, on 2006 October 31 as a transient brightening, by ~4.5 mag during a ~15 day period, of a normal A-type star (GSC 3656-1328) in the Cassiopeia constellation. Analysis of both spectroscopic observations and the light curve indicates that this event was caused by gravitational microlensing rather than an intrinsically variable star. Discovery of this single event over a 30 year period is roughly consistent with the expected microlensing rate for the whole sky down to V = 12 mag stars. However, the probability for finding events with such a high magnification (~ 50) is much smaller, by a factor ~1/50, which implies that the true event rate may be higher than expected. This discovery indicates the potential of all sky variability surveys, employing frequent sampling by telescopes with small apertures and wide fields of view, for finding such rare transient events, and using the observations to explore galactic disk structure and search for exo-planets., Comment: 13 pages, 2 tables, 3 figures, accepted by ApJ

Published
2007
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7. Monte-Carlo Simulator and Ancillary Response Generator of Suzaku XRT/XIS System for Spatially Extended Source Analysis

Author

Ishisaki, Y., Maeda, Y., Fujimoto, R., Ozaki, M., Ebisawa, K., Takahashi, T., Ueda, Y., Ogasaka, Y., Ptak, A., Mukai, K., Hamaguchi, K., Hirayama, M., Kotani, T., Kubo, H., Shibata, R., Ebara, M., Furuzawa, A., Iizuka, R., Inoue, H., Mori, H., Okada, S., Yokoyama, Y., Matsumoto, H., Nakajima, H., Yamaguchi, H., Anabuki, N., Tawa, N., Nagai, M., Katsuda, S., Hayashida, K., Bamba, A., Miller, E. D., Sato, K., and Yamasaki, N. Y.

Subjects
Astrophysics
Abstract

We have developed a framework for the Monte-Carlo simulation of the X-Ray Telescopes (XRT) and the X-ray Imaging Spectrometers (XIS) onboard Suzaku, mainly for the scientific analysis of spatially and spectroscopically complex celestial sources. A photon-by-photon instrumental simulator is built on the ANL platform, which has been successfully used in ASCA data analysis. The simulator has a modular structure, in which the XRT simulation is based on a ray-tracing library, while the XIS simulation utilizes a spectral "Redistribution Matrix File" (RMF), generated separately by other tools. Instrumental characteristics and calibration results, e.g., XRT geometry, reflectivity, mutual alignments, thermal shield transmission, build-up of the contamination on the XIS optical blocking filters (OBF), are incorporated as completely as possible. Most of this information is available in the form of the FITS (Flexible Image Transport System) files in the standard calibration database (CALDB). This simulator can also be utilized to generate an "Ancillary Response File" (ARF), which describes the XRT response and the amount of OBF contamination. The ARF is dependent on the spatial distribution of the celestial target and the photon accumulation region on the detector, as well as observing conditions such as the observation date and satellite attitude. We describe principles of the simulator and the ARF generator, and demonstrate their performance in comparison with in-flight data., Comment: 19 pages with 8 figures, accepted for publication in PASJ Vol 58, Suzaku special issue

Published
2006
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8. Resolve Instrument on X-ray Astronomy Recovery Mission (XARM)

Author

Ishisaki, Y., Ezoe, Y., Yamada, S., Ichinohe, Y., Fujimoto, R., Takei, Y., Yasuda, S., Ishida, M., Yamasaki, N. Y., Maeda, Y., Tsujimoto, M., Iizuka, R., Koyama, S., Noda, H., Tamagawa, T., Sawada, M., Sato, K., Kitamoto, S., Hoshino, A., Brown, G. V., Eckart, M. E., Hayashi, T., Kelley, R. L., Kilbourne, C. A., Leutenegger, M. A., Mori, H., Okajima, T., Porter, F. S., Soong, Y., McCammon, D., Szymkowiak, A. E., and The XARM Resolve Team

Published
2018
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10. Ray-Tracing Simulation and In-Orbit Performance of the ASTRO-H Hard X-Ray Telescope (HXT)

Author

Matsumoto, H, Awaki, H, Furuzawa, A, Ishida, M, Kunieda, H, Haba, Y, Hayashi, T, Iizuka, R, Ishibashi, K, Itoh, M, Kosaka, T, Maeda, Y, Mitsuishi, I, Miyazawa, T, Mori, H, Nagano, H, Namba, Y, Ogasaka, Y, Ogi, K, Okajima, T, Sugita, S, Suzuki, Y, Tamura, K, Tawara, Y, Uesugi, K, and Yamauchi, S

Subjects
Astrophysics
Abstract

A ray-trace simulation code for the Hard X-ray Telescope (HXT) on board the Hitomi (ASTRO-H) satellite is beingdeveloped. The half power diameter and effective area simulated based on the code are consistent with groundmeasurements within 10%. The HXT observed the pulsar wind nebula G21.5-0.9 for 105 ksec. We confirmed that theencircled energy function and the half power diameter obtained from the data are consistent with the ground measurements.

Published
2016
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13. Gametes- and Embryo-Oviduct Interactions

Author

Suzuki, S., Oshiba, Y., Endo, Y., Komatsu, S., Kitai, H., Omura, S., Ohba, M., Ueno, M., Iizuka, R., Mashiach, Shlomo, editor, Ben-Rafael, Zion, editor, Laufer, Neri, editor, and Schenker, Joseph G., editor

Published
1990
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17. 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

18. 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

19. 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

20. 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

22. 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

23. Possible Risks and Protective Factors of Upper Respiratory Tract Infections in Healthy Japanese Office Workers

Author

Sato T, Miyazaki K, Iizuka R, and Shida K

Subjects
0301 basic medicine, Gerontology, Saliva, medicine.medical_specialty, Respiratory tract infections, business.industry, Incidence (epidemiology), Common cold, medicine.disease, Omics, Office workers, 03 medical and health sciences, 030104 developmental biology, 0302 clinical medicine, Internal medicine, Epidemiology, medicine, Granulysin, business, 030215 immunology
Abstract

Objective: In order to determine the risks and protective factors of upper respiratory tract infections (URTIs) in healthy office workers, we conducted a preliminary epidemiological survey and analysis of saliva parameter levels. Methods: One hundred and forty-six (98 men, 48 women; aged 20-59 years) healthy, full-time office workers in Tokyo and its suburbs participated in a questionnaire survey on lifestyle habits and daily physical condition, including symptoms of URTIs, from October 2012 to March 2013. Salivary parameters (secretory IgA, beta-defensin 2, LL-37, granulysin, lysozyme, cortisol) levels were also measured to analyze the correlation to URTI incidence and lifestyle habits. Results: Both the incidence rate and frequency of URTIs per person during the investigation period were highest among participants in their 50s and lowest among participants in their 30s. Participants who lived with their family showed higher URTI incidence than those who lived alone, while those with exercise habits showed lower URTI incidence. Higher saliva cortisol levels significantly correlated with high URTI incidence, while higher salivary granulysin levels significantly correlated with low URTI incidence. Conclusions: The risk factors of URTI incidence among healthy, full-time office workers include not only aging, but also living with family and higher salivary cortisol levels, and the protective factors are exercise habits and higher salivary granulysin levels.

Published
2017

29. 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

31. Large X-ray flares on stars detected with MAXI/GSC: A universal correlation between the duration of a flare and its X-ray luminosity

Author

Tsuboi, Y, Yamazaki, K, Sugawara, Y, Kawagoe, A, Kaneto, S, Iizuka, R, Matsumura, T, Nakahira, S, Higa, M, Matsuoka, M, Sugizaki, M, Ueda, Y, Kawai, Nobuyuki, Morii, M, Suzuki, Motoko, Mihara, T, Tomida, H, Ueno, S, Negoro, H, Daikyuji, A, Ebisawa, K, Eguchi, S, Hiroi, K, Ishikawa, M, Isobe, N, Kawasaki, K, Kimura, M, Kitayama, H, Kohama, M, kotani, tarou, Nakagawa, Y.~E., Nakajima, M, Ozawa, H, Shidatsu, M, Sootome, T, sugimori, kousuke, Suwa, F, Tsunemi, H, Usui, Ryuichi, Yamamoto, T, Yamaoka, K, and Yoshida, A

Subjects
FOS: Physical sciences, Astrophysics, 01 natural sciences, law.invention, Luminosity, law, stars: rotation, 0103 physical sciences, stars: activity, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, stars: late-type, X-ray, Radiant energy, Astronomy and Astrophysics, stars: variables: general, Stars, Orders of magnitude (time), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, stars: flare, Astrophysics - High Energy Astrophysical Phenomena, Rapid rotation, Flare
Abstract

著者人数: 42名, Accepted: 2016-07-29, 資料番号: SA1160182000

Published
2016

47. GAS BULK MOTION IN THE PERSEUS CLUSTER MEASURED WITHSuzaku

Author

Tamura, T., primary, Yamasaki, N. Y., additional, Iizuka, R., additional, Fukazawa, Y., additional, Hayashida, K., additional, Ueda, S., additional, Matsushita, K., additional, Sato, K., additional, Nakazawa, K., additional, Ota, N., additional, and Takizawa, M., additional

Published
2014
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