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169 results on '"Shigeo Yamauchi"'

1. Detection of polarized gamma-ray emission from the Crab nebula with the Hitomi Soft Gamma-ray Detector

Author

Felix Aharonian, Hiroki Akamatsu, Fumie Akimoto, Steven W Allen, Lorella Angelini, Marc Audard, Hisamitsu Awaki, Magnus Axelsson, Aya Bamba, Marshall W Bautz, Roger Blandford, Laura W Brenneman, Gregory V Brown, Esra Bulbul, Edward M Cackett, Maria Chernyakova, Meng P Chiao, Paolo S Coppi, Elisa Costantini, Jelle de Plaa, Cor P de Vries, Jan-Willem den Herder, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E Eckart, Teruaki Enoto, Yuichiro Ezoe, Andrew C Fabian, Carlo Ferrigno, Adam R Foster, Ryuichi Fujimoto, Yasushi Fukazawa, Akihiro Furuzawa, Massimiliano Galeazzi, Luigi C Gallo, Poshak Gandhi, Margherita Giustini, Andrea Goldwurm, Liyi Gu, Matteo Guainazzi, Yoshito Haba, Kouichi Hagino, Kenji Hamaguchi, Ilana M Harrus, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Kiyoshi Hayashida, Junko S Hiraga, Ann Hornschemeier, Akio Hoshino, John P Hughes, Yuto Ichinohe, Ryo Iizuka, Hajime Inoue, Yoshiyuki Inoue, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Masachika Iwai, Jelle Kaastra, Tim Kallman, Tsuneyoshi Kamae, Jun Kataoka, Satoru Katsuda, Nobuyuki Kawai, Richard L Kelley, Caroline A Kilbourne, Takao Kitaguchi, Shunji Kitamoto, Tetsu Kitayama, Takayoshi Kohmura, Motohide Kokubun, Katsuji Koyama, Shu Koyama, Peter Kretschmar, Hans A Krimm, Aya Kubota, Hideyo Kunieda, Philippe Laurent, Shiu-Hang Lee, Maurice A Leutenegger, Olivier Limousin, Michael Loewenstein, Knox S Long, David Lumb, Greg Madejski, Yoshitomo Maeda, Daniel Maier, Kazuo Makishima, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian R McNamara, Missagh Mehdipour, Eric D Miller, Jon M Miller, Shin Mineshige, Kazuhisa Mitsuda, Ikuyuki Mitsuishi, Takuya Miyazawa, Tsunefumi Mizuno, Hideyuki Mori, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard F Mushotzky, Takao Nakagawa, Hiroshi Nakajima, Takeshi Nakamori, Shinya Nakashima, Kazuhiro Nakazawa, Kumiko K Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Takaya Ohashi, Masanori Ohno, Takashi Okajima, Naomi Ota, Masanobu Ozaki, Frits Paerels, Stéphane Paltani, Robert Petre, Ciro Pinto, Frederick S Porter, Katja Pottschmidt, Christopher S Reynolds, Samar Safi-Harb, Shinya Saito, Kazuhiro Sakai, Toru Sasaki, Goro Sato, Kosuke Sato, Rie Sato, Makoto Sawada, Norbert Schartel, Peter J Serlemtsos, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall K Smith, Yang Soong, Łukasz Stawarz, Yasuharu Sugawara, Satoshi Sugita, Andrew Szymkowiak, Hiroyasu Tajima, Hiromitsu Takahashi, Tadayuki Takahashi, Shin’ichiro Takeda, Yoh Takei, Toru Tamagawa, Takayuki Tamura, Takaaki Tanaka, Yasuo Tanaka, Yasuyuki T Tanaka, Makoto S Tashiro, Yuzuru Tawara, Yukikatsu Terada, Yuichi Terashima, Francesco Tombesi, Hiroshi Tomida, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Go Tsuru, Hiroyuki Uchida, Hideki Uchiyama, Yasunobu Uchiyama, Shutaro Ueda, Yoshihiro Ueda, Shin’ichiro Uno, C Megan Urry, Eugenio Ursino, Shin Watanabe, Norbert Werner, Dan R Wilkins, Brian J Williams, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Y Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Yoichi Yatsu, Daisuke Yonetoku, Irina Zhuravleva, Abderahmen Zoghbi, and Yuusuke Uchida

Published
2018
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2. Atomic data and spectral modeling constraints from high-resolution X-ray observations of the Perseus cluster with Hitomi

Author

Hitomi Collaboration, Felix Aharonian, Hiroki Akamatsu, Fumie Akimoto, Steven W Allen, Lorella Angelini, Marc Audard, Hisamitsu Awaki, Magnus Axelsson, Aya Bamba, Marshall W Bautz, Roger Blandford, Laura W Brenneman, Gregory V Brown, Esra Bulbul, Edward M Cackett, Maria Chernyakova, Meng P Chiao, Paolo S Coppi, Elisa Costantini, Jelle de Plaa, Cor P de Vries, Jan-Willem den Herder, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E Eckart, Teruaki Enoto, Yuichiro Ezoe, Andrew C Fabian, Carlo Ferrigno, Adam R Foster, Ryuichi Fujimoto, Yasushi Fukazawa, Akihiro Furuzawa, Massimiliano Galeazzi, Luigi C Gallo, Poshak Gandhi, Margherita Giustini, Andrea Goldwurm, Liyi Gu, Matteo Guainazzi, Yoshito Haba, Kouichi Hagino, Kenji Hamaguchi, Ilana M Harrus, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Kiyoshi Hayashida, Natalie Hell, Junko S Hiraga, Ann Hornschemeier, Akio Hoshino, John P Hughes, Yuto Ichinohe, Ryo Iizuka, Hajime Inoue, Yoshiyuki Inoue, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Masachika Iwai, Jelle Kaastra, Tim Kallman, Tsuneyoshi Kamae, Jun Kataoka, Satoru Katsuda, Nobuyuki Kawai, Richard L Kelley, Caroline A Kilbourne, Takao Kitaguchi, Shunji Kitamoto, Tetsu Kitayama, Takayoshi Kohmura, Motohide Kokubun, Katsuji Koyama, Shu Koyama, Peter Kretschmar, Hans A Krimm, Aya Kubota, Hideyo Kunieda, Philippe Laurent, Shiu-Hang Lee, Maurice A Leutenegger, Olivier Limousin, Michael Loewenstein, Knox S Long, David Lumb, Greg Madejski, Yoshitomo Maeda, Daniel Maier, Kazuo Makishima, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian R McNamara, Missagh Mehdipour, Eric D Miller, Jon M Miller, Shin Mineshige, Kazuhisa Mitsuda, Ikuyuki Mitsuishi, Takuya Miyazawa, Tsunefumi Mizuno, Hideyuki Mori, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard F Mushotzky, Takao Nakagawa, Hiroshi Nakajima, Takeshi Nakamori, Shinya Nakashima, Kazuhiro Nakazawa, Kumiko K Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Takaya Ohashi, Masanori Ohno, Takashi Okajima, Naomi Ota, Masanobu Ozaki, Frits Paerels, Stéphane Paltani, Robert Petre, Ciro Pinto, Frederick S Porter, Katja Pottschmidt, Christopher S Reynolds, Samar Safi-Harb, Shinya Saito, Kazuhiro Sakai, Toru Sasaki, Goro Sato, Kosuke Sato, Rie Sato, Makoto Sawada, Norbert Schartel, Peter J Serlemtsos, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall K Smith, Yang Soong, Łukasz Stawarz, Yasuharu Sugawara, Satoshi Sugita, Andrew Szymkowiak, Hiroyasu Tajima, Hiromitsu Takahashi, Tadayuki Takahashi, Shin’ichiro Takeda, Yoh Takei, Toru Tamagawa, Takayuki Tamura, Takaaki Tanaka, Yasuo Tanaka, Yasuyuki T Tanaka, Makoto S Tashiro, Yuzuru Tawara, Yukikatsu Terada, Yuichi Terashima, Francesco Tombesi, Hiroshi Tomida, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Go Tsuru, Hiroyuki Uchida, Hideki Uchiyama, Yasunobu Uchiyama, Shutaro Ueda, Yoshihiro Ueda, Shin’ichiro Uno, C Megan Urry, Eugenio Ursino, Shin Watanabe, Norbert Werner, Dan R Wilkins, Brian J Williams, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Y Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Yoichi Yatsu, Daisuke Yonetoku, Irina Zhuravleva, Abderahmen Zoghbi, and A J J Raassen

Published
2018
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3. Hitomi X-ray observation of the pulsar wind nebula G21.5−0.9

Author

Felix Aharonian, Hiroki Akamatsu, Fumie Akimoto, Steven W Allen, Lorella Angelini, Marc Audard, Hisamitsu Awaki, Magnus Axelsson, Aya Bamba, Marshall W Bautz, Roger Blandford, Laura W Brenneman, Gregory V Brown, Esra Bulbul, Edward M Cackett, Maria Chernyakova, Meng P Chiao, Paolo S Coppi, Elisa Costantini, Jelle de Plaa, Cor P de Vries, Jan-Willem den Herder, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E Eckart, Teruaki Enoto, Yuichiro Ezoe, Andrew C Fabian, Carlo Ferrigno, Adam R Foster, Ryuichi Fujimoto, Yasushi Fukazawa, Akihiro Furuzawa, Massimiliano Galeazzi, Luigi C Gallo, Poshak Gandhi, Margherita Giustini, Andrea Goldwurm, Liyi Gu, Matteo Guainazzi, Yoshito Haba, Kouichi Hagino, Kenji Hamaguchi, Ilana M Harrus, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Kiyoshi Hayashida, Junko S Hiraga, Ann Hornschemeier, Akio Hoshino, John P Hughes, Yuto Ichinohe, Ryo Iizuka, Hajime Inoue, Yoshiyuki Inoue, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Masachika Iwai, Jelle Kaastra, Tim Kallman, Tsuneyoshi Kamae, Jun Kataoka, Satoru Katsuda, Nobuyuki Kawai, Richard L Kelley, Caroline A Kilbourne, Takao Kitaguchi, Shunji Kitamoto, Tetsu Kitayama, Takayoshi Kohmura, Motohide Kokubun, Katsuji Koyama, Shu Koyama, Peter Kretschmar, Hans A Krimm, Aya Kubota, Hideyo Kunieda, Philippe Laurent, Shiu-Hang Lee, Maurice A Leutenegger, Olivier Limousin, Michael Loewenstein, Knox S Long, David Lumb, Greg Madejski, Yoshitomo Maeda, Daniel Maier, Kazuo Makishima, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian R McNamara, Missagh Mehdipour, Eric D Miller, Jon M Miller, Shin Mineshige, Kazuhisa Mitsuda, Ikuyuki Mitsuishi, Takuya Miyazawa, Tsunefumi Mizuno, Hideyuki Mori, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard F Mushotzky, Takao Nakagawa, Hiroshi Nakajima, Takeshi Nakamori, Shinya Nakashima, Kazuhiro Nakazawa, Kumiko K Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Takaya Ohashi, Masanori Ohno, Takashi Okajima, Naomi Ota, Masanobu Ozaki, Frits Paerels, Stéphane Paltani, Robert Petre, Ciro Pinto, Frederick S Porter, Katja Pottschmidt, Christopher S Reynolds, Samar Safi-Harb, Shinya Saito, Kazuhiro Sakai, Toru Sasaki, Goro Sato, Kosuke Sato, Rie Sato, Makoto Sawada, Norbert Schartel, Peter J Serlemtsos, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall K Smith, Yang Soong, Łukasz Stawarz, Yasuharu Sugawara, Satoshi Sugita, Andrew Szymkowiak, Hiroyasu Tajima, Hiromitsu Takahashi, Tadayuki Takahashi, Shin’ichiro Takeda, Yoh Takei, Toru Tamagawa, Takayuki Tamura, Takaaki Tanaka, Yasuo Tanaka, Yasuyuki T Tanaka, Makoto S Tashiro, Yuzuru Tawara, Yukikatsu Terada, Yuichi Terashima, Francesco Tombesi, Hiroshi Tomida, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Go Tsuru, Hiroyuki Uchida, Hideki Uchiyama, Yasunobu Uchiyama, Shutaro Ueda, Yoshihiro Ueda, Shin’ichiro Uno, C Megan Urry, Eugenio Ursino, Shin Watanabe, Norbert Werner, Dan R Wilkins, Brian J Williams, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Y Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Yoichi Yatsu, Daisuke Yonetoku, Irina Zhuravleva, Abderahmen Zoghbi, Toshiki Sato, Nozomu Nakaniwa, Hiroaki Murakami, and Benson Guest

Published
2018
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4. Suzaku Observations of Fe K-shell Lines in the Supernova Remnant W51C and Hard X-ray Sources in the Proximity

Author

Aika Shimaguchi, Kumiko K Nobukawa, Shigeo Yamauchi, Masayoshi Nobukawa, and Yutaka Fujita

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract

In this paper, we investigated the Fe K-shell lines in the supernova remnant W51C and hard X-ray sources in the proximity. We measured the intensities of Fe I K$\alpha$ and Fe XXV He$\alpha$ lines at 6.40 keV and 6.68 keV, respectively, and found that the intensity of the 6.68 keV line is consistent with the background level expected from previous studies, while that of the 6.40 keV line is higher at the significance level of 2.0${\sigma}$. Given the presence of gamma-ray emission and high ionization rate point spatially coincident with the remnant, we conclude that the enhanced 6.40 keV line most likely originates from the interaction between low-energy cosmic rays and molecular clouds. Also, we discovered an enhanced 6.68 keV line emission from the compact H II region G49.0-0.3 at the significance level of 3.4${\sigma}$. Spectral analysis revealed that the temperature and abundance of the thermal plasma with the 6.68 keV line is $kT = 3.0^{+0.8}_{-0.7}$ keV and $Z = 0.5 \pm 0.2$ solar, respectively. These values are explained by the thermal plasma generated by the stellar winds of O stars., Comment: 8 pages, 4 figures, accepted for publication in Publications of the Astronomical Society of Japan (PASJ)

Published
2022
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5. Detailed design of the science operations for the XRISM mission

Author

Ken Ebisawa, Aya Kubota, Eric L. Miller, Yuusuke Uchida, Takao Kitaguchi, Yasuharu Sugawara, Yohko Tsuboi, Satoru Katsuda, Katsuhiro Hayashi, Shigeo Yamauchi, Shin Watanabe, Koji Mukai, S. Eguchi, Tsubasa Tamba, Hiromitsu Takahashi, Megumi Shidatsu, Kazuhiro Nakazawa, Laura A. Burns, Hideki Uchiyama, Takayuki Tamura, Naomi Ota, Hirokazu Odaka, Shinya Nakashima, Tsunefumi Mizuno, Matthew Holland, Masanori Ohno, Yukikatsu Terada, Yasushi Fukazawa, Michael Loewenstein, Makoto Tashiro, Chris Baluta, Shin'ichiro Uno, Masayoshi Nobukawa, Tahir Yaqoob, Yuichi Terashima, Makoto Sawada, R. Sato, Ryo Iizuka, and Atsushi Tanimoto

Subjects
Data processing, business.industry, Computer science, Mechanical Engineering, FOS: Physical sciences, Astronomy and Astrophysics, Plan (drawing), Pipeline (software), Electronic, Optical and Magnetic Materials, Task (project management), Fiscal year, Space and Planetary Science, Control and Systems Engineering, Agency (sociology), Systems engineering, Data center, Astrophysics - Instrumentation and Methods for Astrophysics, Aerospace, business, Instrumentation and Methods for Astrophysics (astro-ph.IM), Instrumentation
Abstract

XRISM is an X-ray astronomical mission by the JAXA, NASA, ESA and other international participants, that is planned for launch in 2022 (Japanese fiscal year), to quickly restore high-resolution X-ray spectroscopy of astrophysical objects. To enhance the scientific outputs of the mission, the Science Operations Team (SOT) is structured independently from the instrument teams and the Mission Operations Team. The responsibilities of the SOT are divided into four categories: 1) guest observer program and data distributions, 2) distribution of analysis software and the calibration database, 3) guest observer support activities, and 4) performance verification and optimization activities. As the first step, lessons on the science operations learned from past Japanese X-ray missions are reviewed, and 15 kinds of lessons are identified. Among them, a) the importance of early preparation of the operations from the ground stage, b) construction of an independent team for science operations separate from the instrument development, and c) operations with well-defined duties by appointed members are recognized as key lessons. Then, the team structure and the task division between the mission and science operations are defined; the tasks are shared among Japan, US, and Europe and are performed by three centers, the SOC, SDC, and ESAC, respectively. The SOC is designed to perform tasks close to the spacecraft operations, such as spacecraft planning, quick-look health checks, pre-pipeline processing, etc., and the SDC covers tasks regarding data calibration processing, maintenance of analysis tools, etc. The data-archive and user-support activities are covered both by the SOC and SDC. Finally, the science-operations tasks and tools are defined and prepared before launch., Comment: 42 pages, 7 figures, 8 table, Accepted for Publication in JATIS (SPIE)

Published
2021

6. A systematic comparison of ionization temperatures between ionizing and recombining plasmas in supernova remnants

Author

Masayoshi Nobukawa, Shigeo Yamauchi, and Katsuji Koyama

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Plasma, Astrophysics, Electron, 01 natural sciences, Ionizing radiation, Supernova, Space and Planetary Science, Ionization, 0103 physical sciences, Coulomb, Electron temperature, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics
Abstract

The temperatures of the plasma in the supernova remnants (SNRs) are initially very low just after the shock heating. The electron temperature (kT_{e}) increases quickly by Coulomb interaction, and then the energetic electrons gradually ionize atoms to increase the ionization temperature (kT_{i}). The observational fact is that most of the young and middle-to-old aged SNRs have lower kT_{i} than kT_{e} after the shock heating. The temperature evolution in the shell-like SNRs has been explained by this ionizing plasma (IP) scenario. On the other hand, in the last decade, a significant fraction of the mixed morphology SNRs was found to exhibit a recombining plasma (RP) with higher kT_{i} than kT_{e}. The origin and the evolution mechanism of the RP SNRs have been puzzling. To address this puzzle, this paper presents the kT_{e} and kT_{i} profiles using the observed results by follow-up Suzaku observations, and then proposes a new scenario for the temperature and morphology evolutions in the IP and RP SNRs., Accepted for publication in PASJ

Published
2021

7. Spectral and timing properties of the black hole candidate X1755-338 observed in 1989-1995

Author

Shigeo Yamauchi and Sakiho Maeda

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), FOS: Physical sciences, Astronomy and Astrophysics, Radius, Astrophysics, Thermal emission, Spectral line, Flux (metallurgy), Accretion disc, Space and Planetary Science, Inclination angle, Astrophysics - High Energy Astrophysical Phenomena, Intensity (heat transfer), Line (formation)
Abstract

We report results of an analysis of the black hole (BH) candidate source X1755-338 in 1989, 1990, and 1991 with Ginga, and in 1995 with ASCA. The spectra were well represented by a model consisting of a soft thermal emission from an accretion disk and a hard X-ray tail. The normalization of the multi-color disk model, relating to the inner disk radius, was similar to each other. The unabsorbed X-ray fluxes from the disk component in the 0.01-10 keV band were estimated to be 1.3x10^{-9}, 3.0x10^{-9}, 9.8x10^{-10}, and 2.4x10^{-9} erg s^{-1} cm^{-2} in 1989, 1990, 1991, and 1995, respectively, and are proportional to kT_{in}^4, where kT_{in} is a temperature at the inner disk radius. Based on the standard accretion disk model for a non-rotating BH, our results suggest either a small BH mass or a large inclination angle. Otherwise, X1755-338 is a rotating BH. The hard X-ray intensity was found to be variable, while the soft X-ray intensity was stable. Although the previous work showed the existence of an iron line at 6.7 keV, no clear iron line feature was found in all the spectra. We infer that most of the iron line flux reported in the previous work was due to contamination of the Galactic diffuse X-ray emission., Comment: Accepted for publication in PASJ

Published
2021
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8. X-ray emission from the mixed-morphology supernova remnant HB 9

Author

Shigeo Yamauchi, Kumiko K. Nobukawa, Mariko Saito, Thomas G. Pannuti, and Aya Bamba

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Astrophysics::High Energy Astrophysical Phenomena, X-ray, FOS: Physical sciences, Astronomy and Astrophysics, Plasma, Astrophysics, Spectral line, Ionizing radiation, Interstellar medium, Space and Planetary Science, Ionization, Astrophysics - High Energy Astrophysical Phenomena, Ejecta, Supernova remnant
Abstract

We present the results of a spectral analysis of the central region of the mixed-morphology supernova remnant HB 9. A prior Ginga observation of this source detected a hard X-ray component above 4 keV and the origin of this particular X-ray component is still unknown. Our results demonstrate that the extracted X-ray spectra are best represented by a model consisting of a collisional ionization equilibrium plasma with a temperature of ~0.1-0.2 keV (interstellar matter component) and an ionizing plasma with a temperature of ~0.6-0.7 keV and an ionization timescale of >1 x 10^{11} cm^{-3} s (ejecta component). No significant X-ray emission was found in the central region above 4 keV. The recombining plasma model reported by a previous work does not explain our spectra., Accepted for publication in PASJ

Published
2020

9. Discovery of annular X-ray emission centered on MAXI J1421-613: Dust-scattering X-rays?

Author

Masayoshi Nobukawa, Shigeo Yamauchi, and Kumiko K. Nobukawa

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Photon, Spectral shape analysis, Scattering, Astrophysics::High Energy Astrophysical Phenomena, Extinction (astronomy), FOS: Physical sciences, Flux, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Radius, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Supernova remnant, Astrophysics::Galaxy Astrophysics, Intensity (heat transfer)
Abstract

We report the discovery of an annular emission of $\sim$3'-9' radius around the center of a transient source, an X-ray burster MAXI J1421-613, in the Suzaku follow-up analysis. The spectrum of the annular emission shows no significant emission-line structure, and is well explained by an absorbed power law model with a photon index of $\sim$4.2. These features exclude the possibility that the annular emission is a shell-like component of a supernova remnant. The spectral shape, the time history, and the X-ray flux of the annular emission agree with the scenario that the emission is due to a dust-scattering echo. The annular emission is made under a rare condition of the dust-scattering echo, where the central X-ray source, MAXI J1421-613, exhibits a short time outburst with three X-ray bursts and immediately re-enters a long quiescent period. The distribution of the hydrogen column density along the annular emission follows that of the CO intensity, which means that MAXI J1421-613 is located behind the CO cloud. We estimate the distance to MAXI J1421-613 to be $\sim$3~kpc assuming that the dust layer responsible for the annular emission is located at the same position as the CO cloud., Comment: 11 pages, 3 figures, accepted for publication in Publications of the Astronomical Society of Japan (PASJ)

Published
2020

10. Discovery of recombining plasma associated with the candidate supernova remnant G189.6+3.3 with Suzaku

Author

Thomas G. Pannuti, Kumiko K. Nobukawa, Moe Oya, and Shigeo Yamauchi

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Continuum (design consultancy), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Plasma, 01 natural sciences, Interstellar medium, Space and Planetary Science, Ionization, 0103 physical sciences, Radiative transfer, Astrophysics - High Energy Astrophysical Phenomena, Electronic band structure, Ejecta, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract

We present the results of an X-ray spectral analysis of the northeast region of the candidate supernova remnant G189.6+3.3 with Suzaku. K-shell lines from highly ionized Ne, Mg, Si, and S were detected in the spectrum for the first time. In addition, a radiative recombining continuum (RRC) from He-like Si was clearly seen near 2.5 keV. This detection of an RRC reveals for the first time that G189.6+3.3 possesses an X-ray-emitting recombining plasma (RP). The extracted X-ray spectrum in the 0.6-10.0 keV energy band is well fitted with a model consisting of a collisional ionization equilibrium plasma component (associated with the interstellar medium) and an RP component (associated with the ejecta). The spectral feature shows that G189.6+3.3 is most likely to be a middle-aged SNR with an RP., Comment: Accepted for publication in PASJ

Published
2020
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11. Characterization of diffuse X-ray emission from IGR~J17448-3232: an implication of a line of sight merging activity

Author

Shoko Watanabe, Kumiko K. Nobukawa, Shigeo Yamauchi, and Hiroki Akamatsu

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Photon, Line-of-sight, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, X-ray, FOS: Physical sciences, Astronomy and Astrophysics, Plasma, Astrophysics, 01 natural sciences, Power law, Galaxy, Space and Planetary Science, Intracluster medium, 0103 physical sciences, Cluster (physics), Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics
Abstract

Results of the spectral analysis for the galaxy cluster IGR J17448-3232 are presented. The intracluster medium (ICM) in the central region (r34 keV or a CIE+power law model with a temperature of 9.4 keV and a photon index of 1.1. The two component models can represent the intensity ratio of Fe XXVI Ly alpha/Fe XXV He alpha lines. On the other hand, the spectrum in the outer region (r>300'') can be explained by a single CIE plasma model with a temperature of 5-8 keV. Based on the spectral feature and its circular structure, we propose that the NEI plasma was produced by merging along the line-of-sight direction., Accepted for publication in PASJ

Published
2019
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12. X-ray spectra of Sgr A East and diffuse X-ray background near the Galactic center

Author

Hideki Uchiyama, Masayoshi Nobukawa, Akiko Ono, Katsuji Koyama, Shigeo Yamauchi, and Kumiko K. Nobukawa

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Galactic Center, X-ray background, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Space and Planetary Science, Surface brightness, Astrophysics - High Energy Astrophysical Phenomena, Supernova remnant, Sagittarius, X ray spectra, Line (formation)
Abstract

This paper reports the analysis procedure and results of simultaneous spectral fits of the Suzaku archive data for Sagittarius (Sgr) A East and the nearby Galactic center X-ray emission (GCXE). The results are that the mixed-morphology supernova remnant Sgr A East has a recombining plasma (RP) with Cr and Mn He$\alpha$ lines, and a power-law component (PL) with an Fe I K$\alpha$ line. The nearby GCXE has a $\sim$1.5-times larger surface brightness than the mean GCXE far from Sgr A East, although the spectral shape is almost identical. Based on these results, we interpret that the origins of the RP and the PL with the Fe I K$\alpha$ line are past big flares of Sgr A$^*$., Comment: Accepted for publication in PASJ

Published
2019
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13. Neutral iron line in the supernova remnant IC 443 and implications for MeV cosmic rays

Author

Shigeo Yamauchi, Arisa Hirayama, Kumiko K. Nobukawa, Aika Shimaguchi, Yutaka Fujita, and Masayoshi Nobukawa

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Molecular cloud, Astrophysics::High Energy Astrophysical Phenomena, Nuclear Theory, FOS: Physical sciences, Astronomy and Astrophysics, Cosmic ray, Astrophysics, Plasma, 01 natural sciences, Space and Planetary Science, Ionization, 0103 physical sciences, Physics::Accelerator Physics, Supernova remnant, Astrophysics - High Energy Astrophysical Phenomena, Nuclear Experiment, 010303 astronomy & astrophysics, Equivalent width, Intensity (heat transfer), Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract

We report a discovery of bright blob-like enhancements of an Fe I K$\alpha$ line in the northwest and the middle of the supernova remnant (SNR) IC 443. The distribution of the line emission is associated with molecular clouds interacting with the shock front, and is totally different from that of the plasma. The Fe I K$\alpha$ line has a large equivalent width. The most plausible scenario for the origin of the line emission is that the MeV protons accelerated in the shell leak into the molecular clouds and ionize the Fe atoms therein. The observed Fe I K$\alpha$ line intensity is consistent with the prediction of a theoretical model, in which MeV protons are accelerated along with GeV and TeV protons at the SNR., Comment: 13 pages, 3 figures, accepted for publication in PASJ

Published
2019
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14. New Scenario of plasma evolution in IC 443

Author

Katsuji Koyama, Kumiko K. Nobukawa, Masayoshi Nobukawa, Shigeo Yamauchi, and Arisa Hirayama

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Cosmic ray, Plasma, Astrophysics, 01 natural sciences, Power law, Ionizing radiation, Supernova, Quality (physics), Space and Planetary Science, Ionization, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract

Most of young and middle-aged supernova remnants (SNRs) exhibit an ionizing plasma (IP), an ionizing process following a shock heated SNR gas. On the other hand, significant fractions of SNRs exhibit a recombining plasma (RP). The origin and the mechanisms of the RP, however, are not yet well understood. This paper proposes a new model that the RP is followed after the IP process taken at the first epoch of the SNR evolution. Using the high quality and wide band (0.6-10 keV) spectrum of IC 443, we nicely fitted with a model of two RP (two-RP model) plus a power law (PL) with an Fe I Kalpha line component. The ionization temperature in one RP monotonously increases from Ne-Ca, while that in the other RP shows a drastic increase from Cr-Ni. Origin and mechanism of the two-RP and PL with an Fe I Kalpha line components are possibly due to a different evolution of two plasmas and ionization by the low-energy cosmic ray., Accepted for publication in PASJ

Published
2018

15. Detection of polarized gamma-ray emission from the Crab nebula with Hitomi Soft Gamma-ray Detector

Author

Akio Hoshino, Katsuhiro Hayashi, Manabu Ishida, Hideki Uchiyama, Takayuki Tamura, Shunji Kitamoto, Shin'ichiro Takeda, Shinya Saito, Daisuke Yonetoku, Peter J. Serlemtsos, Yoshitaka Ishisaki, Masachika Iwai, Hiroshi Nakajima, Megumi Shidatsu, Kumi Ishikawa, Hans A. Krimm, Ken Ebisawa, Yasuyuki T. Tanaka, Massimiliano Galeazzi, Andrew C. Fabian, Brian R. McNamara, Shu Koyama, Samar Safi-Harb, Jan-Willem den Herder, R. Sato, Isamu Hatsukade, Hironori Matsumoto, Yoshitomo Maeda, Missagh Mehdipour, Teruaki Enoto, Hirokazu Odaka, Jelle de Plaa, Hiroshi Tsunemi, Maurice A. Leutenegger, Francesco Tombesi, Jelle Kaastra, Richard L. Kelley, Kazuhiro Nakazawa, Ikuyuki Mitsuishi, Takuya Miyazawa, G. Sato, Yohko Tsuboi, Frederick S. Porter, Norbert Werner, Fumie Akimoto, Junko S. Hiraga, Magnus Axelsson, Shinya Yamada, Ciro Pinto, David H. Lumb, Shigeo Yamauchi, Maxim Markevitch, Yuto Ichinohe, Takeshi Go Tsuru, Kosuke Sato, Koji Mori, Caroline A. Kilbourne, Yuichi Terashima, Kyoko Matsushita, Timothy R. Kallman, Philippe Laurent, Olivier Limousin, Toru Tamagawa, Luigi C. Gallo, Aya Bamba, Roger Blandford, Kiyoshi Hayashida, Yasunobu Uchiyama, Cor P. de Vries, Tsuneyoshi Kamae, Hirofumi Noda, Gregory V. Brown, Carlo Ferrigno, Yoshihiro Ueda, Yuusuke Uchida, Eric D. Miller, Yuichiro Ezoe, Andrea Goldwurm, Hiromi Seta, Frits Paerels, Katja Pottschmidt, Kazuhiro Sakai, Shin'ichiro Uno, Yoshito Haba, Stéphane Paltani, Hiromitsu Takahashi, Kazuhisa Mitsuda, Masanori Ohno, Satoshi Sugita, Masahiro Tsujimoto, Christopher S. Reynolds, Shin Mineshige, Ryuichi Fujimoto, Peter Kretschmar, Masayoshi Nobukawa, Yoh Takei, Tahir Yaqoob, Jon M. Miller, Dan R. Wilkins, Meng P. Chiao, Matteo Guainazzi, Aurora Simionescu, Hisamitsu Awaki, Paolo De Coppi, Katsuji Koyama, Masanobu Ozaki, Kumiko K. Nobukawa, Yasuharu Sugawara, Daniel Maier, Tadayuki Takahashi, Jun Kataoka, Aya Kubota, Hiroyuki Uchida, Laura Brenneman, John P. Hughes, Takayoshi Kohmura, Takaaki Tanaka, Hajime Inoue, Lorella Angelini, Toru Sasaki, Greg Madejski, Shutaro Ueda, Takao Nakagawa, Tadayasu Dotani, Maria Chernyakova, Motohide Kokubun, Takao Kitaguchi, Irina Zhuravleva, Shin Watanabe, Dan McCammon, Hideyuki Mori, Randall K. Smith, Edward M. Cackett, Norbert Schartel, Margherita Giustini, Megan E. Eckart, Tsunefumi Mizuno, Liyi Gu, Chris Done, Takeshi Nakamori, Takaya Ohashi, Shiu-Hang Lee, Michael Loewenstein, Adam R. Foster, Poshak Gandhi, Yasushi Fukazawa, Kenji Hamaguchi, Satoru Katsuda, Knox S. Long, Ilana M. Harrus, Yuzuru Tawara, Hideyo Kunieda, Lukasz Stawarz, C. Megan Urry, Richard F. Mushotzky, Nobuyuki Kawai, Brian J. Williams, Tetsu Kitayama, Felix Aharonian, Yoshiyuki Inoue, Noriko Y. Yamasaki, Eugenio Ursino, Takayuki Hayashi, Yukikatsu Terada, Makoto Yamauchi, Yasuo Tanaka, Steven W. Allen, Kazuo Makishima, Marc Audard, Shinya Nakashima, Naomi Ota, Hiroyasu Tajima, Hiroshi Murakami, Hiroshi Tomida, Hiroya Yamaguchi, Ryo Iizuka, Kouichi Hagino, Yoichi Yatsu, Kazutaka Yamaoka, Koji Mukai, Abderahmen Zoghbi, Makoto Tashiro, Ann Hornschemeier, Makoto Sawada, Marshall W. Bautz, Takashi Okajima, Esra Bulbul, Yang Soong, Akihiro Furuzawa, Hiroki Akamatsu, Andrew Szymkowiak, Robert Petre, Elisa Costantini, 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), 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, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
Photon, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, 01 natural sciences, polarimeters [instrumentation], X-rays: individual (Crab), symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, Pulsar, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Nebula, polarization, Brewster's angle, Spectrometer, 010308 nuclear & particles physics, Gamma ray, instrumentation: polarimeters, Astronomy and Astrophysics, Polarization (waves), Crab Nebula, individual (Crab) [X-rays], Space and Planetary Science, symbols, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena
Abstract

著者人数: 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; 内田, 悠介), Accepted: 2018-09-30, 資料番号: SA1180351000

Published
2018

16. Hitomi (ASTRO-H) X-ray Astronomy Satellite

Author

Laura Brenneman, Hironori Matsumoto, Kirk Gilmore, Takayuki Yuasa, D. Lumb, Manabu Ishida, Aurora Simionescu, Takao Nakagawa, Junichiro Katsuta, Esra Bulbul, Meng P. Chiao, Philippe Laurent, Jelle de Plaa, Hiroyuki Ogawa, Keith Arnaud, Keiji Ogi, John P. Doty, B. Ramsey, Yuzuru Tawara, C. Megan Urry, Eric D. Miller, Peter Shirron, Gregory V. Brown, Dan R. Wilkins, Hiroshi Tsunemi, Richard F. Mushotzky, Nobuyuki Kawai, Brian J. Williams, Steven W. Allen, Naoko Iyomoto, Taro Kawano, Katja Pottschmidt, Yang Soong, Tadayuki Takahashi, Yasuharu Sugawara, Ikuyuki Mitsuishi, Margherita Giustini, Greg Madejski, Tetsu Kitayama, Megumi Shidatsu, Hideyuki Mori, Łukasz Stawarz, Randall K. Smith, Satoshi Sugita, Norbert Schartel, James Pontius, Kazuhiro Nakazawa, Eugenio Ursino, Katsuhiro Hayashi, Toshio Nakano, Satoru Katsuda, Cor P. de Vries, Adam R. Foster, Masanobu Ozaki, Kenji Minesugi, Tomomi Watanabe, Yuichi Terashima, Christopher S. Reynolds, Hiroaki Sameshima, Alex Koujelev, Naohisa Anabuki, Isamu Hatsukade, Masaharu Nomachi, Yoichi Yatsu, Yasunobu Uchiyama, Steve O' Dell, Ann Hornschemeier, Akio Hoshino, Yasuo Tanaka, M. Pohl, Kyoko Matsushita, Masahiro Tsujimoto, Hideki Uchiyama, Mark O. Kimball, Arvind Parmar, Gary A. Sneiderman, Yoshiyuki Inoue, Toru Tamagawa, Yukikatsu Terada, Shinya Nakashima, Tsuneyoshi Kamae, Dmitry Khangulyan, Kiyoshi Hayashida, Rie Sato, Aya Bamba, Roger Blandford, Kazunori Ishibashi, Shinya Saito, Caroline A. Kilbourne, Toshio Murakami, Takeda Shin'ichiro, Missagh Mehdipour, Motohide Kokubun, Masachika Iwai, Dan McCammon, Michael J. DiPirro, Marshall W. Bautz, Shunji Kitamoto, Naomi Ota, Brian R. McNamara, Frits Paerels, Stéphane Paltani, Magnus Axelsson, Edgar Canavan, Nobutaka Bando, Peter J. Serlemitsos, Shu Koyama, Felix Aharonian, Matteo Guainazzi, Joseph Miko, Masayoshi Nobukawa, Thomas G. Bialas, Koji Mori, Makoto Yamauchi, Uno Shin'ichiro, Hirokazu Odaka, Toru Sasaki, Mina Ogawa, Philipp Azzarello, Atsushi Wada, Tsuyoshi Okazaki, Ken Ebisawa, Takeshi Go Tsuru, Yoshitomo Maeda, Jon M. Miller, A. L. King, Cynthia Simmons, Hirofumi Noda, Hiromitsu Takahashi, Kazuhisa Mitsuda, Carlo Ferrigno, Hiroyasu Tajima, Kazuo Makishima, Erin Kara, Fumie Akimoto, Shigeo Kawasaki, Kumi Ishikawa, Kosuke Sato, Hiroshi Nakajima, Knox S. Long, Jun Kataoka, Keisuke Shinozaki, Kazuyuki Hirose, Keisuke Tamura, Teruaki Enoto, Yoh Takei, Yoshito Haba, Shinya Yamada, Richard L. Kelley, Yoshihiro Ueda, Megan E. Eckart, Takaya Ohashi, Shin-ichiro Sakai, Kevin R. Boyce, D. Haas, Atsushi Okamoto, Kazuhiro Sakai, Ryo Nagino, Makoto Asai, Maurice A. Leutenegger, Michael Loewenstein, Daniel R. Wik, Yohko Tsuboi, Maria Chernyakova, Shiro Ueno, Koji Mukai, Hiroshi Murakami, Takeshi Nakamori, Hiroshi Tomida, Tahir Yaqoob, Norbert Werner, Paolo Coppi, Abderahmen Zoghbi, Shin Watanabe, Kosei Ishimura, Hideyo Kunieda, Candace Masters, Yusuke Nishioka, Shigeo Yamauchi, Maxim Markevitch, Yuto Ichinohe, Andrew C. Fabian, Ryuichi Fujimoto, Kenji Hamaguchi, Liyi Gu, Edward M. Cackett, Chris Done, Junko S. Hiraga, Chris Baluta, Noriko Y. Yamasaki, Maki Shida, Makoto Tashiro, Takanobu Shimada, Yasuyuki T. Tanaka, Massimiliano Galeazzi, Ilana M. Harrus, Naoko Iwata, Timothy R. Kallman, Takuya Miyazawa, Kumiko K. Nobukawa, Madoka Kawaharada, Hisamitsu Awaki, Takaaki Tanaka, Tadayasu Dotani, Goro Sato, Ciro Pinto, Hiroya Yamaguchi, Harvey Moseley, Yoshiharu Namba, Shutaro Ueda, Masayuki Itoh, Takayoshi Kohmura, Daisuke Yonetoku, Yoshitaka Ishisaki, Hans A. Krimm, Hiromi Seta, Atsumasa Yoshida, Kouichi Hagino, Yuichiro Ezoe, Samar Safi-Harb, John P. Hughes, Daniel Maier, Hajime Inoue, Lorella Angelini, Yasuko Shibano, Frederick S. Porter, Saori Konami, Takayuki Tamura, Shin Mineshige, Peter Kretschmar, Yoichi Sato, Helen Russell, Hiroyuki Uchida, Elisa Costantini, Chikara Natsukari, Housei Nagano, Jan-Willem den Herder, Francesco Tombesi, Jelle Kaastra, Daniel S. McGuinness, Masanori Ohno, Hiroyuki Sugita, Katsuji Koyama, Tsunefumi Mizuno, Theodore Muench, Shiu-Hang Lee, Poshak Gandhi, Yasushi Fukazawa, Stefan Funk, Luigi C. Gallo, Tatsuro Kosaka, Andrea Goldwurm, Ryo Iizuka, Masayuki Ohta, Kazutaka Yamaoka, Marc Audard, Makoto Sawada, Takashi Okajima, Franco Moroso, Akihiro Furuzawa, Aya Kubota, Chris Jewell, Olivier Limousin, Takayuki Hayashi, Takao Kitaguchi, Takahiro Yamada, Hiroki Akamatsu, Andrew Szymkowiak, Robert Petre, Irina Zhuravleva, Dublin Institute for Advanced Studies (DIAS), SRON Netherlands Institute for Space Research (SRON), Climate and Environmental Physics [Bern] (CEP), Physikalisches Institut [Bern], Universität Bern [Bern]-Universität Bern [Bern], Columbia Astrophysics Laboratory (CAL), Columbia University [New York], Stockholm University, Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), Stanford University [Stanford], 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), Stanford University, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Universität Bern [Bern] (UNIBE)-Universität Bern [Bern] (UNIBE), 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, 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)

Subjects
Space operations, X-ray telescope, microcalorimeter, 01 natural sciences, x-ray astronomy, 010309 optics, gamma-ray astronomy, 0103 physical sciences, 010303 astronomy & astrophysics, Instrumentation, ComputingMilieux_MISCELLANEOUS, Remote sensing, [PHYS]Physics [physics], X-ray astronomy, Spacecraft, business.industry, Mechanical Engineering, Astronomy and Astrophysics, hard x-ray, Gamma-ray astronomy, First light, Electronic, Optical and Magnetic Materials, Spacecraft system, x-ray, Space and Planetary Science, Control and Systems Engineering, gamma ray, Satellite, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

著者人数: 270名（所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 高橋, 忠幸; 国分, 紀秀; 満田, 和久; Baluta, Chris; 坂東, 信尚; 堂谷, 忠靖; 海老沢, 研; 林, 克洋; 廣瀬, 和之; 飯塚, 亮; 石田, 学; 石川, 久美; 石村, 康生; 岩井, 将親; 岩田, 直子; 河野, 太郎; 川崎, 繁男; 小山, 志勇; 前田, 良知; 峯杉, 賢治; 中川, 貴雄; 夏苅, 権; 小川, 博之; 小川, 美奈; 太田, 方之; 岡崎, 健; 尾崎, 正伸; 坂井, 真一郎; 鮫島, 寛明; 佐藤, 悟郎; 佐藤, 理江; 柴野, 靖子; 志田, 真樹; 嶋田, 貴信; Simionescu, Aurora; 菅原, 泰晴; 竹井, 洋; 田村, 隆幸; 田中, 靖郎; 田代, 信; 冨田, 洋; 辻本, 匡弘; 上田, 周太朗; 上野, 史郎; 和田, 篤始; 渡辺, 伸; 山田, 隆弘; 山崎, 典子）, Number of authors: 270 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS): Takahashi, Tadayuki; Kokubun, Motohide; Mitsuda, Kazuhisa; Baluta, Chris; Bando, Nobutaka; Dotani, Tadayasu; Ebisawa, Ken; Hayashi, Katsuhiro; Hirose, Kazuyuki; Iizuka, Ryo; Ishida, Manabu; Ishikawa, Kumi; Ishimura, Kosei; Iwai, Masachika; Iwata, Naoko; Kawano, Taro; Kawasaki, Shigeo; Koyama, Shu; Maeda, Yoshitomo; Minesugi, Kenji; Nakagawa, Takao; Natsukari, Chikara; Ogawa, Hiroyuki; Ogawa, Mina; Ohta, Masayuki; Okazaki, Tsuyoshi; Ozaki, Masanobu; Sakai, Shinichiro; Sameshima, Hiroaki; Sato, Goro; Sato, Rie; Shibano, Yasuko; Shida, Maki; Shimada, Takanobu; Simionescu, Aurora; Sugawara, Yasuharu; Takei, Yoh; Tamura, Takayuki; Tanaka, Yasuo; Tashiro, Makoto; Tomida, Hiroshi; Tsujimoto, Masahiro; Ueda, Shutaro; Ueno, Shiro; Wada, Atsushi; Watanabe, Shin; Yamada, Takahiro; Yamasaki, Noriko Y.), Accepted: 2018-02-05, 資料番号: SA1170333000

Published
2018

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

Author

Hideyuki Mori, Hisamitsu Awaki, Yoshito Haba, Hideyo Kunieda, Y. Tawara, Shigeo Yamauchi, Keisuke Tamura, Hironori Matsumoto, T. Hayashi, Masayuki Itoh, Satoshi Sugita, Ryo Iizuka, Takuya Miyazawa, Akihiro Furuzawa, Manabu Ishida, Takashi Okajima, Kazunori Ishibashi, Yoshitomo Maeda, and Ikuyuki Mitsuishi

Subjects
Photon, FOS: Physical sciences, X-ray telescope, 01 natural sciences, Encircled energy, 010309 optics, multilayer supermirror, Optics, Pulsar, 0103 physical sciences, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Instrumentation, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, business.industry, Mechanical Engineering, Antenna aperture, Astronomy and Astrophysics, Electronic, Optical and Magnetic Materials, Optical axis, Imaging spectroscopy, hard x-rays, Space and Planetary Science, Control and Systems Engineering, Satellite, x-ray telescope, business, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

著者人数: 19名, Accepted: 2018-01-22, 資料番号: SA1170310000

Published
2018

19. Measurements of resonant scattering in the Perseus Cluster core with Hitomi SXS

Author

Randall Smith, Hirokazu Odaka, Kumiko K. Nobukawa, Shin Watanabe, Hiroki Akamatsu, Goro Sato, Robert Petre, Ciro Pinto, G. U. Liyi, Shinya Yamada, Michael Loewenstein, Shutaro Ueda, Chris Done, Kazuhiro Sakai, Koji Mori, Kenji Hamaguchi, Elisa Costantini, Ilana M. Harrus, Carlo Ferrigno, Norbert Schartel, Yang Soong, Takayoshi Kohmura, Satoru Katsuda, Knox S. Long, Hiroshi Tsunemi, Ikuyuki Mitsuishi, Isamu Hatsukade, Ryo Iizuka, Kazutaka Yamaoka, Kouichi Hagino, Yuichiro Ezoe, Hironori Matsumoto, Makoto Sawada, Takashi Okajima, Akihiro Furuzawa, Francesco Tombesi, Kazuo Makishima, Yasuyuki T. Tanaka, Caroline A. Kilbourne, H. Tomida, Eugenio Ursino, Kumi Ishikawa, Yoshiyuki Inoue, Jon M. Miller, Jun Kataoka, Cor P. de Vries, Hiromi Seta, Yuichi Terashima, Hiromitsu Takahashi, Kazuhisa Mitsuda, Takao Nakagawa, L. E.E. Shiu-Hang, Marshall W. Bautz, Yukikatsu Terada, Christopher S. Reynolds, Teruaki Enoto, Missagh Mehdipour, Motohide Kokubun, Andrew E. Szymkowiak, Maurice A. Leutenegger, Meng P. Chiao, John P. Hughes, Yohko Tsuboi, Norbert Werner, Takeshi Go Tsuru, Peter J. Serlemtsos, Yoshitaka Ishisaki, Katsuji Koyama, Kiyoshi Hayashida, Daniel Maier, Hajime Inoue, Lorella Angelini, Aurora Simionescu, Hiroshi Nakajima, Kosuke Sato, Yoshitomo Maeda, David H. Lumb, Fumie Akimoto, Margherita Giustini, Manabu Ishida, Esra Bulbul, Shigeo Yamauchi, Maxim Markevitch, Tsuneyoshi Kamae, Yuto Ichinohe, Makoto Yamauchi, Hans A. Krimm, Masanori Ohno, Anna Ogorzalek, Yoshihiro Ueda, Yoshito Haba, Steven W. Allen, Maki Furukawa, Kyoko Matsushita, Samar Safi-Harb, B. J. Williams, Stéphane Paltani, Masayoshi Nobukawa, Yuzuru Tawara, Timothy R. Kallman, Hiroya Yamaguchi, Junko S. Hiraga, Magnus Axelsson, O. T.A. Naomi, Toru Tamagawa, Katsuhiro Hayashi, Rie Sato, Takuya Miyazawa, Maria Chernyakova, Akio Hoshino, Hirofumi Noda, Yasunobu Uchiyama, Frits Paerels, Hisamitsu Awaki, Jan-Willem den Herder, Yasuo Tanaka, Yasuharu Sugawara, U. N.O. Shiníchiro, Łukasz Stawarz, Takaaki Tanaka, Matteo Guainazzi, Tadayasu Dotani, Hideki Uchiyama, Toru Sasaki, Jelle Kaastra, Koji Mukai, Abderahmen Zoghbi, Luigi C. Gallo, Edward M. Cackett, Shunji Kitamoto, Shinya Saito, Laura Brenneman, Takao Kitaguchi, Paolo De Coppi, Yoichi Yatsu, Masachika Iwai, Megan E. Eckart, Takaya Ohashi, Richard F. Mushotzky, Andrew C. Fabian, Kazuhiro Nakazawa, Tahir Yaqoob, Daisuke Yonetoku, Hideyo Kunieda, Nobuyuki Kawai, Megumi Shidatsu, Brian R. McNamara, Ryuichi Fujimoto, Tetsu Kitayama, Shu Koyama, Noriko Y. Yamasaki, Ken Ebisawa, Massimiliano Galeazzi, Takeshi Nakamori, Felix Aharonian, Aya Bamba, Ann Hornschemeier, Roger Blandford, Adam R. Foster, Takayuki Hayashi, Philippe Laurent, Makoto Tashiro, Shin'ichiro Takeda, Gregory V. Brown, Masahiro Tsujimoto, Jelle de Plaa, Dan R. Wilkins, Tadayuki Takahashi, Marc Audard, Hiroshi Murakami, Greg Madejski, Hideyuki Mori, Shinya Nakashima, Hiroyasu Tajima, Satoshi Sugita, Masanobu Ozaki, Katja Pottschmidt, C. Megan Urry, Tsunefumi Mizuno, Dan McCammon, Shin Mineshige, Peter Kretschmar, Richard L. Kelley, Yoh Takei, Poshak Gandhi, Yasushi Fukazawa, Eric D. Miller, Takayuki Tamura, Aya Kubota, Irina Zhuravleva, Andrea Goldwurm, Frederick S. Porter, Hiroyuki Uchida, Olivier Limousin, 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, clusters: individual (Perseus Cluster) [galaxies], 01 natural sciences, Settore FIS/05 - Astronomia e Astrofisica, Ionization, 0103 physical sciences, Radiative transfer, Emission spectrum, Spectral resolution, 010306 general physics, Anisotropy, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Line (formation), High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Astronomy and Astrophysics, Computational physics, Amplitude, clusters: intracluster medium [galaxies], Space and Planetary Science, X-rays: galaxies: clusters, galaxies: clusters [X-rays], Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
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: 2017-10-08, 資料番号: SA1170335000

Published
2018

20. Temperature structure in the Perseus cluster core observed with Hitomi

Author

Laura Brenneman, Missagh Mehdipour, Motohide Kokubun, Manabu Ishida, Shinya Yamada, Kazuhiro Sakai, Kyoko Matsushita, Timothy R. Kallman, Toru Tamagawa, Hiroya Yamaguchi, Kouichi Hagino, Yuichiro Ezoe, Marc Audard, Frits Paerels, Ciro Pinto, Shin'ichiro Uno, Olivier Limousin, Matteo Guainazzi, Koji Mukai, Abderahmen Zoghbi, Toru Sasaki, Daisuke Yonetoku, Satoshi Sugita, Hiroki Akamatsu, Kumiko K. Norukawa, Yoshitaka Ishisaki, Andrew Szymkowiak, Dan R. Wilkins, Hans A. Krimm, Marshall W. Bautz, Samar Safi-Harb, Katsuhiro Hayashi, Tadayuki Takahashi, Masanobu Ozaki, Robert Petre, Takayoshi Kohmura, Aya Kubota, Elisa Costantini, Yoichi Yatsu, Kazutaka Yamaoka, Hirokazu Odaka, Frederick S. Porter, Satoru Katsuda, Greg Madejski, Hironori Matsumoto, Yoshiyuki Inoue, Knox S. Long, Takao Nakagawa, Irina Zhuravleva, Dan McCammon, Chris Done, Takeshi Nakamori, Yukikatsu Terada, Hiroshi Murakami, Hideyuki Mori, Shinya Saito, Makoto Sawada, Takashi Okajima, Randall K. Smith, Paolo De Coppi, Masachika Iwai, Makoto Yamauchi, Hiromitsu Takahashi, Kazuhisa Mitsuda, Hiroshi Tomida, Yuzuru Tawara, C. Megan Urry, Richard F. Mushotzky, Teruaki Enoto, Maurice A. Leutenegger, Nobuyuki Kawai, Norbert Schartel, Brian J. Williams, Meng P. Chiao, Kumi Ishikawa, G. Sato, Takao Kitaguchi, Maki Furukawa, Shiu-Hang Lee, Michael Loewenstein, Akihiro Furuzawa, Masayoshi Nobukawa, Tahir Yaqoob, Yasuharu Sugawara, Margherita Giustini, Jan-Willem den Herder, Tetsu Kitayama, Kenji Hamaguchi, Megumi Shidatsu, Felix Aharonian, Yasuo Tanaka, Luigi C. Gallo, Shinya Nakashima, Ann Hornschemeier, Aurora Simionescu, Andrea Goldwurm, Naomi Ota, Steven W. Allen, Eugenio Ursino, Richard L. Kelley, Takuya Miyazawa, Hiroshi Nakajima, Ilana M. Harrus, Takayuki Hayashi, David H. Lumb, Katja Pottschmidt, Ryo Iizuka, Liyi Gu, Hiroyasu Tajima, Takeshi Go Tsuru, Kosuke Sato, Shin Mineshige, P. J. Serlemitsos, Peter Kretschmar, Jon M. Miller, Yoshihiro Ueda, Tsunefumi Mizuno, Tsuneyoshi Kamae, Philippe Laurent, Ryuichi Fujimoto, Shin'ichiro Takeda, Gregory V. Brown, Koji Mori, Eric D. Miller, Hiromi Seta, Hirofumi Noda, Adam R. Foster, Poshak Gandhi, Yasushi Fukazawa, Cor P. de Vries, Ken Ebisawa, Yasuyuki T. Tanaka, Masanori Ohno, Christopher S. Reynolds, Massimiliano Galeazzi, Carlo Ferrigno, Masahiro Tsujimoto, Hiroyuki Uchida, Jelle de Plaa, John P. Hughes, Francesco Tombesi, Jelle Kaastra, Katsuji Koyama, Hiroshi Tsunemi, Yasunobu Uchiyama, Daniel Maier, Hajime Inoue, Lorella Angelini, Andrew C. Fabian, Shutaro Ueda, Ikuyuki Mitsuishi, Brian R. McNamara, Shu Koyama, Yuichi Terashima, Stéphane Paltani, Kiyoshi Hayashida, Yoshitomo Maeda, Isamu Hatsukade, Makoto Tashiro, Caroline A. Kilbourne, Esra Bulbul, Hisamitsu Awaki, Yang Soong, Takaaki Tanaka, Tadayasu Dotani, Kazuo Makishima, Megan E. Eckart, Takaya Ohashi, Jun Kataoka, R. Sato, Hideyo Kunieda, Lukasz Stawarz, Junko S. Hiraga, Magnus Axelsson, Noriko Y. Yamasaki, Yohko Tsuboi, Norbert Werner, Fumie Akimoto, Shigeo Yamauchi, Maxim Markevitch, Yuto Ichinohe, Akio Hoshino, Hideki Uchiyama, Takayuki Tamura, Shunji Kitamoto, Kazuhiro Nakazawa, Yuichi Kato, Aya Bamba, Roger Blandford, Yoh Takei, Yoshito Haba, Maria Chernyakova, Shin Watanabe, Edward M. Cackett, 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, 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)-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), 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 ), and Commissariat à l'énergie atomique et aux énergies alternatives ( CEA )

Subjects
[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, observational [methods], energy resolution, FOS: Physical sciences, Excitation temperature, helium, quantum number, clusters: individual (Perseus) [galaxies], 01 natural sciences, plasma: model, Ion, iron, Settore FIS/05 - Astronomia e Astrofisica, Ionization, Intracluster medium, gas, 0103 physical sciences, excited state, ionization, X-ray: emission, structure, plasma: thermal, cluster, 010303 astronomy & astrophysics, fine structure, Line (formation), High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, galaxies: clusters: individual (Perseus), central region, temperature, Astronomy and Astrophysics, Plasma, observatory, Temperature gradient, Space and Planetary Science, X-rays: galaxies: clusters, Excited state, galaxies: clusters [X-rays], ion, spectrometer, methods: observational, Atomic physics, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
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: 2017-12-14, 資料番号: SA1170336000

Published
2018

21. Glimpse of the highly obscured HMXB IGR J16318-4848 with Hitomi

Author

Hitomi Collaboration, Felix Aharonian, Hiroki Akamatsu, Fumie Akimoto, Steven W Allen, Lorella Angelini, Marc Audard, Hisamitsu Awaki, Magnus Axelsson, Aya Bamba, Marshall W Bautz, Roger Blandford, Laura W Brenneman, Gregory V Brown, Esra Bulbul, Edward M Cackett, Maria Chernyakova, Meng P Chiao, Paolo S Coppi, Elisa Costantini, Jelle de Plaa, Cor P de Vries, Jan-Willem den Herder, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E Eckart, Teruaki Enoto, Yuichiro Ezoe, Andrew C Fabian, Carlo Ferrigno, Adam R Foster, Ryuichi Fujimoto, Yasushi Fukazawa, Akihiro Furuzawa, Massimiliano Galeazzi, Luigi C Gallo, Poshak Gandhi, Margherita Giustini, Andrea Goldwurm, Liyi Gu, Matteo Guainazzi, Yoshito Haba, Kouichi Hagino, Kenji Hamaguchi, Ilana M Harrus, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Kiyoshi Hayashida, Junko S Hiraga, Ann Hornschemeier, Akio Hoshino, John P Hughes, Yuto Ichinohe, Ryo Iizuka, Hajime Inoue, Yoshiyuki Inoue, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Masachika Iwai, Jelle Kaastra, Tim Kallman, Tsuneyoshi Kamae, Jun Kataoka, Satoru Katsuda, Nobuyuki Kawai, Richard L Kelley, Caroline A Kilbourne, Takao Kitaguchi, Shunji Kitamoto, Tetsu Kitayama, Takayoshi Kohmura, Motohide Kokubun, Katsuji Koyama, Shu Koyama, Peter Kretschmar, Hans A Krimm, Aya Kubota, Hideyo Kunieda, Philippe Laurent, Shiu-Hang Lee, Maurice A Leutenegger, Olivier O Limousin, Michael Loewenstein, Knox S Long, David Lumb, Greg Madejski, Yoshitomo Maeda, Daniel Maier, Kazuo Makishima, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian R McNamara, Missagh Mehdipour, Eric D Miller, Jon M Miller, Shin Mineshige, Kazuhisa Mitsuda, Ikuyuki Mitsuishi, Takuya Miyazawa, Tsunefumi Mizuno, Hideyuki Mori, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard F Mushotzky, Takao Nakagawa, Hiroshi Nakajima, Takeshi Nakamori, Shinya Nakashima, Kazuhiro Nakazawa, Kumiko K Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Takaya Ohashi, Masanori Ohno, Takashi Okajima, Naomi Ota, Masanobu Ozaki, Frits Paerels, Stéphane Paltani, Robert Petre, Ciro Pinto, Frederick S Porter, Katja Pottschmidt, Christopher S Reynolds, Samar Safi-Harb, Shinya Saito, Kazuhiro Sakai, Toru Sasaki, Goro Sato, Kosuke Sato, Rie Sato, Makoto Sawada, Norbert Schartel, Peter J Serlemtsos, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall K Smith, Yang Soong, Łukasz Stawarz, Yasuharu Sugawara, Satoshi Sugita, Andrew Szymkowiak, Hiroyasu Tajima, Hiromitsu Takahashi, Tadayuki Takahashi, Shiníchiro Takeda, Yoh Takei, Toru Tamagawa, Takayuki Tamura, Takaaki Tanaka, Yasuo Tanaka, Yasuyuki T Tanaka, Makoto S Tashiro, Yuzuru Tawara, Yukikatsu Terada, Yuichi Terashima, Francesco Tombesi, Hiroshi Tomida, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Go Tsuru, Hiroyuki Uchida, Hideki Uchiyama, Yasunobu Uchiyama, Shutaro Ueda, Yoshihiro Ueda, Shiníchiro Uno, C Megan Urry, Eugenio Ursino, Shin Watanabe, Norbert Werner, Dan R Wilkins, Brian J Williams, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Y Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Yoichi Yatsu, Daisuke Yonetoku, Irina Zhuravleva, Abderahmen Zoghbi, Nozomi Nakaniwa, 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, 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, 01 natural sciences, Spectral line, X-rays: binaries, general [binaries], Settore FIS/05 - Astronomia e Astrofisica, individual (IGR J16318-4848) [stars], Ionization, 0103 physical sciences, Continuum (set theory), 010306 general physics, Absorption (electromagnetic radiation), 010303 astronomy & astrophysics, Line (formation), Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Scattering, stars: individual (IGR J16318-4848), Astronomy and Astrophysics, binaries: general, Space and Planetary Science, binaries [X-rays], Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Energy (signal processing), Doppler broadening
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; 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; 中庭, 望）, Number of authors: Hitomi Collaboration 193 (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.; Nakaniwa, Nozomi), Accepted: 2017-11-02, 資料番号: SA1170342000

Published
2018

22. Hitomi X-ray observation of the pulsar wind nebula G21.5$−$0.9

Author

Tsuneyoshi Kamae, Chris Done, Takeshi Nakamori, Hirofumi Noda, Philippe Laurent, Gregory V. Brown, Masahiro Tsujimoto, Luigi C. Gallo, Andrea Goldwurm, Akio Hoshino, Edward M. Cackett, Makoto Tashiro, Yoichi Yatsu, Kazutaka Yamaoka, Makoto Yamauchi, Makoto Sawada, Esra Bulbul, Yasuo Tanaka, Katsuji Koyama, Hiromitsu Takahashi, Kazuhisa Mitsuda, Tsunefumi Mizuno, Jon M. Miller, Takashi Okajima, Katsuhiro Hayashi, Yang Soong, Daisuke Yonetoku, Peter J. Serlemtsos, Yoshitaka Ishisaki, Hans A. Krimm, Akihiro Furuzawa, Olivier Limousin, Shiu-Hang Lee, Takao Kitaguchi, Laura Brenneman, Hideki Uchiyama, Samar Safi-Harb, Koji Mukai, Poshak Gandhi, Yasushi Fukazawa, Abderahmen Zoghbi, Ann Hornschemeier, Marc Audard, Hiroki Akamatsu, Andrew Szymkowiak, D. Lumb, Koji Mori, Hiroshi Tsunemi, Kazuhiro Nakazawa, Jan-Willem den Herder, Robert Petre, Shinya Saito, Aya Kubota, Takayuki Hayashi, Shinya Nakashima, Carlo Ferrigno, Eric D. Miller, Shin'ichiro Uno, Masachika Iwai, Dan McCammon, Takao Nakagawa, Irina Zhuravleva, Satoshi Sugita, Naomi Ota, Nozomu Nakaniwa, Ikuyuki Mitsuishi, Richard L. Kelley, Missagh Mehdipour, Motohide Kokubun, Dan R. Wilkins, Tadayuki Takahashi, Marshall W. Bautz, Francesco Tombesi, Jelle Kaastra, Katja Pottschmidt, Shunji Kitamoto, Masanobu Ozaki, Yuzuru Tawara, Margherita Giustini, Ken Ebisawa, Ryo Iizuka, Greg Madejski, Takeshi Go Tsuru, Shin Mineshige, Toshiki Sato, Liyi Gu, Hiroyasu Tajima, Aya Bamba, Roger Blandford, Yuichi Terashima, C. Megan Urry, Richard F. Mushotzky, Peter Kretschmar, Kosuke Sato, Knox S. Long, Steven W. Allen, Hideyuki Mori, Hiroyuki Uchida, Yoshihiro Ueda, Kyoko Matsushita, Nobuyuki Kawai, Brian J. Williams, Hiroshi Murakami, Tetsu Kitayama, Randall K. Smith, Hiroshi Tomida, Norbert Schartel, Toru Tamagawa, Łukasz Stawarz, Rie Sato, Hiroya Yamaguchi, Hisamitsu Awaki, Takaaki Tanaka, Frits Paerels, Tadayasu Dotani, Yasuharu Sugawara, Ciro Pinto, Paolo Coppi, Kiyoshi Hayashida, Frederick S. Porter, Matteo Guainazzi, Isamu Hatsukade, Toru Sasaki, Megan E. Eckart, Takaya Ohashi, Yasunobu Uchiyama, Kouichi Hagino, Yuichiro Ezoe, Megumi Shidatsu, Kumi Ishikawa, Takayuki Tamura, Stéphane Paltani, Hideyo Kunieda, Eugenio Ursino, Adam R. Foster, Ryuichi Fujimoto, Caroline A. Kilbourne, Yoh Takei, Yoshito Haba, Noriko Y. Yamasaki, Elisa Costantini, Shin'ichiro Takeda, Takayoshi Kohmura, Maria Chernyakova, Shin Watanabe, Aurora Simionescu, Hiroshi Nakajima, Satoru Katsuda, Magnus Axelsson, Meng P. Chiao, Jelle de Plaa, Yasuyuki T. Tanaka, Massimiliano Galeazzi, Yohko Tsuboi, Norbert Werner, Andrew C. Fabian, Kazuo Makishima, Fumie Akimoto, Jun Kataoka, Brian R. McNamara, Shigeo Yamauchi, Maxim Markevitch, Yuto Ichinohe, Shu Koyama, Masayoshi Nobukawa, Tahir Yaqoob, Hironori Matsumoto, Yoshitomo Maeda, Cor P. de Vries, Benson Guest, Masanori Ohno, Christopher S. Reynolds, Hirokazu Odaka, Michael Loewenstein, Kenji Hamaguchi, Ilana M. Harrus, Manabu Ishida, Yoshiyuki Inoue, Yukikatsu Terada, Hiroaki Murakami, Timothy R. Kallman, Takuya Miyazawa, Shinya Yamada, Kazuhiro Sakai, Felix Aharonian, Junko S. Hiraga, Hiromi Seta, Teruaki Enoto, John P. Hughes, Daniel Maier, Hajime Inoue, Lorella Angelini, Maurice A. Leutenegger, Kumiko K. Nobukawa, Goro Sato, Shutaro Ueda, 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, 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)-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 ), 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
Photon, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, pulsars: individual (PSRJ1833-1034), 01 natural sciences, Pulsar wind nebula, Power law, Spectral line, 010309 optics, Settore FIS/05 - Astronomia e Astrofisica, Pulsar, 0103 physical sciences, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ISM: supernova remnants, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Spectrometer, supernova remnants [ISM], individual (PSR J1833-1034) [pulsars], Astronomy and Astrophysics, ISM: individual objects (G21.5-0.9), Space and Planetary Science, Spectral energy distribution, Astrophysics - High Energy Astrophysical Phenomena, individual objects (G21.5-0.9) [ISM], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

著者人数: 196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; 佐藤, 寿紀; 中庭, 望), 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.; Sato, Toshiki; Nakaniwa, Nozomu), Accepted: 2018-02-14, 資料番号: SA1180104000

Published
2018

23. Hitomi observation of radio galaxy NGC 1275: The first X-ray microcalorimeter spectroscopy of Fe-K$\alpha$ line emission from an active galactic nucleus

Author

Yasuo Tanaka, Hideki Uchiyama, Takao Nakagawa, Margherita Giustini, Shunji Kitamoto, Peter J. Serlemitsos, Marc Audard, Jon M. Miller, Kumi Ishikawa, Hirokazu Odaka, Yuzuru Tawara, Takeshi Go Tsuru, Kosuke Sato, Koji Mukai, Abderahmen Zoghbi, Kazuhiro Nakazawa, Yasuharu Sugawara, Yoshihiro Ueda, C. Megan Urry, Richard F. Mushotzky, Nobuyuki Kawai, Ann Hornschemeier, Katja Pottschmidt, Aya Kubota, Hironori Matsumoto, Richard L. Kelley, Brian J. Williams, Luigi C. Gallo, Tetsu Kitayama, Megumi Shidatsu, Felix Aharonian, Shin'ichiro Takeda, Paolo De Coppi, Teruaki Enoto, David H. Lumb, Shin Mineshige, Kyoko Matsushita, Maurice A. Leutenegger, Masayoshi Nobukawa, Tahir Yaqoob, Irina Zhuravleva, Olivier Limousin, Steven W. Allen, Eugenio Ursino, Toru Tamagawa, Missagh Mehdipour, Adam R. Foster, Jan-Willem den Herder, Takayuki Hayashi, Rie Sato, Peter Kretschmar, Taiki Kawamuro, Aurora Simionescu, Makoto Yamauchi, Hiromitsu Takahashi, Manabu Ishida, Kazuhisa Mitsuda, Shiu-Hang Lee, Michael Loewenstein, Frits Paerels, Tsuneyoshi Kamae, Meng P. Chiao, Takao Kitaguchi, Kenji Hamaguchi, Aya Bamba, Matteo Guainazzi, Kouichi Hagino, Philippe Laurent, Jelle de Plaa, Hiroshi Tsunemi, Kazuo Makishima, Toru Sasaki, Roger Blandford, Koji Mori, Timothy R. Kallman, Ilana M. Harrus, Ikuyuki Mitsuishi, Laura Brenneman, Hiroki Akamatsu, Francesco Tombesi, Daisuke Yonetoku, Jelle Kaastra, Yoshitaka Ishisaki, Makoto Tashiro, Andrew Szymkowiak, Satoru Katsuda, Esra Bulbul, Hans A. Krimm, Eric D. Miller, Shin'ichiro Uno, Andrea Goldwurm, Hirofumi Noda, Knox S. Long, Samar Safi-Harb, Yoshitomo Maeda, Stephane Ṕaltani, Carlo Ferrigno, Yang Soong, Liyi Gu, Satoshi Sugita, Hiroshi Nakajima, Cor P. de Vries, Marshall W. Bautz, Robert Petre, Yuichi Terashima, Masanori Ohno, Christopher S. Reynolds, Shinya Nakashima, Shinya Saito, Hisamitsu Awaki, Yoh Takei, Yoshito Haba, Tsunefumi Mizuno, Masanobu Ozaki, Katsuji Koyama, Kiyoshi Hayashida, Takaaki Tanaka, Yuichiro Ezoe, Masachika Iwai, Tadayasu Dotani, Jun Kataoka, Naomi Ota, Hiroya Yamaguchi, Yohko Tsuboi, Takuya Miyazawa, Dan R. Wilkins, Norbert Werner, Fumie Akimoto, Motohide Kokubun, Kumiko K. Nobukawa, Gregory V. Brown, Elisa Costantini, Megan E. Eckart, Shigeo Yamauchi, Maxim Markevitch, Yuto Ichinohe, Tadayuki Takahashi, Goro Sato, Takaya Ohashi, Poshak Gandhi, Katsuhiro Hayashi, Yasushi Fukazawa, Hiroyasu Tajima, Maria Chernyakova, Shin Watanabe, Hideyo Kunieda, Greg Madejski, Dan McCammon, Shutaro Ueda, Masahiro Tsujimoto, Ryuichi Fujimoto, Junko S. Hiraga, Magnus Axelsson, Lukasz Stawarz, Hiroshi Murakami, Noriko Y. Yamasaki, Frederick S. Porter, Hiromi Seta, Ken Ebisawa, Yasuyuki T. Tanaka, Massimiliano Galeazzi, Hideyuki Mori, Hiroshi Tomida, Randall K. Smith, Edward M. Cackett, Hiroyuki Uchida, Chris Done, Takayuki Tamura, Norbert Schartel, John P. Hughes, Daniel Maier, Hajime Inoue, Lorella Angelini, Takeshi Nakamori, Ryo Iizuka, Andrew C. Fabian, Yoichi Yatsu, Kazutaka Yamaoka, Brian R. McNamara, Ciro Pinto, Shu Koyama, Makoto Sawada, Yasunobu Uchiyama, Takashi Okajima, Akihiro Furuzawa, Takayoshi Kohmura, Isamu Hatsukade, Caroline A. Kilbourne, Shinya Yamada, Kazuhiro Sakai, Yoshiyuki Inoue, Yukikatsu Terada, Akio Hoshino, 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
Active galactic nucleus, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, individual (NGC 1275) [galaxies], [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], galaxies: active, observational [methods], galaxies: radio galaxy, radio galaxy [galaxies], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 010309 optics, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, galaxies: individual (NGC 1275), Spectroscopy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Astronomy and Astrophysics, Torus, Galaxy, galaxies [X-rays], Full width at half maximum, X-rays: galaxies, Space and Planetary Science, active [galaxies], H-alpha, methods: observational, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Equivalent width
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; 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; Lee, Shiu-Hang; 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; Hagino, Kouichi; Hayashi, Katsuhiro; Iizuka, Ryo; Inoue, Yoshiyuki; Ishida, Manabu; Ishikawa, Kumi; Iwai, Masachika; Kokubun, Motohide; Koyama, Shu; Lee, Shiu-Hang; 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: 2017-11-16, 資料番号: SA1170338000

Published
2018

24. Origin of the low-temperature plasma in the Galactic center X-ray emission

Author

Katsuji Koyama, Shigeo Yamauchi, Kumiko K. Nobukawa, Hideki Uchiyama, Miku Shimizu, and Masayoshi Nobukawa

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Galactic Center, X-ray, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Plasma, 01 natural sciences, Spectral line, Stars, Space and Planetary Science, 0103 physical sciences, Thermal, Surface brightness, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Line (formation)
Abstract

The Galactic Center X-ray Emission (GCXE) is composed of high temperature (7 keV) and low temperature (1 keV) plasmas (HTP and LTP, respectively). The global structure of the HTP is roughly uniform over the Galactic center (GC) region, and the origin of the HTP has been extensively studied. On the other hand, the LTP is more clumpy, and the origin has not been studied in detail. In the S XV He alpha line map, a pair of horn-like soft diffuse sources are seen at the symmetric positions with respect to Sagittarius A^{star}. The X-ray spectra of the pair are well represented by an absorbed thin thermal plasma model of a temperature and N_H of 0.6-0.7 keV and 4x10^{22} cm^{-2}, respectively. The N_H values indicate that the pair are located near at the GC. Then the dynamical time scales of the pair are 10^{5} yr. The Si and S abundances and the surface brightnesses in the S XV He alpha line band are 0.7-1.2 and 0.6-1.3 solar, and (2.0-2.4)x10^{-15} erg s^{-1} cm^{-2} arcmin^{-2}, respectively. The temperature, abundances, and surface brightness are similar to those of the LTP in the GCXE, while the abundances are far larger than those of known point sources, typically coronal active stars and RS CVn-type active binaries. Based on these results, possible origin of the LTP is discussed., Comment: Accepted for publication in PASJ

Published
2018
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25. Solar abundance ratios of the iron-peak elements in the Perseus cluster

Author

Yasuo Tanaka, Hideki Uchiyama, Hironori Matsumoto, T. Hayashi, Cor P. de Vries, Shin'ichiro Uno, Shinya Nakashima, Ann Hornschemeier, Satoshi Sugita, Naomi Ota, Masanori Ohno, Christopher S. Reynolds, Megumi Shidatsu, Kumi Ishikawa, Lukasz Stawarz, Hiroshi Murakami, Shunji Kitamoto, Hiroshi Tomida, Masanobu Ozaki, Katsuji Koyama, Kenji Hamaguchi, Kazuhiro Nakazawa, Hiroyasu Tajima, Katja Pottschmidt, Marshall W. Bautz, Daisuke Yonetoku, Yoshitaka Ishisaki, Shin Mineshige, Hans A. Krimm, Marc Audard, Motohide Kokubun, Chris Done, Peter Kretschmar, Katsuhiro Hayashi, Jon M. Miller, Samar Safi-Harb, Hiroshi Tsunemi, Aya Bamba, Ikuyuki Mitsuishi, Takeshi Nakamori, Dan McCammon, Hiromi Seta, Olivier Limousine, Roger Blandford, Hirokazu Odaka, Andrew C. Fabian, Yohko Tsuboi, Norbert Werner, Fumie Akimoto, Shigeo Yamauchi, Hiroya Yamaguchi, Daniel R. Wik, David H. Lumb, Yuichi Terashima, Richard L. Kelley, Hiroyuki Uchida, Kiyoshi Hayashida, Shinya Yamada, Brian R. McNamara, Kyoko Matsushita, Shu Koyama, John P. Hughes, Maxim Markevitch, Yuto Ichinohe, Makoto Yamauchi, Hiromitsu Takahashi, Kazuhisa Mitsuda, Shinya Saito, Yasunobu Uchiyama, Kouichi Hagino, C. Megan Urry, Shiu-Hang Lee, Missagh Mehdipour, Kazuhiro Sakai, Michael Loewenstein, Yuichiro Ezoe, Masachika Iwai, Hajime Inoue, Yoh Takei, Abderahmen Zoghbi, Ciro Pinto, Yoshito Haba, Jun Kataoka, Richard F. Mushotzky, Toru Tamagawa, Gregory V. Brown, Hiroshi Nakajima, Steven W. Allen, Lorella Angelini, Kumiko K. Nobukawa, Junko S. Hiraga, Magnus Axelsson, Takuya Miyazawa, Tsunefumi Mizuno, Meng P. Chiao, Stéphane Paltani, Rie Sato, Ryuichi Fujimoto, Peter J. Serlemitsos, Ryo Iizuka, Goro Sato, Nobuyuki Kawai, Yoichi Yatsu, Brian J. Williams, Kazutaka Yamaoka, Maria Chernyakova, Eric D. Miller, Ilana M. Harrus, Frits Paerels, Poshak Gandhi, Yasushi Fukazawa, Shin Watanabe, Ken Ebisawa, Yasuyuki T. Tanaka, Shutaro Ueda, Tetsu Kitayama, P. Laurent, Massimiliano Galeazzi, Koji Mukai, Makoto Tashiro, Masahiro Tsujimoto, Edward M. Cackett, Matteo Guainazzi, Frederick S. Porter, Takeshi Go Tsuru, Kosuke Sato, Aya Kubota, Timothy R. Kallman, Makoto Sawada, Esra Bulbul, Paolo De Coppi, Felix Aharonian, Takao Kitaguchi, Teruaki Enoto, Kazuo Makishima, Toru Sasaki, Maurice A. Leutenegger, Takao Nakagawa, Masayoshi Nobukawa, Takayoshi Kohmura, Laura Brenneman, Takayuki Tamura, Irina Zhuravleva, Tahir Yaqoob, Yang Soong, Tsuneyoshi Kamae, Takashi Okajima, Yoshihiro Ueda, Yasuharu Sugawara, Eugenio Ursino, Adam R. Foster, Manabu Ishida, Isamu Hatsukade, Satoru Katsuda, Knox S. Long, Yoshiyuki Inoue, Luigi C. Gallo, Akihiro Furuzawa, Hirofumi Noda, Koji Mori, Caroline A. Kilbourne, Yukikatsu Terada, Carlo Ferrigno, Hiroki Akamatsu, Andrew Szymkowiak, Dan R. Wilkins, Daniel Maier, Tadayuki Takahashi, Robert Petre, Margherita Giustini, Elisa Costantini, Jan-Willem den Herder, Greg Madejski, Francesco Tombesi, Jelle Kaastra, Hideyuki Mori, Randall K. Smith, Norbert Schartel, Shin'ichiro Takeda, Aurora Simionescu, Jelle de Plaa, Andrea Goldwurm, Megan E. Eckart, Takaya Ohashi, Hideyo Kunieda, Noriko Y. Yamasaki, Y. Tawara, Yoshitomo Maeda, Hisamitsu Awaki, Takaaki Tanaka, Tadayasu Dotani, Liyi Gu, Akio Hoshino, 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), and Apollo - University of Cambridge Repository

Subjects
Milky Way, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Settore FIS/05 - Astronomia e Astrofisica, Nucleosynthesis, Intracluster medium, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Solar mass, Multidisciplinary, White dwarf, Astronomy, Iron peak, Hitomi Collaboration, Supernova, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
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, 將親; 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.), Accepted: 2017-09-21, 資料番号: SA1170128000

Published
2017

26. First discovery of iron line emission generated by low-energy cosmic rays

Author

Kumiko K. Nobukawa, Hideki Uchiyama, Katsuji Koyama, Shigeo Yamauchi, and Masayoshi Nobukawa

Subjects
Physics, Interstellar medium, Supernova, Astrophysics::High Energy Astrophysical Phenomena, Molecular cloud, Galactic Center, Physics::Accelerator Physics, Cosmic ray, Astrophysics, Electron, Astrophysics::Galaxy Astrophysics, Galaxy, Line (formation)
Abstract

Cosmic rays (CRs) in our galaxy are thought to be generated via diffusive shock acceleration. Gamma-ray observations have revealed that protons and/or electrons are accelerated to energies up to 100 TeV in supernova remnants (SNRs), and hence SNRs are the most plausible source of CR production. Whereas low-energy cosmic rays (LECRs) below the MeV band have important information on the initial acceleration mechanism, there has been very little information on LECRs due to lack of an effective probe. Interacting with neutral iron atoms in the interstellar medium, LECRs produce fluorescent X-ray line emission at 6.40 keV. The 6.40 keV line observation can be a unique probe to investigate LECRs. Analyzing the Suzaku data, we discovered the 6.40 keV line emission from several SNRs interacting with molecular clouds (W28, W44, Kes 67, Kes 69, Kes 78, Kes 79, and 3C391). The 6.40 keV line emission would be produced by MeV protons with the energy density of $>10$ eV cm$^{-3}$. Furthermore, we discovered the 6.40 keV line emission from a giant molecular cloud located near the Galactic center. The energy density of MeV protons is estimated to be 80 eV cm$^{-3}$. The diffusion length of MeV protons is only a few tens of parsecs, and thus the MeV protons should be produced in situ. Surprisingly, there is no SNR in the vicinity. The LECRs would possibly be generated by stochastic acceleration via Alfven turbulence.

Published
2017

27. Measurement of Low-Energy Cosmic Rays via the Neutral Iron Line

Author

Shigetaka Saji, Kumiko K. Nobukawa, Arisa Hirayama, Masayoshi Nobukawa, Shigeo Yamauchi, Katsuji Koyama, and Hironori Matsumoto

Subjects
Physics, History, Low energy, Cosmic ray, Astrophysics, Computer Science Applications, Education, Line (formation)
Published
2019

28. Ray-tracing simulation and in-orbit performance of the ASTRO-H hard x-ray telescope (HXT)

Author

Satoshi Sugita, Kazunori Ishibashi, Ryo Iizuka, Tatsuro Kosaka, Yoshitomo Maeda, Yutaka Suzuki, Yoshito Haba, Hisamitsu Awaki, Housei Nagano, Masayuki Itoh, K. Uesugi, Yoshiharu Namba, Takuya Miyazawa, Hideyuki Mori, Hideyo Kunieda, Keisuke Tamura, Y. Ogasaka, Shigeo Yamauchi, Yuzuru Tawara, Ikuyuki Mitsuishi, Keiji Ogi, Manabu Ishida, Takayuki Hayashi, Takashi Okajima, Akihiro Furuzawa, and Hironori Matsumoto

Subjects
010302 applied physics, Physics, X-ray astronomy, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, X-ray telescope, Astrophysics, Orbital mechanics, 01 natural sciences, Pulsar wind nebula, Encircled energy, law.invention, 010309 optics, Telescope, law, 0103 physical sciences, Ray tracing (graphics), Satellite
Abstract

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

Published
2016

29. Scale heights and equivalent widths of the iron K-shell lines in the Galactic diffuse X-ray emission

Author

Hideki Uchiyama, Katsuji Koyama, Kumiko K. Nobukawa, Shigeo Yamauchi, and Masayoshi Nobukawa

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Galactic ridge, Galactic Center, Electron shell, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Spectral line, Space and Planetary Science, Bulge, 0103 physical sciences, K-alpha, Disc, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Line (formation)
Abstract

This paper reports the analysis of the X-ray spectra of the Galactic diffuse X-ray emission (GDXE) in the Suzaku archive. The fluxes of the Fe I K alpha (6.4 keV), Fe XXV,He alpha (6.7 keV) and Fe XXVI Ly alpha (6.97 keV) lines are separately determined. From the latitude distributions, we confirm that the GDXE is decomposed into the Galactic center (GCXE), the Galactic bulge (GBXE) and the Galactic ridge (GRXE) X-ray emissions. The scale heights (SHs) of the Fe XXV He alpha line of the GCXE, GBXE and GRXE are determined to be ~40, ~310 and ~140 pc, while those of the Fe I K alpha line are ~30, ~160 and ~70 pc, respectively. The mean equivalent widths (EWs) of the sum of the Fe XXV He alpha and Fe XXVI Ly alpha lines are ~750 eV, ~600 eV and ~550 eV, while those of the Fe I K alpha line are ~150~eV, ~60~eV and ~100~eV for the GCXE, GBXE and GRXE, respectively. The origin of the GBXE, GRXE and GCXE is separately discussed based on the new results of the SHs and EWs, in comparison with those of the Cataclysmic Variables (CVs), Active Binaries (ABs) and Coronal Active stars (CAs)., Comment: Accepted for publication in PASJ

Published
2016
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30. The ASTRO-H (Hitomi) x-ray astronomy satellite

Author

Yasuharu Sugawara, Luigi C. Gallo, Manabu Ishida, Hiroya Yamaguchi, Makoto Yamauchi, Hiromitsu Takahashi, Kazuhisa Mitsuda, Eric J. Miller, Ciro Pinto, Grzegorz Madejski, Meng P. Chiao, Yoshiharu Namba, Kumiko K. Nobukawa, Goro Sato, Harvey Moseley, Takayoshi Kohmura, Mina Ogawa, Greg Brown, Kevin R. Boyce, Missagh Mehdipour, Shutaro Ueda, Satoru Katsuda, Philipp Azzarello, Shin'ichiro Uno, Atsushi Wada, Takao Kitaguchi, Knox S. Long, Yohko Tsuboi, Nobutaka Bando, Shin-ichiro Sakai, Hajime Inoue, Masayuki Itoh, Kazuyuki Hirose, Norbert Werner, Fumie Akimoto, Timothy R. Kallman, Shigeo Yamauchi, Maxim Markevitch, Yuto Ichinohe, Naohisa Anabuki, Satoshi Sugita, Yoshiyuki Inoue, Olivier Limousin, Meg Urry, Kouichi Hagino, Akio Hoshino, Kumi Ishikawa, Cor P. de Vries, Teruaki Enoto, Yasuo Tanaka, M. Pohl, Masanobu Ozaki, Kenji Minesugi, Peter Shirron, Maurice A. Leutenegger, Koji Mori, Hideki Uchiyama, Yukikatsu Terada, D. Haas, Keith A. Arnaud, Masanori Ohno, Christopher S. Reynolds, Hiromi Seta, Yusuke Nishioka, Carlo Ferrigno, Edgar Canavan, Katsuji Koyama, Daniel R. Wik, Shunji Kitamoto, Keisuke Shinozaki, Katsuhiro Hayashi, Dan McCammon, David H. Lumb, Kyoko Matsushita, Hiroyuki Uchida, John P. Hughes, Daniel Maier, Lorella Angelini, Taro Kawano, Cynthia Simmons, Shiro Ueno, Koji Mukai, Abderahmen Zoghbi, Makoto Asai, Toru Tamagawa, Rie Sato, Keisuke Tamura, Yuzuru Tawara, Łukasz Stawarz, Motohide Kokubun, Hiroshi Murakami, Hiroshi Tomida, F. Scott Porter, Hiroshi Tsunemi, Ikuyuki Mitsuishi, Michael J. DiPirro, Richard F. Mushotzky, Nobuyuki Kawai, Brian J. Williams, Richard L. Kelley, Hirokazu Odaka, Matteo Guainazzi, Kazuo Makishima, Yuichiro Ezoe, Takahiro Yamada, Hiroki Akamatsu, Andrew Szymkowiak, Philippe Laurent, James Pontius, Yasunobu Uchiyama, Tetsu Kitayama, Megumi Shidatsu, Felix Aharonian, Shigeo Kawasaki, Takanobu Shimada, Laura Brenneman, Toru Sasaki, Isamu Hatsukade, A. L. King, Takuya Miyazawa, Toshio Nakano, Atsumasa Yoshida, Robert Petre, Shinya Yamada, Stéphane Paltani, Eugenio Ursino, Adam R. Foster, Takayuki Hayashi, Shiu-Hang Lee, Toshio Murakami, Chris Done, Takeshi Nakamori, Kazuhiro Sakai, Ryo Nagino, Yuichi Terashima, Caroline A. Kilbourne, Michael Loewenstein, Shin Mineshige, Peter Kretschmar, John P. Doty, Candace Masters, Yoichi Sato, Junko S. Hiraga, Magnus Axelsson, Kenji Hamaguchi, Marshall W. Bautz, Junichiro Katsuta, Hiroaki Sameshima, Ilana M. Harrus, Thomas G. Bialas, Elisa Costantini, Daniel S. McGuinness, Yoichi Yatsu, Kazutaka Yamaoka, Naoko Iwata, Mark O. Kimball, Arvind Parmar, Yasuko Shibano, Norbert Schartel, Helen Russell, Gary A. Sneiderman, Steve Allen, Kiyoshi Hayashida, Makoto Sawada, Megan E. Eckart, Takaya Ohashi, Dmitry Khangulyan, Kosei Ishimura, Tatsuro Kosaka, Andrea Goldwurm, Takashi Okajima, Hirofumi Noda, Franco Moroso, F. B. S. Paerels, Hiroyuki Sugita, Alex Koujelev, Masaharu Nomachi, Tomomi Watanabe, Marc Audard, Tsunefumi Mizuno, Hideyo Kunieda, Keiji Ogi, Akihiro Furuzawa, Brian D. Ramsey, Masayoshi Nobukawa, Shinya Saito, Poshak Gandhi, Yasushi Fukazawa, Liyi Gu, Peter J. Serlemitsos, Noriko Y. Yamasaki, Tsuyoshi Okazaki, Takeshi Go Tsuru, Kosuke Sato, Aya Kubota, Chris Jewell, Yoshitomo Maeda, Yoshihiro Ueda, Shinya Nakashima, Irina Zhuravleva, Andrew C. Fabian, Tahir Yaqoob, Housei Nagano, Erin Kara, Brian R. McNamara, Naomi Ota, Shu Koyama, Joseph Miko, Madoka Kawaharada, Hisamitsu Awaki, Steve O'Dell, Takaaki Tanaka, Hironori Matsumoto, Tadayasu Dotani, Ken Ebisawa, Dan R. Wilkins, Hiroyasu Tajima, Yasuyuki T. Tanaka, Massimiliano Galeazzi, Chikara Natsukari, Jan-Willem den Herder, Tadayuki Takahashi, Francois Lebrun, Hiroshi Nakajima, Yoh Takei, Hideyuki Mori, Yoshito Haba, Jun Kataoka, Randall K. Smith, Atsushi Okamoto, Maria Chernyakova, Shin Watanabe, Edward M. Cackett, Shin'ichiro Takeda, Takayuki Tamura, Francesco Tombesi, Jelle Kaastra, Maki Shida, Chris Baluta, Kirk Gilmore, Aurora Simionescu, Ann Hornschemeier, Kazuhiro Nakazawa, Jelle de Plaa, Naoko Iyomoto, Atsushi Harayama, Aya Bamba, Katja Pottschmidt, Roger Blandford, Kazunori Ishibashi, Makoto Tashiro, Esra Bulbul, Yang Soong, Paolo De Coppi, Daisuke Yonetoku, Yoshitaka Ishisaki, Hans A. Krimm, Samar Safi-Harb, Masahiro Tsujimoto, Ryuichi Fujimoto, Takao Nakagawa, Hiroyuki Ogawa, Margherita Giustini, Tuneyoshi Kamae, Takayuki Yuasa, Ryo Iizuka, Masayuki Ohta, Jon M. Miller, and Theodore Muench

Subjects
Physics, X-ray astronomy, Spacecraft, business.industry, Astronomy, High resolution, First light, Gamma-ray astronomy, 01 natural sciences, Spacecraft system, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Satellite, 010306 general physics, business, 010303 astronomy & astrophysics
Abstract

The Hitomi (ASTRO-H) mission is the sixth Japanese X-ray astronomy satellite developed by a large international collaboration, including Japan, USA, Canada, and Europe. The mission aimed to provide the highest energy resolution ever achieved at E > 2 keV, using a microcalorimeter instrument, and to cover a wide energy range spanning four decades in energy from soft X-rays to gamma-rays. After a successful launch on 2016 February 17, the spacecraft lost its function on 2016 March 26, but the commissioning phase for about a month provided valuable information on the on-board instruments and the spacecraft system, including astrophysical results obtained from first light observations. The paper describes the Hitomi (ASTRO-H) mission, its capabilities, the initial operation, and the instruments/spacecraft performances confirmed during the commissioning operations for about a month.

Published
2016

31. Suzaku observations of two diffuse hard X-ray source regions, G22.0+0.0 and G23.5+0.1

Author

Shigeo Yamauchi, Aya Bamba, and Mayu Sumita

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Photon, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Spectral properties, X-ray, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Thermal emission, Astrophysics::Cosmology and Extragalactic Astrophysics, Galactic plane, 01 natural sciences, Spectral line, Pulsar, Space and Planetary Science, 0103 physical sciences, Thermal, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

G22.0+0.0 and G23.5+0.1 are diffuse hard X-ray sources discovered in the ASCA Galactic Plane Survey. We present Suzaku results of spectral analysis for these sources. G22.0+0.0 is confirmed to be a largely extended emission. The spectra were represented by a highly absorbed power-law model with a photon index of 1.7+/-0.3 and a moderately absorbed thermal emission with a temperature of 0.34^{+0.11}_{-0.08} keV. The difference in the N_{H} values between the two components suggests that the thermal component is unrelated with the power-law component and is a foreground emission located in the same line-of-sight. G23.5+0.1 is an extended source with a size of 3'.5. The spectra were fitted with an absorbed power-law model with a photon index of 2.4^{+0.5}_{-0.4}. The spatial and spectral properties show that both are candidates of old pulsar wind nebulae (PWNe). In addition to the extended sources, we analyzed spectra of three point sources found in the observed fields. Based on the spectral features, we discuss origin of the sources., Accepted for publication in PASJ

Published
2015

32. Iron emission line from the spiral galaxy M101

Author

Shigeo Yamauchi

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Spiral galaxy, 010308 nuclear & particles physics, Space and Planetary Science, 0103 physical sciences, FOS: Physical sciences, Astronomy and Astrophysics, Emission spectrum, Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, 01 natural sciences
Abstract

Archival Suzaku data of the face-on spiral galaxy M101 were analyzed. An intense emission line at 6.72^{+0.10}_{-0.12} keV was detected in the central region. This line is identified with a K-line from He-like iron, which indicates the existence of a thin thermal plasma with a temperature of several keV. The iron line luminosity within the central 5 arcmin radius region is estimated to be (2-12)x10^{37} erg s^{-1}. The origin of the iron emission line is discussed., Accepted for publication in PASJ

Published
2015

33. A New Candidate of an X-Ray Luminous Cluster of Galaxies behind the Galactic Plane

Author

Aya Bamba, Shigeo Yamauchi, and Katsuji Koyama

Subjects
Physics, Luminous infrared galaxy, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galactic plane, Space and Planetary Science, Galaxy group, Elliptical galaxy, Brightest cluster galaxy, Disc, Astrophysics::Galaxy Astrophysics, Galaxy cluster
Abstract

We present Suzaku results of an X-ray source, AX J185905+0333, discovered in the ASCA galactic plane survey. The radial profile of AX J185905+0333 is larger than that of the point-spread function. No intensity variation was found during the observation. These facts indicate that AX J185905+0333 is an extended source. A large low-energy absorption, equivalent to NH of (8–10) 10cm , was found, which supports that AX J185905+0333 is an extragalactic object behind the galactic plane. The X-ray spectrum exhibits a clear emission line at 4.82 keV, and is represented by a thin-thermal plasma model of 6.6 keV temperature with a redshift of 0.391. Then, the X-ray luminosity was calculated to be 2.7 10 erg s . These results strongly support that AX J185905+0333 is an X-ray luminous cluster of galaxies behind the galactic plane.

Published
2011

34. A New Candidate of a Cluster of Galaxies, 2XMM J045637.2+522411

Author

Aya Bamba, M. Ueno, Shigeo Yamauchi, and Katsuji Koyama

Subjects
Physics, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, Low-ionization nuclear emission-line region, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Light curve, Spectral line, Space and Planetary Science, Emission spectrum, Supernova remnant, Galaxy cluster, Line (formation)
Abstract

We present XMM-Newton and Suzaku results of an X-ray source, 2XMM J045637.2+522411, found during an observation of a galactic supernova remnant (SNR), G156.2+5.7. By comparing its radial profile with the point-spread function, we found that 2XMM J045637.2+522411 is an extended source. X-ray spectra exhibited a line-like structure at 5.7-5.8 keV. Since no abundant element emits an X-ray line at 5-6 keV in the rest-frame, and the most intense emission line in the 5-7 keV energy band is a Fe-K line, the line is likely to be a redshifted Fe-K line. The overall spectra can be represented by a thin-thermal plasma model with a temperature of 3-4 keV and a redshift of 0.15-0.17. No intensity variation was found in the light curve. The observational results indicate that 2XMM J045637.2+522411 is likely to be a cluster of galaxies.

Published
2010

35. A New Supernova Remnant Candidate and an Associated Outflow in the Sagittarius C Region

Author

Shigeo Yamauchi, Katsuji Koyama, Takeshi Go Tsuru, Masayoshi Nobukawa, Hiroshi Nakajima, and Hironori Matsumoto

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Line-of-sight, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, C region, Astrophysics - Astrophysics of Galaxies, Physics::Fluid Dynamics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Thermal, Chimney, Outflow, Astrophysics - High Energy Astrophysical Phenomena, Supernova remnant, Absorption (electromagnetic radiation), Sagittarius, Astrophysics::Galaxy Astrophysics
Abstract

We present the Suzaku results on a new candidate of a supernova remnant (SNR) in the Sagittarius C region. We detected diffuse X-rays of an elliptical shape (G359.41-0.12) and a chimney-like structure (the Chimney), both of which were fitted with a thin thermal the model of kBT ~1 keV temperature. The absorption columns are same between these two structures, indicating that both are located at the same distance in the same line of sight. The narrow band image and one-dimensional profile of S XV Kalpha at 2.45 keV show that the Chimney is emanating from G359.41-0.12. Therefore, these two sources are physically connected with each other. The sum of the thermal energies of the Chimney and G359.41-0.12 is estimated to be 1.4x10^50 erg, typical for a galactic SNR. G359.41-0.12 is likely to be a new SNR candidate and the Chimney is an associated outflow., 10 pages, 4 figures

Published
2009

36. Iron Emission Lines on the Galactic Ridge Observed with Suzaku

Author

Ezoe Yuichiro, Shigeo Yamauchi, Hiromitsu Takahashi, Yasuo Tanaka, Hironori Matsumoto, Ken Ebisawa, Katsuji Koyama, and Noriko Y. Yamasaki

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, Galactic ridge, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy, X-rays: stars, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galactic plane, X-rays: ISM, Galaxy: disk, X-rays: spectra, Space and Planetary Science, Emission spectrum, Disc, X-rays: diffuse background, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract

In order to elucidate origin of the Galactic Ridge X-ray Emission, we analyzed Suzaku data taken at various regions along the Galactic plane and studied their Fe-K emission line features. Suzaku resolved the Fe line complex into three narrow lines at ~6.4 keV,~6.7 keV and ~6.97 keV, which are K-lines from neutral (or low-ionized), He-like, and H-like iron ions, respectively. The 6.7 keV line is clearly seen in all the observed regions and its longitudinal distribution is consistent with that determined from previous observations. The 6.4 keV emission line was also found in various Galactic plane regions (b~0). Differences in flux ratios of the 6.4 keV/6.7 keV and 6.97 keV/6.7 keV lines between the Galactic plane and the Galactic center regions are studied and its implication is discussed., Comment: Accepted for publication in PASJ Suzaku 3rd special issue

Published
2009

37. X-Ray Reflection Nebulae with Large Equivalent Widths of the Neutral Iron K$\alpha$ Line in the Sagittarius C Region

Author

Atsushi Senda, Katsuji Koyama, Hironori Matsumoto, Takeshi Go Tsuru, Masayoshi Nobukawa, Shigeo Yamauchi, Hiroshi Nakajima, and Hiroshi Murakami

Subjects
Physics, Space and Planetary Science, Reflection nebula, Galactic Center, X-ray, Astronomy and Astrophysics, Astrophysics, C region, Spectral line
Abstract

This paper reports on the first results of the Suzaku observation in the Sgr C region. We detected four diffuse clumps with strong line emission at 6.4keV, Ka from neutral or low-ionized Fe. One of them, M359.38-0.00, is newly discovered with Suzaku. The X-ray spectra of the two bright clumps, M359.43-0.07 and M359.47-0.15, after subtracting the Galactic center diffuse X-ray emission (GCDX), exhibit strong Ka line from FeI with large equivalent widths (EWs) of 2.0-2.2keV and clear Kb of FeI. The GCDX in the Sgr C region is composed of the 6.4keV- and 6.7keV-associated components. These are phenomenologically decomposed by taking relations between EWs of the 6.4keV and 6.7keV lines. Then the former EWs against the associated continuum in the bright clump regions are estimated to be 2.4(+2.3_-0.7)keV. Since the two different approaches give similar large EWs of 2keV, we strongly suggest that the 6.4keV clumps in the Sgr C region are due to X-ray reflection/fluorescence (the X-ray reflection nebulae).

Published
2009

38. Suzaku Spectroscopy of an X-Ray Reflection Nebula and a New Supernova Remnant Candidate in the SgrB1 Region

Author

Hironori Matsumoto, Hiroshi Murakami, Yojiro Takikawa, Katsuji Koyama, Shigeo Yamauchi, Hiroshi Nakajima, Takeshi Go Tsuru, Masayoshi Nobukawa, Yoshiaki Hyodo, and Tatsuya Inui

Subjects
Physics, Reflection nebula, Astrophysics (astro-ph), Galactic Center, X-ray, FOS: Physical sciences, Astronomy and Astrophysics, Plasma, Astrophysics, Space and Planetary Science, Emission spectrum, Spectroscopy, Supernova remnant, Sagittarius
Abstract

We made a 100 ks observation of the Sagittarius (Sgr) B1 region at (l, b) = (0.5, -0.1) near to the Galactic center (GC) with the Suzaku/XIS. Emission lines of S XV, Fe I, Fe XXV, and Fe XXVI were clearly detected in the spectrum. We found that the Fe XXV and Fe XXVI line emissions smoothly distribute over the Sgr B1 and B2 regions connecting from the GC. This result suggests that the GC hot plasma extends at least up to the Sgr B region with a constant temperature. There are two diffuse X-ray sources in the observed region. One of the two (G0.42-0.04) is newly discovered, and exhibits a strong S XV Ka emission line, suggesting a candidate for a supernova remnant located in the GC region. The other one (M0.51-0.10), having a prominent Fe I Ka emission line and a strongly absorbed continuum, is likely to be an X-ray reflection nebula. There is no near source bright enough to irradiate M0.51-0.10. However, the Fe I Ka emission can be explained if Sgr A* was ~ 10^6 times brighter 300 years ago, the light travel time for 100 pc to M0.51-0.10, than it is at present., 10 pages, 10 figures

Published
2008

39. Suzaku Detection of an Intense X-Ray Flare from an A-Type Star, HD161084

Author

Yohko Tsuboi, Shigeo Yamauchi, Yoshitomo Maeda, Katsuji Koyama, Masahiro Tsujimoto, Yasuharu Sugawara, and Junichiro Miura

Subjects
Physics, Subgiant, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Galactic Center, Extinction (astronomy), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Spectroscopic parallax, Luminosity, law.invention, Stars, Space and Planetary Science, law, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, Astrophysics::Galaxy Astrophysics, Flare
Abstract

We report a serendipitous detection of an intense X-ray flare from the Tycho reference source HD 161084 during a Suzaku observation of the Galactic Center region for 20 ks. The X-ray Imaging Spectrometer (XIS) recorded a flare from this A1-type dwarf or subgiant star with a flux of 1.4x10^{-12} erg s^{-1} cm^{-2} (0.5--10 keV) and a decay time scale of 0.5 hr. The spectrum is hard with a prominent Fe XXV K alpha emission line at 6.7 keV, which is explained by a 5 keV thin-thermal plasma model attenuated by a 1.4x10^{21} cm^{-2} extinction. The low extinction, which is consistent with the optical reddening, indicates that the source is a foreground star toward the Galactic Center region. Based on the spectroscopic parallax distance of 530 pc, the peak X-ray luminosity amounts to 1x10^{32} erg s^{-1} (0.5--10 keV). This is much larger than the X-ray luminosity of ordinary late-type main-sequence stars, and the X-ray emission is unattributable to a hidden late-type companion that comprises a wide binary system with the A-star. We discuss possible natures of HD 161084 and suggest that it is most likely an interacting binary with elevated magnetic activity in the companion such as the Algol-type system. The flux detected by Suzaku during the burst is 100 times larger than the quiescent level measured using the archived XMM-Newton and Chandra data. The large flux amplification makes this star a unique example among sources of this class., Comment: 8 pages, 6 figures, 2 tables, PASJ in press

Published
2008

40. Suzaku Detection of Extended/Diffuse Hard X-Ray Emission from the Galactic Center

Author

Tadayuki Takahashi, Ken-ichi Tamura, Yoshitomo Maeda, Takayuki Yuasa, Shigeo Yamauchi, Hiromitsu Takahashi, Kazuhiro Nakazawa, Ken Ebisawa, Takeshi Go Tsuru, Aya Bamba, Atsushi Senda, Katsuji Koyama, Yoshiaki Hyodo, Motohide Kokubun, and Kazuo Makishima

Subjects
Physics, Photon, Astrophysics::High Energy Astrophysical Phenomena, Detector, Galactic Center, Astrophysics (astro-ph), Imaging spectrometer, FOS: Physical sciences, Astronomy and Astrophysics, Plasma, Astrophysics, Power law, Spectral line, Space and Planetary Science, Surface brightness
Abstract

著者人数: 15名, Accepted: 2007-07-28, 資料番号: SA1000326000

Published
2008

41. A Bright Transient X-Ray Source Near the Galactic Center Found in Archival Ginga Data from 1987

Author

Yoshio Nakagawa, Shunji Kitamoto, Shigeo Yamauchi, and Keisuke Sudoh

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Galactic Center, X-ray, Astronomy, Energy flux, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Light curve, Intensity (physics), Neutron star, Space and Planetary Science, Sky, Transient (oscillation), media_common
Abstract

A bright transient X-ray source was detected in the direction of the galactic center with Ginga in 1987 March. A sky position was determined from both data obtained with the All Sky Monitor (ASM) and cross-scan data obtained with the Large Area proportional Counters (LAC). Based on the sky position derived from both the ASM and the LAC data, this source was designated as GS 1741� 288. At the beginning of the Ginga observations, GS 1741� 288 was in the active state: its energy flux in the 2–10 keV energy band was � 10 � 8 erg s � 1 cm � 2 .T he ASM light curve showed that the intensity gradually decayed with an e-folding time of 190 ˙ 9 d. No remarkable feature, such as periodic or quasi-periodic oscillations was found. The spectral and temporal properties suggest that GS 1741� 288 is likely to be a low-mass X-ray binary system containing a weakly magnetized neutron star. Possible identification of the source is also discussed.

Published
2007

42. Discoveries of Diffuse Iron Line Sources from the Sgr B Region

Author

Katsuji Koyama, Chan Yang Soong, Shigeo Yamauchi, Tatsuya Inui, Yoshitomo Maeda, Yoshiaki Hyodo, Kai-Wing, Steven E. Kissel, Takeshi Go Tsuru, Hironori Matsumoto, and Hiroshi Murakami

Subjects
On board, Physics, High energy, Space and Planetary Science, Reflection nebula, Image (category theory), Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Line (formation)
Abstract

The radio complex Sgr B region is observed with the X-Ray Imaging Spectrometers (XIS) on board Suzaku. This region exhibits diffuse iron lines at 6.4, 6.7 and 6.9 keV, which are K$\alpha$ lines of Fe \emissiontype{I} (neutral iron), Fe\emissiontype{XXV} (He-like iron) and Fe\emissiontype{XXVI} (H-like iron), respectively. The high energy resolving power of the XIS provides the separate maps of the K-shell transition lines from Fe\emissiontype{I} (6.4 keV) and Fe\emissiontype{XXV} (6.7 keV). Although the 6.7 keV line is smoothly distributed over the Sgr B region, a local excess is found near at $(l, b) = (\timeform {0D.61}, \timeform{0D.01})$, possibly a new SNR. The plasma temperature is \textit{kT} $\sim$3 keV and the age is estimated to be around several$\times10^{3}$ years. The 6.4 keV image is clumpy with local excesses nearby Sgr B2 and at $(l, b) = (\timeform{0D.74}, -\timeform{0D.09})$. Like Sgr B2, this excess may be another candidate of an X-ray reflection nebula (XRN)., Comment: 12 pages, 10 figures

Published
2007

43. Iron and Nickel Line Diagnostics for the Galactic Center Diffuse Emission

Author

Hiromitsu Takahashi, Hironori Matsumoto, Atsushi Senda, Katsuji Koyama, Hiroshi Nakajima, Yoshitomo Maeda, Jun Kataoka, Takeshi Go Tsuru, Tadayuki Takahashi, Noriko Y. Yamazaki, Yohko Tsuboi, Hiroshi Murakami, Shigeo Yamauchi, Yoshiaki Hyodo, Tatsuya Inui, Gregory V. Brown, and Stephen S. Holt

Subjects
X-ray spectra, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Spectral line, ISM: abundances, Ion, Ionization, Emission spectrum, Collisional excitation, Astrophysics::Galaxy Astrophysics, Line (formation), abundances [ISM], Physics, Galaxy: center, Astrophysics (astro-ph), Astronomy and Astrophysics, center [Galaxy], Space and Planetary Science, dust, extinction [ISM], K-alpha, Electron temperature, ISM: dust, extinction
Abstract

著者人数: 17名, Accepted: 2006-08-16, 資料番号: SA1000358000

Published
2007

44. Hard X-Ray Investigation of the Galactic Center Region with Suzaku

Author

Yasuo Tanaka, Tsuneyoshi Kamae, Atsushi Senda, Katsuji Koyama, Motohide Kokubun, Hiromitsu Takahashi, Suzaku Team, Hiroshi Murakami, Ken-ichi Tamura, Kazuhiro Nakazawa, Aya Bamba, Shigeo Yamauchi, Tsunefumi Mizuno, Yasushi Fukazawa, Kazuo Makishima, Takayuki Yuasa, Tadayuki Takahashi, Noriko Y. Yamasaki, Yoshitomo Maeda, and Ken Ebisawa

Subjects
Physics, Physics and Astronomy (miscellaneous), Galactic Center, X-ray, Astronomy, Astrophysics
Published
2007

46. Forty Cases of Spontaneous Pneumothorax Treated with Video-Assisted Thoracoscopy at Our Hospital in 2004: For Establishment of the Clinical Pathway

Author

Kazuo Shimizu, Naoyuki Yoshino, Mitsunori Hino, Shigeo Yamauchi, Kiyoshi Koizumi, and Hirotoshi Kubokura

Subjects
medicine.medical_specialty, Clinical pathway, Pneumothorax, business.industry, Cardiothoracic surgery, Radiography, Video assisted thoracic surgery, Anesthesia, medicine, Video assisted thoracoscopy, business, medicine.disease, Surgery
Abstract

We treated 40 consecutive cases of spontaneous pneumothorax (SP) with video-assisted thoracic surgery (VATS) in 2004. To develop and introduce a clinical pathway (CP) of VATS for patients with SP, we reviewed the 40 cases in this study. All patients were managed before and after surgery according to the newly established program through manuals and an ordering system (including intravenous infusion, radiography, laboratory tests, and prescriptions). The 40 patients were 35 men (87.5%) and 5 women, with an average age of 30.5 years. In addition, 27 patients (67.5%) were younger than 30 years. The operation sites were right, 18 cases; left, 20 cases; and bilateral, 2 cases. The average surgical duration was 65.6 minutes (excluding 2 bilateral cases). The postoperative duration of thoracic drainage was 1.7 days, and the drain was removed the day after surgery in 35 of 38 patients (excluding the bilateral cases). Only 2 patients (5%) required drainage for more than 1 week. The postoperative stay was 3.2 days; 21 patients (52.5%) were discharged on the second day after surgery, and 8 patients (20%) were discharged on the third day. In addition, 2 patients required hospitalization for more than 1 week. These results show that our programmed management system using VATS for patients with SP is effective and appropriate as a clinical pathway.

Published
2007

47. Intraoperative mapping of the right atrial free wall during sinus rhythm: variety of activation patterns and incidence of postoperative atrial fibrillation

Author

Hajime Imura, Kazuo Shimizu, Nobuo Hatori, Hiromasa Yamashita, Hidetsugu Ogasawara, Shigeo Yamauchi, Shun-ichiro Sakamoto, and Yuji Maruyama

Subjects
Adult, Male, Pulmonary and Respiratory Medicine, medicine.medical_specialty, Heart disease, Sinus bradycardia, Atrial Function, Right, Electrocardiography, Postoperative Complications, Heart Conduction System, Risk Factors, Internal medicine, Atrial Fibrillation, medicine, Humans, Sinus rhythm, Heart Atria, Cardiac Surgical Procedures, Atrium (heart), Aged, Aged, 80 and over, Intraoperative Care, medicine.diagnostic_test, business.industry, Atrial fibrillation, General Medicine, Middle Aged, medicine.disease, Cardiac surgery, medicine.anatomical_structure, Anesthesia, Circulatory system, Electrocardiography, Ambulatory, Cardiology, Female, Surgery, medicine.symptom, Cardiology and Cardiovascular Medicine, business
Abstract

Objective: The atrial conduction properties associated with cardiac disease are speculated as the background of postoperative atrial fibrillation (POAF). We examined the atrial conduction patterns and conduction properties during sinus rhythm (SR) in patients that had undergone cardiac operations and evaluated the incidence of POAF in all patients. Methods: Fifty-two patients with stable SR who underwent cardiac surgery, with a diagnosis of valvular disease in 25, ischemic heart disease in 24, and others in 3, were enrolled in this study. The epicardial recordings were made using a mapping system with 60 unipolar electrodes placed on the right atrium (RA) intraoperatively. The activation patternsof theRAwere assessed, and the longitudinal, transverseand obliqueconductionvelocity andmax anisotropic ratiowere also examined. Results: Sinus activation was initiated from various sites (single origin at the high-lateral RA in 40, mid-lateral RA in 4, low-lateral RA in 2, and multiple origins in 6 patients) and it demonstrated anisotropic conduction (1.8 0.6) with the longitudinal conduction being more rapid than transverse and oblique conduction. Fifteen patients demonstrated non-uniform activation patterns such as, a localized conduction delay in seven, functional conduction block in two and mosaic-activation pattern associated with multiple origins in six. A total of 21 patients (44%) developed POAF. A conduction delay and mosaic activation pattern was found significantly more often in patients with POAF than in patients who remained in sinus rhythm. Multivariate analysis revealed that non-uniform activation pattern (odds ratio = 8.71; 95% confidence interval [CI] = 1.74—43.67; p = 0.008) and TR (odds ratio = 4.95; 95% CI = 1.14—21.37; p = 0.032) were independently associated with the development of POAF. Although all patients had converted to SR at the time of discharge, the administration of antiarrhythmic drugs caused sinus bradycardia in two patients who demonstrated a mosaic activation pattern in RA. Conclusions: Cardiac surgery patients exhibited a variety of sinus activation patterns, which also provided an arrhythmogenic substrate for POAF. A better understanding of the sinus activation using an intraoperative mapping system may provide benefit in the clinical management of POAF.

Published
2006

48. Synchrotron X-Ray SNR Candidates Discovered in the ASCA Galactic Plane Survey

Author

M. Ueno, Shigeo Yamauchi, Ken Ebisawa, Kazuya Koyama, Hiroya Yamaguchi, and Aya Bamba

Subjects
Physics, High energy particle, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Astronomy and Astrophysics, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galactic plane, Near-Earth supernova, Spectral line, Synchrotron, law.invention, Supernova, Space and Planetary Science, law, Ultra-high-energy cosmic ray, Astrophysics::Galaxy Astrophysics
Abstract

Shell-like supernova remnants (SNRs) are primary candidates for the origin of Galactic cosmic rays. However, among the known SNRs (about 220), only a small fraction has been known to exhibit the synchrotron X-ray spectrum, that is considered to be a piece of evidence for high energy particle acceleration. Synchrotron X-ray emitting SNRs are known to be systematically radio-quiet compared to the SNRs that do not emit synchrotron X-rays. Therefore, most synchrotron X-ray emitting SNR candidates may have escaped detection in the previous systematic radio surveys. On the other hand, hard X-ray surveys are effective to search for synchrotron X-ray emitting SNRs, because of its penetration power. Thus we have searched for SNRs in the ASCA Galactic Plane Survey data, the first Galactic imaging survey in 2 keV, and discovered 14 candidates. Deep follow-up observations with ASCA, XMM, or Chandra on 5 of them revealed 2 sources to be synchrotron X-ray emitting SNRs. Furthermore we confirmed non-thermal X-ray spectra from the other 3 sources, though the origin is yet unknown. We report the observational results and discuss the X-ray origin.

Published
2005

49. An Ultrasoft Transient X-Ray Source in the Norma Region Discovered with Ginga

Author

Shigeo Yamauchi

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, Spectral properties, Bremsstrahlung, X-ray, Astronomy, Astronomy and Astrophysics, Astrophysics, Black hole, Space and Planetary Science, Position (vector), Thermal, Black-body radiation, Transient (oscillation)
Abstract

A new X-ray source was discovered in the Norma region with Ginga in 1988 April. The source position, derived from one-dimensional scan data, and its spectral properties are presented. The X-ray emission was dominant below ∼ 6keV and not found in other observations. Thus, it is thought to be an ultrasoft transient X-ray source. The X-ray spectrum, constructed by a scan fit technique, was well represented by either blackbody, thermal bremsstrahlung, power-law, or multicolor disk models. Although all of the spectral models were acceptable from a statistical point of view, the ultrasoft nature of the spectrum and the transient behavior suggest that this source is a candidate source of black hole binaries.

Published
2005

50. X-Ray Emission from a Supernova Remnant, G344.7−0.1, Observed in the ASCA Galactic Plane Survey

Author

Aya Bamba, Katsuji Koyama, Masaru Ueno, and Shigeo Yamauchi

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, X-ray, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Plasma, Astrophysics, Galactic plane, Space and Planetary Science, Ionization, Thermal, Emission spectrum, Supernova remnant, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract

X-ray emission from a cataloged radio supernova remnant (SNR), G344.7−0.1, was observed in the ASCA Galactic Plane Survey. The X-ray image showed extended emission with a diameter of 6 � –8 � . The X-ray spectrum exhibited emission lines from He-like Si, S, Ar, and Ca, which indicates that the X-rays have a thermal plasma origin. The spectrum was represented by a thin thermal plasma model with a temperature of 0.7–0.8keV. The model fit showed that S and Ca are overabundant relative to the solar values. In addition to the emission lines from highly ionized atoms, an emission line at an energy of ∼ 6.4keV was found. This line is attributable to a K transition line from low-ionized iron. The strong Fe-Kα line may suggest the existence of an Fe-rich plasma.

Published
2005

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