Updated on 2021/06/22

写真b

 
KITAMOTO Shunji
 
*Items subject to periodic update by Rikkyo University (The rest are reprinted from information registered on researchmap.)
Affiliation*
College of Science Department of Physics
Graduate School of Science Field of Study: Physics
Graduate School of Science Field of Study: Physics
Title*
Professor
Degree
理学修士 ( 大阪大学 ) / 理学博士 ( 大阪大学 )
Contact information
Mail Address
Research Theme*
  • X線観測衛星のデータ解析を行うことにより、中性子星や、ブラックホールに関連する物理現象の観測的研究を進めている。同時に、宇宙X線天体を観測するための装置開発を行っている。衛星搭載用X線検出器の開発は、JAXA宇宙科学研究本部等との共同で進めている。独自の研究として超高精度X線望遠鏡の開発をめざして、X線結像光学の研究とX線撮像技術の研究を進めている。

  • Research Interests
  • Astrophysics

  • Campus Career*
    • 4 2001 - Present 
      College of Science   Department of Physics   Professor
    • 4 2001 - Present 
      Graduate School of Science   Field of Study: Physics   Professor
    • 4 2001 - Present 
      Graduate School of Science   Field of Study: Physics   Professor
     

    Research Areas

    • Natural Science / Experimental studies related to particle-, nuclear-, cosmic ray and astro-physics

    Research History

    • 4 2001 - Present 
      RIKKYO UNIVERSITY   College of Science Department of Physics   Professor

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    • 4 2001 - Present 
      RIKKYO UNIVERSITY   Graduate School of Science Field of Study: Physics   Professor

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    • 4 2001 - Present 
      RIKKYO UNIVERSITY   Graduate School of Science Field of Study: Physics   Professor

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    • 4 1996 - 3 2001 
      Osaka University   Graduate School of Science

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    • 4 1995 - 3 1996 
      Osaka University   School of Science

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    • 4 1985 - 3 1995 
      Osaka University   School of Science

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    Education

    • - 3 1985 
      Osaka University   Graduate School, Division of Natural Science

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      Country: Japan

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    • - 3 1985 
      Osaka University   Graduate School, Division of Natural Science

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      Country: Japan

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    • - 3 1980 
      Osaka University   Faculty of Science

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      Country: Japan

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    Committee Memberships

    • 9 2008 - Present 
      The Physical Society of Japan   Jr. Session Committee member

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    • 9 2010 - 3 2012 
      日本物理学会   理事

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      Committee type:Academic society

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    • 10 2009 - 9 2010 
      日本物理学会   宇宙線・宇宙物理領域 代表

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      Committee type:Academic society

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    • 1 2004 - 12 2007 
      日本天文学会   理事

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      Committee type:Academic society

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    • 1 2001 - 1 2004 
      日本天文学会   早川基金選考委員

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      Committee type:Academic society

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    • 1 1999 - 1 2002 
      日本天文学会   天文教材委員

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      Committee type:Academic society

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    Papers

    • Status of x-ray imaging and spectroscopy mission (XRISM)

      Makoto S. Tashiro, Hironori Maejima, Kenichi Toda, Richard L. Kelley, Lillian Reichenthal, Leslie Hartz, Robert Petre, Brian J. Williams, Matteo Guainazzi, Elisa Costantini, Ryuichi Fujimoto, Kiyoshi Hayashida, Joy Henegar-Leon, Matt Holland, Yoshitaka Ishisaki, Caroline Kilbourne, Mike Loewenstein, Kyoko Matsushita, Koji Mori, Takashi Okajima, F. Scott Porter, Gary Sneiderman, Yoh Takei, Yukikatsu Terada, Hiroshi Tomida, Hiroya Yamaguchi, Shin Watanabe, Hiroki Akamatsu, Yoshitaka Arai, Marc Audard, Hisamitsu Awaki, Iurii Babyk, Aya Bamba, Nobutaka Bando, Ehud Behar, Thomas Bialas, Rozenn Boissay-Malaquin, Laura Brenneman, Greg Brown, Edgar Canavan, Meng Chiao, Brian Comber, Lia Corrales, Renata Cumbee, Cor de Vries, Jan-Willem den Herder, Johannes Dercksen, Maria Diaz-Trigo, Michael DiPirro, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Carlo Ferrigno, Yutaka Fujita, Yasushi Fukazawa, Akihiro Furuzawa, Luigi Gallo, Nathalie Gorter, Martin Grim, Liyi Gu, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, David Hawthorn, Katsuhiro Hayashi, Natalie Hell, Junko Hiraga, Edmund Hodges-Kluck, Takafumi Horiuchi, Ann Hornschemeier, Akio Hoshino, Yuto Ichinohe, Sayuri Iga, Ryo Iizuka, Manabu Ishida, Naoki Ishihama, Kumi Ishikawa, Kosei Ishimura, Tess Jaffe, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Steven Kenyon, Mark Kimball, Takao Kitaguti, Shunji Kitamoto, Shogo Kobayashi, Akihide Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Muzi Li, Tom Lockard, Yoshitomo Maeda, Maxim Markevitch, Connor Martz, Hironori Matsumoto, Keiichi Matsuzaki, Dan McCammon, Brian McLaughlin, Brian McNamara, Joseph Miko, Eric Miller, Jon Miller, Kenji Minesugi, Shinji Mitani, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Hideto Nakamura, Kazuhiro Nakazawa, Chikara Natsukari, Kenichiro Nigo, Yusuke Nishioka, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Mina Ogawa, Takaya Ohashi, Masahiro Ohno, Masayuki Ohta, Atsushi Okamoto, Naomi Ota, Masanobu Ozaki, Stephane Paltani, Paul Plucinsky, Katja Pottschmidt, Michael Sampson, Takahiro Sasaki, Kosuke Sato, Rie Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Yasuko Shibano, Maki Shida, Megumi Shidatsu, Shuhei Shigeto, Keisuke Shinozaki, Peter Shirron, Aurora Simionescu, Randall Smith, Kazunori Someya, Yang Soong, Keisuke Sugawara, Yasuharu Sugawara, Andy Szymkowiak, Hiromitsu Takahashi, Toshiaki Takeshima, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Hiroyuki Uchida, Yuusuke Uchida, Hideki Uchiyama, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Tomomi Watanabe, Michael Wittheof, Rob Wolfs, Shinya Yamada, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Keiichi Yanagase, Tahir Yaqoob, Susumu Yasuda, Tessei Yoshida, Nasa Yoshioka, Irina Zhuravleva

      Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray   13 12 2020

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      Publishing type:Research paper (international conference proceedings)   Publisher:SPIE  

      DOI: 10.1117/12.2565812

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    • X-ray transmission measurements of the gate valve for the x-ray astronomy satellite XRISM

      Takuya Midooka, Masahiro Tsujimoto, Shunji Kitamoto, Nozomi Nakaniwa, Yoshitomo Maeda, Shinjiro Hayakawa, Manabu Ishida, Ken Ebisawa, Mayu Tominaga

      Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray   13 12 2020

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      Publishing type:Research paper (international conference proceedings)   Publisher:SPIE  

      DOI: 10.1117/12.2559451

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    • The Modulating Optical Depth of the Photoelectric Absorption Edge with a Pulse Phase in Accretion-powered X-Ray Pulsars

      Yuki Yoshida, Shunji Kitamoto

      The Astrophysical Journal880 ( 2 ) 101 - 101   31 7 2019

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      Publishing type:Research paper (scientific journal)   Publisher:American Astronomical Society  

      DOI: 10.3847/1538-4357/ab2b3d

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      Other Link: https://iopscience.iop.org/article/10.3847/1538-4357/ab2b3d

    • Hitomi X-ray observation of the pulsar wind nebula G21.5-0.9 Peer-reviewed

      Hitomi Collaboration

      PASJ   3 4 2018

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:the Astronomical Society of Japan  

      We present results from the Hitomi X-ray observation of a young composite-type supernova remnant (SNR) G21.5−0.9, whose emission is dominated by the pulsar wind nebula (PWN) contribution. The X-ray spectra in the 0.8–80 keV range obtained with the Soft X-ray Spectrometer (SXS), Soft X-ray Imager, and Hard X-ray Imager (HXI) show a significant break in the continuum as previously found with the NuSTAR observation. After taking into account all known emissions from the SNR other than the PWN itself, we find that the Hitomi spectra can be fitted with a broken power law with photon indices of Γ1 = 1.74 ± 0.02 and Γ2 = 2.14 ± 0.01 below and above the break at 7.1 ± 0.3 keV, which is significantly lower than the NuSTAR result (∼9.0 keV). The spectral break cannot be reproduced by time-dependent particle injection one-zone spectral energy distribution models, which strongly indicates that a more complex emission model is needed, as suggested by recent theoretical models. We also search for narrow emission or absorption lines with the SXS, and perform a timing analysis of PSR J1833−1034 with the HXI and the Soft Gamma-ray Detector. No significant pulsation is found from the pulsar. However, unexpectedly, narrow absorption line features are detected in the SXS data at 4.2345 keV and 9.296 keV with a significance of 3.65 σ. While the origin of these features is not understood, their mere detection opens up a new field of research and was only possible with the high resolution, sensitivity, and ability to measure extended sources provided by an X-ray microcalorimeter.

      DOI: 10.1093/pasj/psy027

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    • Atmospheric gas dynamics in the Perseus cluster observed with Hitomi Peer-reviewed

      Hitomi Collaboration

      Publications of the Astronomical Society of Japan,70 ( 2 )   3 2018

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:the Astronomical Society of Japan,  

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    • Performance of the helium dewar and the cryocoolers of the Hitomi soft x-ray spectrometer

      Ryuichi Fujimoto, Yoh Takei, Kazuhisa Mitsuda, Noriko Y. Yamasaki, Masahiro Tsujimoto, Shu Koyama, Kumi Ishikawa, Hiroyuki Sugita, Yoichi Sato, Keisuke Shinozaki, Atsushi Okamoto, Shunji Kitamoto, Akio Hoshino, Kosuke Sato, Yuichiro Ezoe, Yoshitaka Ishisaki, Shinya Yamada, Hiromi Seta, Takaya Ohashi, Toru Tamagawa, Hirofumi Noda, Makoto Sawada, Makoto Tashiro, Yoichi Yatsu, Ikuyuki Mitsuishi, Kenichi Kanao, Seiji Yoshida, Mikio Miyaoka, Shoji Tsunematsu, Kiyomi Otsuka, Katsuhiro Narasaki, Michael J. DiPirro, Peter J. Shirron, Gary A. Sneiderman, Caroline A. Kilbourne, Frederick Scott Porter, Meng P. Chiao, Megan E. Eckart

      Journal of Astronomical Telescopes, Instruments, and Systems4   1 1 2018

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      © 2018 Society of Photo-Optical Instrumentation Engineers (SPIE). The soft x-ray spectrometer (SXS) was a cryogenic high-resolution x-ray spectrometer onboard the Hitomi (ASTRO-H) satellite that achieved energy resolution of 5 eV at 6 keV, by operating the detector array at 50 mK using an adiabatic demagnetization refrigerator (ADR). The cooling chain from room temperature to the ADR heat sink was composed of two-stage Stirling cryocoolers, a4He Joule-Thomson cryocooler, and superfluid liquid helium and was installed in a dewar. It was designed to achieve a helium lifetime of more than 3 years with a minimum of 30 L. The satellite was launched on February 17, 2016, and the SXS worked perfectly in orbit, until March 26 when the satellite lost its function. It was demonstrated that the heat load on the helium tank was about 0.7 mW, which would have satisfied the lifetime requirement. This paper describes the design, results of ground performance tests, prelaunch operations, and initial operation and performance in orbit of the flight dewar and the cryocoolers.

      DOI: 10.1117/1.JATIS.4.1.011208

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    • Solar abundance ratios of the iron-peak elements in the Perseus cluster Peer-reviewed

      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, 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 Limousine, 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, StPhane 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. Serlemitsos, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall K. Smith, Yang Soong, Lukasz 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, Cor P. de Vries, Shin Watanabe, Norbert Werner, Daniel R. Wik, 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

      NATURE551 ( 7681 ) 478 - +   11 2017

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:NATURE PUBLISHING GROUP  

      The metal abundance of the hot plasma that permeates galaxy clusters represents the accumulation of heavy elements produced by billions of supernovae(1). Therefore, X-ray spectroscopy of the intracluster medium provides an opportunity to investigate the nature of supernova explosions integrated over cosmic time. In particular, the abundance of the iron-peak elements (chromium, manganese, iron and nickel) is key to understanding how the progenitors of typical type Ia supernovae evolve and explode(2-6). Recent X-ray studies of the intracluster medium found that the abundance ratios of these elements differ substantially from those seen in the Sun(7-11), suggesting differences between the nature of type Ia supernovae in the clusters and in the Milky Way. However, because the K-shell transition lines of chromium and manganese are weak and those of iron and nickel are very close in photon energy, highresolution spectroscopy is required for an accurate determination of the abundances of these elements. Here we report observations of the Perseus cluster, with statistically significant detections of the resonance emission from chromium, manganese and nickel. Our measurements, combined with the latest atomic models, reveal that these elements have near-solar abundance ratios with respect to iron, in contrast to previous claims. Comparison between our results and modern nucleosynthesis calculations(12-14) disfavours the hypothesis that type Ia supernova progenitors are exclusively white dwarfs with masses well below the Chandrasekhar limit (about 1.4 times the mass of the Sun). The observed abundance pattern of the iron-peak elements can be explained by taking into account a combination of near-and sub-Chandrasekhar-mass type Ia supernova systems, adding to the mounting evidence that both progenitor types make a substantial contribution to cosmic chemical enrichment(5,15,16).

      DOI: 10.1038/nature24301

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    • The Intensity Modulation of the Fluorescent Line by a Finite Light Speed Effect in Accretion-powered X-Ray Pulsars Peer-reviewed

      Yuki Yoshida, Shunji Kitamoto, Akio Hoshino

      ASTROPHYSICAL JOURNAL849 ( 2 )   11 2017

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:IOP PUBLISHING LTD  

      The X-ray line diagnostic method is a powerful tool for an investigation of plasma around accretion-powered X-ray pulsars. We point out an apparent intensity modulation of emission lines, with their rotation period of neutron stars, due to the finite speed of light ( we call this effect the "finite light speed effect") if the line emission mechanism is a kind of reprocessing, such as fluorescence or recombination after ionization by X-ray irradiation from pulsars. The modulation amplitude is determined by the size of the emission region, which is in competition with the smearing effect by the light crossing time in the emission region. This is efficient if the size of the emission region is roughly comparable to that of the rotation period multiplied by the speed of light. We apply this effect to a symbiotic X-ray pulsar, GX 1+4, where a spin modulation of the intense iron line of which has been reported. The finite light speed effect can explain the observed intensity modulation if its fluorescent region is the size of similar to 10(12) cm.

      DOI: 10.3847/1538-4357/aa9023

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    • Orbital modulations of X-ray light curves of Cygnus X-1 in its low/hard and high/soft states Peer-reviewed

      Juri Sugimoto, Shunji Kitamoto, Tatehiro Mihara, Masaru Matsuoka

      PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN69 ( 3 ) 52   6 2017

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:OXFORD UNIV PRESS  

      The black hole binary Cygnus X-1 has a 5.6-d orbital period. We first detected a clear intensity modulation with the orbital period in its high/soft state with six-year MAXI data, as well as in its low/hard state. In the low/hard state, the folded light curves showed an intensity drop at the superior conjunction of the black hole by a modulation factor (MF), which is the amplitude divided by the average, of 8 +/- 1%, 4 +/- 1%, and 3 +/- 2% for 2-4, 4-10, and 10-20 keV bands, respectively, showing a spectral hardening at the superior conjunction of the black hole. Spectral analysis in the low/hard state, with a model consisting of a power law and a photoelectric absorption, showed that the hydrogen column density, NH, increased from (2.9 +/- 0.4) x 10(21) cm(-2) to (4.7 +/- 1.1) x 10(21) cm(-2) around the superior conjunction. The flux of the power-law component decreased by 6 +/- 1%. On the other hand, MFs for the folded light curves in the high/soft state, were 4 +/- 1% and 4 +/- 2% for the 2-4 keV and 4-10 keV bands, respectively. We applied a model consisting of a power law and a disk blackbody with a photoelectric absorption. A modulation of the flux of the power-law component was found to be 7 +/- 5% in MF, while the modulation of NH was less than 1 x 10(21) cm(-2). These results can be interpreted as follows: the modulation of both states can be mainly explained by scattering of X-rays by an ionized stellar wind, but, only at the superior conjunction in the low/hard state, a large photoelectric absorption appears because of the low ionization state of the wind in the line of sight at phase 0. Such a condition can be established by reasonable parameters of an inhomogeneous wind and the observed luminosities.

      DOI: 10.1093/pasj/psx028

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    • A Suzaku View of Accretion- powered X-Ray Pulsar GX 1+4 Peer-reviewed

      Yuki Yoshida, Shunji Kitamoto, Hiroo Suzuki, Akio Hoshino, Sachindra Naik, Gaurava K. Jaisawal

      ASTROPHYSICAL JOURNAL838 ( 1 ) 30 - 44   3 2017

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:IOP PUBLISHING LTD  

      We present results obtained from a Suzaku observation of the accretion-powered X-ray pulsar GX. 1+ 4. A broadband continuum spectrum of the pulsar was found to be better described by a simple model consisting of a blackbody component and an exponential cutoff power law than the previously used compTT continuum model. Though the pulse profile had a sharp dip in soft X-rays (< 10 keV), phase-resolved spectroscopy confirmed that the dimming was not due to an increase in photoelectric absorption. Phase-sliced spectral analysis showed the presence of a significant spectral modulation beyond 10 keV except for the dip phase. A search for the presence of a cyclotron resonance scattering feature in the Suzaku spectra yielded a negative result. Iron K-shell (Ka and Kb) emission lines from nearly neutral iron ions (< Fe III) were clearly detected in the source spectrum. A significant Ka emission line from almost neutral Ni atoms was detected for the first time in this source. We estimated an iron abundance of similar to 80% of the solar value and an Ni/Fe abundance ratio of about two times the solar value. We searched for an iron Lya emission line and found a significant improvement in the spectral fitting by inclusion of this line. We found a clear intensity modulation of the iron Ka line with the pulse phase with an amplitude of 7%. This finding favored an inhomogeneous fluorescent region with a radius much smaller than the size (similar to 3. x. 10(12) cm) estimated by an assumption of homogeneous matter.

      DOI: 10.3847/1538-4357/aa6301

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    • Hitomi Constraints on the 3.5 keV Line in the Perseus Galaxy Cluster Peer-reviewed

      F. A. Aharonian, H. Akamatsu, F. Akimoto, S. W. Allen, L. Angelini, K. A. Arnaud, M. Audard, H. Awaki, M. Axelsson, A. Bamba, M. W. Bautz, R. D. Blandford, E. Bulbul, L. W. Brenneman, G. V. Brown, E. M. Cackett, M. Chernyakova, M. P. Chiao, P. Coppi, E. Costantini, J. de Plaa, J. -W. den Herder, C. Done, T. Dotani, K. Ebisawa, M. E. Eckart, T. Enoto, Y. Ezoe, A. C. Fabian, C. Ferrigno, A. R. Foster, R. Fujimoto, Y. Fukazawa, A. Furuzawa, M. Galeazzi, L. C. Gallo, P. Gandhi, M. Giustini, A. Goldwurm, L. Gu, M. Guainazzi, Y. Haba, K. Hagino, K. Hamaguchi, I. Harrus, I. Hatsukade, K. Hayashi, T. Hayashi, K. Hayashida, J. Hiraga, A. E. Hornschemeier, A. Hoshino, J. P. Hughes, Y. Ichinohe, R. Iizuka, H. Inoue, S. Inoue, Y. Inoue, K. Ishibashi, M. Ishida, K. Ishikawa, Y. Ishisaki, M. Itoh, M. Iwai, N. Iyomoto, J. S. Kaastra, T. Kallman, T. Kamae, E. Kara, J. Kataoka, S. Katsuda, J. Katsuta, M. Kawaharada, N. Kawai, R. L. Kelley, D. Khangulyan, C. A. Kilbourne, A. L. King, T. Kitaguchi, S. Kitamoto, T. Kitayama, T. Kohmura, M. Kokubun, S. Koyama, K. Koyama, P. Kretschmar, H. A. Krimm, A. Kubota, H. Kunieda, P. Laurent, F. Lebrun, S. -H. Lee, M. A. Leutenegger, O. Limousin, M. Loewenstein, K. S. Long, D. H. Lumb, G. M. Madejski, Y. Maeda, D. Maier, K. Makishima, M. Markevitch, H. Matsumoto, K. Matsushita, D. McCammon, B. R. McNamara, M. Mehdipour, E. D. Miller, J. M. Miller, S. Mineshige, K. Mitsuda, I. Mitsuishi, T. Miyazawa, T. Mizuno, H. Mori, K. Mori, H. Moseley, K. Mukai, H. Murakami, T. Murakami, R. F. Mushotzky, T. Nakagawa, H. Nakajima, T. Nakamori, T. Nakano, S. Nakashima, K. Nakazawa, K. Nobukawa, M. Nobukawa, H. Noda, M. Nomachi, S. L. O'Dell, H. Odaka, T. Ohashi, M. Ohno, T. Okajima, N. Ota, M. Ozaki, F. Paerels, S. Paltani, A. Parmar, R. Petre, C. Pinto, M. Pohl, F. S. Porter, K. Pottschmidt, B. D. Ramsey, C. S. Reynolds, H. R. Russell, S. Safi-Harb, S. Saito, K. Sakai, H. Sameshima, T. Sasaki, G. Sato, K. Sato, R. Sato, M. Sawada, N. Schartel, P. J. Serlemitsos, H. Seta, M. Shidatsu, A. Simionescu, R. K. Smith, Y. Soong, L. Stawarz, Y. Sugawara, S. Sugita, A. E. Szymkowiak, H. Tajima, H. Takahashi, T. Takahashi, S. Takeda, Y. Takei, T. Tamagawa, K. Tamura, T. Tamura, T. Tanaka, Yasuo Tanaka, Yasuyuki Tanaka, M. Tashiro, Y. Tawara, Y. Terada, Y. Terashima, F. Tombesi, H. Tomida, Y. Tsuboi, M. Tsujimoto, H. Tsunemi, T. Tsuru, H. Uchida, H. Uchiyama, Y. Uchiyama, S. Ueda, Y. Ueda, S. Ueno, S. Uno, C. M. Urry, E. Ursino, C. P. de Vries, S. Watanabe, N. Werner, D. R. Wik, D. R. Wilkins, B. J. Williams, S. Yamada, H. Yamaguchi, K. Yamaoka, N. Y. Yamasaki, M. Yamauchi, S. Yamauchi, T. Yaqoob, Y. Yatsu, D. Yonetoku, A. Yoshida, I. Zhuravleva, A. Zoghbi

      ASTROPHYSICAL JOURNAL LETTERS837 ( 1 ) L15 - L23   3 2017

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:IOP PUBLISHING LTD  

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

      DOI: 10.3847/2041-8213/aa61fa

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    • The quiescent intracluster medium in the core of the Perseus cluster Peer-reviewed

      Felix Aharonian, Hiroki Akamatsu, Fumie Akimoto, Steven W. Allen, Naohisa Anabuki, Lorella Angelini, Keith Arnaud, Marc Audard, Hisamitsu Awaki, Magnus Axelsson, Aya Bamba, Marshall Bautz, Roger Blandford, Laura Brenneman, Gregory V. Brown, Esra Bulbul, Edward Cackett, Maria Chernyakova, Meng Chiao, Paolo Coppi, Elisa Costantini, Jelle de Plaa, Jan-Willem den Herder, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan Eckart, Teruaki Enoto, Yuichiro Ezoe, Andrew C. Fabian, Carlo Ferrigno, Adam Foster, Ryuichi Fujimoto, Yasushi Fukazawa, Akihiro Furuzawa, Massimiliano Galeazzi, Luigi Gallo, Poshak Gandhi, Margherita Giustini, Andrea Goldwurm, Liyi Gu, Matteo Guainazzi, Yoshito Haba, Kouichi Hagino, Kenji Hamaguchi, Ilana Harrus, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Kiyoshi Hayashida, Junko Hiraga, Ann Hornschemeier, Akio Hoshino, John Hughes, Ryo Iizuka, Hajime Inoue, Yoshiyuki Inoue, Kazunori Ishibashi, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Masayuki Itoh, Naoko Iyomoto, Jelle Kaastra, Timothy Kallman, Tuneyoshi Kamae, Erin Kara, Jun Kataoka, Satoru Katsuda, Junichiro Katsuta, Madoka Kawaharada, Nobuyuki Kawai, Richard Kelley, Dmitry Khangulyan, Caroline Kilbourne, Ashley King, Takao Kitaguchi, Shunji Kitamoto, Tetsu Kitayama, Takayoshi Kohmura, Motohide Kokubun, Shu Koyama, Katsuji Koyama, Peter Kretschmar, Hans Krimm, Aya Kubota, Hideyo Kunieda, Philippe Laurent, Francois Lebrun, Shiu-Hang Lee, Maurice Leutenegger, Olivier Limousin, Michael Loewenstein, Knox S. Long, David Lumb, Grzegorz Madejski, Yoshitomo Maeda, Daniel Maier, Kazuo Makishima, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, Missagh Mehdipour, Eric Miller, Jon Miller, Shin Mineshige, Kazuhisa Mitsuda, Ikuyuki Mitsuishi, Takuya Miyazawa, Tsunefumi Mizuno, Hideyuki Mori, Koji Mori, Harvey Moseley, Koji Mukai, Hiroshi Murakami, Toshio Murakami, Richard Mushotzky, Ryo Nagino, Takao Nakagawa, Hiroshi Nakajima, Takeshi Nakamori, Toshio Nakano, Shinya Nakashima, Kazuhiro Nakazawa, Masayoshi Nobukawa, Hirofumi Noda, Masaharu Nomachi, Steve O'Dell, Hirokazu Odaka, Takaya Ohashi, Masanori Ohno, Takashi Okajima, Naomi Ota, Masanobu Ozaki, Frits Paerels, Stephane Paltani, Arvind Parmar, Robert Petre, Ciro Pinto, Martin Pohl, F. Scott Porter, Katja Pottschmidt, Brian Ramsey, Christopher Reynolds, Helen Russell, Samar Safi-Harb, Shinya Saito, Kazuhiro Sakai, Hiroaki Sameshima, Goro Sato, Kosuke Sato, Rie Sato, Makoto Sawada, Norbert Schartel, Peter Serlemitsos, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Yang Soong, Lukasz Stawarz, Yasuharu Sugawara, Satoshi Sugita, Andrew Szymkowiak, Hiroyasu Tajima, Hiromitsu Takahashi, Tadayuki Takahashi, Shin'ichiro Takeda, Yoh Takei, Toru Tamagawa, Keisuke Tamura, Takayuki Tamura, Takaaki Tanaka, Yasuo Tanaka, Yasuyuki Tanaka, Makoto Tashiro, Yuzuru Tawara, Yukikatsu Terada, Yuichi Terashima, Francesco Tombesi, Hiroshi Tomida, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Hiroyuki Uchida, Hideki Uchiyama, Yasunobu Uchiyama, Shutaro Ueda, Yoshihiro Ueda, Shiro Ueno, Shin'ichiro Uno, Meg Urry, Eugenio Ursino, Cor De Vries, Shin Watanabe, Norbert Werner, Daniel Wik, Dan Wilkins, Brian Williams, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Y. Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Yoichi Yatsu, Daisuke Yonetoku, Atsumasa Yoshida, Takayuki Yuasa, Irina Zhuravleva, Abderahmen Zoghbi

      NATURE535 ( 7610 ) 117 - +   7 2016

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:NATURE PUBLISHING GROUP  

      Clusters of galaxies are the most massive gravitationally bound objects in the Universe and are still forming. They are thus important probes(1) of cosmological parameters and many astrophysical processes. However, knowledge of the dynamics of the pervasive hot gas, the mass of which is much larger than the combined mass of all the stars in the cluster, is lacking. Such knowledge would enable insights into the injection of mechanical energy by the central supermassive black hole and the use of hydrostatic equilibrium for determining cluster masses. X-rays from the core of the Perseus cluster are emitted by the 50-million-kelvin diffuse hot plasma filling its gravitational potential well. The active galactic nucleus of the central galaxy NGC 1275 is pumping jetted energy into the surrounding intracluster medium, creating buoyant bubbles filled with relativistic plasma. These bubbles probably induce motions in the intracluster medium and heat the inner gas, preventing runaway radiative cooling-a process known as active galactic nucleus feedback(2-6). Here we report X-ray observations of the core of the Perseus cluster, which reveal a remarkably quiescent atmosphere in which the gas has a line-of-sight velocity dispersion of 164 +/- 10 kilometres per second in the region 30-60 kiloparsecs from the central nucleus. A gradient in the line-of-sight velocity of 150 +/- 70 kilometres per second is found across the 60-kiloparsec image of the cluster core. Turbulent pressure support in the gas is four per cent of the thermodynamic pressure, with large-scale shear at most doubling this estimate. We infer that a total cluster mass determined from hydrostatic equilibrium in a central region would require little correction for turbulent pressure.

      DOI: 10.1038/nature18627

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    • MAXI observations of long-term variations of Cygnus X-1 in the low/hard and the high/soft states Peer-reviewed

      Juri Sugimoto, Tatehiro Mihara, Shunji Kitamoto, Masaru Matsuoka, Mutsumi Sugizaki, Hitoshi Negoro, Satoshi Nakahira, Kazuo Makishima

      Publications of the Astronomical Society of Japan68 ( S17 ) 17   1 6 2016

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:The Astronomical Society of Japan  

      © 2016 The Author. The long-term X-ray variability of the black hole binary Cygnus X-1 was studied with five years of MAXI data from 2009 to 2014, which include substantial periods of the high/soft state, as well as the low/hard state. In each state, normalized power spectrum densities (NPSDs) were calculated in three energy bands of 2-4 keV, 4-10 keV, and 10-20 keV. The NPSDs for frequencies from 10 -7 Hz to 10 -4 Hz are all approximated by a power-law function with an index -1.35-1.29. The fractional RMS variation η, calculated in the above frequency range, was found to show the following three properties: (1) η slightly decreases with energy in the low/hard state; (2) η increases towards higher energies in the high/soft state; and (3) in the 10-20 keV band, η is three times higher in the high/soft state than in the low/hard state. These properties were confirmed through studies of intensity-correlated changes of the MAXI spectra. Of these three findings, the first one is consistent with that seen in the short-term variability during the low/hard state. The latter two can be understood as a result of high variability of the hard-tail component seen in the high/soft state with the above very low frequency range, although the origin of the variability remains inconclusive.

      DOI: 10.1093/pasj/psw004

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    • Performance of the helium dewar and cryocoolers of ASTRO-H SXS

      Ryuichi Fujimoto, Yoh Takei, Kazuhisa Mitsuda, Noriko Y. Yamasaki, Masahiro Tsujimoto, Shu Koyama, Kumi Ishikawa, Hiroyuki Sugita, Yoichi Sato, Keisuke Shinozaki, Atsushi Okamoto, Shunji Kitamoto, Akio Hoshino, Kosuke Sato, Yuichiro Ezoe, Yoshitaka Ishisaki, Shinya Yamada, Hiromi Seta, Takaya Ohashi, Toru Tamagawa, Hirofumi Noda, Makoto Sawada, Makoto Tashiro, Yoichi Yatsu, Ikuyuki Mitsuishi, Kenichi Kanao, Seiji Yoshida, Mikio Miyaoka, Shoji Tsunematsu, Kiyomi Otsuka, Katsuhiro Narasaki, Michael J. DiPirro, Peter J. Shirron, Gary A. Sneiderman, Caroline A. Kilbourne, F. Scott Porter, Meng P. Chiao, Megan E. Eckart, Richard L. Kelley

      Proceedings of SPIE - The International Society for Optical Engineering9905   1 1 2016

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      © 2016 SPIE. The Soft X-ray Spectrometer (SXS) is a cryogenic high-resolution X-ray spectrometer onboard the ASTRO-H satellite, that achieves energy resolution better than 7 eV at 6 keV, by operating the detector array at 50 mK using an adiabatic demagnetization refrigerator. The cooling chain from room temperature to the ADR heat sink is composed of 2-stage Stirling cryocoolers, a 4He Joule-Thomson cryocooler, and super uid liquid He, and is installed in a dewar. It is designed to achieve a helium lifetime of more than 3 years with a minimum of 30 liters. The satellite was launched on 2016 February 17, and the SXS worked perfectly in orbit, until March 26 when the satellite lost its function. It was demonstrated that the heat load on the He tank was about 0.7 mW, which would have satisfied the lifetime requirement. This paper describes the design, results of ground performance tests, prelaunch operations, and initial operation and performance in orbit of the flight dewar and cryocoolers.

      DOI: 10.1117/12.2232933

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    • In-orbit operation of the ASTRO-H SXS Peer-reviewed

      Tsujimoto Masahiro, Mitsuda Kazuhisa, Kelley Richard L, den Herder Jan-Willem A, Akamatsu Hiroki, Bialas Thomas G, Boyce Kevin R, Brown Gregory V, Chiao Meng P, Costantini Elisa, de Vries Cor P, DiPirro Michael J, Eckart Megan E, Ezoe Yuichiro, Fujimoto Ryuichi, Haas Daniel, Hoshino Akio, Ishikawa Kumi, Ishisaki Yoshitaka, Iyomoto Naoko, Kilbourne Caroline A, Kitamoto Shunji, Koyama Shu, Leutenegger Maurice A, McCammon Dan, Mitsuishi Ikuyuki, Murakami Hiroshi, Murakami Masahide, Noda Hirofumi, Ogawa Mina, Ota Naomi, Paltani Stephane, Porter Frederick S, Sato Kosuke, Sato Yoichi, Sawada Makoto, Seta Hiromi, Shinozaki Keisuke, Shirron Peter J, Sneiderman Gary A, Sugita Hiroyuki, Szymkowiak Andrew E, Takei Yoh, Tamagawa Toru, Tashiro Makoto S, Terada Yukikatsu, Yamada Shinya, Yamasaki Noriko Y, Yatsu Yoichi

      SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY9905   2016

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    • The Astro-H High Resolution Soft X-Ray Spectrometer Peer-reviewed

      Kelley Richard L, Akamatsu Hiroki, Azzarell Phillipp, Bialas Tom, Boyce Kevin R, Brown Gregory V, Canavan Edgar, Chiao Meng P, Costantini Elisa, DiPirro Michael J, Eckart Megan E, Ezoe Yuichiro, Fujimoto Ryuichi, Haas Daniel, den Herder Jan-Willem, Hoshino Akio, Ishikawa Kumi, Ishisaki Yoshitaka, Iyomoto Naoko, Kilbourne Caroline A, Kimball Mark, Kitamoto Shunji, Konami Saori, Koyama Shu, Leutenegger Maurice A, McCammon Dan, Miko Joseph, Mitsuda Kazuhisa, Mitsuishi Ikuyuki, Moseley Harvey, Murakami Hiroshi, Murakami Masahide, Noda Hirofumi, Ogawa Mina, Ohashi Takaya, Okamoto Atsushi, Ota Naomi, Paltani Stephane, Porter F. Scott, Sakai Kazuhiro, Sato Kosuke, Sato Yohichi, Sawada Makoto, Seta Hiromi, Shinozaki Keisuke, Shirron Peter J, Sneiderman Gary A, Sugita Hiroyuki, Szymkowiak Andrew E, Takei Yoh, Tamagawa Toni, Tashiro Makoto, Terada Yukikatsu, Tsujimoto Masahiro, de Vries Cor P, Yamada Shinya, Yamasaki Noriko Y, Yatsu Yoichi

      SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY9905   2016

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    • New multiwavelength observations of the Of?p star CPD-28 degrees 2561 Peer-reviewed

      S. Hubrig, M. Schoeller, A. F. Kholtygin, H. Tsumura, A. Hoshino, S. Kitamoto, L. Oskinova, R. Ignace, H. Todt, I. Ilyin

      MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY447 ( 2 ) 1885 - 1894   2 2015

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:OXFORD UNIV PRESS  

      A rather strong mean longitudinal magnetic field of the order of a few hundred gauss was detected a few years ago in the Of?p star CPD -28 degrees 2561 using FORS2 (FOcal Reducer low dispersion Spectrograph 2) low-resolution spectropolarimetric observations. In this work, we present additional low-resolution spectropolarimetric observations obtained during several weeks in 2013 December using FORS 2 mounted at the 8-m Antu telescope of the Very Large Telescope (VLT). These observations cover a little less than half of the stellar rotation period of 73.41 d mentioned in the literature. The behaviour of the mean longitudinal magnetic field is consistent with the assumption of a single-wave variation during the stellar rotation cycle, indicating a dominant dipolar contribution to the magnetic field topology. The estimated polar strength of the surface dipole B-d is larger than 1.15 kG. Further, we compared the behaviour of the line profiles of various elements at different rotation phases associated with different magnetic field strengths. The strongest contribution of the emission component is observed at the phases when the magnetic field shows a negative or positive extremum. The comparison of the spectral behaviour of CPD -28 degrees 2561 with that of another Of?p star, HD 148937 of similar spectral type, reveals remarkable differences in the degree of variability between both stars. Finally, we present new X-ray observations obtained with the Suzaku X-ray Observatory. We report that the star is X-ray bright with log L-X/L-bol approximate to -5.7. The low-resolution X-ray spectra reveal the presence of a plasma heated up to 24 MK. We associate the 24 MK plasma in CPD -28 degrees 2561 with the presence of a kG strong magnetic field capable to confine stellar wind.

      DOI: 10.1093/mnras/stu2516

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    • A new clocking method for a charge coupled device Peer-reviewed

      Umezu Rika, Kitamoto Shunji, Murakami Hiroshi

      REVIEW OF SCIENTIFIC INSTRUMENTS85 ( 7 )   7 2014

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    • X-ray development of the classical nova V2672 Ophiuchi with Suzaku Peer-reviewed

      Dai Takei, Masahiro Tsujimoto, Jeremy J. Drake, Shunji Kitamoto

      PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN66 ( 2 )   4 2014

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:OXFORD UNIV PRESS  

      We report on the Suzaku detection of a rapid flare-like X-ray flux amplification early in the development of the classical nova V2672 Ophiuchi. Two target-of-opportunity similar to 25 ks X-ray observations were made 12 and 22 d after the outburst. The flux amplification was found in the latter half of day 12. Time-sliced spectra are characterized by a growing supersoft excess with edge-like structures and a relatively stable optically-thin thermal component with K alpha emission lines from highly ionized Si. The observed spectral evolution is consistent with a model that has a time development of circumstellar absorption, for which we obtained a decline rate of similar to 10%-40% on a time scale of 0.2 d on day 12. Such a rapid drop of absorption and short-term flux variability on day 12 suggests inhomogeneous ejecta with dense blobs/holes in the line-of-sight. Then on day 22 the fluxes of both supersoft and thin-thermal plasma components became significantly fainter. Based on the serendipitous results we discuss the nature of this source in the context of both short- and long-term X-ray behavior.

      DOI: 10.1093/pasj/psu019

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    • Soft x-ray spectrometer (SXS): the high-resolution cryogenic spectrometer onboard ASTRO-H Peer-reviewed

      Mitsuda Kazuhisa, Kelley Richard L, Akamatsu Hiroki, Bialas Thomas, Boyce Kevin R, Brown Gregory V, Canavan Edgar, Chiao Meng, Costantini Elisa, den Herder Jan-Willem, de Vries Cor, DiPirro Michael J, Eckart Megan E, Ezoe Yuichiro, Fujimoto Ryuichi, Haas Daniel, Hoshino Akio, Ishikawa Kumi, Ishisaki Yoshitaka, Iyomoto Naoko, Kilbourne Caroline A, Kimball Mark, Kitamoto Shunji, Konami Saori, Leutenegger Maurice A, McCammon Dan, Miko Joseph, Mitsuishi Ikuyuki, Murakami Hiroshi, Murakami Masahide, Noda Hirofumi, Ogawa Mina, Ohashi Takaya, Okamoto Atsushi, Ota Naomi, Paltani Stephane, Porter F. Scott, Sato Kosuke, Sato Yoichi, Sawada Makoto, Seta Hitomi, Shinozaki Keisuke, Shirron Peter J, Sneiderman Gary A, Sugita Hiroyuki, Szymkowiak Andrew, Takei Yoh, Tamagawa Toru, Tashiro Makoto S, Terada Yukikatsu, Tsujimoto Masahiro, Yamada Shinya, Yamasaki Noriko Y

      SPACE TELESCOPES AND INSTRUMENTATION 2014: ULTRAVIOLET TO GAMMA RAY9144   2014

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    • X-ray eclipse diagnosis of the evolving mass loss in the recurrent nova U Scorpii 2010 Peer-reviewed

      D. Takei, J. J. Drake, M. Tsujimoto, J. U. Ness, J. P. Osborne, S. Starrfield, S. Kitamoto

      Astrophysical Journal Letters769 ( 1 )   20 5 2013

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      We report the Suzaku detection of the earliest X-ray eclipse seen in the recurrent nova U Scorpii 2010. A target-of-opportunity observation 15 days after the outburst found a 27% ± 5% dimming in the 0.2-1.0 keV energy band at the predicted center of an eclipse. In comparison with the X-ray eclipse depths seen at two later epochs by XMM-Newton, the source region shrank by about 10%-20% between days 15 and 35 after the outburst. The X-ray eclipses appear to be deeper than or similar to contemporaneous optical eclipses, suggesting the X-ray and optical source region extents are comparable on day 15. We raise the possibility of the energy dependency in the photon escape regions, and that this would be a result of the supersoft X-ray opacity being higher than the Thomson scattering opacity at the photosphere due to bound-free transitions in abundant metals that are not fully ionized. Assuming a spherically symmetric model, we constrain the mass-loss rate as a function of time. For a ratio of actual to Thomson opacity of 10-100 in supersoft X-rays, we find an ejecta mass of about 10-7-10-6 M . © 2013. The American Astronomical Society. All rights reserved..

      DOI: 10.1088/2041-8205/769/1/L4

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    • Self-Charge-Filling (SCF) Effect of Suzaku XIS Peer-reviewed

      Todoroki Shotaro, Kitamoto Shunji, Yoshida Yuki, Murakami Hiroshi

      PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN64 ( 5 )   25 10 2012

    • The High-Resolution X-Ray Microcalorimeter Spectrometer, SXS, on Astro-H Peer-reviewed

      Mitsuda Kazuhisa, Kelley Richard L, Boyce Kevin R, Brown Gregory V, Costantini Elisa, DiPirro Michael J, Ezoe Yuichiro, Fujimoto Ryuichi, Gendreau Keith C, den Herder Jan-Willem, Hoshino Akio, Ishisaki Yoshitaka, Kilbourne Caroline A, Kitamoto Shunji, McCammon Dan, Murakami Masahide, Murakami Hiroshi, Ogawa Mina, Ohashi Takaya, Okamoto Atsushi, Paltani Stephane, Pohl Martin, Porter F. Scott, Sato Yoichi, Shinozaki Keisuke, Shirron Peter J, Sneiderman Gary A, Sugita Hiroyuki, Szymkowiak Andrew, Takei Yoh, Tamagawa Toru, Tashiro Makoto, Terada Yukikatsu, Tsujimoto Masahiro, de Vries Cor, Yamasaki Noriko Y

      JOURNAL OF LOW TEMPERATURE PHYSICS167 ( 5-6 ) 795 - 802   6 2012

    • A Self Charge Filling (SCF) effect of Suzaku-XIS Peer-reviewed

      Todoroki Shotaro, Kitamoto Shunji, Murakami Hiroshi

      SUZAKU 2011: EXPLORING THE X-RAY UNIVERSE: SUZAKU AND BEYOND1427   2012

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    • Suzaku Observations of Six Early Type Stars Peer-reviewed

      Kitamoto Shunji, Yoshida Masaki, Shimizu Yusuke, Murakami Hiroshi

      SUZAKU 2011: EXPLORING THE X-RAY UNIVERSE: SUZAKU AND BEYOND1427   2012

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    • Detection of X-Ray Emission from the Unidentified TeV Gamma-Ray Source TeV J2032+4130 Peer-reviewed

      Murakami, Hiroshi, Kitamoto, Shunji, Kawachi, Akiko, Nakamori, Takeshi

      PASJ63 ( SP3 ) S873 - S878   12 2011

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    • Observation of the Cygnus OB2 Association with Suzaku and Long Term Light Curves Peer-reviewed

      Yoshida, Masaki, Kitamoto, Shunji, Murakami, Hiroshi

      PASJ2011 ( SP3 ) S717 - S728   12 2011

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    • X-Ray Study of Rekindled Accretion in the Classical Nova V2491 Cygni Peer-reviewed

      Takei, Dai, Ness, Jan-Uwe, Tsujimoto, Masahiro, Kitamoto, Shunji, Drake, Jeremy J, Osborne, Julian P, Takahashi, Hiromitsu, Kinugasa, Kenzo

      PASJ2011 ( SP3 ) S729 - S783   12 2011

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    • Suzaku Observation of the Anomalous X-Ray Pulsar 1E 1841-045 Peer-reviewed

      Mikio Morii, Shunji Ktamoto, Noriaki Shibazaki, Nobuyuki Kawai, Makoto Arimoto, Masaru Ueno, Takayoshi Kohmura, Yukikatsu Terada, Shigeo Yamauchi, Hiromitsu Takahashi

      PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN62 ( 5 ) 1249 - 1259   10 2010

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:OXFORD UNIV PRESS  

      We report on the results of a Suzaku observation of the anomalous X-ray pulsar (AXP) IE 1841-045 at the center of the supernova remnant Kes 73. We confirmed that the energy-dependent spectral models obtained by previous separate observations were also satisfied over a wide energy range from 0.4 to similar to 70 keV, simultaneously. Here, the models below similar to 10 keV were a combination of blackbody (BB) and power-law (PL) functions, or of two BBs with different temperatures at 0.6-7.0 keV (Morii et al. 2003. PASJ, 55, L45), and that above similar to 20 keV was a PL function (Kuiper et al. 2004, ApJ, 613, 1173). The combination BB + PL + PL was found to best represent the phase-averaged spectrum. Phase-resolved spectroscopy indicated the existence of two emission regions, one with a thermal and the other with a non-thermal nature. The combination BB + BB + PL was also found to represent the phase-averaged spectrum well. However, we found that this model is physically unacceptable due to an excessively large area of the emission region of the blackbody. Nonetheless, we found that the temperatures and radii of the two blackbody components showed moderate correlations in the phase-resolved spectra. The fact that the same correlations have been observed between the phase-averaged spectra of various magnetars (Nakagawa et al. 2009, PASJ, 61, 109) suggests that a self-similar function can approximate the intrinsic energy spectra of magnetars below similar to 10 keV.

      DOI: 10.1093/pasj/62.5.1249

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    • Cooling system for the soft X-ray spectrometer onboard Astro-H Peer-reviewed

      Ryuichi Fujimoto, Kazuhisa Mitsuda, Noriko Yamasaki, Yoh Takei, Masahiro Tsujimoto, Hiroyuki Sugita, Yoichi Sato, Keisuke Shinozaki, Takaya Ohashi, Yoshitaka Ishisaki, Yuichiro Ezoe, Masahide Murakami, Shunji Kitamoto, Hiroshi Murakami, Toru Tamagawa, Madoka Kawaharada, Hiroya Yamaguchi, Kosuke Sato, Kenichi Kanao, Seiji Yoshida, Mike DiPirro, Peter Shirron, Gary Sneiderman, Richard L. Kelley, F. Scott Porter, Caroline A. Kilbourne, John Crow, Andrea Mattern, Ali Kashani, Dan McCammon, Jan-Willem den Herder

      CRYOGENICS50 ( 9 ) 488 - 493   9 2010

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:ELSEVIER SCI LTD  

      The Soft X-ray Spectrometer (SXS) is a cryogenic high resolution X-ray spectrometer onboard the X-ray astronomy satellite Astro-H which will be launched in 2014. The detector array is cooled down to 50 mK using an adiabatic demagnetization refrigerator (ADR). The cooling chain from the room temperature to the ADR heat-sink is composed of superfluid liquid He, a Joule-Thomson cryocooler, and double-stage Stirling cryocoolers. It is designed to keep 301 of liquid He for more than 5 years in the normal case, and longer than 3 years even if one of the cryocoolers fails. Cryogen-free operation is also possible in the normal case. It is fully redundant from the room temperature to the ADR heat-sink. (c) 2010 Elsevier Ltd. All rights reserved.

      DOI: 10.1016/j.cryogenics.2010.02.004

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    • A report on the XIS calibration of the 2 × 3 mode and window option and the current status of the XIS NXB database

      Ikegami, Yoshio, Mori, Koji, Aoyama, Shoichi, Kimura, Shoichi, Samukawa, Maina, Yamashita, Toshiya, Kato, Takeshi, Kimura, Yuki, Ishizaki, Yoshinori, Ogawa, Kazuki, Uchiyama, Hideki, Ozawa, Midori, Matsumoto, Hironori, Tsuru, Takeshi Go, Koyama, Katsuji, Hayashida, Kiyoshi, Tsunemi, Hiroshi, Dotani, Tadayasu, Ozaki, Masanobu, Bamba, Aya, Tsujimoto, Masahiro, Kohmura, Takayoshi, Kitamoto, Shunji, Murakami, Hiroshi, Suzaku XIS Team

      Proceedings of the 3rd Suzaku Conference   414 - 415   2 2010

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    • EUV transmission of Optical Blocking Filter and Optical Blocking Layer for Soft X-ray Imager (SXI) onboard Astro-H

      Watanabe, Tatsuo, Kohmura, Takayoshi, Kitamoto, Shunji, Murakami, Hiroshi, Takenaka, Eri, Nagasaki, Kenta, Higashi, Keiichi, Yoshida, Masaki, Tsunemi, Hiroshi, Hayasida, Kiyoshi, Anabuki, Naohisa, Nakajima, Hiroshi, Sakaguchi, Rui, Shigeyama, Kazuo, Tsuru, Takeshi Go, Matsumoto, Hironori, Dotani, Tadayasu, Ozaki, Masanobu, Bamba, Aya, Fujinaga, Takahisa, Mori, Koji, SXI Team

      Proceedings of the 3rd Suzaku Conference   418 - 419   2 2010

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    • X-ray polarimeter with a transmission multilayer

      Shunji Kitamoto, Hiroshi Murakami, Youich Shishido, Norimitsu Gotoh, Takuma Shibata, Kousuke Saito, Takeshi Watanabe, Jun'ichi Kanai, Eri Takenaka, Kenta Nagasaki, Masaki Yoshida, Dai Takei, Mikio Morii

      REVIEW OF SCIENTIFIC INSTRUMENTS81 ( 2 ) 81b3105K   2 2010

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:AMER INST PHYSICS  

      We fabricated a novel x-ray polarimeter with a transmission multilayer and measured its performance with synchrotron radiation. A self standing multilayer with seven Mo/Si bilayers was installed with an incident angle of 45 degrees in front of a back-illuminated CCD. The multilayer can be rotated around the normal direction of the CCD keeping an incident angle of 45 degrees. This polarimeter can be easily installed along the optical axis of x-ray optics. By using the CCD as a photon counting detector with a moderate energy resolution, the polarization of photons in a designed energy band can be measured along with the image. At high photon energies, where the multilayer is transparent, the polarimeter can be used for imaging and spectroscopic observations. We confirmed a modulation factor of 45% with 45% and 17% transmission for P- and S-polarization, respectively.

      DOI: 10.1063/1.3294330

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    • Cooling system for the Soft X-ray Spectrometer (SXS) onboard ASTRO-H Peer-reviewed

      Ryuichi Fujimoto, Kazuhisa Mitsuda, Noriko Yamasaki, Yoh Takei, Masahiro Tsujimoto, Hiroyuki Sugita, Yoichi Sato, Keisuke Shinozaki, Atsushi Okamoto, Takaya Ohashi, Yoshitaka Ishisaki, Yuichiro Ezoe, Kumi Ishikawa, Masahide Murakami, Shunji Kitamoto, Hiroshi Murakami, Toru Tamagawa, Madoka Kawaharada, Hiroya Yamaguchi, Kosuke Sato, Akio Hoshino, Kenichi Kanao, Seiji Yoshida, Mikio Miyaoka, Michael DiPirro, Peter Shirron, Gary Sneiderman, Richard L. Kelley, F. Scott Porter, Caroline A. Kilbourne, John Crow, Andrea Mattern, Ali Kashani, Dan McCammon

      SPACE TELESCOPES AND INSTRUMENTATION 2010: ULTRAVIOLET TO GAMMA RAY7732 ( 9 ) 488 - 493   2010

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      Language:English   Publishing type:Research paper (international conference proceedings)   Publisher:SPIE-INT SOC OPTICAL ENGINEERING  

      The Soft X-ray Spectrometer (SXS) is a cryogenic high resolution X-ray spectrometer onboard the X-ray astronomy satellite ASTRO-H. The detector array is cooled down to 50 mK using a 3-stage adiabatic demagnetization refrigerator (ADR). The cooling chain from room temperature to the ADR heat-sink is composed of superfluid liquid He, a He-4 Joule-Thomson cryocooler, and 2-stage Stirling cryocoolers. It is designed to keep 30 L of liquid He for more than 3 years in the nominal case. It is also designed with redundant subsystems throughout from room temperature to the ADR heat-sink, to alleviate failure of a single cryocooler or loss of liquid He.

      DOI: 10.1117/12.856909

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    • The High-Resolution X-ray Microcalorimeter Spectrometer System for the SXS on ASTRO-H Peer-reviewed

      Mitsuda Kazuhisa, Kelley Richard L, Boyce Kevin R, Brown Gregory V, Costantini Elisa, DiPirro Michael J, Ezoe Yuichiro, Fujimoto Ryuichi, Gendreau Keith C, den Herder Jan-Willem, Hoshino Akio, Ishisaki Yoshitaka, Kilbourne Caroline A, Kitamoto Shunji, McCammon Dan, Murakami Masahide, Murakami Hiroshi, Ogawa Mina, Ohashi Takaya, Okamoto Atsushi, Paltani Stephane, Pohl Martin, Porter F. Scott, Sato Yoichi, Shinozaki Keisuke, Shirron Peter J, Sneiderman Gary A, Sugita Hiroyuki, Szymkowiak Andrew, Takei Yoh, Tamagawa Toru, Tashiro Makoto, Terada Yukikatsu, Tsujimoto Masahiro, de Vries Cor, Yamaguchi Hiroya, Yamasaki Noriko Y

      SPACE TELESCOPES AND INSTRUMENTATION 2010: ULTRAVIOLET TO GAMMA RAY7732   2010

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    • Super-Hard X-Ray Emission from eta Carinae Observed with Suzaku Peer-reviewed

      Akiko Sekiguchi, Masahiro Tsujimoto, Shunji Kitamoto, Manabu Ishida, Kenji Hamaguchi, Hideyuki Mori, Yohko Tsuboi

      PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN61 ( 4 ) 629 - 637   8 2009

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:OXFORD UNIV PRESS  

      We present the Suzaku results of eta Carinae in the 5-50 keV range conducted twice around the apastron in 2005 August for 50 ks and in 2006 February for 20 ks. The X-ray Imaging Spectrometer (XIS) produced hard (5-12 keV) band spectra, resolving K shell lines from highly ionized Fe and Ni. The Hard X-ray Detector yielded a significant detection in the super-hard (15-50 keV) band, which was uncontaminated by near-by sources. We constrained the temperature of the optically thin thermal plasma emission dominant in the hard band to be 3-4 keV using the K-shell line features with the XIS. We found significant excess emission above the thermal emission in the super-hard band with the PIN, confirming the previous INTEGRAL ISGRI report. The entire 5-50 keV spectra were fitted by a combination of a thermal plasma model plus a flat power-law, or a very hot thermal bremsstrahlung model for the excess emission. No significant change of the excess emission was found at different epochs within the systematic and statistical uncertainties, and no flare-like flux amplification was seen in the hard band, indicating that the excess emission is a steady phenomenon. We argue that the super-hard emission is attributable to the inverse Compton of stellar UV photons by non-thermal electrons or to the thermal bremsstrahlung of very hot plasma, and not to the bremsstrahlung by non-thermal electrons colliding with cold ambient matter.

      DOI: 10.1093/pasj/61.4.629

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    • SUZAKU DETECTION OF SUPERHARD X-RAY EMISSION FROM THE CLASSICAL NOVA V2491 CYGNI Peer-reviewed

      D. Takei, M. Tsujimoto, S. Kitamoto, J. -U. Ness, J. J. Drake, H. Takahashi, K. Mukai

      ASTROPHYSICAL JOURNAL LETTERS697 ( 1 ) L54 - L57   5 2009

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      We report the detection of superhard (> 10 keV) X-ray emission extending up to 70 keV from the classical nova V2491 Cygni using the Suzaku observatory. We conducted two similar to 20 ks target-of-opportunity observations 9 and 29 days after the outburst on 2008 April 11, yielding wide energy range spectra by combining the X-ray Imaging Spectrometer and the Hard X-ray Detector. On day 9, a spectrum was obtained at 1.0-70 keV with the Fe xxv K alpha line feature and a very flat continuum, which is explained by thermal plasma with a 3 keV temperature and power-law emission with a photon index of 0.1 attenuated by a heavy extinction of 1.4 x 10(23) cm(-2). The 15-70 keV luminosity at 10.5 kpc is 6 x 10(35) erg s(-1). The superhard emission was not present on day 29. This is the highest energy at which X-rays have been detected from a classical nova. We argue a nonthermal origin for the emission, which suggests the presence of accelerated charged particles in the nova explosion.

      DOI: 10.1088/0004-637X/697/1/L54

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    • SWIFT X-RAY AND ULTRAVIOLET MONITORING OF THE CLASSICAL NOVA V458 VUL (NOVA VUL 2007) Peer-reviewed

      J. -U. Ness, J. J. Drake, A. P. Beardmore, D. Boyd, M. F. Bode, S. Brady, P. A. Evans, B. T. Gaensicke, S. Kitamoto, C. Knigge, I. Miller, J. P. Osborne, K. L. Page, P. Rodriguez-Gil, G. Schwarz, B. Staels, D. Steeghs, D. Takei, M. Tsujimoto, R. Wesson, A. Zijlstra

      ASTRONOMICAL JOURNAL137 ( 5 ) 4160 - 4168   5 2009

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      We describe the highly variable X-ray and UV emission of V458 Vul (Nova Vul 2007), observed by Swift between 1 and 422 days after outburst. Initially bright only in the UV, V458 Vul became a variable hard X-ray source due to optically thin thermal emission at kT = 0.64 keV with an X-ray band unabsorbed luminosity of 2.3 x 10(34) erg s(-1) during days 71-140. The X-ray spectrum at this time requires a low Fe abundance (0.2(-0.1)(+ 0.3) solar), consistent with a Suzaku measurement around the same time. On day 315 we find a new X-ray spectral component which can be described by a blackbody with temperature of kT = 23(-5)(+9) eV, while the previous hard X-ray component has declined by a factor of 3.8. The spectrum of this soft X-ray component resembles those typically seen in the class of supersoft sources (SSS) which suggests that the nova ejecta were starting to clear and/or that the white dwarf photosphere is shrinking to the point at which its thermal emission reaches into the X-ray band. We find a high degree of variability in the soft component with a flare rising by an order of magnitude in count rate in 0.2 days. In the following observations on days 342.4-383.6, the soft component was not seen, only to emerge again on day 397. The hard component continued to evolve, and we found an anticorrelation between the hard X-ray emission and the UV emission, yielding a Spearman rank probability of 97%. After day 397, the hard component was still present, was variable, and continued to fade at an extremely slow rate but could not be analyzed owing to pile-up contamination from the bright SSS component.

      DOI: 10.1088/0004-6256/137/5/4160

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    • Search for Near-Infrared Pulsation of the Anomalous X-Ray Pulsar 4U 0142+61 Peer-reviewed

      Mikio Morii, Naoto Kobayashi, Nobuyuki Kawai, Hiroshi Terada, Yasuyuki T. Tanaka, Shunji Kitamoto, Noriaki Shibazaki

      PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN61 ( 1 ) 51 - 56   2 2009

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:OXFORD UNIV PRESS  

      We have searched for pulsation of the anomalous X-ray pulsar (AXP) 4U 0142+61 in the K' band (lambda(eff) = 2.11 mu m) using the fast-readout mode of Infrared Camera and Spectrograph (IRCS) at the Subaru 8.2 m telescope. We found no significant signal at the pulse frequency expected by the precise ephemeris based on an X-ray monitoring observation with RXTE. Nonetheless, we obtained the best upper limit of 17% (90% C.L.) for the root-means-quare pulse fraction in the K' band. Combined with the i' band pulsation (Dhillon et a]. 2005, MNRAS, 363, 609), the slope of the pulsed component (F-nu alpha nu(alpha) in units of Jy) was constrained to alpha > -0.87 (90% C.L.) for an interstellar extinction of A(V) = 3.5.

      DOI: 10.1093/pasj/61.1.51

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    • X-Ray Spectroscopy of the Classical Nova V458 Vulpeculae with Suzaku Peer-reviewed

      Masahiro Tsujimoto, Dai Takei, Jeremy J. Drake, Jan-Uwe Ness, Shunji Kitamoto

      PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN61   S69 - S76   1 2009

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:OXFORD UNIV PRESS  

      We conducted a target of opportunity X-ray observation of the classical nova V458 Vulpeculae 88 d after the explosion using the Suzaku satellite. With a similar to 20 ks exposure, the X-ray Imaging Spectrometer detected X-ray emission significantly harder than typical super-soft Source emission. The X-ray spectrum shows K alpha lines from N, Ne, Mg, Si, and S, and L-series emission from Fe in highly ionized states. The spectrum can be described by a single-temperature (similar to 0.64 keV) thin thermal plasma model in collisional equilibrium with a hydrogen-equivalent extinction column density of similar to 3 x 10(21) cm(-2), a flux of similar to 10(-12) erg s(-1) cm(-2), and a luminosity of similar to 6 x 10(34) erg s(-1) in the 0.3-3.0 keV band at an assumed distance of 13 kpc. We found a hint of an enhancement of N and deficiencies of O and Fe relative to other metals. The observed X-ray properties can be interpreted as the emission arising from shocks of ejecta from an ONe-type nova.

      DOI: 10.1093/pasj/61.sp1.S69

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    • Development of an EUV polarimeter with a transmission multilayer Peer-reviewed

      S. Kitamoto, H. Murakami, Y. Shishido, K. Saito, T. Watanabe, J. Kanai, E. Takenaka, K. Nagasaki, D. Takei, M. Morii

      Proceedings of SPIE - The International Society for Optical Engineering7435   2009

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      We developed an EUV polarimeter consisting of a transmission multilayer and a back-illumination CCD. The transmission of the multilayer at an incident angle of45-deg depends on the polarization angle. We developed a polarimeter by using the transmission. Advantages of usage a transmission multilayer are as follows. 1) The mechanics is simple, because we do not need to move the detectors. 2) High energy photons, where the multilayer is transparent, can be measured as a normal observation, if we use a CCD as a photon counting. 3) By removing the multilayer from the optical axis, normal observation with a CCD can be performed. A stand alone multilayer of Mo/Si was fabricated, which consists of seven layer-pairs with a thickness of 20 nm. We evaluated the performance of the polarimeter using a synchrotron beam line. We confirmed a modulation factor of 47% around 95 eV. © 2009 Copyright SPIE - The International Society for Optical Engineering.

      DOI: 10.1117/12.825074

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    • The X-ray microcalorimeter on the NeXT mission

      Kazuhisa Mitsuda, Noriko Y. Yamasaki, Keisuke Shinozaki, Yoh Takei, Takao Nakagawai, Hiroyuki Sugitai, Yohichi Satoh, Ryuichi Fujimoto, Takaya Ohashi, Yoshitaka Ishisaki, Yuichiro Ezoe, Masahide Murakami, Makoto Tashiro, Yukikatsu Terada, Shunji Kitamoto, Toru Tamagawa, Madoka Kawaharada, Tatehiro Mihara, Richard L. Kelley, Caroline A. Kilbourne, F. Scott Porter, Peter J. Shirron, Michael J. Dipirro, Dan Mccammon, Jan Willem Den Herder

      Proceedings of SPIE - The International Society for Optical Engineering7011   1 12 2008

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      The Soft X-ray Spectrometer (SXS) onboard the NeXT (New exploration X-ray Telescope) is an X-ray spectrometer utilizing an X-ray microcalorimeter array. Combined with the soft X-ray telescope of 6 m focal length, the instrument will have a ∼ 290cm2 effective at 6.7 keV. With the large effective area and the energy resolution as good as 6 eV (FWHM), the instrument is very suited for the high-resolution spectroscopy of iron K emission line. One of the major scientific objectives of SXS is to determine turbulent and/or macroscopic motions of the hot gas in clusters of galaxies of up to z ∼ 1. The instruments will use 6 × 6 or 8 × 8 format microcalorimeter array which is similar to that of Suzaku XRS. The detector will be cooled to a cryogenic temperature of 50 mK by multi-stage cooling system consisting of adiabatic demagnetization refrigerator, super fluid He, a 3He Joule Thomson cooler, and double-stage Stirling cycle cooler.

      DOI: 10.1117/12.787952

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    • Suzaku results on Cygnus X-1 in the low/hard state Peer-reviewed

      Makishima Kazuo, Takahashi Hiromitsu, Yamada Shin'ya, Done Chris, Kubota Aya, Dotani Tadayasu, Ebisawa Ken, Itoh Takeshi, Kitamoto Shunji, Negoro Hitoshi, Ueda Yoshihiro, Yamaoka Kazutaka

      PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN60 ( 3 ) 585 - 604   25 6 2008

    • Suzaku spectroscopy of extended X-ray emission in M17

      Yoshiaki Hyodo, Masahiro Tsujimoto, Masahiro Tsujimoto, Kenji Hamaguchi, Kenji Hamaguchi, Katsuji Koyama, Shunji Kitamoto, Yoshitomo Maeda, Yohko Tsuboi, Yuichiro Ezoe

      Publications of the Astronomical Society of Japan60   24 4 2008

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      We present the results of a Suzaku spectroscopic study of soft extended X-ray emission in the H II region of M17. The spectrum of the extended emission was obtained with a high signal-to-noise ratio in a spatially resolved manner using the X-ray Imaging Spectrometer (XIS). We established that contamination by unresolved point sources, the Galactic Ridge X-ray emission, the cosmic X-ray background, and the local hot bubble emission is negligible in the background-subtracted XIS spectrum of the diffuse emission. Half a dozen emission lines were clearly resolved for the first time, including Kα lines of highly ionized O, Ne, and Mg as well as L-series complex of Fe at 0.51.5 keV. Based on diagnosis of these lines, we obtained the following results: (1) the extended emission is an optically thin thermal plasma, represented well by a single temperature of ∼ 3.0 ± 0.4MK, (2) the abundances of elements with emission lines in the diffuse spectrum are 0.1-0.3 solar, while those of bright discrete sources are 0.3-1.5 solar, (3) the metal abundances relative to each other in the diffuse emission are consistent with solar, except for a Ne enhancement of a factor of ∼ 2, (4) both the plasma temperature and the chemical composition of the diffuse emission show no spatial variation across the studied spatial scale of ∼ 5 pc. © 2008. Astronomical Society of Japan.

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    • Detection of a rare supersoft outburst event during a Suzaku observation of 1E0102.2-7219 Peer-reviewed

      Takei Dai, Tsujimoto Masahiro, Kitamoto Shunji, Mor Mikio, Ebisawa Ken, Maeda Yoshitomo, Miller Eric D

      PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN60   S231 - S239   20 2 2008

    • Broadband X-ray spectroscopy of A0535+262 with Suzaku Peer-reviewed

      S. Naik, T. Dotani, Y. Terada, M. Nakajima, T. Mihara, M. Suzuki, K. Makishima, K. Sudoh, S. Kitamoto, F. Nagase, T. Enoto, H. Takahashi

      ASTROPHYSICAL JOURNAL672 ( 1 ) 516 - 523   1 2008

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:IOP PUBLISHING LTD  

      The transient X-ray binary pulsar A0535+262 was observed with Suzaku on 2005 September 14 when the source was in the declining phase of the August-September minor outburst. The similar to 103 s X-ray pulse profile was strongly energy dependent, with a double-peaked profile in the soft X-ray energy band (< 3 keV) and a single-peaked smooth profile in hard X-rays. The width of the primary dip is found to increase with energy. The broadband energy spectrum of the pulsar is well described with a negative and positive power law with exponential (NPEX) continuum model, along with a blackbody component for soft excess. A weak iron K alpha emission line with an equivalent width similar to 25 eV was detected in the source spectrum. The blackbody component is found to be pulsating over the pulse phase, implying that the accretion column and/or the inner edge of the accretion disk may be the possible emission site of the soft excess in A0535+262. The higher value of the column density is believed to be the cause of the secondary dip in the soft X-ray energy band. The iron line equivalent width is found to be constant (within errors) over the pulse phase. However, a sinusoidal type of flux variation of the iron emission line, in phase with the hard X-ray flux, suggests that the inner accretion disk is the possible emission region of the iron fluorescence line.

      DOI: 10.1086/523295

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    • EUV-Imaging experiments of a normal Incident telescope with an adaptive optics system Peer-reviewed

      S. Kitamoto, T. Ogita, T. Shibata, E. Takenaka, N. Gotoh, Y. Shishido, D. Takei, M. Yoshida, M. Moriia, H. Murakami

      Proceedings of SPIE - The International Society for Optical Engineering7015   2008

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      Language:English   Publishing type:Research paper (international conference proceedings)  

      We are developing a normal incident EUV-telescope for a future space experiment, using an adaptive optics. The primary mirror and the secondary mirror were coated with Mo/Si multi-layers. The secondary mirror is a deformable mirror. The reference wave is produced with a 1 micro-m pin hole laser and its wave front shape is used for a correction of the EUV wave shape. The imaging experiments with optical was performed with the adaptive optics system. The imaging with 13.5nm EUV was also performed but without the adaptive optics system. The optical image is almost diffraction limited. A ray trace simulation was performed and a correction method in our system, where the EUV wave form is corrected using the optical reference lights, was investigated.

      DOI: 10.1117/12.787740

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    • Low/hard state spectra of GRO J1655-40 observed with Suzaku Peer-reviewed

      Takahashi H, Fukazawa Y, Mizuno T, Hirasawa A, Kitamoto S, Sudoh K, Ogita T, Kubota A, Makishima K, Itoh T, Parmar A.N, Ebisawa K, Naik S, Dotani T, Kokubun M, Ohnuki K, Takahashi T, Yaqoob T, Angelini L, Ueda Y, Yamaoka K, Kotani T, Kawai N, Namlki M, Kohmura T, Negoro H

      Publications of the Astronomical Society of Japan60 ( SPEC. ISS. 1 )   2008

    • Oxygen line mapping of SN 1006 with Suzaku Peer-reviewed

      Bamba, Aya, Yamaguchi, Hiroya, Koyama, Katsuji, Hiraga, Junko S, Holt, Steve, Hughes, John P, Katagiri, Hideaki, Kataoka, Jun, Katsuda, Satoru, Kitamoto, Shunji, Kokubun, Motohide, Matsumoto, Hironori, Miyata, Emi, Mori, Koji, Nakajima, Hiroshi, Ozaki, Masanobu, Petre, Rob, Sekiguchi, Akiko, Takahashi, Tadayuki, Tanaka, Takaaki, Terada, Yukikatsu, Tomida, Hiroshi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Uchiyama, Yasunobu, Ueno, Masaru, Watanabe, Shin

      Advances in Space Research41 ( 3 ) 411 - 415   2008

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      DOI: 10.1016/j.asr.2007.03.055

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    • Ground bakeout experiment of the optical blocking filter (OBF) for the Suzaku XIS

      Mori, Hideyuki, Tsuru, Takeshi Go, Matsumoto, Hironori, Uchiyama, Hideki, Ozawa, Midori, Takikawa, Yohjiro, Nobukawa, Masayoshi, Koyama, Katsuji, Torii, Ken'ichi, Tawa, Noriaki, Kitamoto, Shunji, Sudoh, Keisuke, Kohmura, Takayoshi

      Proceedings of the SPIE6686   id.66860O   9 2007

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      DOI: 10.1117/12.732293

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    • Suzaku observation of diffuse X-ray emission from the Carina Nebula

      Kenji Hamaguchi, Robert Petre, Hironori Matsumoto, Masahiro Tsujimoto, Stephen S. Holt, Yuichiro Ezoe, Hideki Ozawa, Yohko Tsuboi, Yang Soong, Shunji Kitamoto, Akiko Sekiguchi, Motohide Kokubun

      PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN59 ( S151 ) S151 - S161   1 2007

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:OXFORD UNIV PRESS  

      We studied extended X-ray emission from the Carina Nebula taken with the Suzaku CCD camera XIS on 2005 August 29. The X-ray morphology, plasma temperature, and absorption to the plasma are consistent with the earlier Einstein results. The Suzaku spectra newly revealed emission lines from various species, including oxygen, but not from nitrogen. This result restricts the N/O ratio to be significantly low, compared with evolved massive stellar winds, suggesting that the diffuse emission originated in an old supernova remnant or a super shell produced by multiple supernova remnants. The X-ray spectra from the north and south of eta Car showed distinct differences between 0.3-2 keV. The south spectrum shows strong L-shell lines of iron ions and K-shell lines of silicon ions, while the north spectrum shows them weak in intensity. This means that the silicon and iron abundances are a factor of 2-4 higher in the south region than in the north region. The abundance variation may be produced by an SNR ejecta, or related to dust formation around the star-forming core.

      DOI: 10.1093/pasj/59.sp1.S151

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    • The X-ray observatory Suzaku

      Kazuhisa Mitsuda, Mark Bautz, Hajime Inoue, Richard L. Kelley, Katsuji Koyama, Hideyo Kunieda, Kazuo Makshima, Yoshiaki Ogawara, Robert Petre, Tadayuki Takahashi, Hiroshi Tsunemi, Nicholas E. White, Naohisa Anabuki, Lorella Angelini, Keith Arnaud, Hisamitsu Awaki, Aya Bamba, Kevin Boyce, Gregory V. Brown, Kai-Wing Chan, Jean Cottam, Tadayasu Dotanli, John Doty, Ken Ebisawa, Yuichiro Ezoe, Andrew C. Fabian, Enectali Figueroa, Ryuichi Fujimoto, Yasushi Fukazawa, Tae Furusho, Akihiro Furuzawa, Keith Gendreau, Richard E. Griffiths, Yoshito Haba, Kenji Hamaguchi, Ilana Harrus, Gunther Hasinger, Isamu Hatsukade, Kiyoshi Hayashida, Patrick J. Henry, Junko S. Hiraga, Stephen S. Holt, Ann Hornschemeier, John P. Hughes, Una Hwang, Manabu Ishida, Yoshitaka Ishisaki, Naoki Isobe, Masayuki Itoh, Naoko Iyomoto, Steven M. Kahn, Tuneyoshi Kamae, Hideaki Katagiri, Jun Kataoka, Haruyoshi Katayama, Nobuyuki Kawai, Caroline Kilbourne, Kenzo Kinugasa, Steve Kissel, Shunji Kitamoto, Mitsuhiro Kohama, Takayoshi Kohmura, Motohide Kokubun, Taro Kotani, Jun'ichi Kotoku, Aya Kubota, Greg M. Madejski, Yoshitomo Maeda, Fumiyoshi Makino, Alex Markowitz, Chiho Matsumoto, Hironori Matsumoto, Masaru Matsuoka, Kyoko Matsushita, Dan McCammon, Tatehiko Mihara, Kazutami Misaki, Emi Miyata, Tsunefumi Mizuno, Koji Mori, Hideyuki Mori, Mikio Morii, Harvey Moseley, Koji Mukai, Hiroshi Murakami, Toshio Murakami, Richard Mushotzky, Fumiaki Nagase, Masaaki Namiki, Hitoshi Negoro, Kazubiro Nakazawa, John A. Nousek, Takashi Okajima, Yasushi Ogasaka, Takaya Ohashi, Tai Oshima, Naomi Ota, Masanobu Ozaki, Hideki Ozawa, Arvind N. Parmar, William D. Pence, F. Scott Porter, James N. Reeves, George R. Ricker, Ikuya Sakurai, Wilton T. Sanders, Atsushi Senda, Peter Serlemitsos, Ryo Shibata, Yang Soong, Randall Smith, Motoko Suzuki, Andrew E. Szymkowiak, Hiromitsu Takahashi, Torn Tamagawa, Keisuke Tamura, Takayuki Tamura, Yasuo Tanaka, Makoto Tashiro, Yuzuru Tawara, Yukikatsu Terada, Yuichi Terashima, Hiroshi Tomida, Ken'ichi Torii, Yohko Tsuboi, Masahiro Tsujimoto, Takeshi Go Tsuru, Martin J. L. Turner, Yoshihiro Ueda, Shiro Ueno, Masaru Ueno, Shin'ichiro Uno, Yuji Urata, Shin Watanabe, Norimasa Yamamoto, Kazutaka Yamaoka, Noriko Y. Yamasaki, Koujun Yamashita, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Daisuke Yonetoku, Atsumasa Yoshida

      PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN59 ( S1 ) S1 - S7   1 2007

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:OXFORD UNIV PRESS  

      High-sensitivity wide-band X-ray spectroscopy is the key feature of the Suzaku X-ray observatory, launched on 2005 July 10. This paper summarizes the spacecraft, in-orbit performance, operations, and data processing that are related to observations. The scientific instruments, the high-throughput X-ray telescopes, X-ray CCD cameras, non-imaging hard X-ray detector are also described.

      DOI: 10.1093/pasj/59.sp1.S1

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    • X-ray Imaging Spectrometer (XIS) on board Suzaku

      Katsuji Koyama, Hiroshi Tsunemi, Tadayasu Dotani, Mark W. Bautz, Kiyoshi Hayashida, Takeshi Go Tsuru, Hironori Matsumoto, Yoshiaki Ogawara, George R. Ricker, John Doty, Steven E. Kissel, Rick Foster, Hiroshi Nakajima, Hiroya Yamaguchi, Hideyuki Mori, Masaaki Sakano, Kenji Hamaguchi, Mamiko Nishiuchi, Emi Miyata, Ken'ichi Torii, Masaaki Namiki, Satoru Katsuda, Daisuke Matsuura, Tomofumi Miyauchi, Naohisa Anabuki, Noriaki Tawa, Masanobu Ozaki, Hiroshi Murakami, Yoshitomo Maeda, Yoshinori Ichikawa, Gregory Y. Prigozhin, Edward A. Boughan, Beverly LaMarr, Eric D. Miller, Barry E. Burke, James A. Gregory, Allen Pillsbury, Aya Bamba, Junko S. Hiraga, Atsushi Senda, Haruyoshi Katayama, Shunji Kitamoto, Masahiro Tsujimoto, Takayoshi Kohmura, Yohko Tsubol, Hisamitsu Awak

      PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN59 ( S23 ) S23 - S33   1 2007

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:OXFORD UNIV PRESS  

      The XIS is an X-ray Imaging Spectrometer system, consisting of state-of-the-art charge-coupled devices (CCDs) optimized for X-ray detection, camera bodies, and control electronics. Four sets of XIS sensors are placed at the focal planes of the grazing-incidence, nested thin-foil mirrors (XRT: X-Ray Telescope) orboard the Suzaku satellite. Three of the XIS sensors have front-illuminated CCDs, while the other has a back-illuminated CCD. Coupled with the XRT, the energy range of 0.2-12 keV with energy resolution of 130 eV at 5.9 keV, and a field of view of 18' x 18' are realized. Since the Suzaku launch on 2005 July 10, the XIS has been functioning well.

      DOI: 10.1093/pasj/59.sp1.S23

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    • Millenium study of SN 1006 with suzaku Peer-reviewed

      Bamba Aya, Yamaguchi Hiroya, Koyama Katsuji, Hiraga Junko S, Holt Steve, Hughes John P, Katagiri Hideaki, Kataoka Jun, Kitamoto Shunji, Kokubun Motohide, Matumoto Hironori, Miyata Emi, Mori Koji, Nakajima Hiroshi, Ozaki Masanobu, Petre Robert, Sekiguchi Akiko, Takahashi Tadayuki, Tanaka Takaaki, Terada Yukikatsu, Tomida Hiroshi, Tsunemi Hiroshi, Tsub Yohko, Tsujimoto Masahiro, Uchiyama Yasunobu, Ueno Masaru, Watanabe Shin

      PROGRESS OF THEORETICAL PHYSICS SUPPLEMENT ( 169 ) 142 - 145   2007

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    • Orbital calibration of the XIS Peer-reviewed

      K. Hayashida, K. Toru, M. Namiki, N. Anabuki, S. Katsuda, N. Tawa, T. Miyauchi, K. Hasuike, M. Nagai, H. Tsunemi, H. Matsumoto, T.G. Tsuru, H. Mori, H. Nakajima, H. Yamaguchi, Y. Hyodo, T. Inui, H. Uchiyama, M. Ozawa, K. Koyama, E.D. Miller, M.W. Bautz, B. LaMarr, S.E. Kissel, T. Dotani, H. Murakami, M. Ozaki, T. Anada, A. Bamba, J. Hiraga, A. Senda, D. Takei, S. Kitamoto, K. Mori, S. Maeno

      Progress of Theoretical Physics Supplement ( 169 ) 316 - 321   2007

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    • Suzaku observations of cyclotron resonances in binary X-ray pulsars Peer-reviewed

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

      Advances in Space Research40 ( 10 ) 1485 - 1490   2007

    • X-ray emission-line profiles of three early-type stars observed with chandra

      Norimasa Yamamoto, Haruko Takano, Shunji Kitamoto, Takayoshi Kohmura

      Publications of the Astronomical Society of Japan59 ( 1 ) 237 - 244   2007

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:Oxford University Press  

      We analyzed the X-ray emission-line profiles of three early-type stars (ζ Pup, δ Ori, and τ Sco) obtained with Chandra. A phenomenological model, where X-ray sources are distributing in wind above some lower limit radius, can fit the line profiles of ζ Pup and δ Ori
      however, the fitting requires a much smaller absorption than expected from the mass-loss rate. This suggests that, if this phenomenological model represents the real X-ray emission region, there is substantial ionization or clumping of the stellar wind. The parameters derived from the line profile of τ Sco indicate that the X-ray-emitting plasma is concentrated on the stellar surface, suggesting the existence of a confined plasma on the stellar surface. © 2007. Astronomical Society of Japan.

      DOI: 10.1093/pasj/59.1.237

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    • Cyclotron resonance energies at a low X-ray luminosity: A0535+262 observed with Suzaku

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

      ASTROPHYSICAL JOURNAL648 ( 2 ) L139 - L142   9 2006

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:UNIV CHICAGO PRESS  

      The binary X-ray pulsar A0535 + 262 was observed with the Suzaku X-ray observatory on 2005 September 14 for a net exposure of 22 ks. The source was in the declining phase of a minor outburst, exhibiting 3-50 keV luminosity of similar to 3.7 x 10(35) ergs s(-1) at an assumed distance of 2 kpc. In spite of the very low source intensity ( about 30 mcrab at 20 keV), its electron cyclotron resonance was detected clearly with the Suzaku Hard X-Ray Detector, in absorption at about 45 keV. The resonance energy is found to be essentially the same as that measured when the source is almost 2 orders of magnitude more luminous. These results are compared with the luminosity-dependent changes in the cyclotron resonance energy, observed from 4U 0115 + 63 and X0331 + 53.

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    • Periodic long-term X-ray radio variability of Cygnus X-1

      北本 俊二

      MNRAS368   1025 - 1039   1 1 2006

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    • Suzaku broadband observations of galactic black hole binaries: Low/hard state spectra of GRO J1655-40 Peer-reviewed

      Takahashi H, Fukazawa Y, Mizuno T, Hirasawa A, Kitamoto S, Sudoh K, Ogita T, Kubota A, Makishima K, Kokubun M, Itoh T, Parmar A.N, Dotani T, Ebisawa K, Naik S, Takahashi T, Ohnuki K, Yaqoob T, Angelini L, Ueda Y, Yamaoka K, Kotani T, Kawai N, Namiki M, Kohmura T, Negoro H

      European Space Agency, (Special Publication) ESA SP ( 622 SP ) 325 - 332   2006

    • The development of a back-illuminated supportless CCD for SXI onboard next Peer-reviewed

      T.G. Tsuru, S. Takagi, H. Matsumoto, T. Inui, M. Ozawa, K. Koyama, H. Tsunemi, K. Hayashida, E. Miyata, H. Ozawa, M. Touhiguchi, D. Matsuura, T. Dotani, M. Ozaki, H. Murakami, T. Kohmura, S. Kitamoto, H. Awaki

      European Space Agency, (Special Publication) ESA SP2 ( 604 ) 975 - 976   2006

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    • Development of a new radiation detector utilizing CNTs as anodes,

      北本 俊二

      Physica, E29   505 - 509   1 1 2005

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    • Soft Lag and its Implication of X-Ray Time Variation in GRS 1915+105

      北本 俊二

      ApJ621   951 - 958   1 1 2005

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    • The development of a back-illuminated supportless CCD for SXI onboard the NeXT satellite Peer-reviewed

      T.G. Tsuru, S. Takagi, H. Matsumoto, T. Inui, K. Koyama, H. Tsunemi, K. Hayashida, E. Miyata, T. Dotani, M. Ozaki, H. Awaki, S. Kitamoto, T. Kohmura

      Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment541 ( 1-2 ) 392 - 397   2005

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    • X-ray imaging spectrometers (XIS) of Astro-E2 Peer-reviewed

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

      Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment541 ( 1-2 ) 357 - 364   2005

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    • GX339-4;the distance, state transition, hysteresis and spectral correlations

      北本 俊二

      MNRAS351 ( 3 ) 791 - 807   1 1 2004

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    • Development of an ultra-high precision X-ray telescope

      S Kitamoto, H Takano, H Saitoh, N Yamamoto, T Kohmura, K Suga, H Sekiguchi, Y Ohkawa, J Kanai, S Chiba

      PROGRESS OF THEORETICAL PHYSICS SUPPLEMENT155 ( 155 ) 363 - 364   2004

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:PROGRESS THEORETICAL PHYSICS PUBLICATION OFFICE  

      We are developing an ultra-high precision soft X-ray telescope. The design of the telescope is a normal incident one for the 13.5 nm band using Mo/Si multilayers. Two ideas are introduced, an optical measurement system to monitor the precision of the optics system, and an adaptive optics system with a deformable mirror. Using an X-ray-optical separation filter, we can always monitor the deformation of the optics by optical light. With this information, we can control the deformable mirror in order to compensate for the system distortion as a closed loop system. Here, we report the current status of this project.

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    • X-ray time variation of GRS 1915+105

      Y Ohkawa, S Kitamoto, T Kohmura

      PROGRESS OF THEORETICAL PHYSICS SUPPLEMENT155 ( 155 ) 393 - 394   2004

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:PROGRESS THEORETICAL PHYSICS PUBLICATION OFFICE  

      The X-ray time variation of GRS 1915+105 is analyzed, focusing on the phase lag properties in the class theta. An energy dependent soft lag is derived. This energy dependence can be interpreted in terms of the Comptonization of high energy photons by relatively soft electrons. A Monte Carlo simulation of the Comptonization is calculated. In this computation, photons with a power-law spectrum are scattered by soft electrons. This model can account for both the spectral properties and the time variation. With this model, the size of the electron cloud which is responsible for the Comptonization is derived to be similar to3.2 x 10(7-8) cm.

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    • Soft X-ray Transmission of Optical Blocking Filter for the X-ray CCD Camera onboard Astro-E2

      S. Kitamoto

      NIMA505.683-687   4 2003

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    • Soft X-ray transmission of optical blocking filter for the X-ray CCD cameras onboad Astro E2

      北本 俊二

      NIMA505.683-687 ( 205 ) 683 - 687   1 1 2003

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    • 放射光を使った原子物理と天文物理との接点 ― 原子イオンの光電離実験 ―

      北本 俊二

      放射光 ( 4 ) 19 - 28   1 1 2002

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    • A novel method to estimate the thickness of the depletion layer of an X-ray CCD

      北本 俊二

      NIMA   232 - 239   1 1 2002

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    • Long-term X-ray variability and state transition of GX 339-4

      AKH Kong, PA Charles, E Kuulkers, S Kitamoto

      MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY329 ( 3 ) 588 - 596   1 2002

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:BLACKWELL PUBLISHING LTD  

      With extensive monitoring data spanning over 30 years from Vela 5B, Ariel 5, Ginga, Compton Gamma Ray Observatory, Rossi X-ray Timing Explorer and BeppoSAX, we find evidence for long-term X-ray variability on time-scales similar to 190-240d from the black hole low-mass X-ray binary system GX339-4. Such variability resembles the outburst cycle of Z Cam-type dwarf novae, in which the standard disc instability model plays a crucial role. If such a model is applicable to GX 339-4, then the observed variability might be due to the irradiation of an unstable accretion disc. We show that within the framework of the X-ray irradiation model, when the accretion rate exceeds a critical value, GX 339-4 enters a 'flat-topped' high/soft state, such as seen in 1998, which we suggest corresponds to the 'standstill' state of Z Cam systems.

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    • Energy spectra and normalized power spectral densities of X-ray nova GS 2000 + 25

      Kentaro Terada, Shunji Kitamoto, Hitoshi Negoro, Sayuri Iga

      Publications of the Astronomical Society of Japan54 ( 4 ) 609 - 627   2002

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:Astronomical Society of Japan  

      The X-ray energy spectra and Normalized Power Spectral Densities (NPSDs) of an X-ray nova, GS 2000 + 25, were investigated. The X-ray energy spectra of the source consist of two components: a hard component, which can be represented by a power-law, and an ultra-soft component, represented by radiation from an optically-thick accretion disk (the disk component). In a model in which the power-law component is the Compton-scattered radiation, it is found that the temperature of the incident blackbody radiation to the Compton cloud decreases from 0.8 kev to 0.2 kev according to the decay of the intensity, which coincides with that of the inner accretion disk. When the source changed from the high-state to the low-state, both the photon index of the power-law component (or Compton y-parameter) and the NPSD of the hard component dramatically changed as did GS 1124-683. That is, the photon index changed from 2.2-2.6 to 1.7-1.8 and the absolute values of the NPSDs at 0.3 Hz of the hard component in the low-state became about 10-times larger than those of the hard component in the high-state. These X-ray properties were similar to those of other black-hole candidates, such as Cyg X-1, GX 339-4, and LMC X-3.

      DOI: 10.1093/pasj/54.4.609

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    • 「あすか」が見た星形成領域と若い星

      北本 俊二

      日本物理学会誌56 ( 12 ) 905 - 908   1 1 2001

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    • Measurement of the response characteristics around K Absorption Edges of dead-layer materials of a Charge-Coupled-Device

      北本 俊二

      NIMA   191 - 199   1 1 2001

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    • Temporal and Spectral Variations of the Superposed Shot as Causes of Power Spectral Densities and Hard X-ray Time Lags of Cygnus X-1

      北本 俊二

      ApJ ( 554 ) 528 - 533   1 1 2001

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    • Delayed iron lines in centaurus X-3

      T. Kohmura, S. Kitamoto, K. Torii

      Astrophysical Journal562 ( 2 ) 943 - 949   2001

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:Institute of Physics Publishing  

      We present the study of the aperiodic time variation of the binary X-ray pulsar Centaurus X-3 observed with the Rossi X-Ray Timing Explorer (RXTE). We extracted light curves from six energy bands and calculated cross-spectral functions between the energy band containing the iron K lines (iron band) and the remaining bands. We discovered, for the first time, that the temporal variation of iron band emission is delayed as compared with that of the other energy X-rays by 0.39 + 0.10 ms (1 σ error) We also discovered that the time difference shows a general trend such that the higher energy X-rays are advanced in comparison with the lower energy X-rays with the exception of the iron band. Assuming that the iron emission lines are fluorescent lines in origin and are emitted by circumstellar matter, we derived 5.6 + 1.5 ms for the time delay of the temporal variation of the iron line from the average temporal variation in the energy band above the iron absorption edge, taking into account the energy spectral shape and the photoelectric absorption cross section. This result leads to a determination of (1.7 ± 0.5) × 108 cm for the distance between the original X-ray source and the reprocessor, which emits the iron lines. The general trend of the hard X-ray advance is considered to be related to the X-ray emission mechanism on the neutron star. © 2001. The American Astronomical Society. All rights reserved.

      DOI: 10.1086/323848

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    • X-ray imaging spectrometers for Astro-E: Ground calibration in soft X-ray range

      Hayashida K, Kitamoto S, Miyata E, Tsunemi H, Yoshita K, Kohmura T, Mori K, Katayama K, Katayama H, Shouho M, Ohta M, Dotani T, Ozaki M, Koyama K, Awaki H

      Proceedings of SPIE - The International Society for Optical Engineering4012   123 - 136   2000

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      Language:Japanese   Publishing type:Research paper (scientific journal)   Publisher:Proceedings of SPIE - The International Society for Optical Engineering  

      Soft X-ray response of X-ray Imaging Spectrometers (XIS) for the Astro-E satellite is measured with a grating spectrometer system at Osaka. First, relation between incident X-ray energy and output pulse height peak (E-PH relation) is examined with an SX grating. It is found that jump in the E-PH relation around Si-K edge is at most 2.7 eV. Second, quantum efficiency (QE) of the XIS in 0.4-2.2 kev range is measured relatively to the reference CCD of which absolute QE was calibrated with a gas proportional counter. The QE is fitted with a model in which CCD gate structures are considered. Systematic error on the QE results is estimated by referring an independent measurement. Third, tuning and improvement of the response function is performed. We employ six components to reproduce the response profile of the XIS. In this paper, improvement of one component which is originated in the events absorbed in the channel-stop is presented. Neverthless, Astro-E was lost due to the launch failure. We overview the XIS project in its flight model phase, modified points of the design, problems and solutions etc., in order to be utilized in a possible recovery of the satellite.

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    • Hard X-ray response of the XIS-CCD for ASTRO-E: qualification of the X-ray CCD detector Peer-reviewed

      M. Nishiuchi, K. Koyama, H. Awaki, T. Tsuru, M. Sakano, K. Hamaguchi, H. Murakami, H. Tsunemi, K. Hayashida, S. Kitamoto, E. Miyata, T. Dotani, M. Ozaki, M. Bautz, J. Doty, S. Kissel, R. Foster, G. Ricker

      Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment436 ( 1-2 ) 79 - 84   1999

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    • Concept of the X-ray Astronomy Recovery Mission

      Makoto Tashiro, Makoto Tashiro, Hironori Maejima, Kenichi Toda, Richard Kelley, Lillian Reichenthal, James Lobell, Robert Petre, Matteo Guainazzi, Elisa Costantini, Mark Edison, Ryuichi Fujimoto, Martin Grim, Kiyoshi Hayashida, Jan Willem Den Herder, Yoshitaka Ishisaki, Stéphane Paltani, Kyoko Matsushita, Koji Mori, Gary Sneiderman, Yoh Takei, Yukikatsu Terada, Hiroshi Tomida, Hiroki Akamatsu, Lorella Angelini, Yoshitaka Arai, Hisamitsu Awaki, Lurli Babyk, Lurli Babyk, Aya Bamba, Peter Barfknecht, Kim Barnstable, Thomas Bialas, Branimir Blagojevic, Joseph Bonafede, Clifford Brambora, Laura Brenneman, Greg Brown, Kimberly Brown, Laura Burns, Edgar Canavan, Tim Carnahan, Meng Chiao, Brian Comber, Lia Corrales, Cor De Vries, Johannes Dercksen, Maria DIaz-Trigo, Tyrone DIllard, Michael DIpirro, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan Eckart, Teruaki Enoto, Yuichiro Ezoe, Carlo Ferrigno, Yutaka Fujita, Yasushi Fukazawa, Akihiro Furuzawa, Luigi Gallo, Steve Graham, Liyi Gu, Kohichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Dean Hawes, Takayuki Hayashi, Cailey Hegarty, Natalie Hell, Junko Hiraga, Edmund Hodges-Kluck, Matt Holland, Ann Hornschemeier, Akio Hoshino, Yuto Ichinohe, Ryo Iizuka, Kazunori Ishibashi, Manabu Ishida, Kumi Ishikawa, Kosei Ishimura, Bryan James, Timothy Kallman, Erin Kara, Satoru Katsuda, Steven Kenyon, Caroline Kilbourne, Mark Kimball, Takao Kitaguchi, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Shu Koyama, Aya Kubota, Maurice Leutenegger, Maurice Leutenegger, Tom Lockard, Mike Loewenstein, Yoshitomo Maeda, Lynette Marbley

      Proceedings of SPIE - The International Society for Optical Engineering10699   1 1 2018

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      © 2018 SPIE. The ASTRO-H mission was designed and developed through an international collaboration of JAXA, NASA, ESA, and the CSA. It was successfully launched on February 17, 2016, and then named Hitomi. During the in-orbit verification phase, the on-board observational instruments functioned as expected. The intricate coolant and refrigeration systems for soft X-ray spectrometer (SXS, a quantum micro-calorimeter) and soft X-ray imager (SXI, an X-ray CCD) also functioned as expected. However, on March 26, 2016, operations were prematurely terminated by a series of abnormal events and mishaps triggered by the attitude control system. These errors led to a fatal event: the loss of the solar panels on the Hitomi mission. The X-ray Astronomy Recovery Mission (or, XARM) is proposed to regain the key scientific advances anticipated by the international collaboration behind Hitomi. XARM will recover this science in the shortest time possible by focusing on one of the main science goals of Hitomi,"Resolving astrophysical problems by precise high-resolution X-ray spectroscopy".1This decision was reached after evaluating the performance of the instruments aboard Hitomi and the mission's initial scientific results, and considering the landscape of planned international X-ray astrophysics missions in 2020's and 2030's. Hitomi opened the door to high-resolution spectroscopy in the X-ray universe. It revealed a number of discrepancies between new observational results and prior theoretical predictions. Yet, the resolution pioneered by Hitomi is also the key to answering these and other fundamental questions. The high spectral resolution realized by XARM will not offer mere refinements; rather, it will enable qualitative leaps in astrophysics and plasma physics. XARM has therefore been given a broad scientific charge: "Revealing material circulation and energy transfer in cosmic plasmas and elucidating evolution of cosmic structures and objects". To fulfill this charge, four categories of science objectives that were defined for Hitomi will also be pursued by XARM; these include (1) Structure formation of the Universe and evolution of clusters of galaxies; (2) Circulation history of baryonic matters in the Universe; (3) Transport and circulation of energy in the Universe; (4) New science with unprecedented high resolution X-ray spectroscopy. In order to achieve these scientific objectives, XARM will carry a 6 × 6 pixelized X-ray micro-calorimeter on the focal plane of an X-ray mirror assembly, and an aligned X-ray CCD camera covering the same energy band and a wider field of view. This paper introduces the science objectives, mission concept, and observing plan of XARM.

      DOI: 10.1117/12.2309455

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    • MAXIで観測したCyg X‐3のクエンチ状態

      三原建弘, 石川ありさ, 石川ありさ, 松岡勝, 杉崎睦, 北本俊二, 小谷太郎, 坪井昌人, 中平聡志

      日本物理学会講演概要集69 ( 1 ) 134   5 3 2014

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    • ASTRO‐H衛星搭載X線CCDカメラ(SXI)の軟X線帯域の較正

      幸村孝由, 池田翔馬, 金子健太, 矢部一成, 常深博, 林田清, 中嶋大, 穴吹直久, 上田周太朗, 菅裕哲, 鶴剛, 内田裕之, 大西隆雄, 堂谷忠靖, 尾崎正伸, 冨田洋, 北本俊二, 村上弘志, 梅津里香, 小松飛斗

      日本放射光学会年会・放射光科学合同シンポジウム予稿集26th   133   12 1 2013

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    • ASTRO‐H搭載X線CCDカメラ(SXI)の軟X線に対する検出効率の測定

      池田翔馬, 幸村孝由, 金子健太, 矢部一成, 常深博, 林田清, 穴吹直久, 中嶋大, 薙野綾, 上田周太朗, 菅裕哲, 米森愛美, 鶴剛, 内田裕之, 大西隆雄, 堂谷忠靖, 尾崎正伸, 冨田洋, 北本俊二, 村上弘志, 梅津里香, 小松飛斗, 杉本樹理

      日本天文学会年会講演予稿集2012   271   20 8 2012

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    • ASTRO‐H搭載X線CCD(SXI)の可視光遮断膜のX線透過率測定

      河合耕平, 幸村孝由, 池田翔馬, 金子健太, 常深博, 林田清, 穴吹直久, 中嶋大, 上田周太朗, 鶴剛, 堂谷忠靖, 尾崎正伸, 藤永貴久, 松田桂子, 北本俊二, 村上弘志, 平賀純子, 森浩二

      日本放射光学会年会・放射光科学合同シンポジウム予稿集25th   78   6 1 2012

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    • 14aSP-13 The measurement of quantum efficiency for the Soft X-ray Imager (SXI) on board ASTRO-H

      Kohmura Takayoshi, Ueda Shutaro, Kan Hiroaki, Yonemori Manami, Tsuru Takeshi, Uchida Hiroyuki, Onishi Takao, Dotani Tadayasu, Ozaki Masanobu, Tomida Hiroshi, Kitamoto Shunji, Ikeda Shoma, Murakami Hiroshi, Umetus Rika, Komatsu Tobito, Kaneko Kenta, Yabe Kazunari, Tsunemi Hiroshi, Hayashida Kiyoshi, Nakajima Hiroshi, Anabuki Naohisa, Nagino Ryo

      Meeting Abstracts of the Physical Society of Japan67 ( 0 )   2012

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      Language:Japanese   Publisher:The Physical Society of Japan  

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    • ASTRO‐H搭載X線CCD(SXI)の可視光遮断膜のX線透過率測定

      河合耕平, 幸村孝由, 池田翔馬, 金子健太, 常深博, 林田清, 穴吹直久, 中嶋大, 上田周太朗, 鶴剛, 堂谷忠靖, 尾崎正伸, 藤永貴久, 松田桂子, 北本俊二, 村上弘志, 平賀純子, 森浩二

      日本天文学会年会講演予稿集2011   293   20 8 2011

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    • X線天文衛星ASTRO‐H搭載CCD(SXI)用可視光遮断膜の性能評価

      池田翔馬, 幸村孝由, 河合耕平, 渡辺辰雄, 金子健太, 常深博, 林田清, 穴吹直久, 中嶋大, 上田周太朗, 鶴剛, 堂谷忠靖, 尾崎正伸, 藤永貴久, 松田桂子, 北本俊二, 村上弘志, 平賀純子, 森浩二

      日本天文学会年会講演予稿集2011   293   20 8 2011

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    • X線天文衛星ASTRO‐H搭載X線CCDカメラSXIの可視光・紫外線遮光対策

      河合耕平, 幸村孝由, 渡辺辰雄, 池田翔馬, 牛山薫, 金子健太, 常深博, 林田清, 中嶋大, 穴吹直久, 上田周太朗, 鶴剛, 堂谷忠靖, 尾崎正伸, 馬場彩, 北本俊二, 村上弘志, 八木橋伸佳, 水野瑛己, 轟章太郎, 坂田和也

      日本天文学会年会講演予稿集2011   254   20 2 2011

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    • X線天文衛星ASTRO‐H搭載X線CCD(SXI)の紫外線対策

      渡辺辰雄, 幸村孝由, 河合耕平, 小川大樹, 池田翔馬, 金子健太, 牛山薫, 川島成輝, 北本俊二, 村上弘志, 吉田正樹, 東慶一, 常深博, 林田清, 穴吹直久, 中嶋大, 鶴剛, 堂谷忠靖, 尾崎正伸, 馬場彩, 平賀純子, 森浩二

      日本放射光学会年会・放射光科学合同シンポジウム予稿集24th   152   7 1 2011

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    • ASTRO‐H衛星搭載X線用CCDの可視光・紫外線遮光対策

      河合耕平, 幸村孝由, 渡辺辰雄, 池田翔馬, 牛山薫, 金子健太, 常深博, 林田清, 中嶋大, 鶴剛, 堂谷忠靖, 尾崎正伸, 馬場彩, 北本俊二, 村上弘志, 八木橋伸佳, 水野瑛己, 轟章太郎, 坂田和也

      PFシンポジウム要旨集28th   88   2011

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    • X線天文衛星ASTRO‐H搭載X線CCDカメラ(SXI)の可視光遮断対策

      河合耕平, 幸村孝由, 渡辺辰雄, 小川大樹, 池田翔馬, 牛山薫, 常深博, 林田清, 中嶋大, 穴吹直久, 上田周太朗, 鶴剛, 堂谷忠靖, 尾崎正伸, 北本俊二, 村上弘志

      日本天文学会年会講演予稿集2010   229   20 8 2010

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    • すざく衛星搭載XISのOBFの破れの評価

      轟章太郎, 北本俊二, 村上弘志, 松本浩典, 林田清, 常深博, 中嶋大, 幸村孝由, 小山勝二, 鶴剛, 森浩二, 常谷忠靖, 尾崎正伸, 辻本匡弘, 馬場彩

      日本天文学会年会講演予稿集2010   237   20 8 2010

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    • 宇宙X線用CCDの赤外線遮光対策

      小川大樹, 幸村孝由, 河合耕平, 渡辺辰雄, 池田翔馬, 牛山薫, 金子健太, 川島成輝, 高橋泰樹, 工藤幸寛, 常深博, 林田清, 中嶋大, 鶴剛, 堂谷忠靖, 尾崎正伸, 北本俊二, 村上弘志, 鎌田有紀子

      日本天文学会年会講演予稿集2010   229   20 8 2010

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    • X線天文衛星Astro‐H搭載X線CCDカメラ(SXI)の紫外線対策 III

      渡辺辰雄, 幸村孝由, 河合耕平, 北本俊二, 村上弘志, 竹中恵理, 長崎健太, 吉田正樹, 東慶一, 常深博, 林田清, 穴吹直久, 中嶋大, 鶴剛, 松本浩典, 堂谷忠靖, 尾崎正伸, 馬場彩, 藤永貴久, 松田圭子, 平賀純子, 森浩二

      日本天文学会年会講演予稿集2010   254   20 2 2010

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    • すざく衛星搭載X線CCDカメラ(XIS)のP‐sumモードの較正(II)

      幸村孝由, 渡辺辰雄, 河合耕平, 東慶一, 北本俊二, 村上弘志, 常深博, 林田清, 中島大, 小山勝二, 鶴剛, 松本浩典, 堂谷忠靖, 尾崎正伸, 辻本匡弘, 馬場彩, 森浩二

      日本天文学会年会講演予稿集2010   256   20 2 2010

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    • 11pSG-9 Development of the Optical and EUV blocking layer for the X-ray CCD (SXI) on board ASTRO-H

      Kohmura Takayoshi, Tsunemi Hiroshi, Hayashida Kiyoshi, Nakajima Hiroshi, Anabuki Naohisa, Uchida Hiroyuki, Ueda Shutaro, Tsuru Takeshi, Dotani Tadayasu, Ozaki Masanobu, Bamba Aya, Kawai Kohei, Mori Koji, Hiraga Junko, Watanabe Tatsuo, Ogawa Taiki, Ikeda Shoma, Ushiyama Kaoru, Kaneko Kenta, Kitamoto Shunji, Murakami Hiroshi

      Meeting Abstracts of the Physical Society of Japan65 ( 0 )   2010

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    • X線天文衛星ASTRO‐H搭載X線CCDカメラ(SXI)の紫外線対策 II

      幸村孝由, 渡辺辰雄, 北本俊二, 村上弘志, 竹中恵里, 長崎健太, 東慶一, 吉田雅樹, 常深博, 林田清, 穴吹直久, 中嶋大, 阪口塁, 繁山和夫, 鶴剛, 松本浩典, 堂谷忠靖, 尾崎正伸, 馬場彩, 藤永貴久, 平賀純子, 森浩二

      日本天文学会年会講演予稿集2009   270   20 8 2009

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    • すざく衛星搭載X線CCDカメラXISのP‐sumモードの較正

      東慶一, 北本俊二, 村上弘志, 幸村孝由, 渡邊辰雄, 森浩二, 鶴剛, 松本浩典, 小山勝二, 林田清, 常深博, 堂谷忠靖, 辻本匡弘, 馬場彩

      日本天文学会年会講演予稿集2009   261   20 8 2009

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    • 10aSD-11 Development status of the Soft X-ray Spectrometer (SXS) onboard Astro-H (II)

      Fujimoto Ryuichi, Sato Kosuke, Mitsuda Kazuhisa, Yamasaki Noriko, Takei Yoh, Tsujimoto Masahiro, Sugita Hiroyuki, Sato Yoichi, Shinozaki Keisuke, Ohashi Takaya, Ishisaki Yoshitaka, Ezoe Yuichiro, Murakami Masahide, Tashiro Makoto, Terada Yukikatsu, Tamagawa Toru, Mihara Tatehiro, Kawaharada Madoka, Yamaguchi Hiroya, Kitamoto Shunji, Murakami Hiroshi, Kelley R.L, Kilbourne C.A, Porter F.S, McCammon D, den Herder J.-W

      Meeting abstracts of the Physical Society of Japan64 ( 2 )   18 8 2009

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    • 28pSH-5 Development of mirocalorimeter SXS designed for ASTRO-H

      Takei Y, Mitsuda K, Yamasaki N, Tsujimoto M, Shinozaki K, Sugita H, Sato Y, Fujimoto R, Sato K, Ohashi T, Ishisaki Y, Ezoe Y, Murakami M, Tashiro M. S, Terada Y, Tamagawa T, Mihara T, Kawaharada M, Yamaguchi H, Kitamoto S, Murakami H, Kelley Richard L, Kilbourne C. A, Porter F. S, Shirron P. J, DiPirro M. J, Sneiderman Gary A, McCammon D, Herder J.-W. den, ASTRO-H SXS tea

      Meeting abstracts of the Physical Society of Japan64 ( 1 )   3 3 2009

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    • X線天文衛星ASTRO‐H搭載X線CCDカメラ(SXI)の紫外線対策

      幸村孝由, 渡辺辰雄, 北本俊二, 村上弘志, 森井幹雄, 武井大, 竹中恵里, 長崎健太, 吉田雅樹, 常深博, 林田清, 穴吹直久, 中島大, 鶴剛, 松本浩典, 堂谷忠靖, 尾崎正伸, 馬場彩, 藤永貴久, 平賀純子, 森浩二

      日本天文学会年会講演予稿集2009   256   20 2 2009

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    • 「すざく」搭載X線CCDカメラ(XIS)の時刻付けの較正 その2

      松田桂子, 堂谷忠靖, 尾崎正伸, 馬場彩, 辻本匡弘, 鶴剛, 松本浩典, 小山勝二, 林田清, 常深博, 森浩二, 北本俊二, 村上弘志

      日本天文学会年会講演予稿集2009   258   20 2 2009

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    • 「すざく」搭載X線CCDカメラ(XIS)の時刻付けの較正

      松田桂子, 堂谷忠靖, 尾崎正伸, 馬場彩, 鶴剛, 松本浩典, 小山勝二, 林田清, 常深博, 森浩二, 北本俊二, 村上弘志, 幸村孝由

      日本天文学会年会講演予稿集2008   256   20 8 2008

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    • 「すざく」衛星によるLow‐Hard状態におけるCygX‐1の観測

      山田真也, 牧島一夫, 伊藤健, 中澤知洋, 久保田あや, 高橋弘充, 堂谷忠靖, 海老沢研, 北本俊二, 山岡和貴, 根来均

      日本物理学会講演概要集62 ( 2 ) 106   21 8 2007

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    • NeXT衛星搭載X線CCDカメラSXIシステム開発の現状

      鶴剛, 松本浩典, 高木慎一郎, 小澤碧, 乾達也, 小山勝二, 常深博, 林田清, 宮田恵美, 小澤秀樹, 東樋口正邦, 松浦大介, 堂谷忠靖, 尾崎正伸, 村上弘志, 幸村孝由, 北本俊二, 粟木久光

      日本天文学会年会講演予稿集2006   256   20 8 2006

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    • 「すざく」ファーストライト:X線CCDカメラXIS

      林田清, 鳥居研一, 並木雅章, 常深博, 穴吹直久, 鶴剛, 松本浩典, 小山勝二, 堂谷忠靖, 尾崎正伸, 村上弘志, 片山晴善, 北本俊二, 幸村孝由, 粟木久光, 馬場彩, 千田篤史, BAUTZ Mark, KISSEL Steve, LAMARR Beverly, FOSTER Rick, MILLER Eric

      日本天文学会年会講演予稿集2006   281   20 2 2006

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    • 23pSH-4 Suzaku Observation of Black hole binary GRO J1655-40

      Takahashi H, Onuki K, Takahashi T, Ebisawa K, Dotani T, Ito T, Kokubun M, Makishima K, Namiki M, Kotani T, Parmr Arvind, Mizuno T, Done Chris, the Suzaku team, Fukazawa Y, Sudoh K, Ogita T, Kitamoto S, Kubota A, Yamaoka K, Ueda Y

      Meeting Abstracts of the Physical Society of Japan61 ( 0 )   2006

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    • Soft X-ray Imager (SXI) onboard the NeXT satellite Peer-reviewed

      T.G. Tsuru, S.-I. Takagi, H. Matsumoto, T. Inui, M. Ozawa, K. Koyama, H. Tsunemi, K. Hayashida, E. Miyata, H. Ozawa, M. Touhiguchi, D. Matsuura, T. Dotani, M. Ozaki, H. Murakami, T. Kohmura, S. Kitamoto, H. Awaki

      Proceedings of SPIE - The International Society for Optical Engineering6266 II   2006

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      DOI: 10.1117/12.670649

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    • Astro‐E2衛星の現状:X線CCD検出器(XIS)

      松本浩典, 鶴剛, 小山勝二, 常深博, 林田清, 鳥居研一, 宮田恵美, 粟木久光, 北本俊二, 幸村孝由, 堂谷忠靖, 尾崎正伸

      日本天文学会年会講演予稿集2005   310   20 8 2005

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    • NeXT衛星搭載Soft X‐ray Imager(SXI)の開発

      鶴剛, 松本浩典, 小山勝二, 高木慎一郎, 乾達也, 常深博, 林田清, 宮田恵美, 堂谷忠靖, 尾崎正伸, 北本俊二, 幸村孝由, 粟木久光

      日本天文学会年会講演予稿集2004   256   2004

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    • Wide band X-ray Imager (WXI) and Soft Gamma-ray Detector (SGD) for the NeXT Mission Peer-reviewed

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

      Proceedings of SPIE - The International Society for Optical Engineering5488 ( PART 2 ) 549 - 560   2004

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      DOI: 10.1117/12.551500

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    • ASTRO‐EII搭載のCCDカメラXIS(I)

      林田清, 常深博, 宮田恵美, 小山勝二, 鶴剛, 松本浩典, 堂谷忠靖, 尾崎正伸, 北本俊二, 粟木久光, BAUTZ M, RICKER G, FOSTER R

      日本天文学会年会講演予稿集2003   231   2003

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    • X-ray imaging spectrometer (XIS) on board Astro-E2 Peer-reviewed

      T. Dotani, M. Ozaki, H. Murakami, K. Koyama, T. Tsuru, H. Matsumoto, H. Tsunemi, K. Hayashida, E. Miyata, S. Kitamoto, H. Awaki, M. Bautz, J. Doty, G. Ricker, R. Foster, G. Prigozhin, S. Kissel, B. Burke, A. Pillsbury

      Proceedings of SPIE - The International Society for Optical Engineering4851 ( 2 ) 1071 - 1079   2002

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      DOI: 10.1117/12.461313

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    • XIS読み出し回路を用いた国産CCDの性能評価(II)

      馬場彩, 辻本匡弘, 今西健介, 河野誠, 村上弘志, 濱口健二, 鶴剛, 小山勝二, 北本俊二, 林田清, 片山晴善, 常深博

      日本天文学会年会講演予稿集2001   267   2001

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    • Astro‐E衛星搭載X線CCDカメラXIS:開発の概要とファーストライト

      常深博, 北本俊二, 林田清, 宮田恵美, 吉田久美, 幸村孝由, 森浩二, 片山晴善, 荘保信, 大田基在, 小山勝二, 鶴剛, 粟木久光, 坂野正明, 西内満美子, 浜口健二, 村上弘志, 今西健介, 堂谷忠靖, 尾崎正伸, RICKER G, BAUTZ M, DOTY J, KISSEL S, FOSTER R

      日本天文学会年会講演予稿集2000   172   2000

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    • Optical follow-up observations of the ASCA Large Sky Survey Peer-reviewed

      Akiyama, M, Ohta, K, Yamada, T, Ueda, Y, Takahashi, T, Sakano, M, Tsuru, T, Boyle, B, Koyama, K, Kitamoto, S, Itoh, M

      HOT UNIVERSE ( 188 ) 465 - 466   1998

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    • Soft X-ray response of the proto-type CCD camera (XIS) for Astro-E Peer-reviewed

      K. Hayashida, S. Kitamoto, E. Miyata, H. Tsunemi, K. Hashimotodani, K. Katayama, T. Kohmura, R. Asakura, K. Yoshita, H. Katayama, M. Shouho, K. Koyoma, T.G. Tsuru, H. Awaki, T. Dotani

      Proceedings of SPIE - The International Society for Optical Engineering3445   278 - 290   1998

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    • Test report on EM behavior of the X-ray CCD camera (XIS) installed on ASTRO-E.

      片山和典, 幸村孝由, 朝倉励子, 橋本谷磨志, 戸練景, 常深博, 北本俊二, 鶴剛, 尾崎正伸

      日本天文学会年会講演予稿集1998   181   1998

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    • Astro‐E搭載用X線CCDカメラ(XIS)の開発 II

      粟木久光, 小山勝二, 鶴剛, 常深博, 北本俊二, 林田清, 堂谷忠靖, RICKER G R, BAUTZ M W

      日本天文学会年会講演予稿集1997   184   1997

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    • Plan of X-ray spectrometry for polarized light imaging.

      小山勝二, 田沢雄二, 鶴剛, 粟木久光, 富田洋, 尾崎正伸, 常深博, 北本俊二, 林田清

      宇宙放射線シンポジウム1995   36 - 39   3 1996

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    • ASTRO‐E搭載用X線CCDカメラ(XIS)の開発

      粟木久光, 鶴剛, 常深博, 北本俊二, 林田清, 堂谷忠靖, RICKER G R, BAUTZ M W, DOTY J P

      日本天文学会年会講演予稿集1995   224   1995

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    • 衛星搭載用X線CCDカメラの開発 (II)

      冨田洋, 松本浩典, 鶴剛, 尾崎正伸, 常深博, 北本俊二, 林田清, 宮口和久, 山本晃永

      日本天文学会年会講演予稿集1995   226   1995

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    • 宇宙まるごとQ&A

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      大阪大学出版会(杉山清寛、福田光順、山中千博、下田正 編)  4 2003 

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      Language:Japanese Book type:Other

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    • 宇宙スペクトル博物館<X線編>見えない星空への招待

      ( Role: Other)

      裳華房  4 1999 

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      Language:Japanese Book type:Other

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    • X線でさぐるブラックホール

      ( Role: Other)

      裳華房ポピュラーサイエンス  4 1998 

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      Language:Japanese Book type:Other

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    • The Hot Universe

      Editors: Koyama, Katsuji, Kitamoto, Shunji, Itoh, Masayuki (E

      Springer  1998 

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    Professional Memberships

    • 1983 - Present 
      日本物理学会

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    • 1983 
      Th Astronomical Society of Japan

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    •  
      International Astronomical Union

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    Works

    • 回折限界X線望遠鏡の性能評価 Other

      4 2004
      -
      4 2005

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      Work type:Other  

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    • ブラックホールの直接観測を目指した超高分解能X線望遠鏡の開発 Other

      4 2002
      -
      4 2003

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      Work type:Other  

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    Research Projects

    • 超高精度X線望遠鏡の開発研究、ブラックホールの研究、星からのX線放射の研究

      科学研究費補助金 

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      4 2001 - Present

      Grant type:Competitive

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    • 銀河団の暗黒物質の直接測定の可能性の研究

      日本学術振興会  科学研究費助成事業 

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      4 2013 - 3 2015

      Grant type:Competitive

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    • 新型エックス線管長系の試作研究

      科学研究費助成事業 

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      4 2010 - 3 2012

      Grant type:Competitive

      研究の最終目標は、ブラックホール候補天体の撮像をして、ブラックホール候補天体が本当にブラックホールであることを示すことである。そのために、これまでも超高精度撮像を目指して、研究を行ってきた(参考文献 Kitamoto et al. 2007. “X-ray imaging and adaptive optics system for a 13.5nm telescope”, SPIE 他)。この構想の延長として、本研究では、超高精度撮像装置のひとつの候補であるX線干渉計(http://maxim.gsfc.nasa.gov/docs/science/science.html)の試作実験を行う。本研究では、最近思いついた新型X線干渉計のアイデアの実証実験を行う。この実証ができれば、X線干渉計による天体観測、X線によるブラックホール撮像に大きく近づくことになる。

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    • 超高角度分解能エックス線望遠鏡からエックス線干渉計への発展的研究

      日本学術振興会  科学研究費助成事業 

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      4 2007 - 3 2010

      Grant type:Competitive

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    • 多層膜と電荷結合素子の組み合わせによるエックス線偏光計の開発

      科学研究費助成事業 

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      4 2007 - 3 2009

      Grant type:Competitive

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    • 時間変動で探るブラックホールへの物質流入とブラックホール撮像への挑戦

      文部科学省  科学研究費助成事業 

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      4 2005 - 3 2007

      Grant type:Competitive

      公募

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    • 回折限界X線望遠鏡の性能評価

      JAXA  受託研究(一般受託研究) 

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      4 2004 - 3 2007

      Grant type:Competitive

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    • 見えない信号をキャッチせよ

      民間財団等  日産財団 

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      4 2004 - 3 2005

      Grant type:Competitive

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    • X線の短時間変動とX線による直接撮像で迫るブラックホールへの物質流入の研究

      文部科学省  科学研究費助成事業 

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      4 2003 - 3 2005

      Grant type:Competitive

      公募

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    • ブラックホールの直接観測を目指した超高分解能X線望遠鏡の開発

      日本宇宙フォーラム  受託研究(一般受託研究) 

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      4 2003 - 3 2004

      Grant type:Competitive

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    • X線光学における能動光学系の応用

      科学研究費助成事業 

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      4 2002 - 3 2004

      Grant type:Competitive

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    • X線によるマゼラン星雲の星形成

      科学研究費助成事業 

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      4 1998 - 3 2002

      Grant type:Competitive

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    • 画素の小さなCCDの開発研究

      科学研究費助成事業 

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      4 1996 - 3 2001

      Grant type:Competitive

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    • 高効率・高分散X線分光器の開発研究

      日本学術振興会  科学研究費助成事業 

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      4 1997 - 3 1999

      Grant type:Competitive

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    • 軟X線光学、軟X線検出器

      科学研究費補助金 

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      Grant type:Competitive

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    Industrial property rights

    • X線分光測定装置

      北本俊二

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      Applicant:JST

      Application no:平成10年特許願第248718  Date applied:2 9 1998

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