2024/10/02 更新

写真b

キタモト シユンジ
北本 俊二
KITAMOTO Shunji
*大学が定期的に情報更新している項目(その他は、researchmapの登録情報を転載)
所属*
理学部 物理学科
理学研究科 物理学専攻 博士課程後期課程
理学研究科 物理学専攻 博士課程前期課程
職名*
特別専任教授
学位
理学博士 ( 大阪大学 ) / 理学修士 ( 大阪大学 )
連絡先
メールアドレス
研究テーマ*
  • 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。

  • 研究キーワード
  • 宇宙物理

  • 学内職務経歴*
    • 2023年4月 - 現在 
      理学部   物理学科   特別専任教授
    • 2023年4月 - 現在 
      理学研究科   物理学専攻 博士課程前期課程   特別専任教授
    • 2023年4月 - 現在 
      理学研究科   物理学専攻 博士課程後期課程   特別専任教授
    • 2001年4月 - 2023年3月 
      理学部   物理学科   教授
    • 2005年4月 - 2023年3月 
      理学研究科   物理学専攻 博士課程前期課程   教授
    • 2005年4月 - 2023年3月 
      理学研究科   物理学専攻 博士課程後期課程   教授

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    研究分野

    • 自然科学一般 / 素粒子、原子核、宇宙線、宇宙物理にする実験

    経歴

    • 2001年4月 - 現在 
      立教大学   理学研究科 物理学専攻博士課程後期課程   教授

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    • 2001年4月 - 現在 
      立教大学   理学研究科 物理学専攻博士課程前期課程   教授

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    • 2001年4月 - 現在 
      立教大学   理学部 物理学科   教授

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    • 1996年4月 - 2001年3月 
      大阪大学大学院理学研究科   助教授

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    • 1995年4月 - 1996年3月 
      大阪大学理学部   助教授

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    • 1985年4月 - 1995年3月 
      大阪大学理学部   助手

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    学歴

    • 1982年4月 - 1985年3月 
      大阪大学   大学院理学研究科 博士後期課程   物理学専攻

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      国名: 日本国

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    • 1980年4月 - 1982年3月 
      大阪大学   大学院理学研究科 博士前期課程 物理学専攻

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    • - 1980年3月 
      大阪大学   理学部   物理学科

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      国名: 日本国

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    委員歴

    • 2008年9月 - 現在 
      日本物理学会   Jr. セッション委員会委員

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    • 2021年6月 - 2023年5月 
      日本天文学会   理事

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      団体区分:学協会

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

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      団体区分:学協会

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

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      団体区分:学協会

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

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      団体区分:学協会

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

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      団体区分:学協会

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

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      団体区分:学協会

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    論文

    • Dark matter search in the Perseus cluster with simultaneous analysis of Hitomi and Suzaku data

          2024年3月

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    • Relative timing calibration of the Resolve x-ray microcalorimeter onboard XRISM using the modulated x-ray source

      Tomoki Omama, Masahiro Tsujimoto, Makoto Sawada, Caroline A. Kilbourne, Cor de Vries, Megan E. Eckart, Yoshitaka Ishisaki, Shunji Kitamoto, Maurice A. Leutenegger, Frederick S. Porter, Rob Wolfs

      SPACE TELESCOPES AND INSTRUMENTATION 2022: ULTRAVIOLET TO GAMMA RAY12181   2022年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)   出版者・発行元:SPIE-INT SOC OPTICAL ENGINEERING  

      The Resolve instrument onboard the X-Ray Imaging and Spectroscopy Mission (XRISM) hosts an x-ray microcalorimeter that consists of 36 pixels in an array operated at 50 mK. It is currently under development and will be launched in 2022. X-ray microcalorimeters are known for their high spectral resolution, but they also excel in timing resolution for the necessity of cross-correlating event signals with templates in the time domain for accurate energy derivation. Primary and redundant modulated x-ray sources (MXS) are installed in Resolve for the purpose of correcting changes in the energy scale of the microcalorimeters while minimizing additional background; each source is switched on for intervals of O (1 ms) with a duty cycle of similar to 1 %. The MXS can also be utilized for calibrating relative timing as a function of pixel, event grade, and energy. We had a week-long run in 2022 June using the flight model hardware during the spacecraft level test with several different settings. We describe the method and the result of the relative timing calibration using this data set.

      DOI: 10.1117/12.2629753

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    • Pulse parameters optimization of the modulated X-ray sources for the Resolve microcalorimeter spectrometer on XRISM

      Makoto Sawada, Renata Cumbee, Cor de Vries, Megan E. Eckart, Ryuichi Fujimoto, Yoshitaka Ishisaki, Caroline A. Kilbourne, Shunji Kitamoto, Maurice A. Leutenegger, Frederick S. Porter, Yoh Takei, Masahiro Tsujimoto

      SPACE TELESCOPES AND INSTRUMENTATION 2022: ULTRAVIOLET TO GAMMA RAY12181   2022年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)   出版者・発行元:SPIE-INT SOC OPTICAL ENGINEERING  

      Resolve is an X-ray microcalorimeter spectrometer on the X-Ray Imaging and Spectroscopy Mission (XRISM) to be launched in Japanese fiscal year 2022. Resolve is required to achieve an energy resolution of 7 eV at FWHM at 6 keV. To satisfy this requirement, it is necessary to correct the in-orbit gain drift. For this purpose, Resolve is equipped with multiple gain tracking calibration sources, including the modulated X-ray sources (MXS). The MXS will be operated in a pulsed mode, in which calibration X-rays illuminating the detector array are emitted at a duty cycle of similar to 1%. The low duty cycle allows us to monitor the gain drift with a small loss of the observing efficiency. However, the use of the MXS has drawbacks such as increase in the instrumental background due to exponentially decaying afterglow emission following each MXS pulse and the loss of throughput due to changes in the event-grade branching ratio. To minimize these effects, an optimization of the MXS operating parameters is needed. Based on the results of the MXS component-level tests, we established an analytical model that describes the MXS pulse and afterglow count rates. We obtained the optimal pulse parameters for various gain tracking intervals and estimated the effects of using the MXS on observation data. We further studied the trade-off between these effects and resolution degradation using the actual in-orbit drift observed with the Soft X-ray Spectrometer on the Hitomi satellite. Our study forms the basis of strategies for the in-orbit gain drift correction of Resolve.

      DOI: 10.1117/12.2630133

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

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

      Journal of Astronomical Telescopes, Instruments, and Systems7 ( 2 )   2021年4月

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      掲載種別:研究論文(学術雑誌)  

      Resolve onboard the x-ray satellite X-Ray Imaging and Spectroscopy Mission (XRISM) is a cryogenic instrument with an x-ray microcalorimeter in a Dewar. A lid partially transparent to x-rays (called gate valve or GV) is installed at the top of the Dewar along the optical axis. Because observations will be made through the GV for the first few months, the x-ray transmission calibration of the GV is crucial for initial scientific outcomes. We present the results of our ground calibration campaign of the GV, which is composed of a Be window and a stainless steel mesh. For the stainless steel mesh, we measured its transmission using the x-ray beamline at ISAS. For the Be window, we used synchrotron facilities to measure the transmission and modeled the data with (i) photoelectric absorption and incoherent scattering of Be, (ii) photoelectric absorption of contaminants, and (iii) coherent scattering of Be changing at specific energies. We discuss the physical interpretation of the transmission discontinuity caused by the Bragg diffraction in polycrystal Be, which we incorporated into our transmission phenomenological model. We present the x-ray diffraction measurement on the sample to support our interpretation. The measurements and the constructed model meet the calibration requirements of the GV. We also performed a spectral fitting of the Crab nebula observed with Hitomi SXS and confirmed improvements of the model parameters.

      DOI: 10.1117/1.JATIS.7.2.028005

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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 Ray11444   2020年12月13日

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      掲載種別:研究論文(国際会議プロシーディングス)   出版者・発行元:SPIE  

      Resolve onboard the X-ray satellite XRISM is a cryogenic instrument with an X-ray microcalorimeter in a Dewar. A lid partially transparent to X-rays is installed at the top of the Dewar along the optical axis, which is called the gate valve (GV). Because observations will be made through the GV for the first few months, the X-ray transmission calibration of the GV is crucial for initial scientific outcomes. We present the results of our ground calibration campaign of the GV, which is composed of a Be window and a stainless steel mesh. For the stainless steel mesh, we measured its transmission using the X-ray beamline at ISAS for the first time. For the Be window, we used synchrotron facilities to measure the transmission and modeled the data with (i) photoelectric absorption and incoherent scattering of Be, (ii) photoelectric absorption of contaminants, and (iii) coherent scattering of Be. We discuss the physical interpretation of the transmission discontinuity caused by the Bragg diffraction in poly-crystal Be, which we incorporated into our phenomenological model. The measurements and the constructed model meet the calibration requirements of the GV. We also performed a spectral fitting of the Crab nebula data observed with Hitomi SXS and confirmed improvements of the model.

      DOI: 10.1117/12.2559451

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    • 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 Ray11444   2020年12月13日

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      掲載種別:研究論文(国際会議プロシーディングス)   出版者・発行元:SPIE  

      © 2020 SPIE The X-Ray Imaging and Spectroscopy Mission (XRISM) is the successor to the 2016 Hitomi mission that ended prematurely. Like Hitomi, the primary science goals are to examine astrophysical problems with precise high-resolution X-ray spectroscopy. XRISM promises to discover new horizons in X-ray astronomy. XRISM carries a 6 x 6 pixelized X-ray micro-calorimeter on the focal plane of an X-ray mirror assembly and a co-aligned X-ray CCD camera that covers the same energy band over a large field of view. XRISM utilizes Hitomi heritage, but all designs were reviewed. The attitude and orbit control system were improved in hardware and software. The number of star sensors were increased from two to three to improve coverage and robustness in onboard attitude determination and to obtain a wider field of view sun sensor. The fault detection, isolation, and reconfiguration (FDIR) system was carefully examined and reconfigured. Together with a planned increase of ground support stations, the survivability of the spacecraft is significantly improved.

      DOI: 10.1117/12.2565812

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    • Cooling system for the Resolve onboard XRISM

      Yuichiro Ezoe, Yoshitaka Ishisaki, Ryuichi Fujimoto, Yoh Takei, Takafumi Horiuchi, Masahiro Tsujimoto, Kumi Ishikawa, Susumu Yasuda, Keiichi Yanagase, Yasuko Shibano, Kosuke Sato, Shunji, Kitamoto, Seiji Yoshida, Keiichi Kanao, Shoji Tsunematsu, Kiyomi Otsuka, Syou Mizunuma, Masahito Isshiki, Richard L. Kelley, Calorine A. Kilbourne, Frederick S. Porter, Michael J. DiPirro, Peter Shirron

      Cryogenics108   103016 - 103016   2020年6月

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      掲載種別:研究論文(学術雑誌)   出版者・発行元:Elsevier BV  

      DOI: 10.1016/j.cryogenics.2019.103016

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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   2019年7月31日

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      掲載種別:研究論文(学術雑誌)   出版者・発行元:American Astronomical Society  

      DOI: 10.3847/1538-4357/ab2b3d

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      その他リンク: https://iopscience.iop.org/article/10.3847/1538-4357/ab2b3d

    • An application of the Ghosh & Lamb model to the accretion-powered X-ray pulsar X Persei

      Fumiaki Yatabe, Kazuo Makishima, Tatehiro Mihara, Motoki Nakajima, Mutsumi Sugizaki, Shunji Kitamoto, Yuki Yoshida, Toshihiro Takagi

      Publications of the Astronomical Society of Japan70 ( 5 )   2018年9月6日

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      掲載種別:研究論文(学術雑誌)   出版者・発行元:Oxford University Press (OUP)  

      Abstract

      The accretion-induced pulse period changes of the Be/X-ray binary pulsar X Persei were investigated over the period of 1996 January to 2017 September. This study utilized the monitoring data acquired with the RXTE All-Sky Monitor in 1.5–12 keV and the MAXI Gas-Slit Camera in 2–20 keV. The source intensity changed by a factor of 5–6 over this period. The pulsar was spinning down for 1996–2003, and has been spinning up since 2003, as already reported. The spin-up/down rate and the 3–12 keV flux, determined every 250 d, showed a clear negative correlation, which can be successfully explained by the accretion torque model proposed by Ghosh and Lamb (1979, ApJ, 234, 296). When the mass, radius, and distance of the neutron star were allowed to vary over a range of 1.0–2.4 solar masses, 9.5–15 km, and 0.77–0.85 kpc, respectively, the magnetic field strength of B = (4–25) × 1013 G gave the best fits to the observations. In contrast, the observed results cannot be explained by the values of B ∼ 1012 G previously suggested for X Persei, as long as the mass, radius, and distance are required to take reasonable values. Assuming a distance of 0.81 ± 0.04 kpc as indicated by optical astrometry, the mass of the neutron star is estimated as M = 2.03 ± 0.17 solar masses.

      DOI: 10.1093/pasj/psy088

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    • Hitomi X-ray observation of the pulsar wind nebula G21.5-0.9 査読有り

      Hitomi Collaboration

      PASJ70 ( 3 )   2018年4月3日

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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 査読有り

      Hitomi Collaboration

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

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:the Astronomical Society of Japan,  

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    • Ground calibration of the Astro-H (Hitomi) soft x-ray spectrometer 査読有り

      Eckart M.E, Adams J.S, Boyce K.R, Brown G.V, Chiao M.P, Fujimoto R, Haas D, Den Herder J.-W, Hoshino A, Ishisaki Y, Kilbourne C.A, Kitamoto S, Leutenegger M.A, McCammon D, Mitsuda K, Porter F.S, Sato K, Sawada M, Seta H, Sneiderman G.A, Szymkowiak A.E, Takei Y, Tashiro M.S, Tsujimoto M, De Vries C.P, Watanabe T, Yamada S, Yamasaki N.Y

      Journal of Astronomical Telescopes, Instruments, and Systems4 ( 2 )   2018年

    • 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   2018年1月1日

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

      Yuki Yoshida, Shunji Kitamoto, Akio Hoshino

      ASTROPHYSICAL JOURNAL849 ( 2 )   2017年11月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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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    • Solar abundance ratios of the iron-peak elements in the Perseus cluster 査読有り

      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 - +   2017年11月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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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    • Orbital modulations of X-ray light curves of Cygnus X-1 in its low/hard and high/soft states 査読有り

      Juri Sugimoto, Shunji Kitamoto, Tatehiro Mihara, Masaru Matsuoka

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

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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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    • Hitomi Constraints on the 3.5 keV Line in the Perseus Galaxy Cluster 査読有り

      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   2017年3月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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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    • A Suzaku View of Accretion- powered X-Ray Pulsar GX 1+4 査読有り

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

      ASTROPHYSICAL JOURNAL838 ( 1 ) 30 - 44   2017年3月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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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    • The quiescent intracluster medium in the core of the Perseus cluster 査読有り

      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 - +   2016年7月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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 査読有り

      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   2016年6月1日

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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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    • 21pCD-11 ASTRO-H搭載 精密軟X線分光装置SXSの現状

      田代 信, 満田 和久, 山崎 典子, 竹井 洋, 辻本 匡弘, 小川 美奈, 小山 志勇, 酒井 和広, 杉田 寛之, 佐藤 洋一, 篠崎 慶亮, 岡本 篤, 藤本 龍一, 大橋 隆哉, 石崎 欣尚, 江副 祐一郎, 山田 真也, 瀬田 裕美, 寺田 幸功, 北本 俊二, 星野 晶夫, 玉川 徹, 石川 久美, 野田 博文, 佐藤 浩介, 太田 直美, 澤田 真理, 三石 郁之, 村上 正秀, 村上 弘志, 伊豫本 直子, Kelley R. L., Kilbourne C. A., Porter F. S., Boyce K. R., Eckart M. E., Chiao M. P., Leutenegger M. A., Brown G. V., McCammon D., Szymkowiak A., Herder J. -W. den, Haas D., Vries C. de, Costantini E., Akamatsu H., Paltani S., ASTRO-H SXSチーム

      日本物理学会講演概要集71   509 - 509   2016年

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

      DOI: 10.11316/jpsgaiyo.71.1.0_509

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    • ASTRO-H (ひとみ) 衛星搭載 精密軟X線分光装置 SXS の軌道上での性能

      藤本 龍一, 満田 和久, 山崎 典子, 竹井 洋, 辻本 匡弘, 小川 美奈, 小山 志勇, 石川 久美, 杉田 寛之, 佐藤 洋一, 篠崎 慶亮, 岡本 篤, 大橋 隆哉, 石崎 欣尚, 江副 祐一郎, 山田 真也, 瀬田 裕美, 田代 信, 寺田 幸功, 北本 俊二, 星野 晶夫, 玉川 徹, 佐藤 浩介, 澤田 真理, 野田 博文, 三石 郁之, 村上 弘志, 太田 直美, 伊豫本 直子, 村上 正秀, Kelley R. L., Kilbourne C. A., Porter F. S., Boyce K. R., Sneiderman G. A., DiPirro M. J., Shirron P. J., Bialas T., Eckart M. E., Chiao M. P., Leutenegger M. A., Watanabe T., Sakai K., Brown G. V., McCammon D., Szymkowiak A., Herder J. -W. den, Haas D., Vries C. de, Costantini E., Akamatsu H., Paltani S., 他 ASTRO-H SXS チーム

      日本物理学会講演概要集71   367 - 367   2016年

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      記述言語:日本語   出版者・発行元:一般社団法人 日本物理学会  

      <p>2016年2月17日に打ち上げられたASTRO-H (ひとみ) 衛星に搭載された精密X線分光装置 SXS (Soft X-ray Spectrometer) は,40日弱の限られた期間ではあったが,軌道上において正常に動作し,天体のデータも取得できた.SXS の軌道上での性能について報告する.</p>

      DOI: 10.11316/jpsgaiyo.71.2.0_367

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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   2016年1月1日

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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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    • The Astro-H High Resolution Soft X-Ray Spectrometer 査読有り

      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年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)  

      DOI: 10.1117/12.2232509

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    • In-orbit operation of the ASTRO-H SXS 査読有り

      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年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)  

      DOI: 10.1117/12.2231784

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    • New multiwavelength observations of the Of?p star CPD -28° 2561 査読有り

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

      Monthly Notices of the Royal Astronomical Society447 ( 2 ) 1885 - 1894   2015年2月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:the Royal Astronomical Society  

      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° 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 Bd 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° 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 LX/Lbol ≈ -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° 2561 with the presence of a kG strong magnetic field capable to confine stellar wind.

      DOI: 10.1093/mnras/stu2516

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    • 23pDK-4 ASTRO-H搭載精密軟X線分光装置SXSの開発の現状(VI)

      石崎 欣尚, 満田 和久, 山崎 典子, 竹井 洋, 辻本 匡弘, 小川 美奈, 杉田 寛之, 佐藤 洋一, 篠崎 慶亮, 岡本 篤, 藤本 龍一, 大橋 隆哉, 江副 祐一郎, 山田 真也, 小波 さおり, 田代 信, 寺田 幸功, 瀬田 裕美, 北本 俊二, 星野 晶夫, 玉川 徹, 石川 久美, 野田 博文, 佐藤 浩介, 太田 直美, 澤田 真理, 三石 郁之, 村上 正秀, 村上 弘志, 伊豫本 直子, Kelley R.L., Kilbourne C.A., Porter F.S., Boyce K.R., Eckart M.E., Chiao M.P., Leutenegger M.A., Brown G.V., McCammon D., Szymkowiak A., Herder J.-W. den, Haas D., de Vries C., Costantini E., Akamatsu H., Paltani S., ASTRO-H SXSチーム

      日本物理学会講演概要集70   471 - 471   2015年

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

      DOI: 10.11316/jpsgaiyo.70.1.0_471

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    • 24aDJ-8 MAXIによるはくちょう座X-1のHard状態、Soft状態の長期変動

      三原 建弘, 杉本 樹梨, 北本 俊二, 松岡 勝, 杉崎 睦, 根来 均, 中平 聡志

      日本物理学会講演概要集70   500 - 500   2015年

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

      DOI: 10.11316/jpsgaiyo.70.1.0_500

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    • A new clocking method for a charge coupled device 査読有り

      Umezu Rika, Kitamoto Shunji, Murakami Hiroshi

      REVIEW OF SCIENTIFIC INSTRUMENTS85 ( 7 )   2014年7月

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    • X-ray development of the classical nova V2672 Ophiuchi with Suzaku 査読有り

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

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

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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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    • X-ray γ-ray polarimetry small satellite PolariS

      Kiyoshi Hayashida, Daisuke Yonetoku, Shuichi Gunji, Toru Tamagawa, Tatehiro Mihara, Tsunefumi Mizuno, Hiromitsu Takahashi, Tadayasu Dotani, Hidetoshi Kubo, Yoichi Yatsu, Fuyuku Tokanai, Takeshi Nakamori, Shinpei Shibata, Asami Hayato, Akihiro Furuzawa, Yuji Kishimoto, Shunji Kitamoto, Kenji Toma, Masaaki Sadamoto, Keigo Yoshinaga, Juyong Kim, Shunichiro Ide, Fumiyoshi Kamitsukasa, Naohisa Anabuki, Hiroshi Tsunemi, Jun Katagiri, Juri Sugimoto

      Proceedings of SPIE - The International Society for Optical Engineering9144   2014年

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      掲載種別:研究論文(国際会議プロシーディングス)  

      PolariS (Polarimetry Satellite) is a Japanese small satellite mission dedicated to polarimetry of X-ray and γ-ray sources. The primary aim of the mission is to perform hard X-ray (10-80 keV) polarimetry of sources brighter than 10 mCrab. For this purpose, PolariS employs three hard X-ray telescopes and scattering type imaging polarimeters. PolariS will measure the X-ray polarization for tens of sources including extragalactic ones mostly for the first time. The second purpose of the mission is γ-ray polarimetry of transient sources, such as γ-ray bursts (GRBs). Wide field polarimeters based on similar concept as that used in the IKAROS/GAP but with higher sensitivity will be used, and polarization measurement of 10 GRBs per year is expected.

      DOI: 10.1117/12.2056685

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    • X-ray gamma-ray Polarimetry Small Satellite PolariS

      Kiyoshi Hayashida, Daisuke Yonetoku, Shuichi Gunji, Toru Tamagawa, Tatehiro Mihara, Tsunefumi Mizuno, Hiromitsu Takahashi, Tadayasu Dotani, Hidetoshi Kubo, Yoichi Yatsu, Fuyuki Tokanai, Takeshi Nakamori, Shinpei Shibata, Asami Hayato, Akihiro Furuzawa, Yuji Kishimoto, Shunji Kitamoto, Kenji Toma, Masaaki Sadamoto, Keigo Yoshinaga, Kim Juyong, Shunichiro Ide, Fumiyoshi Kamitsukasa, Naohisa Anabuki, Hiroshi Tsunemi, Jun Katagiri, Juri Sugimoto

      SPACE TELESCOPES AND INSTRUMENTATION 2014: ULTRAVIOLET TO GAMMA RAY9144   2014年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)   出版者・発行元:SPIE-INT SOC OPTICAL ENGINEERING  

      PolariS (Polarimetry Satellite) is a Japanese small satellite mission dedicated to polarimetry of X-ray and gamma-ray sources. The primary aim of the mission is to perform hard X-ray (10-80 keV) polarimetry of sources brighter than 10 mCrab. For this purpose, PolariS employs three hard X-ray telescopes and scattering type imaging polarimeters. PolariS will measure the X-ray polarization for tens of sources including extragalactic ones mostly for the first time. The second purpose of the mission is gamma-ray polarimetry of transient sources, such as gamma-ray bursts (GRBs). Wide field polarimeters based on similar concept as that used in the IKAROS/GAP but with higher sensitivity will be used, and polarization measurement of 10 GRBs per year is expected.

      DOI: 10.1117/12.2056685

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    • Soft x-ray spectrometer (SXS): the high-resolution cryogenic spectrometer onboard ASTRO-H 査読有り

      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年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)  

      DOI: 10.1117/12.2057199

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    • X-ray eclipse diagnosis of the evolving mass loss in the recurrent nova U Scorpii 2010 査読有り

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

      Astrophysical Journal Letters769 ( 1 )   2013年5月20日

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      記述言語:英語   掲載種別:研究論文(学術雑誌)  

      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 査読有り

      Todoroki Shotaro, Kitamoto Shunji, Yoshida Yuki, Murakami Hiroshi

      PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN64 ( 5 ) "101 - 1"-"101-6"   2012年10月25日

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      記述言語:英語   出版者・発行元:Astronomical Society of Japan  

      DOI: 10.1093/pasj/64.5.101

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    • The High-Resolution X-Ray Microcalorimeter Spectrometer, SXS, on Astro-H 査読有り

      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   2012年6月

    • X-Ray Inerferometer with a X-Ray Beamsplitter 査読有り

      S. Kitamoto, K. Sakata, H. Murakami, Y. Yoshida, H. Seta

      SPACE TELESCOPES AND INSTRUMENTATION 2012: ULTRAVIOLET TO GAMMA RAY8443   2012年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)   出版者・発行元:SPIE-INT SOC OPTICAL ENGINEERING  

      We report our examination of a new X-ray interferometer for observation of celestial objects and our recent work for preparation of laboratory experiments. The new X-ray interferometer is consisting of two flat mirrors and one flat beam splitter which are used as grazing incident optics. The aimed wave length is a O-K band or a C-K band. The beam splitter and the mirrors are fabricated by Mo/Si multilayer. We measured their flatness and found that the measured flatness is acceptable for the test experiment. A pin hole X-ray source is also preparing for a laboratory experiment in order to demonstrate a X-ray interference. We investigated a possible observation of accretion disks around BHs and nearby stars. With a reasonable size of the base line, we can measure their size and possibly we can obtain an evidence of a black hole shadow.

      DOI: 10.1117/12.926058

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    • A Self Charge Filling (SCF) effect of Suzaku-XIS 査読有り

      Todoroki Shotaro, Kitamoto Shunji, Murakami Hiroshi

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

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    • Suzaku Observations of Six Early Type Stars 査読有り

      Kitamoto Shunji, Yoshida Masaki, Shimizu Yusuke, Murakami Hiroshi

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

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    • Detection of X-Ray Emission from the Unidentified TeV Gamma-Ray Source TeV J2032+4130 査読有り

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

      PASJ63 ( SP3 ) S873 - S878   2011年12月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)  

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    • X-Ray Study of Rekindled Accretion in the Classical Nova V2491 Cygni 査読有り

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

      PASJ2011 ( SP3 ) S729 - S783   2011年12月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)  

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    • Observation of the Cygnus OB2 Association with Suzaku and Long Term Light Curves 査読有り

      Yoshida, Masaki, Kitamoto, Shunji, Murakami, Hiroshi

      PASJ2011 ( SP3 ) S717 - S728   2011年12月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)  

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    • A New X-ray Interferometer 査読有り

      S. Kitamoto, H. Murakami, D. Takei, K. Sakata, Y. Yoshida

      Proceedings of SPIE - The International Society for Optical Engineering8147   2011年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)   出版者・発行元:SPIE-INT SOC OPTICAL ENGINEERING  

      We report a study of a new X-ray interferometer with a beam splitter for future observation of celestial objects. A possible configuration of an interferometer is proposed. By using a beam splitter, the length of the interferometer becomes short and without a formation flight of satellites a reasonable X-ray interferometric observation can be possible. An observation of early type stars is discussed. A laboratory experiment for performance verification is also discussed.

      DOI: 10.1117/12.894244

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    • Suzaku Observation of the Anomalous X-Ray Pulsar 1E 1841-045 査読有り

      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   2010年10月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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 査読有り

      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   2010年9月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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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    • 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 ( 9 ) 418 - 419   2010年2月

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)   出版者・発行元:宇宙航空研究開発機構  

      著者人数: 22人資料番号: AA0064574161レポート番号: JAXA-SP-09-008E

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    • A report on the XIS calibration of the 2 × 2 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 ( 9 ) 414 - 415   2010年2月

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)   出版者・発行元:宇宙航空研究開発機構  

      著者人数: 25人(含チーム1)資料番号: AA0064574159レポート番号: JAXA-SP-09-008E

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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&apos;ichi Kanai, Eri Takenaka, Kenta Nagasaki, Masaki Yoshida, Dai Takei, Mikio Morii

      REVIEW OF SCIENTIFIC INSTRUMENTS81 ( 2 ) 81b3105K   2010年2月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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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    • Imaging Experiment of an Adaptive Optics with a Normal-Incident EUV Telescope 査読有り

      H. Murakami, S. Kitamoto, E. Takenaka, T. Shibata, M. Yoshida, K. Higashi, D. Takei

      Proceedings of SPIE - The International Society for Optical Engineering7803   2010年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)  

      We report experimental results of our normal-incident EUV telescope tuned to a 13.5 nm band, with an adaptive optics. The optics consists of a spherical primary mirror and a secondary deformable mirror. A laser plasma source irradiates optical and EUV lights to the system. The system also equips a reference laser, optical light from which are nearly spherical and reflected by mirrors through the light path along the objective light. We controlled the deformable mirror to correct the wave form by referring that of the reference laser. At first, we attempted a normal AO control, where we controlled deformable mirror so that the wave form of the reference laser becomes spherical. Although we verified an improvement of angular resolution with this method, the resolution is not good enough comparing with the diffraction limit. The degradation is due to the difference between the paths of objective light and the reference laser. Then we modify the target wave form to control the deformable mirror, as the EUV image becomes best. We confirmed the validity of this control and performed a 2.1 arcsec resolution in both optical and EUV lights. © 2010 Copyright SPIE - The International Society for Optical Engineering.

      DOI: 10.1117/12.863535

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    • Suzaku observation of TeV J2032+4130 査読有り

      H. Murakami, S. Kitamoto

      X-RAY ASTRONOMY-2009: PRESENT STATUS, MULTI-WAVELENGTH APPROACH AND FUTURE PERSPECTIVES, PROCEEDINGS1248   41 - 42   2010年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)   出版者・発行元:AMER INST PHYSICS  

      TeV J2032+4130 is the first unidentified TeV gamma-ray source discovered by HEGRA. The position is coincident with OB association Cyg OB2. Recently, the Fermi Gamma-ray Space Telescope discovered a gamma-ray pulsar in this field. Subsequent radio observation also detected the pulsation, and determined the accurate position. The TeV gamma-ray emission would be originated by the pulsar wind nebula. We observed TeV J2032+4130 with Suzaku for about 40 ksec. We discovered diffuse X-ray emission at the position of the gamma-ray pulsar.

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    • Measuring the EUV and optical transmission of optical blocking layer for x-ray CCD camera

      Takayoshi Kohmura, Kohei Kawai, Tatsuo Watanabe, Taiki Ogawa, Shoma Ikeda, Kaoru Ushiyama, Kenta Kaneko, Shunji Kitamoto, Hiroshi Murakami, Eri Takenaka, Kenta Nagasaki, Keiichi Higashi, Masaki Yoshida, Hiroshi Tsunemi, Kiyoshi Hayasida, Naohisa Anabuki, Hiroshi Nakajima, Rui Sakaguchi, Kazuo Shigeyama, Ueda Shutaro, Takeshi Go Tsuru, Tadayasu Dotani, Masanobu Ozaki, Aya Bamba, Junko S. Hiraga, Koji Mori

      SPACE TELESCOPES AND INSTRUMENTATION 2010: ULTRAVIOLET TO GAMMA RAY7732   2010年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)   出版者・発行元:SPIE-INT SOC OPTICAL ENGINEERING  

      We have developed a new back-illuminated (BI) CCD which has an Optical Blocking Layer (OBL) directly coating its X-ray illumination surface with Aluminum-Polyimide-Aluminum instead of Optical Blocking Filter (OBF). OBL is composed of a thin polyimide layer sandwiched by two Al layers. Polyimide and Al has a capability to cut EUV and optical light, respectively. The X-ray CCD is affected by large doses of extreme ultraviolet (EUV) radiation from Earth sun-lit atmosphere (airglow) in orbit as well as the optical light.In order to evaluate the performance of the EUV-attenuating polyimide of the OBL, we measured the EUV transmission of both the OBL and the OBF at energies between 15-72 eV by utilizing a beam line located at the Photon Factory in High Energy Accelerator Research Organization (KEK-PF). We obtained the EUV transmission to be 3% at 41 eV which is the same as the expected transmission from the designed thickness of the polyimide layer. We also found no significant change of the EUV transmission of polyimide over the nine month interval spanned by out two experiments.We also measured the optical transmission of the OBL at wavelengths between 500-900 angstrom to evaluate the performance of the Al that attenuates optical light, and found the optical transmission to be less than 4x10(-5).

      DOI: 10.1117/12.856767

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    • The High-Resolution X-ray Microcalorimeter Spectrometer System for the SXS on ASTRO-H 査読有り

      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年

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    • Cooling system for the Soft X-ray Spectrometer (SXS) onboard ASTRO-H 査読有り

      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年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)   出版者・発行元: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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    • Super-Hard X-Ray Emission from eta Carinae Observed with Suzaku 査読有り

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

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

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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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    • SWIFT X-RAY AND ULTRAVIOLET MONITORING OF THE CLASSICAL NOVA V458 VUL (NOVA VUL 2007) 査読有り

      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   2009年5月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:IOP PUBLISHING LTD  

      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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    • SUZAKU DETECTION OF SUPERHARD X-RAY EMISSION FROM THE CLASSICAL NOVA V2491 CYGNI 査読有り

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

      ASTROPHYSICAL JOURNAL LETTERS697 ( 1 ) L54 - L57   2009年5月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:IOP PUBLISHING LTD  

      We report the detection of superhard (&gt; 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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    • Search for Near-Infrared Pulsation of the Anomalous X-Ray Pulsar 4U 0142+61 査読有り

      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   2009年2月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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 &gt; -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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    • EUV Imaging Experiment of an Adaptive Optics Telescope

      S. Kitamoto, T. Shibata, E. Takenaka, M. Yoshida, H. Murakami, Y. Shishido, N. Gotoh, K. Nagasaki, D. Takei, M. Morii

      Proceedings of SPIE - The International Society for Optical Engineering7437   2009年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)   出版者・発行元:SPIE  

      We report an experimental result of our normal-incident EUV telescope tuned to a 13.5 nm band, with an adaptive optics. The optics consists of a spherical primary mirror and a secondary mirror. Both are coated by Mo/Si multilayer. The diameter of the primary and the secondary mirrors are 80 mm and 55mm, respectively. The secondary mirror is a deformable mirror with 31 bimorph-piezo electrodes. The EUV from a laser plasma source was exposed to a Ni mesh with 31 micro-m wires. The image of this mesh was obtained by a backilluminated CCD. The reference wave was made by an optical laser source with 1 μm pin-hole. We measure the wave form of this reference wave and control the secondary mirror to get a good EUV image. Since the paths of EUV and the optical light for the reference were different from each other, we modify the target wave from to control the deformable mirror, as the EUV image is best. The higher order Zernike components of the target wave form, as well as the tilts and focus components, were added to the reference wave form made by simply calculated. We confirmed the validity of this control and performed a 2.1 arc-sec resolution.

      DOI: 10.1117/12.824122

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    • Development of an EUV polarimeter with a transmission multilayer 査読有り

      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年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)  

      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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    • X-Ray Spectroscopy of the Classical Nova V458 Vulpeculae with Suzaku 査読有り

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

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

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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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    • 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   2008年12月1日

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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 査読有り

      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   2008年6月25日

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      記述言語:英語   掲載種別:研究論文(学術雑誌)  

      DOI: 10.1093/pasj/60.3.585

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    • 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   2008年4月24日

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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 査読有り

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

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

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      記述言語:英語   掲載種別:研究論文(学術雑誌)  

      DOI: 10.1093/pasj/60.sp1.S231

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    • Spectral characteristics during dip in Cyg X-1

      Keisuke Sudoh, Takayoshi Kohmura, Shunji Kitamoto

      International Conference Recent Advances in Natural Language Processing, RANLP   2008年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)  

      We report the results of spectral analysis for black hole binary Cyg X-1, especially focussed on intensity dips. We used data otained with RXTE from May 5, 2000 for one orbital cycle, and in that time, many intensity dips are found. The dip spectrum are reduced by ∼ 2 % from non-dip spectrum even in the 20-150 keV. We fitted dip and non-dip spectra with two CompPS model, which expresses thermal comptonizaiton of emission from accretion disk by hot electron cloud with defferent optical depth. During dip, column density for softer component is significantly larger than that for harder one, which suggests intensity dip is caused by absorption of softer component. © Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence.

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    • Suzaku observation of AXP 1E 1841-045 in SNR Kes 73 査読有り

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

      AIP Conference Proceedings983   268 - 270   2008年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)  

      Anomalous X-ray pulsars (AXPs) are thought to be magnetars, which are neutron stars with ultra strong magnetic field of 1014-10 15G. Their energy spectra below ∼10keV are modeled well by two components consisting of a blackbody (BB) (∼0.4keV) and rather steep power-law (POW) function (photon index ∼2-4). Kuiper et al. (2004) discovered hard X-ray component above ∼10keV from some AXPs. Here, we present the Suzaku observation of the AXP 1E 1841-045 at the center of supernova remnant Kes 73. By this observation, we could analyze the spectrum from 0.4 to 50 keV at the same time. Then, we could test whether the spectral model above was valid or not in this wide energy range. We found that there were residual in the spectral fits when fit by the model of BB + POW. Fits were improved by adding another BB or POW component. But the meaning of each component became ambiguous in the phase-resolved spectroscopy. Alternatively we found that NPEX model fit well for both phase-averaged spectrum and phase-resolved spectra. In this case, the photon indices were constant during all phase, and spectral variation seemed to be very clear. This fact suggests somewhat fundamental meaning for the emission from magnetars. © 2008 American Institute of Physics.

      DOI: 10.1063/1.2900159

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    • Design of the two-stage series adiabatic demagnetization refrigerator for the NeXT and Spectrum-RG missions

      K. Shinozaki, K. Mitsuda, N. Y. Yamasaki, Y. Takei, M. Dipirro, Y. Ezoe, R. Fujimoto, J. W. Den Herder, M. Hirabayashi, Y. Ishisaki, K. Kanao, M. Kawaharada, R. Kelley, C. Kilbourne, S. Kitamoto, D. McCammon, T. Mihara, M. Murakami, T. Nakagawa, T. Ohashi, F. S. Porter, Y. Satoh, P. Shirron, H. Sugita, T. Tamagawa, M. Tashiro, S. Yoshida

      Proceedings of SPIE - The International Society for Optical Engineering7011   2008年

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      掲載種別:研究論文(学術雑誌)  

      The SXS (Soft X-ray Spectrometer) onboard the coming Japanese X-ray satellite NeXT (New Exploration Xray Telescope) and the SXC (Spectrum-RG X-ray Calorimeter) in Spectrum-RG mission are microcalorimeter array spectrometers which will achieve high spectral resolution of ~ 6 eV in 0.3-10.0 keV energy band. These spectrometers are well-suited to address key problems in high-energy astrophysics. To achieve these high spectral sensitivities, these detectors require to be operated under 50 mK by using very efficient cooling systems including adiabatic demagnetization refrigerator (ADR). For both missions, we propose a two-stage series ADR as a cooling system below 1 K, in which two units of ADR consists of magnetic cooling material, a superconducting magnet, and a heat switch are operated step by step. Three designs of the ADR are proposed for SXS/SXC. In all three designs, ADR can attain the required hold time of 23 hours at 50 mK and cooling power of 0.4μW with a low magnetic fields (1.5/1.5 Tesla or 2.0/3.0 Tesla) in a small configuration (180 mmφ× 319 mm in length). We also fabricated a new portable refrigerator for a technology investigation of two-stage ADR. Two units of ADR have been installed at the bottom of liquid He tank. By using this dewar, important technologies such as an operation of two-stage cooling cycle, tight temperature control less than 1 μK (in rms) stability, a magnetic shielding, saltpills, and gas-gap heat switches are evaluated.

      DOI: 10.1117/12.788634

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    • EUV-Imaging experiments of a normal Incident telescope with an adaptive optics system 査読有り

      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年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)  

      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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    • Oxygen line mapping of SN 1006 with Suzaku 査読有り

      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年

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      記述言語:英語   掲載種別:研究論文(学術雑誌)  

      DOI: 10.1016/j.asr.2007.03.055

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    • Low/hard state spectra of GRO J1655-40 observed with Suzaku 査読有り

      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 ) S69 - S83   2008年

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      記述言語:英語   出版者・発行元:Astronomical Society of Japan  

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      その他リンク: http://orcid.org/0000-0003-3529-3029

    • Broadband X-ray spectroscopy of A0535+262 with Suzaku 査読有り

      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   2008年1月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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 (&lt; 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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    • 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   2007年9月

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)  

      DOI: 10.1117/12.732293

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    • X-ray imaging and adaptive optics system for a 13.5nm telescope

      S. Kitamoto, Y. Ohkubo, M. Tsujimoto, T. Ogita, K. Saitoh, M. Morii, K. Sudoh, N. Gotoh, Y. Shishido, T. Shibata, E. Takenaka

      Proceedings of SPIE - The International Society for Optical Engineering6688   2007年

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      掲載種別:研究論文(国際会議プロシーディングス)  

      We are developing a normal incident X-ray telescope with an adaptive optics system in order to achieve an unprecedented high-angular-resolution. The primary mirror with a diameter of 80mm is a spherical shape with a focal length of 2000 mm, which was coated by Mo/Si multilayer. The secondary mirror is a deformable mirror with 55 mm diameter, which was also coated by Mo/Si multilayer. Optical lights from a pin-hole were measured by a wave-front sensor and used as a reference for a correction of the deformable mirror. All the components were installed in a vacuum chamber. A closed loop control with the wave front sensor and the deformable mirror was successfully performed in the telescope and we confirmed the correction of the wave front. The rms-deviation of a performed wave front from a target shape during the control was ∼30 nm-rms, whereas it without control was more than ∼80 nm-rms. A 13.5 nm X-ray from an electron impact X-ray source was imaged on a backside CCD installed on a focal plane. A mesh made by steel was installed in front of the X-ray source, whose pitch and wire-thickness are 500 micro-m and 50 micro-m. The image of this mesh by optical lights from the X-ray generator is detected by the CCD. The current image quality is ∼2.4 arc-sec and this was comparable to a diffraction limit of an optical wave length with our 80mm primary mirror.

      DOI: 10.1117/12.733655

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    • Orbital Calibration of the XIS(Chapter 12. Instructions of Suzaku Data Analysis, The Extreme Universe in the Suzaku Era) :

      Hayashida Kiyoshi, Torii Ken'ichi, Namiki Masaaki, ANABUKI Naohisa, KATSUDA Satoru, TAWA Noriaki, MIYAUCHI Tomofumi, HASUIKE Kazuto, NAGAI Masaaki, TSUNEMI Hiroshi, MATSUMOTO Hironori, TSURU Takeshi G., MORI Hideyuki, NAKAJIMA Hiroshi, YAMAGUCHI Hiroya, HYODO Yoshiaki, INUI Tatsuya, UCHIYAMA Hideki, OZAWA Midori, KOYAMA Katsuji, MILLER Eric D., BAUTZ Mark W., LAMARR Beverly, KISSEL Steve E., DOTANI Tadayasu, MURAKAMI Hiroshi, OZAKI Masanobu, ANADA Takayasu, BAMBA Aya, HIRAGA Junko, SENDA Atsushi, TAKEI Dai, KITAMOTO Shunji, MORI Koji, MAENO Shouta

      Progress of theoretical physics. Supplement ( 169 ) 316 - 321   2007年

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      記述言語:英語   出版者・発行元:Published for the Yukawa Institute for Theoretical Physics and the Physical Society of Japan  

      Orbital calibrations of the XIS, in terms of the energy scale, energy resolution, and quantum efficiency, are needed not only to confirm the calibrations on the ground but also to examine inevitable performance change in orbit. Fundamentals of the XIS calibration issues have been established and are implemented the softwares and the data base for general observers. We overview the current status of the XIS calibration in orbit.

      DOI: 10.1143/PTPS.169.316

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      その他リンク: http://dl.ndl.go.jp/info:ndljp/pid/10886569

    • Millenium study of SN 1006 with suzaku 査読有り

      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年

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      掲載種別:研究論文(国際会議プロシーディングス)  

      DOI: 10.1143/PTPS.169.142

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    • Suzaku observations of cyclotron resonances in binary X-ray pulsars 査読有り

      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年

    • Orbital calibration of the XIS 査読有り

      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年

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      記述言語:英語   掲載種別:研究論文(学術雑誌)  

      J-GLOBAL

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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   2007年1月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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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    • 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   2007年1月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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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    • 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年

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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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    • 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   2007年1月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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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    • 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   2006年9月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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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    • An application of active optics to X-ray imaging: X-mas (X-ray milli arc-second) project

      Masahiro Tsujimoto, Shunji Kitamoto, Yohsuke Ohkubo, Jun'ichi Sato, Takeshi Watanabe, Keisuke Sudoh, Akiko Sekiguchi, Kazuharu Suga, Hiroyuki Sekiguchi

      Proceedings of SPIE - The International Society for Optical Engineering6272 III   2006年

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      掲載種別:研究論文(国際会議プロシーディングス)  

      We report the current status of the "X-mas" (X-ray milli-arcsecond) project. X-mas is an application of the AO technology to the X-ray optics, aiming to obtain high-resolution defraction-limited X-ray images. Our X-ray telescope employs the Newton optics with a paraboloid primary and a 31-element deformable secondary mirrors. The aperture of the primary mirror is 80 millimeters with the focal length of 2 meters. Multi-layer coating of the mirrors by silicon and molybdenum realizes a large reflectivity of ∼60% for the primary and 30-50% for the secondary mirror at 13.5 nm, which enables us to construct a normal incidence optics at this wavelength. We use a laser guide source and a wave front sensor to optimize the form of the secondary deformable mirror for the purpose of offsetting the large-scale figure errors in the X-ray optics. A back-side illumination X-ray CCD detector manufactured by Hamamatsu Photonics is used for X-ray detections. We have assembled all these elements and started to accumulate data. Closed-loop AO is in operation for the laser guide source. Likely X-ray images are obtained through the telescope. The results in 2005-2006 are presented.

      DOI: 10.1117/12.670937

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    • Wide-band study of X-ray pulsars with Suzaku 査読有り

      Enoto T, Miyawaki R, Kokubun M, Makishima K, Terada Y, Mihara T, Nakajima M, Suzuki M, Bamba A, Senda A, Makishima K, Ishisaki Y, Takahashi H, Tamura K, Naik S, Ebisawa K, Nagase F, Kitamoto S, Sudoh K, Yoshida A, Nakagawa Y, Sugita S, Kohmura T, Kotani T, Kawai N, Yonetoku D, Mori K

      European Space Agency, (Special Publication) ESA SP ( 622 SP ) 453 - 456   2006年

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    • X-ray polarimeter with a multi-layer-coated CCD - art. no. 62662V

      Shunji Kitamoto, Takeshi Watanabe, Jun'ichi Kanai, Keisuke Sudoh, Jun'ichi Satoh, Yosuke Ohkubo, Akiko Sekiguchi, Masahiro Tsujimoto, Kazuharu Suga, Takayoshi Kohmura, Yoshitomo Maeda, Shunsaku Okada, Yumi Itoh, Ryoko Nakamura, Hideyo Kunieda

      Space Telescopes and Instrumentation II: Ultraviolet to Gamma Ray, Pts 1 and 26266   V2662 - V2662   2006年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)   出版者・発行元:SPIE-INT SOC OPTICAL ENGINEERING  

      We report a new type X-ray imaging polarimeter: a multi-layer-coated CCD. When the X-rays are detected by the CCD, with the incident angle of 45 deg, through the coated multi-layer, the transmissions of the P and S polarized photons are different from each other and we can get an image with a selected position angle of the polarization.By the simulation of the transmission of the multi-layer, we designed an optimal number of the layer-pair and their thickness. The target wave length is 135 angstrom, because the Mo/Si multi-layer has a good performance in this energy range. If the dead layer of the back-side CCD is 1000 angstrom, nine layer-pairs make the largest difference between the P and S transmission.We deposited the Mo/Si multi-layer directly on a back-side CCD. The CCD was exposed to the polarized photons from synchrotron radiation with 45 deg incident angle. The detected intensity is measured as a function of the photon energy and of the rotation angle around the photon beam. The detection of the polarization is confirmed. However the measured performance is lower than expected. Some possibilities of the cause are discussed.

      DOI: 10.1117/12.672637

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    • The development of a back-illuminated supportless CCD for SXI onboard next 査読有り

      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年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)  

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    • Suzaku broadband observations of galactic black hole binaries: Low/hard state spectra of GRO J1655-40 査読有り

      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 SP622 ( 622 SP ) 325 - 332   2006年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)  

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      その他リンク: http://orcid.org/0000-0003-3529-3029

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

      北本 俊二

      MNRAS368   1025 - 1039   2006年1月1日

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      記述言語:英語   掲載種別:研究論文(その他学術会議資料等)  

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    • Adaptive X-ray optics with a deformable mirror

      Shunji Kitamoto, Norimasa Yamamoto, Takayoshi Kohmura, Kazuharu Suga, Hiroyuki Sekiguchi, Jun'ichi Sato, Keisuke Sudo, Takeshi Watanabe, Youhei Ohkubo, Akiko Sekiguchi, Masahiro Tsujimoto

      Proceedings of SPIE - The International Society for Optical Engineering5900   1 - 8   2005年

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      掲載種別:研究論文(国際会議プロシーディングス)  

      We are developing a soft x-ray telescope with an adaptive optics system for future astronomical observation with very fine angular resolution of an order of milli-arc-second. From a technical point of view, we are trying to develop a normal incident telescope with multi layers. Thus the wave length is limited to be around 13.5 nm with a band pass of roughly 1nm. Since the x-ray telescope must be installed on a satellite, a stable conditions of temperature, gravity etc, can not be expected. Therefore, we investigate to use an adaptive optics system using an optical light source attached in the telescope. In this paper, we report our present status of the development. The primary mirror is an off-axis paraboloid with 80 mm effective diameter and 2 m focal length. This mirror has been coated with Mo/Si multi-layers. The reflectivity of the 13.5 nm x rays is ranging from 35% to 55%. We use a deformable mirror for the secondary mirror, which has also been coated with Mo/Si multi-layers. This mirror consists of 31 element-bimorph-piezo electrodes. The surface roughness of the mirror is ∼6 nm rms. The reflectivity of the 13.5 nm x rays is roughly 65%. The adaptive optics system using an optical laser and a wave front sensor has been performed. We are using a shack-hartmann sensor (HASO 32) with a micro-lens array and a CCD. A pin hole with one micron diameter is used for the optical light source. The precision of the measurement of the wave front shape is a few nm. X-ray exposure test is now conducting, although the optical adaptive optics system is not yet installed. The x-ray detector is a back illumination CCD. The quantum efficiency for 13.5 nm x ray is ∼50%. The pixel size is 24 micron square. X-ray source is an electron impact source with an Al/Si alloy target. We confirmed that the x-ray intensity around 13.55 nm is bright enough for our experiment. The imaging performance is now trying to improve and the adaptive optics system will be installed in this year.

      DOI: 10.1117/12.620162

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    • X-ray imaging spectrometers (XIS) of Astro-E2 査読有り

      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年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)  

      DOI: 10.1016/j.nima.2005.01.076

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    • The development of a back-illuminated supportless CCD for SXI onboard the NeXT satellite 査読有り

      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年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)  

      DOI: 10.1016/j.nima.2005.01.080

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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   2005年1月1日

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      記述言語:英語   掲載種別:研究論文(その他学術会議資料等)  

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

      北本 俊二

      Physica, E29   505 - 509   2005年1月1日

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      記述言語:英語   掲載種別:研究論文(その他学術会議資料等)  

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    • Soft x-ray transmission of optical blocking filters for the x-ray CCD camera onboard Astro-E2

      S. Kitamoto, T. Kohmura, N. Yamamoto, H. Takano, H. Saito, K. Suga, H. Sekiguchi, S. Chiba, I. Okamoto, K. Hayashida, H. Katayama, T. Enoguchi, Y. Nakashima, T. Shiroshouji, Y. Tawara, T. Furuzawa, T. Tanaka

      Proceedings of SPIE - The International Society for Optical Engineering5168   376 - 385   2004年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)   出版者・発行元:SPIE  

      We measured optical and soft X-ray transmission of Optical Blocking Filters (OBFs) for Charge Coupled Device (CCD) cameras, which will be launched as focal plane detectors of X-ray telescopes onboard the Japanese 5th X-ray astronomical satellite, Astro-E 2. The filters were made from polyimide coated with Al. The X-ray absorption fine structures (XAFSs) at the K. edges of C, N, O and K and L edges of Al were measured. The depth of the absorption edge of O was deep, compared to the other elements of polyimide. This is evidence of the oxidation of Al. The optical transmission is roughly less than 10-6 except for a peak around the wave length of 550nm. Long term change of the soft X-ray transmission was measured. No significant change of the thickness of the oxidation layer was found during half year.

      DOI: 10.1117/12.505589

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

      北本 俊二

      MNRAS351 ( 3 ) 791 - 807   2004年1月1日

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      記述言語:英語   掲載種別:研究論文(その他学術会議資料等)  

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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年

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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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    • 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年

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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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    • Soft X-ray Transmission of Optical Blocking Filter for the X-ray CCD Camera onboard Astro-E2

      S. Kitamoto

      NIMA505.683-687   2003年4月

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      記述言語:日本語   掲載種別:研究論文(学術雑誌)  

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    • Development of an ultra-high precision x-ray optics

      Shunji Kitamoto, Haruko Takano, Harue Saitoh, Norimasa Yamamoto, Takayoshi Kohmura, Kazuharu Suga, Hiroyuki Sekiguchi, Yohei Ohkawa, Jun'ichi Kanai, Shigeto Chiba

      Proceedings of SPIE - The International Society for Optical Engineering5169   268 - 275   2003年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)   出版者・発行元:SPIE  

      We are developing an ultra high precision Soft X-ray telescope. The design of the telescope is a normal incident one for 13.5nm band using Mo/Si multilayers. Two ideas are introduced. One is the optical measurement system in order to monitor the precision of the optics system. The other is the 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 to compensate the system distortion as a closed loop system. We confirmed that the absolute precision of the wave front sensor was less than 3 nm rms. This is also confirmed that the determination of the image center of each micro lens can be ∼1/100 of the pixel size. The precision of the deformable mirror was roughly 5 nm rms. Using the closed loop control the accuracy of the repeatability of the shape of the deformable mirror is less than 2 nm rms. The shape of the primary mirror was an off-axis paraboloide with an effective diameter of 80mm. This primary mirror was coated by Mo/Si multilayers. The reflectivity of the primary mirror at 13.5nm was ranging from 30 to 50%. The X ray-optical separation filter was made from Zr with a thickness of ∼170 nm. The transmission of the filter for low energy X-ray was measured and was roughly 50% at 13.5nm.

      DOI: 10.1117/12.505571

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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   2003年1月1日

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      記述言語:英語   掲載種別:研究論文(その他学術会議資料等)  

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    • Lunar X-ray spectrometer experiment on the selene mission 査読有り

      T. Okada, M. Kato, Y. Yamashita, K. Shirai, Y. Yamamoto, T. Matsuda, H. Tsunemi, S. Kitamoto

      Advances in Space Research30 ( 8 ) 1909 - 1914   2002年

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      掲載種別:研究論文(学術雑誌)  

      Major elemental mapping of lunar surface has been planned using the XRS instrument on the SELENE orbiter. Arrayed charge-coupled devices (CCD) are used due to its high energy resolution. By thermal design of the XRS with radiation cooling, CCD is kept cool enough to reduce excitation of thermal electrons and improve signal-to-noise ratio. During lunar x-ray fluorescence spectrometry, concurrent monitoring of solar x-rays as well as in situ calibration of x-ray fluorescence using a standard sample is performed for quantitative elemental analysis. Observed data are processed with on-board electronics that effectively extracts x-ray events. In one-year mission, the XRS will cover all the lunar surfaces except for polar region and map elemental composition with spatial resolution of 20km. We present instrumentation of the XRS and its current status of development, as well as showing the XRS observation plan of lunar elemental mapping. © 2002 COSPAR. Published by Elsevier Science Ltd. All rights reserved.

      DOI: 10.1016/S0273-1177(02)00487-8

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    • Elemental mapping of asteroid 1989ML from MUSES-C orbiter 査読有り

      T. Okada, M. Kato, K. Shirai, Y. Yamamoto, T. Matsuda, H. Tsunemi, S. Kitamoto

      Advances in Space Research29 ( 8 ) 1237 - 1242   2002年

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      掲載種別:研究論文(学術雑誌)  

      X-ray fluorescence spectrometry of a near-earth asteroid has been planned to determine major elemental composition of the asteroid surface and its regional variation from the MUSES-C orbiter, which will be launched in 2002 by the M-V vehicle. We present the characteristics of the XRS instrument and its observation plan during the mission. We numerically simulated x-ray fluorescence spectrometry of asteroid that rotates in 19-hour period and has surface geologic anomaly and we investigated achievable spatial resolution through the XRS observation during the asteroid rendezvous phase. © 2002 Elsevier Science Ltd. All rights reserved.

      DOI: 10.1016/S0273-1177(02)00142-4

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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   2002年1月1日

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      記述言語:英語   掲載種別:研究論文(その他学術会議資料等)  

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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年

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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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    • 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   2002年1月1日

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      記述言語:日本語   掲載種別:研究論文(その他学術会議資料等)  

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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   2002年1月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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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    • Evaluations of domestic X-ray CCDs with XIS analog electronics 査読有り

      A Bamba, M Kohno, H Murakami, K Imanishi, M Tsujimoto, T Tsuru, K Koyama, H Awaki, S Kitamoto, K Hayashida, H Katayama, T Tsunemi

      NEW CENTURY OF X-RAY ASTRONOMY251   518 - 519   2001年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)   出版者・発行元:ASTRONOMICAL SOC PACIFIC  

      We performed the evaluation of domestic X-ray CCDs and compared with XIS, onboard Chandra and ASTRO-EII. We evaluate them with analog electronics made for XIS. After fine tuning of gain, we found that the energy resolution of the CCD is about 135eV at 5.9 keV (FWHM) and the read-out noise of about 6 electron. This result shows that domestic X-ray CCDs are as good as XIS except for the read-out noise.

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    • Development of the ISAS Ginga archive 査読有り

      K Asai, A Yamagishi, A Yamashita, M Watanabe, T Dotani, K Mitsuda, F Nagase, K Ebisawa, S Yamauchi, A Yoshida, S Kitamoto, Hatsukade, I

      NEW CENTURY OF X-RAY ASTRONOMY251   514 - 515   2001年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)   出版者・発行元:ASTRONOMICAL SOC PACIFIC  

      We report on the development of the ISAS Ginga archive. At ISAS, all the Ginga archive and analysis software were originally developed on the main-frame computers. We are installing them to the UNIX environment with minor modification so that all the analysis will become possible in the modern network computing environment. The archive will be made public from ISAS PLAIN Center (Center for Planning and information systems) in near future.

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    • Delayed iron lines in centaurus X-3

      T. Kohmura, S. Kitamoto, K. Torii

      Astrophysical Journal562 ( 2 ) 943 - 949   2001年

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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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    • 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   2001年1月1日

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      記述言語:英語   掲載種別:研究論文(その他学術会議資料等)  

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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   2001年1月1日

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      記述言語:英語   掲載種別:研究論文(その他学術会議資料等)  

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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   2001年1月1日

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      記述言語:日本語   掲載種別:研究論文(その他学術会議資料等)  

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

      K Hayashida, S Kitamoto, E Miyata, H Tsunemi, E Yoshita, T Kohmura, K Mori, K Katayama, H Katayama, M Shouho, M Ohta, T Dotani, M Ozaki, K Koyama, H Awaki, TG Tsuru, G Ricker, MW Bautz, R Foster, S Kissel

      X-RAY OPTICS, INSTRUMENTS, AND MISSIONS III4012   123 - 136   2000年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)   出版者・発行元:SPIE-INT SOC 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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    • Reports of soft X-ray response of the engineering model of the CCD camera (XIS) for the ASTRO-E mission 査読有り

      K Katayama, T Kohmura, H Katayama, M Shouho, H Tsunemi, S Kitamoto, K Hayashida, E Miyata, K Hashimotodani, K Koyama, G Ricker, M Bautz, R Foster

      BROAD BAND X-RAY SPECTRA OF COSMIC SOURCES25 ( 3-4 ) 881 - 884   2000年

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:PERGAMON PRESS LTD  

      XIS ( X-ray Imaging Spectrometers) are four sets of X-ray CCD cameras, installed on the focal plane of the X-ray telescopes of ASTRO-E satellite, which will be launched in February, 2000. We have been calibrating the low energy ( 0.25 - 2.2 keV) response of the XIS using a spectrometer system in Osaka University. In this paper, we report the results of the calibration of the XIS EM ( Engineering Model ).
      We confirmed the energy resolution is about 130 eV at 5.9 keV (FWHM) and readout noise is similar to 3 - 4 electrons (rms) at -90 degrees C, And we measured the XIS response and energy resolution as a function of incident X-ray energy from 0.25 keV to 2.2 keV almost continuously, and absolute quantum efficiency.
      Based on the procedure we established, we are going to calibrate the XIS FM starts from August, 1998.

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    • Properties of the optical blocking filter of the XIS for the ASTRO-E mission 査読有り

      T Kohmura, K Katayama, R Asakura, S Kitamoto, H Tsunemi, K Hayashida, E Miyata, K Hashimotodani, H Katayama, M Shouho, K Koyama, S Kissel, G Ricker, M Bautz, R Foster

      BROAD BAND X-RAY SPECTRA OF COSMIC SOURCES25 ( 3-4 ) 877 - 880   2000年

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:PERGAMON PRESS LTD  

      The optical and X-ray transmission of the test samples of optical blocking filters (OBF) for the XIS (Xray Imaging Spectrometer; CCD camera onboard the ASTRO-E satellite) were measured. Unexpected high transmission of optical lights was found. The oxidation of the aluminum layer is one possible cause of the high optical transmission. (C) 2000 COSPAR. Published by Elsevier Science Ltd.

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    • MAXI (Monitor of All-sky X-ray image) for JEM on the International Space Station

      T Mihara, M Matsuoka, N Kawai, A Yoshida, T Kotani, H Negoro, H Kubo, Y Shirasaki, BC Rubin, K Torii, H Tsunemi, S Kitamoto, K Hayashida, E Miyata, K Yoshita, M Yamauchi

      BROAD BAND X-RAY SPECTRA OF COSMIC SOURCES25 ( 3-4 ) 897 - 900   2000年

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:PERGAMON PRESS LTD  

      MAXI has been approved as one of the first payloads on JEM-EF (Japanese Experiment Module Exposed Facility) on the International Space Station. It will be developed in collaboration with NASDA (NAtional Space Development Agency of Japan) to be launched in 2003. The objective of MAXI is to monitor X-ray sources over the whole sky with unprecedented sensitivity (less than 3 mCrab in 1 day). Two instruments are planned. The GSC (Gas Slit Cameras) are 1-dim position sensitive proportional counters. The SSC (Solid-state Slit Cameras) contain X-ray CCDs. The GSC covers 2-30 keV with a large window size (more than 5000cm(2)) and a low background rate. The SSC has a smaller window (similar to 200cm(2)), but has a higher energy resolution (E/Delta E similar to 50) and a sensitivity in the lower energies (0.5-10 keV). MAXI will be the first spectroscopic all-sky monitor. Objects to be observed are X-ray transients, AGNs, gamma-ray burst afterglows, CXB and so on. (C) 2000 COSPAR. Published by Elsevier Science Ltd.

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    • X-ray fluorescence spectrometer onboard Muses-C

      Tatsuaki Okada, Manabu Kato, Akio Fujimura, Hiroshi Tsunemi, Shunji Kitamoto

      Advances in Space Research25 ( 2 ) 345 - 348   2000年

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      掲載種別:研究論文(学術雑誌)  

      We present the key scientific objectives of remote x-ray spectrometry in Muses-C mission to a near-earth asteroid and the specification of the onboard x-ray spectrometer, XRS. The XRS will determine major elemental composition of the asteroid surface and its regional variation by observing the x-rays excited by solar x-ray irradiation. Information on surface roughness will be derived from the observations at various phase angles. In-flight calibration will be performed by observation of cosmic x-rays along the trajectory orbit of the Muses-C. In order to improve energy resolution and to extend detection energy range, charged-coupled devices are used as x-ray detectors. In situ calibration of x-ray fluorescence by solar x-ray irradiation into the onboard standard sample will improve the accuracy of quantitative elemental analysis. ©1999 COSPAR. Published by Elsevier Science Ltd.

      DOI: 10.1016/S0273-1177(99)00942-4

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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年

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      記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元: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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    • Soft X-ray response of a CCD with a grating spectrometer 査読有り

      M Shouho, K Katayama, H Katayama, T Kohmura, H Tsunemi, S Kitamoto, K Hayashida, E Miyata, K Hashimotodani, K Yoshita, K Koyama, G Ricker, MW Bautz, R Foster, S Kissel

      NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT436 ( 1-2 ) 85 - 90   1999年10月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:ELSEVIER SCIENCE BV  

      We calibrate the X-ray imaging spectrometers, which are CCD cameras installed on the ASTRO-E satellite, by using dispersed continuous soft X-rays from a grating spectrometer. We obtained the signal-pulse height and energy-resolution as a function of X-ray energies continuously. However, the wings of the line spread function of the grating distorts the center of the signal-pulse height derived by a simple analysis. An estimation of this distortion is presented. We also describe two methods of extracting the pure signal-pulse-height distribution from the data using the spectrometer. A brief description of the low-energy tail is presented. (C) 1999 Elsevier Science B.V. All rights reserved.

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    • Quantum efficiency of the CCD camera (XIS) for the ASTRO-E mission 査読有り

      H Katayama, M Shouho, T Kohmura, K Katayama, K Yoshita, H Tsunemi, S Kitamoto, K Hayashida, E Miyata, K Hashimotodani, K Koyama, G Ricker, MW Bautz, R Foster, S Kissel

      NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT436 ( 1-2 ) 74 - 78   1999年10月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:ELSEVIER SCIENCE BV  

      We measured the optical and the X-ray transmission of the optical blocking filters for the X-ray Imaging Spectrometers (XISs) which are the X-ray CCD cameras of the ASTRO-E satellite. We conclude that the oxidation of the aluminum reduces the optical transmission down to similar to 60-70% of the theoretical value of the aluminum. We achieved optical transmission below 5 x 10(-5) in the range from 4000 to 9500 Angstrom by using aluminum thickness of 1200 Angstrom, while the theoretical calculation requires 800 Angstrom. The measurement of absolute quantum efficiency of XIS is also performed at several particular energies. We confirmed 20% quantum efficiency at 0.5 keV for the XIS engineering model (XIS EM). (C) 1999 Elsevier Science B.V. All rights reserved.

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    • Observation of GRB afterglows with MAXI on JEM/ISS

      A Yoshida, T Mihara, M Matsuoka, N Kawai, T Kotani, H Negoro, H Kubo, Y Shirasaki, BC Rubin, K Torii, H Tsunemi, S Kitamoto, K Hayashida, E Miyata, M Yamauchi

      ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES138 ( 3 ) 439 - 440   1999年9月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:E D P SCIENCES  

      MAXI is an X-ray all-sky-monitor which will be on the Japanese Experiment Module of the International Space Station. Its objective is to monitor X-ray sources over the entire sky with the sensitivity of less than 3mCrab in 1 day. The GRB afterglow is one possible objective. One could expect similar to 25 afterglows to be detected a year at the early stage with this experiment.

      DOI: 10.1051/aas:1999299

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    • X-ray detectors and calibration system for the MAXI mission

      K Torii, M Matsuoka, M Sugizaki, H Tomida, S Ueno, WM Yuan, N Kawai, T Mihara, A Yoshida, H Tsunemi, E Miyata, H Negoro, Sakurai, I, Y Shirasaki, D Akutsu, K Hayashida, S Kitamoto, K Mori, H Ogata, K Yoshita, M Yamauchi

      EUV, X-RAY, AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY X3765 ( No. ) 636 - 644   1999年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)   出版者・発行元:SPIE-INT SOC OPTICAL ENGINEERING  

      Monitor of All-Sky X-ray Image(MAXI) is the first astrophysical payload for the Japanese Experiment Module (JEM) on the International Space Station (ISS). It is designed for monitoring all sky in the X-ray band. Two kinds of X-ray detectors, the Gas Slit Camera (GSC) and the Solid-state Slit Camera (SSC), are employed. The former is the gas proportional counter with one dimensional position sensitivity and the latter is the X-ray CCD. We have designed and constructed the engineering models of both detectors. We have also developed an X-ray irradiation facility in the Tsukuba Space Center (TKSC) of National Space Development Agency of Japan (NASDA). We report the status of the mission and introduce the X-ray irradiation facility.

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    • MAXI mission for the Space Station 査読有り

      M Matsuoka, N Kawai, T Mihara, A Yoshida, H Tsunemi, E Miyata, K Torii, T Kotani, H Kubo, H Matsumoto, H Negoro, BC Rubin, Sakurai, I, Y Shirasaki, K Hayashida, S Kitamoto, M Yamauchi

      SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - 1999, PTS ONE AND TWO458   163 - 168   1999年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)   出版者・発行元:AMER INST PHYSICS  

      MAXI (Monitor of All-sky X-ray Image) is the first astrophysical payload for Japanese Experiment Module (JEM) to be designed for all sky X-ray monitoring. MAXI is a slit scanning camera which consists of two kinds of X-ray detectors; one is one-dimensional position sensitive proportional counters with total area of similar to 5000 cm(2) (here we call GSC) and the other is an X-ray CCD array with total area similar to 200 cm(2) (here we call SSC). The GSC subtends a field of view with an angular dimension of 1 degree times 180 degrees, while the SSC does a field of view with an angular dimension of 1 degree times a little less than 180 degrees. Thus, in the course of one station orbit, MAXI can scan almost all sky with a precision of 1 degree and with X-ray energy range of 0.5 - 30 keV. MAXI with a total weight of about 500 kg will be attached to JEM exposed facility in 2003.

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    • Monitor of All-sky X-ray Image (MAXI) for JEM on the International Space Station

      N Kawai, M Matsuoka, A Yoshida, T Mihara, T Kotani, H Negoro, Y Shirasaki, Sakurai, I, M Namiki, K Torii, H Tsunemi, E Miyata, K Hayashida, S Kitamoto, K Yoshita, Y Hashimoto, M Yamauchi

      ASTRONOMISCHE NACHRICHTEN320 ( 4-5 ) 372 - 372   1999年

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:WILEY-V C H VERLAG GMBH  

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    • X-ray fluorescence spectrometry with the SELENE orbiter

      Tatsuaki Okada, Manabu Kato, Akio Fujimura, Hiroshi Tsunemi, Shunji Kitamoto

      Advances in Space Research23 ( 11 ) 1833 - 1836   1999年

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      掲載種別:研究論文(学術雑誌)  

      X-ray fluorescence spectrometry of the Moon using a CCD-based instrument 'XRS' is planned with the SELENE (Selenological and Engineering Explorer) orbiter, which will be launched in 2003. In the Apollo 15 and 16 missions, elemental mapping of Mg, Al and Si has been performed at the lunar equatorial regions for only 9% of the total surface. Much improved datasets will be obtained by using the XRS to map most of major elements, for 90% coverage of the total surface, and within 20 km spatial resolution. Key scientific objectives are (a) to measure the global average of lunar surface composition for investigation of the overall properties of lunar crust, (b) to map the rock-type distribution to study the formation and evolution of the crust and the maria, and to speculate the origin of the dichotomy, (c) to survey the chemical pattern of lava flows, or bottoms of craters or basins, for surveying the vertical structure and composition of the lunar crust and mantle. We describe the XRS instrument.

      DOI: 10.1016/S0273-1177(99)00547-5

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    • Hard X-ray response of the XIS-CCD for ASTRO-E: qualification of the X-ray CCD detector 査読有り

      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年

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    • The 35 day evolution of the hercules X-1 pulse profile: Ginga observations and their implications

      John E. Deeter, D. Matthew Scott, Paul E. Boynton, Sigenori Miyamoto, Shunji Kitamoto, Shin'ichiro Takahama, Fumiaki Nagase

      Astrophysical Journal502 ( 2 ) 802 - 823   1998年8月1日

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Institute of Physics Publishing  

      We observed Her X-1 using the Ginga observatory in the spring of 1989 with the primary intention of studying the evolution of the pulse profile through the course of the 35 day X-ray HIGH-LOW cycle in that source. These observations cover 16 separate days in two MAIN HIGH states and in the intervening SHORT HIGH state. We have augmented these data with four additional Ginga observations of Her X-1 taken for other purposes but useful for our study. We present light curves in the 1-37 keV energy band for the seven high states covered by these data together with a representative sample of pulse profiles. The signal-to-noise ratio for these profiles is generally excellent, and collectively they provide a sound base for studying the evolution of the pulse profile. Of particular utility is the 1989 May observation, which for the first time provides extensive coverage of a short high state at high photon counting rate. By combining pulse phase and frequency information from all three high state observations in 1989, we are able to determine the phase alignment of main high and short high pulse profiles with high confidence. We identify components in the Her X-1 pulse profile by their distinctive spectral signatures, and we establish the existence of a definite, repetitive pattern of pulse shape variations tied to the 35 day high-low cycle. Comparing pre-Ginga observations of pulse profiles superposed according to the 35 day phase indicates that this pattern has persisted over the past two decades. Moreover, the pulse phase alignment of the 1989 data allows the identification of components common to the main high and short high pulse profiles. One of the key elements of this pattern is the rapid change in pulse profile that occurs roughly 7 days into each main high state. In examining possible mechanisms for this interval of accelerated evolution, we are led to consider a class of models that involve dynamical changes in accretion flow geometry arising from neutron star obliquity. These models, however, suggest asymmetries in the X-ray illumination of the companion star that may conflict with extensive optical observations of the Her X-1 system. By contrast, kinematic changes in the geometrical aspect of obscuring matter flows near or within the magnetosphere that are tied to accretion disk precession provide a mechanism that may be consistent with observations.

      DOI: 10.1086/305910

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    • Discovery of the faint X-ray pulsar AX J1820.5-1434 with ASCA

      K Kinugasa, K Torii, Y Hashimoto, H Tsunemi, K Hayashida, S Kitamoto, Y Kamata, T Dotani, F Nagase, M Sugizaki, Y Ueda, N Kawai, K Makishima, S Yamauchi

      ASTROPHYSICAL JOURNAL495 ( 1 ) 435 - 439   1998年3月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:UNIV CHICAGO PRESS  

      A new X-ray pulsar, AX J1820.5-1434, has been discovered during the ASCA Galactic plane survey project on April 9, at R.A. = 18(h)20(m)29.(s)5, decl. = -14 degrees 34'24 " (equinox 2000.0; error radius 0.'5). A coherent pulsation was detected from the source with an apparent barycentric pulse period of 152.26 +/- 0.04 s. The mean flux, not corrected for the interstellar absorption, was 2.3 x 10(-11) ergs s(-1) cm(-2) in the 2-10 keV energy band. The energy spectra obtained by the GIS and SIS can be fitted by a power-law model (photon index = 0.9 +/- 0.2) with a large column density of 9.8 +/- 1.7 x 10(22) H atoms cm(-2). These parameters indicate that the new pulsar is a highly obscured accretion-driven binary X-ray pulsar. This discovery of a faint pulsar suggests existence of many hidden pulsars in our Galaxy.

      DOI: 10.1086/305291

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    • Continuum x-ray source as a calibration system for charge coupled devices 査読有り

      K Hashimotodani, T Toneri, S Kitamoto, H Tsunemi, K Hayashida, E Miyata, K Katayama, T Kohomura, R Asakura, K Koyama, K Yamamoto, K Miyaguchi, H Suzuki

      REVIEW OF SCIENTIFIC INSTRUMENTS69 ( 2 ) 392 - 395   1998年2月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:AMER INST PHYSICS  

      We present x-ray spectra obtained by a charge coupled device (CCD) from an electron impacting x-ray source using several kinds of electron targets: Au, Al-bronze, Al, and pure Al. The x rays from the source are dispersed by a grating and the dispersed x rays are focused on the CCD. Owing to the fine spatial and moderate energy resolutions of the CCD, fine spectra with 2 eV energy resolution up to 2.2 keV are obtained. X rays from the purl Al target (99.999% purity) provide good continuum x rays except for Al K x rays. This continuum source is useful as a calibration source for low energy x-ray detectors. (C) 1998 American Institute of Physics.

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    • X-ray determination of the black-hole mass in Cygnus X-1 査読有り

      A Kubota, K Makishima, T Dotani, H Inoue, K Mitsuda, F Nagase, H Negoro, Y Ueda, K Ebisawa, S Kitamoto, Y Tanaka

      HOT UNIVERSE ( 188 ) 388 - 389   1998年

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:KLUWER ACADEMIC PUBL  

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    • Where Are the X-Ray Event Grades Formed Inside the Pixel of the Charge-Coupled Device? The Behavior of the Primary Charge Cloud Inside the Charge-Coupled Device.

      Tsunemi Hiroshi, Hiraga Junko, Yoshita Kumi, Kitamoto Shunji

      Japanese Journal of Applied Physics37 ( 5 ) 2734 - 2739   1998年

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      記述言語:英語   出版者・発行元:公益社団法人 応用物理学会  

      We report the use of an improved technique to measure the X-ray detection efficiency of a charge-coupled device (CCD) with a subpixel resolution. This technique makes use of a parallel X-ray beam and metal mesh placed closely on the CCD. The mesh has many circular holes spaced at distance of 4 times the CCD pixel size (multi-pitch mesh). We could identify the interaction position of X-rays both for single events and for split pixel events. By using this method, we demonstrated how various types of X-ray events are formed inside the CCD. We have already shown that the two-pixel split events were formed near the pixel boundary. We clearly showed that the three-pixel events were formed when the interaction position was close to the pixel corner, whereas the four-pixel split events were formed when the interaction position was much closer to the pixel corner. We found that the center of gravity of split events could represent the interaction position with an uncertainty of 0.13 pixel size.

      DOI: 10.1143/JJAP.37.2734

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    • New Technique of the X-Ray Efficiency Measurement of a Charge-Coupled Device with a Subpixel Resolution

      Tsunemi Hiroshi, Yoshita Kumi, Kitamoto Shunji

      Japanese journal of applied physics. Pt. 1, Regular papers & short notes36 ( 5 ) 2906 - 2911   1997年5月15日

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      記述言語:英語   出版者・発行元:社団法人応用物理学会  

      We report the use of a new technique to measure the X-ray detection efficiency of a charge-coupled device (CCD) with subpixel resolution. The new technique makes use of a parallel X-ray beam and metal mesh placed just in front of the CCD. The CCD camera we used is a conventional system using the TC213 (Texas Instrument Japan (TIJ)) whose pixel size is 12 &micro; m &times;12 &micro; m with one million pixels. The mesh has 4 &micro;m diameter holes spaced at 12 &micro;m intervals. We produced an efficiency map within a typical pixel showing the gate structure in detail: a virtual gate, a clock gate and an antiblooming gate. The gate structure we measured is consistent with the manufacturer's design value. By selecting single pixel events, we detected a pixel boundary. Additional plans for application will also be discussed.

      DOI: 10.1143/JJAP.36.2906

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      その他リンク: https://jlc.jst.go.jp/DN/JALC/00046868282?from=CiNii

    • MAXI (monitor of all-sky X-ray image) for JEM on the Space Station

      M Matsuoka, N Kawai, T Mihara, A Yoshida, H Kubo, T Kotani, H Negoro, BC Rubin, HM Shimizu, H Tsunemi, K Hayashida, S Kitamoto, E Miyata, M Yamauchi

      EUX, X-RAY, AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY VIII3114 ( No. ) 414 - 421   1997年

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      記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)   出版者・発行元:SPIE - INT SOC OPTICAL ENGINEERING  

      NASDA (NAtional Space Development Agency of Japan) has selected MAXI as an early payload of the JEM (Japanese Experiment Module) Exposed Facility (EF) on the Space Station. MAXI is designed for all sky X-ray monitoring, and is the first astrophysical payload of four sets of equipment selected for JEM. MAXI will monitor the activities of about 1000-2000 X-ray sources.
      In the present design, MAXI is a slit scanning camera system which consists of two kinds of X-ray detectors; one with one-dimensional position sensitive proportional counters and the other with an X-ray CCD array employed for one-dimensional imaging. MAXI will be able to detect one milli-Crab X-ray sources in a-few-day observations. The whole sky will be covered completely in every orbit of the Space Station. MAXI will be capable of monitoring variability of galactic and extragalactic sources on timescales of days with a sensitivity improvement of a factor of 5 or more over previous missions.
      NASDA and RIKEN have jointly begun the design and construction of MAXI. The payload will be ready for launch in 2003.
      In this paper we will present the scientific objectives of MAXI, a basic design and some simulation results, after introducing the present status of JEM.

      DOI: 10.1117/12.278898

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    • Large hysteretic behavior of stellar black hole candidate X-ray binaries

      Sigenori Miyamoto, Shunji Kitamoto, Kiyoshi Hayashida, Wataru Egoshi

      Astrophysical Journal442 ( 1 ) L13 - L16   1995年3月20日

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Institute of Physics Publishing  

      We show that stellar black hole X-ray binaries have two novel states: the power-law hard state and the power-law soft state, which depend not only on X-ray luminosity but also on previous history of X-ray luminosity, i.e., the states show large hysteretic behavior which is dependent upon X-ray luminosity by a factor of about 100. This large hysteresis probably cannot be explained by already existing accretion disk models. The two states are represented by two (hard and soft) types of power-law spectral components. In the rising phase of the outburst of an X-ray flare or an X-ray nova, the black hole X-ray binary is in the power-law hard state and the power-law component has a photon index (-γ) of about -1.7 (γ = 1.5-1.9) in the X-ray range of 3-40 keV. This state continues until near or just before the maximum X-ray flux (2-100 keV). The state then changes to the power-law soft state, in which the photon index (-γ) of the power-law component changes to about -2.7 (γ = 2.2-3.0) in the X-ray range of 3-40 keV. Following this change, a large multi-temperature disk blackbody component (approximately represented by blackbody radiation of kT = 0.5-1 keV) appears. This state continues until the X-ray flux has decreased to about 1/100 of its maximum. The disk blackbody component then decreases rapidly and the photon index (-γ) of the power-law component changes to about -1.7. This is the beginning of the power-law hard state. In the power-law hard state, slight traces of or no disk blackbody component is observed. The short-term variability of the power-law components and the size of the X-ray emitting regions are different in these two power-law states, implying completely different X-ray production processes. This result was derived from the combined observed results of GS 1124-683, GX 339-4, and Cyg X-1.

      DOI: 10.1086/187804

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    • ORBITAL PERIOD CHANGES OF CYGNUS-X-3

      S KITAMOTO, A HIRANO, K KAWASHIMA, S MIYAMOTO, F NAGASE, NE WHITE, AP SHALE, Y SOONG, M MATSUOKA, N KAWAI, A YOSHIDA

      PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN47 ( 2 ) 233 - 238   1995年

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:ASTRONOMICAL SOC JAPAN  

      We describe the orbital period change of the X-ray binary Cygnus X-3, and present three new times of X-ray minima, obtained using the Ginga and ASCA satellites. Before 1990, the long-term ephemeris of Cyg X-3 required the introduction of a second time derivative, P, of order -(1.27 +/- 0.19) x 10(-10) yr(-1) This value indicates that the first time derivative, P, changes from a positive to a negative value around 1986. However, the new ASCA data points presented here do not confirm this large P variation and indicate a significantly smaller P of -(8.13 +/- 1.15) x 10(-11) yr(-1) and a global period change of P/P = (1.17+/-0.44) x 10(-6) yr(-1). The derived P can be explained by a large mass-loss rate of 0.58 x 10(-6) M(T) yr(-1), where M(T) is the total mass of the Cyg X-3 system. This value is consistent with the expected mass-loss rate of the Wolf-Rayet star of about 10(-6)M(.) yr(-1). The existence of a red-noise type fluctuation is also described.

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    • SPECTRAL EVOLUTION OF THE BRIGHT X-RAY NOVA GS-1124-68 (NOVA-MUSCAE 1991) OBSERVED WITH GINGA 査読有り

      K EBISAWA, M OGAWA, T AOKI, T DOTANI, M TAKIZAWA, Y TANAKA, K YOSHIDA, S MIYAMOTO, S IGA, K HAYASHIDA, S KITAMOTO, K TERADA

      PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN46 ( 4 ) 375 - 394   1994年

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:ASTRONOMICAL SOC JAPAN  

      A bright X-ray nova, GS 1124-68 (Nova Muscae 1991, GRS 1124-68), which later turned out to be a promising black-hole binary with evidence of large mass, was observed with the Large Area Counters onboard Ginga from its discovery in 1991 January to its quiescent state in 1991 September. The X-ray intensity reached a maximum (similar to 8 Crab) eight days after its discovery, then decreased exponentially with an e-folding time of about similar to 30 d. Temporary increases in the luminosity were found similar to 80 d and similar to 200 d after the outburst. The source was last detected at similar to 2 mCrab on the 239th day after the outburst; although subsequent observations were carried out on days 260 and 282, the source was below the detection limit (similar to 0.3 mCrab). GS 1124-68 exhibited such a drastic state transition that was very reminiscent of the high-low transition of black-hole candidates Cyg X-l and GX 339-4, between the 131st day (May 18) and 157th day (June 13) after the outburst. Before the transition, the energy spectrum was characterized by a thermal soft component which was dominant below similar to 8 keV, and a power-law like hard-tail component, which was significant above that energy. After the transition, the energy spectrum became much harder. The spectrum was approximately represented by a single power-law function with a photon index of similar to 1.7. Intense short time variations, which were quite similar to those in the low state of Cyg X-l, GX 339-4 and GS 2023+338, became prominent down to a timescale of milliseconds. The outburst mechanism, the origin of the soft component and the state transition can be favorably explained in terms of an optically thick accretion-disk model around a similar to 6M. black-hole at a distance of similar to 2.5 kpc.

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    • UNIFIED MODEL-FITTING TO VARIABLE X-RAY-SPECTRA OF CYGNUS-X-3

      H NAKAMURA, M MATSUOKA, N KAWAI, A YOSHIDA, S MIYOSHI, S KITAMOTO, K YAMASHITA

      MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY261 ( 2 ) 353 - 365   1993年3月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:BLACKWELL SCIENCE LTD  

      The Japanese X-ray astronomy satellite Ginga has observed Cyg X-3 in high- and low-intensity states. The X-ray spectrum of Cyg X-3 is so variable and complex that no unified model which can well explain all the observed spectra has yet been proposed. Now we have achieved a model functional form which is well fitted to X-ray spectra in most cases. Most parameters of the present 'unified model' have been proposed in previous papers, but an essential point of this model is a successful combination of physical parameters. The model consists of three components: (1) an absorbed power-law component modified with an exponential cut-off at high energy, (2) an absorbed blackbody component and (3) an iron emission line. The model fitting results in the hydrogen column density representing the absorption for the power-law component being thinner than that for the blackbody component. In addition, the observed spectra require an absorption edge at an energy of about 9 keV. In the fitting of our model to the Ginga data, the reduced chi2 value is less than 1.35 [corresponding to the 90 per cent confidence level (dof = 29)] for 85 per cent of the spectra. We present here these parameter values in detail and consider their physical meaning.

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    • GINGA OBSERVATIONS OF GX-3+1 - LONG-TERM VARIABILITIES, BRANCHES, AND X-RAY-BURSTS 査読有り

      K ASAI, T DOTANI, F NAGASE, K MITSUDA, S KITAMOTO, K MAKISHIMA, T TAKESHIMA, K KAWABATA

      PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN45 ( 6 ) 801 - 810   1993年

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:ASTRONOMICAL SOC JAPAN  

      The bright Galactic bulge source GX 3+1 (4U 1744-26) was observed with the Ginga satellite on several occasions from 1987 through 1990. The source has been found to show flux variations of a factor of 2 on the time scales of years. The hardness ratio, which is a measure of the spect;al shape, stayed almost constant during the variations. Two type-I X-ray bursts were detected near to the lower end of the hu( variations. When the variabilities were investigated on a shorter time scale of days, upper and lower banana branches were found to clearly appear in the hardness-intensity diagram. The branches become smeared out if data are accumulated for much longer than a few days in the hardness-intensity diagram. As. indicated by the presence of a banana branch, the short-term variations are correlated variations between the intensity and the hardness and, hence, their nature is very different from that of the long-term variations. This means that the long- and short-term variations have different origins. If the burst detection with Hakucho and Ginga in a low state reflects a red change in the mass accretion rate, the long-term variations may be determined by changes in the mass accretion rate. This would lead to the conclusion that the change in the mass accretion rate may not be responsible for the formation of the banana branches. We also discuss another possible interpretation that the mass accretion rate determines the branches, not the long-term variations.

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    • The X-ray outburst from X0115+634 in 1990 February 査読有り

      Keisuke Tamura, Hiroshi Tsunemi, Shunji Kitamoto, Kiyoshi Hayashida, Fumiaki Nagase

      Astrophysical Journal389 ( 2 ) 676 - 684   1992年4月20日

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Institute of Physics Publishing  

      The all sky monitor (ASM) on board Ginga discovered an X-ray outburst from the recurrent X-ray pulsar, X0115+634, on 1990 February 5. The maximum intensity of about 400 mcrab (1-20 keV) occurred around February 11. We have determined an intrinsic pulse period of 3.614690±0.000002 s as well as the orbital parameters. By combining the present results with previous ones obtained with other satellites, we can study the evolution of the orbital parameters. In particular, we have determined the apsidal motion of the orbit, ω̇=0°.030±0°.016 yr-1 (95% confidence). This determination places constraints on the mass-radius relation of the Be companion. An X-ray spectrum up to 60 keV was obtained with the LAC. We confirmed two absorption-line features that are cyclotron resonance lines originating from a magnetic source with field strength of 1 x 1012 G and magnetic dipole moment, μ, of 1 x 1030 G cm-3. Timing data obtained when the source was faint could not be connected with timings at a higher intensity, suggesting a change in the pulse shape. Based on our estimate of μ, the source was then near the critical accretion luminosity, Lcrit, below which a "propeller" effect becomes effective.

      DOI: 10.1086/171240

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    • ON X-RAY LUMINOSITIES OF THE QUIESCENT X-RAY NOVAE - GS 2000+25 AND GS 2023+338 査読有り

      S MINESHIGE, K EBISAWA, M TAKIZAWA, Y TANAKA, K HAYASHIDA, S KITAMOTO, S MIYAMOTO, K TERADA

      PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN44 ( 2 ) 117 - 123   1992年

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:ASTRONOMICAL SOC JAPAN  

      We present the results of X-ray scan observations of X-ray novae during quiescence, performed with the y Large-Area Proportional Counters (LAC) onboard Ginga. The scans of GS 2000+25 were made 155d before the peak of the 1988 outburst and 382d after the peak. The derived upper limits to the X-ray luminosity in the energy range between 1.2 and 37.1 keV are (3-9)x10(33) erg s-1 for a distance of D almost-equal-to 2 kpc. For such X-ray luminosities, the mass-overflow instability of the companion star is difficult to trigger. GS 2023+338 was X-ray scanned 320d before the peak of the 1989 outburst and 442-443d after the peak. LAC found an X-ray source at a distance of approximately 0.1 arc degree from the position of GS 2023+338 after the eruption. The possibility that this source is GS 2023+338, itself cannot be discarded if its luminosity is highly variable. If this is the case, the quiescent X-ray luminosity of GS 2023+338 is of order 10(34) erg s-1 for a distance of D almost-equal-to 3 kpc, and may be sufficient to trigger a mass-overflow instability. The disk instability model is, on the other hand, viable for both stars.

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    • DISCOVERY OF 2 TRANSIENT-X-RAY SOURCES IN THE VELA-PUPPIS REGION - PULSAR GS 0834-430 AND BURSTER GS 0836-429 査読有り

      T AOKI, T DOTANI, K EBISAWA, M ITOH, F MAKINO, F NAGASE, T TAKESHIMA, T MIHARA, S KITAMOTO

      PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN44 ( 6 ) 641 - 647   1992年

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:ASTRONOMICAL SOC JAPAN  

      We detected an X-ray outburst in the Vela-Puppis region with the All Sky Monitor (ASM) aboard Ginga on 1990 November 22. Following observations by the Large Area proportional Counter (LAC) revealed that this outburst consisted of two transient sources, GS0834-430 and GS0836-429, accidentally in the same field of view of the LAC by a separation of only 0.4 degree. These two transient X-ray sources were subsequentially monitored with the LAC until 1991 May. GS 0834-430 was identified by an X-ray pulsar with a period of 12.s3. This pulsar shows a power-law energy spectrum with a photon index of approximately 0.9, and with a high-energy cutoff that is typical of X-ray pulsars. GS 0836-429 was identified by an X-ray burster, which shows typical type-I bursts approximately every 2 h.

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    • X-RAY VARIABILITY OF GX 339-4 IN ITS VERY HIGH STATE 査読有り

      S MIYAMOTO, K KIMURA, S KITAMOTO, T DOTANI, K EBISAWA

      ASTROPHYSICAL JOURNAL383 ( 2 ) 784 - 807   1991年12月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:UNIV CHICAGO PRESS  

      GX 339-4 was observed with the large area counters (LAC) onboard Ginga in its very high state, where the X-ray intensity was about a factor of 2-3 larger than its high state and it showed very rapid variations on time scales of less than several minutes, which had not been observed earlier in the high state of this source. The X-ray energy spectrum was very soft; it consisted of a low-energy component and a high-energy tail. The low-energy component could be interpreted as being due to disk blackbody radiation (the disk blackbody component) and the high-energy tail as being due to Compton-scattering radiation (the Comptonized blackbody component). The X-ray energy spectrum also showed K-edge absorption of highly ionized iron atoms of about 10(19) cm-2 and an iron emission line with an equivalent width of about 60-100 eV.
      On short time scales of less than several minutes, the X-rays showed rapid time variations. For instance, in power spectral density functions, 6 Hz quasi-periodic oscillations (QPOs), very low frequency noise (VLF noise), and low-frequency noise (LF noise) were recognized. There are three types of power spectral density functions. Time variations such as dips and flip-flops were also observed. These rapid time variations are due to the Comptonized blackbody component.
      On long time scales larger than hours, the disk blackbody component and the Comptonized blackbody component changed independently. However, these changes took place within some restricted regions in an X-ray hardness ratio (color)-intensity or a color-color diagrams. These are a hardness ratio increasing (with the X-ray flux) branch, a hardness ratio decreasing branch, and their crossing region. These two energy spectral branches and their crossing region have three different types of power density spectra: these different branches and regions have different time variations on time scales of less than several minutes. In the hardness ratio increasing branch, the hard Compton-scattering component is the main cause of the long-term time variation of the X-ray flux, and in the hardness ratio decreasing branch, the disk blackbody component is the main cause of the long-term time variation of the X-ray flux.
      On a time lag versus Fourier period diagram, the time lag between time variations of different energy X-rays showed shoulder structures in addition to the large time lags at large Fourier periods similar to those observed in Cygnus X-1. The time variations of the X-rays of 2.3-4.6 keV were most advanced: time variations of X-rays with both lower and higher energy than 2.3-4.6 keV showed time lags relative to those of 2.3-4.6 keV X-rays. These facts together with the X-ray energy spectrum can be explained in terms of a high-energy component being due to a Compton-scattering cloud of size of about 10(9) cm, temperature kT(e) of about 30 keV, and Thomson scattering depth of about 0.5-1.0; the variable blackbody radiation with kT = approximately 1 keV is incident to the large Compton-scattering cloud.

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    • DECREASE IN THE ORBITAL PERIOD OF HERCULES-X-1

      JE DEETER, PE BOYNTON, S MIYAMOTO, S KITAMOTO, F NAGASE, N KAWAI

      ASTROPHYSICAL JOURNAL383 ( 1 ) 324 - 329   1991年12月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:UNIV CHICAGO PRESS  

      From a pulse-timing analysis of Ginga observations of the binary X-ray pulsar Her X-1 obtained during the interval 1989 April-June we have determined local orbital parameters for a SHORT HIGH state. We have also determined an orbital epoch in the adjacent MAIN HIGH state. By comparing these orbital solutions with previously published results, we have detected a decrease in the orbital period for Her X-1 at an average rate of P/P = (- 1.32 +/- 0.16) x 10(-8) yr-1 over the interval 1971-1989. This is substantially larger than the value predicted from current estimates of the mass transfer rate, and motivates consideration of other mechanisms of mass transfer and/or mass loss. A second result from these observations is a close agreement between orbital parameters determined separately in MAIN HIGH and SHORT HIGH states. This agreement places strong constraints on the obliquity of the stellar companion, HZ Her, if undergoing forced precession with a 35 day period. As a consequence further doubt is placed on the slaved-disk model as the underlying cause of the 35 day cycle in Her X-1.

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    • Discovery of a long-term periodic variation in LMC X-3 査読有り

      A. P. Cowley, P. C. Schmidtke, K. Ebisawa, F. Makino, R. A. Remillard, D. Crampton, J. B. Hutchings, S. Kitamoto, A. Treves

      Astrophysical Journal381 ( 2 ) 526 - 533   1991年11月10日

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Institute of Physics Publishing  

      The highly variable X-ray luminosity of LMC X-3 is found to be strongly modulated with a period of ∼198 (or possibly ∼99) days. Observations from both Ginga and HEAO 1 satellites show this periodic variation. For energies &lt
      13 keV, the X-ray intensity and hardness are positively correlated
      for higher energies, there appears to be no correlation. Available optical photometry indicates the mean V brightness also varies by &gt
      1 mag with this same long-term period. The regularity of this "clock" in LMC X-3 suggests that it may be related to an accretion disk precession, similar to that seen in LMC X-4, Her X-1, SS 433, or possibly periodic variations in the mass transfer rate.

      DOI: 10.1086/170676

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    • Cyclotron line features in the spectrum of the transient X-ray pulsar X0115+634

      F. Nagase, T. Dotani, Y. Tanaka, K. Makishima, T. Mihara, T. Sakao, H. Tsunemi, S. Kitamoto, K. Tamura, A. Yoshida, H. Nakamura

      Astrophysical Journal375 ( 2 PART 2 )   1991年7月10日

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      掲載種別:研究論文(学術雑誌)  

      An outburst of the transient X-ray pulsar X0115+634 was detected with the All Sky Monitor (ASM) on board Ginga on 1990 February 5. Follow-up observations with the large-area proportional counters (LACs) revealed complex changes in the energy spectrum which depend on the phase of the 3.6 s pulsation. We find that characteristic structures in the spectra above 10 keV can be best interpreted as two dips at ∼12 and ∼23 keV, although not at all phases. The center energies of the two dips are consistent with the harmonic relation of 1:2, showing phase-dependent ±10% variations with pulse phase. The results strongly suggest that the structures in the spectra are due to cyclotron resonant scattering and the two apparent absorption lines are ascribed to the fundamental and second harmonics. This indicates a magnetic field strength on the neutron star surface of ∼1 × 1012 G. Equivalent widths of the second harmonic line are about 2 times larger than those of the first harmonic line, depending on the pulse phase.

      DOI: 10.1086/186085

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    • A three-year record of the branch behaviour of the Z source GX 5-1 (4U 1758-25)

      M. Van Der Klis, S. Kitamoto, H. Tsunemi, S. Miyamoto

      Monthly Notices of the Royal Astronomical Society248 ( 4 ) 751 - 753   1991年

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Oxford University Press  

      We present a three-year random sample of the X-ray flux variations of the bright Galactic Bulge source GX 5-1 obtained with the Ginga All-Sky Monitor. The data allow us, for the first time, to perform a statistical study of the branch behaviour of a Z source. They cover 98 per cent of the branch pattern displayed by the source (90 per cent confidence). The pattern remained remarkably stable over the three years of observation. The horizontal branch (HB) extends over a factor of 2 in X-ray intensity, the source spends about equal time in the HB and in the normal branch (NB), and no flaring branch is detected. The branch behaviour is random and uncorrelated on time-scales longer than several days. Consequences of these results for near-critical accretion rate models of the NB, and for the magnetic field strength of GX 5-1 relative to other Z sources are discussed.

      DOI: 10.1093/mnras/248.4.751

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    • Discovery of a prominent cyclotron absorption feature from the transient X-ray pulsar X0331+53

      K. Makishima, T. Mihara, M. Ishida, T. Ohashi, T. Sakao, M. Tashiro, T. Tsuru, T. Kii, F. Makino, T. Murakami, F. Nagase, Y. Tanaka, H. Kunieda, Y. Tawara, S. Kitamoto, S. Miyamoto, A. Yoshida, M. J.L. Turner

      Astrophysical Journal365 ( 2 PART 2 )   1990年12月20日

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      掲載種別:研究論文(学術雑誌)  

      A remarkable absorption feature at 28.5 keV, attributable to electron cyclotron resonance, has been discovered in the 1.9-60 keV X-ray spectrum of the recurrent transient X-ray pulsar X0331+53 (V0332+53). The observed resonance energy implies a neutron star surface magnetic field of 2.5(1 + z) × 1012 G, where z is the gravitational redshift. The detection was made with the Ginga observatory in 1989 October, during an outburst of this transient with a flux level of ∼ 0.3 Crab. The feature is very deep and has been resolved with excellent statistics. This is the fourth unambiguous detection of cyclotron resonant scattering features from X-ray pulsars, suggesting that these features are a common phenomenon among these objects. An empirical relation found between the cyclotron resonance energy and the spectral cutoff energy suggests that the magnetic field strengths of the known X-ray pulsars are clustered in a range (1-4) × 1012 G.

      DOI: 10.1086/185888

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    • Outburst, identification, and X-ray light curve of GS 1354-641 (=MX 1353-64?, centaurus X-2?)

      Shunji Kitamoto, Hiroshi Tsunemi, Holger Pedersen, Sergio A. Ilovaisky, Michiel Van Der Klis

      Astrophysical Journal361 ( 2 ) 590 - 595   1990年10月1日

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Institute of Physics Publishing  

      The All Sky Monitor (ASM) on board the Ginga satellite discovered an X-ray nova, GS 1354-64, on 1987 February 13. An optical counterpart was identified on 1987 March 28, which had a visual magnitude of 16.92 mag at discovery. The ASM has monitored almost the entire light curve from the rising phase until it reached the detection limit during the decay. The maximum flux was about (2.9±0.1) × 10-9 ergs s-1 cm-2 in the 1-10 keV band. The decay time constant was about 66 days, assuming an exponential decay. The energy spectrum is well-described by an ultrasoft component with a disk blackbody spectrum, with inner disk temperature of 0.7 keV and radius of 51(cos i)-0.5(D/10 kpc) km, where i is the inclination of the disk and D is the distance to GS 1354-64, plus a hard tail with a power-law shape (photon index = 2.1). Softening of the spectrum during the decay phase was observed, which may be attributed to a temperature decrease of the X-ray emission region or to a decrease of the intervening absorption column density. The position of thel source is consistent with the positions of both MX 1353-64 and Cen X-2. However, the characteristics of GS 1354-64 were markedly different from either of these sources.

      DOI: 10.1086/169222

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    • New observations of the cyclotron absorption feature in Hercules X-1

      T. Mihara, K. Makishima, T. Ohashi, T. Sakao, M. Tashiro, F. Nagase, Y. Tanaka, S. Kitamoto, S. Miyamoto, J. E. Deeter, P. E. Boynton

      Nature346 ( 6281 ) 250 - 252   1990年

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      掲載種別:研究論文(学術雑誌)  

      ALTHOUGH neutron stars are generally believed to be born with intense (1011-1013 G) magnetic fields1,2, which then gradually decay3, measurements of their field strengths remain uncertain. In the special case of X-ray-emitting binary pulsars, a direct estimate of the field strength can be obtained by measuring the energy of spectral features that are due to electron cyclotron resonance4-13. With the Ginga satellite observatory14,15, we have measured a cyclotron feature in the hard X-ray spectrum of the 1.24-s binary pulsar Hercules X-1 with a much greater energy resolution than in previous observations4-9. The spectrum from 10-60 keV can be described with a simple analytical formula12,16,17, which indicates an absorption feature at ∼34 keV rather than an emission feature at ∼50keV. From this we estimate the surface magnetic field strength of Her X-1 to be (2.9±0.3) × 1012 G. © 1990 Nature Publishing Group.

      DOI: 10.1038/346250a0

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    • GS2023+338: A new class of X-ray transient source?

      Shunji Kitamoto, Hiroshi Tsunemi, Sigenori Miyamoto, Koujun Yamashita, Seiko Mizobuchi, Michio Nakagawa, Tadayasu Dotani, Fumiaki Makino

      Nature342 ( 6249 ) 518 - 520   1989年

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      記述言語:英語   掲載種別:研究論文(学術雑誌)  

      TRANSIENT X-ray sources are generally considered to comprise accreting binary systems containing either a black hole or a neutron star1-5. The transient X-ray emission is thought to result from episodic mass transfer to the compact star
      if this is so, transient sources should provide information on the mass-accretion mechanism. On 21 May 1989, the All-Sky Monitor6 (ASM) onboard the satellite Ginga7 discovered an unusual bright X-ray transient source, GS2023+338, in the constellation of Cygnus8. The ASM and Large-Area Counters9 (LAC), also on Ginga, have since monitored the source. Here we report the light curves and spectral evolution observed by the ASM and LAC. From 21 May to 1 June, the intensity varied by up to a factor of 500 on timescales from a few seconds to a few days10. Subsequently the rapid variations persisted, whereas slower ones disappeared. The spectral data fit a power-law model with a photon index of 0.0 to -2.5 and an absorption column density of 1021.7-1022.8 H atoms cm-2. This unusual behaviour remains to be explained. © 1989 Nature Publishing Group.

      DOI: 10.1038/342518a0

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    • X-ray optical properties of molybdenum-carbon, molybdenum-silicon, and nickel-carbon multilayers

      K. Yamashita, H. Tsunemi, S. Kitamoto, I. Hatsukade, Y. Ueno, M. Ohtani

      Review of Scientific Instruments60 ( 7 ) 2006 - 2009   1989年

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      記述言語:英語   掲載種別:研究論文(学術雑誌)  

      We have fabricated multilayer reflectors of molybdenum-carbon, molybdenum-silicon, and nickel-carbon for x rays of 1-200 Å with an electron beam evaporation method in ultrahigh vacuum. The multilayers were deposited on flat and figured substrates of float glass and superpolished glass with a surface roughness of 2-3 Å (rms). The thickness of a layer pair and the number of layer pairs were 30-100 Å and 10-20, respectively. The x-ray characteristics of these multilayer reflectors were evaluated in the 1.5-200 Å region with characteristic x rays (Cu-Kα, Si-Kα, Al-Kα, and C-Kα) and monochromatized synchrotron radiation. Peak reflectivities of molybdenum-carbon were found to be 70% at Cu-Kα and 40% at Al-Kα in grazing incidence and those of molybdenum-silicon to be more than 30% in the 150-170 Å band in near-normal incidence. On the basis of these experimental results, the x-ray optical properties of multilayers are discussed.

      DOI: 10.1063/1.1140861

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    • X-RAY AND RADIO OBSERVATIONS OF FLARES FROM THE RS CANUM VENATICORUM SYSTEM UX ARIETIS 査読有り

      T TSURU, K MAKISHIMA, T OHASHI, H INOUE, K KOYAMA, MJL TURNER, MA BARSTOW, IM MCHARDY, JP PYE, H TSUNEMI, S KITAMOTO, AR TAYLOR, RF NELSON

      PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN41 ( 3 ) 679 - 695   1989年

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:OXFORD UNIV PRESS  

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    • DELAYED HARD X-RAYS FROM CYGNUS X-1 査読有り

      S MIYAMOTO, S KITAMOTO, K MITSUDA, T DOTANI

      NATURE336 ( 6198 ) 450 - 452   1988年12月

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:NATURE PUBLISHING GROUP  

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    • TRANSIENT DIPS OF CYGNUS X-1 OBSERVED FROM TENMA 査読有り

      S KITAMOTO, S MIYAMOTO, Y TANAKA, T OHASHI, Y KONDO, Y TAWARA, M NAKAGAWA

      PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN36 ( 4 ) 731 - 740   1984年

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:ASTRONOMICAL SOC JAPAN  

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    • PULSE-PERIOD CHANGES OF X-RAY PULSARS MEASURED WITH HAKUCHO AND TENMA

      F NAGASE, S HAYAKAWA, T KII, N SATO, T IKEGAMI, N KAWAI, K MAKISHIMA, M MATSUOKA, K MITANI, T MURAKAMI, M ODA, T OHASHI, Y TANAKA, S KITAMOTO

      PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN36 ( 4 ) 667 - 678   1984年

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      記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:ASTRONOMICAL SOC JAPAN  

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    MISC

    • X線天文衛星代替機XARM搭載Resolve冷却系開発の現状

      江副祐一郎, 石崎欣尚, 藤本龍一, 竹井洋, 石川久美, 安田進, 柳瀬慶一, 山崎典子, 佐藤浩介, 北本俊二, 小山志勇, 野田博文, 吉田誠至, 金尾憲一, 恒松正二, KELLEY R. L., KILBOURNE C. A., DIPIRRO M. J., SHIRRON P.

      日本天文学会年会講演予稿集2018   2018年

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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   2018年1月1日

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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,&quot;Resolving astrophysical problems by precise high-resolution X-ray spectroscopy&quot;.1This decision was reached after evaluating the performance of the instruments aboard Hitomi and the mission&#039;s initial scientific results, and considering the landscape of planned international X-ray astrophysics missions in 2020&#039;s and 2030&#039;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: &quot;Revealing material circulation and energy transfer in cosmic plasmas and elucidating evolution of cosmic structures and objects&quot;. 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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    • Transmission measurement of the spare Beryllium window of the SXS onboard the Hitomi satellite in 2.0-12 keV with KEK-PF 査読有り

      Yuki Yoshida, Akio Hoshino, Shunji Kitamoto, Juri Sugimoto, Ryota Ishii, Yuki Ohgi, Sayaka Sato, Satomi Nukamori, Ryuichi Fujimoto, Noriko Y. Yamasaki, Toshiaki Ina, Tomoya Uruga

      Proceedings of SPIE - The International Society for Optical Engineering10397   2017年

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      記述言語:英語   出版者・発行元:SPIE  

      The Soft X-ray Spectrometer (SXS) onboard the Hitomi (ASTRO-H) satellite observed several celestial objects. All the observations with the SXS were performed through a beryllium (Be) window installed on the gate-valve of the SXS dewar. However, the Be window had not been well calibrated before launching. Therefore, we measured the transmission of a spare Be window, which is from the same lot as the flight material. The measurements were preformed in 3.8-30 keV range with BL01B1 at SPring-8, and in 2.5-12 keV range combined with BL11B and BL7C at KEK-PF. In this paper, we report mainly the results of the KEK-PF experiment. With the KEK-PF, we measured five places of the Be window. Their estimated thicknesses are consistent with each other within 1.3 μm. In the five transmission data, we confirmed absorption edges by Fe-K, Ni-K and Mn-K and six edge like features at 3460, 6057, 6915, 7590, 8790 and 9193 eV, which can be interpreted as Bragg diffraction by Be polycrystal. By combining the transmissions measured at KEK-PF and at SPring-8, we estimated Be thickness of 259.73±0.01 μm. The amounts of contaminated materials are roughly comparable with the provided values from the provider. We also performed scanning measurements of whole surface in the Be window. In the results, thickness of Be window was found to be uniform in ±1μm from the measurement with 4 keV X-rays.

      DOI: 10.1117/12.2271942

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    • The evaluation of the Hitomi (Astro-H)/SXS spare beryllium window in 3.8-30 keV 査読有り

      Akio Hoshino, Yuki Yoshida, Shunji Kitamoto, Ryuichi Fujimoto, Noriko Y. Yamasaki, Toshiaki Ina, Tomoya Uruga, Megan Eckart, Maurice Leutenegger

      Proceedings of SPIE - The International Society for Optical Engineering10397   2017年

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      記述言語:英語   出版者・発行元:SPIE  

      During the Hitomi (Astro-H) commissioning observations the SXS dewar gate valve (GV) remained closed to protect the instrument from initial spacecraft outgassing. As a result, the optical path of the observations included the Be window installed on the GV. Both x-ray fluorescence (XRF) analysis and x-ray transmission measurements were performed in June 2016 on the flight-spare Be window which is the same lot as the flight material at SPring-8 in Japan. The beamline operating range is 3.8-30 keV. We used a beam spot size of 1 mm × 0.2 mm to measure two positions on the Be window, at the center of the window and at one position 6.5 mm off-center. We used simultaneous transmission measurements of standard materials for energy calibration. The transmission data clearly showed Fe and Ni K-edges, plus a marginal detection of the Mn K-edge. We found that our transmission data was best fit using the following component Be: 261.86±0.01μm, Cr: 3nm (fixed), Mn: 3.81±0.05nm, Fe: 10.83±0.05nm, Ni: 16.48±0.03nm, Cu: 5nm (fixed). The transmission is reduced 1% at the Fe K-edge. The amount of contaminated materials are comparable to the values of the value provided by the vender. The surface transmission is strained with σ = 0.11% of the unbiased standard deviation calculated variation in the residuals between the measured value and the model.

      DOI: 10.1117/12.2272899

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    • 19aSB-3 Cyg X-3の超ソフト状態(Ultra-soft state)のMAXIとRXTE及びSwift衛星で見た性質(19aSB X線・γ線,宇宙線・宇宙物理領域)

      三原 建弘, 松岡 勝, 中島 基樹, 杉崎 睦, 中平 聡志, 北本 俊二, 小谷 太郎

      日本物理学会講演概要集69 ( 2 ) 36 - 36   2014年8月22日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

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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 - 134   2014年3月5日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

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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   2013年1月12日

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      記述言語:日本語  

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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   2012年8月20日

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      記述言語:日本語  

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    • 物理教育は今 日本物理学会第7回Jr.セッション報告

      北本 俊二, 松尾 正之

      日本物理学会誌67 ( 6 ) 406 - 408   2012年6月

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

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    • 領域委員長として

      北本 俊二

      日本物理學會誌67 ( 4 ) 225 - 225   2012年4月5日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

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    • The calibration status of P-sum mode for XIS on board Suzaku

      Kohmura, T, Kawai, K, Ikeda, S, Kaneko, K, Tsunemi, H, Hayashida, K, Nakajima, H, Koyama, K, Tsuru, T. G, Nobukawa, M, Dotani, T, Ozaki, M, Tsujimoto, M, Matsuta, K, Kitamoto, S, Murakami, H, Higashi, K, Uchiyama, H, Mori, K, Suzaku XIS Team

      SUZAKU 2011: Exploring the X-ray Universe: Suzaku and Beyond. AIP Conference Proceedings1427   247 - 248   2012年3月

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      記述言語:英語  

      DOI: 10.1063/1.3696187

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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   2012年1月6日

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      記述言語:日本語  

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    • Soft X-ray response of the X-ray CCD camera directly coated with Optical Blocking Layer 査読有り

      S. Ikeda, T. Kohmura, K. Kawai, K. Kaneko, T. Watanabe, H. Tsunemi, K. Hayashida, N. Anabuki, H. Nakajima, S. Ueda, T. G. Tsuru, T. Dotani, M. Ozaki, K. Matsuta, T. Fujinaga, S. Kitamoto, H. Murakami, J. Hiraga, K. Mori

      SUZAKU 2011: EXPLORING THE X-RAY UNIVERSE: SUZAKU AND BEYOND1427   253 - 254   2012年

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      記述言語:英語   出版者・発行元:AMER INST PHYSICS  

      We have developed the back-illuminated X-ray CCD camera (BI-CCD) to observe X-ray in space. The X-ray CCD has a sensitivity not only for in X-ray but also in both Optical and UV light, X-ray CCD has to equip a filter to cut off optical light as well as UV light. The X-ray Imaging Spectrometer (XIS) onboard Suzaku satellite equipped with a thin film (OBF : Optical Blocking Filter) to cut off optical light and UV light. OBF is always in danger tearing by the acousmato or vibration during the launch, and it is difficult to handle on the ground because of its thickness. Instead of OBF, we have newly developed and produced OBL (Optical Blocking Layer), which is directly coating on the X-ray CCD surface.

      DOI: 10.1063/1.3696190

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    • Optical, UV and soft X-ray transmission of Optical Blocking Layer for the X-ray CCD 査読有り

      K. Kawai, T. Kohmura, S. Ikeda, K. Kaneko, T. Watanabe, H. Tsunemi, K. Hayashida, N. Anabuki, H. Nakajima, S. Ueda, T. G. Tsuru, T. Dotani, M. Ozaki, K. Matsuta, T. Fujinaga, S. Kitamoto, H. Murakami, J. Hiraga, K. Mori

      SUZAKU 2011: EXPLORING THE X-RAY UNIVERSE: SUZAKU AND BEYOND1427   255 - 256   2012年

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      記述言語:英語   出版者・発行元:AMER INST PHYSICS  

      We have newly developed the back-illuminated (BI)-CCD which has an Optical Blocking Layer (OBL) directly coating its X-ray illumination surface with Aluminum-Polyimide-Aluminum instead of Optical Blocking Filter (OBF). OBL is composed of a thin polyimide layer sandwiched by two Al layers. Al and Polyimide has a capability to cut visible light and EUV, respectively. To evaluate the performance of OBL that cut off EUV as well as transmit soft X-ray, we measured the EUV and Soft X-ray transmission of both OBL at various energy range between 15-2000 eV by utilizing beam line located at the Photon Factory in High Energy Accelerator Research Organization. We obtained the EUV transmission to be similar to 3% at 41eV which is as same as expected transmission from the designed thickness of polyimide layer, and found no significant change of the EUV transmission of polyimide found during 9month. We also obtained the Soft X-ray transmission of OBL, and found the X-ray transmission of OBL was consistent with the result expected from the thickness of OBL. We also measured the Optical transmission of OBL between 500-900 nm to evaluate the performance of Al that cut off optical light, and obtained the optical transmission to be less than 4x10(-5).

      DOI: 10.1063/1.3696191

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    • 14aSP-13 ASTRO-H衛星搭載X線CCDカメラ(SXI)の軟X線検出効率の測定(14aSP X線,宇宙線・宇宙物理領域)

      幸村 孝由, 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, 池田 翔馬, 村上 弘志, 梅津 里香, 小松 飛斗, ASTRO-H SXIチーム, 金子 健太, 矢部 一成, 常深 博, 林田 清, 中嶋 大, 穴吹 直久, 薙野 綾

      日本物理学会講演概要集67 ( 0 ) 119 - 119   2012年

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      記述言語:日本語   出版者・発行元:一般社団法人 日本物理学会  

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    • 「物理学者から見た原子力利用とエネルギー問題」シンポジウム報告

      相原 博昭, 北本 俊二

      日本物理學會誌66 ( 10 ) 783 - 784   2011年10月5日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

      日本物理学会は,東日本大震災と共に起こった福島第一原子力発電所の事故と,今後の原子力利用とエネルギー問題に関して,日本物理学会会員や関連研究者の間で議論するために,緊急シンポジウムを開催した.その経過と内容を報告する.

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    • 「物理学者から見た原子力利用とエネルギー問題」シンポジウム報告

      相原 博昭, 北本 俊二

      日本物理學會誌66 ( 10 ) 783 - 784   2011年10月5日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

      日本物理学会は,東日本大震災と共に起こった福島第一原子力発電所の事故と,今後の原子力利用とエネルギー問題に関して,日本物理学会会員や関連研究者の間で議論するために,緊急シンポジウムを開催した.その経過と内容を報告する.

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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   2011年8月20日

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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   2011年8月20日

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    • 26aGS-13 古典新星による非熱的X線放射の発見(26aGS X線・γ線観測,宇宙線・宇宙物理領域)

      武井 大, 辻本 匡弘, 北本 俊二

      日本物理学会講演概要集66 ( 1 ) 111 - 111   2011年3月3日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

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    • 26aGS-13 古典新星による非熱的X線放射の発見(26aGS X線・γ線観測,宇宙線・宇宙物理領域)

      武井 大, 辻本 匡弘, 北本 俊二

      日本物理学会講演概要集66 ( 1 ) 111 - 111   2011年3月3日

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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

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

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    • X線天文衛星ASTRO‐H搭載X線CCD(SXI)の紫外線対策

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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

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      PFシンポジウム要旨集28th   88   2011年

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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   2010年8月20日

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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

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

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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   2010年8月20日

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    • 第5回ジュニアセッションの報告

      北本 俊二, 並木 雅俊

      日本物理學會誌65 ( 5 ) 356 - 358   2010年5月5日

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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

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

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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   2010年2月20日

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    • 11pSG-9 ASTRO-H衛星搭載X線CCDカメラ(SXI)の可視光・紫外線遮断用フィルムの開発(11pSG X線・γ線,宇宙線・宇宙物理領域)

      幸村 孝由, 常深 博, 林田 清, 中嶋 大, 穴吹 直久, 内田 裕之, 上田 周太朗, 鶴 剛, 堂谷 忠靖, 尾崎 正伸, 馬場 彩, 河合 耕平, 森 浩二, 平賀 純子, ASTRO-H SXIチーム, 渡辺 辰雄, 小川 大樹, 池田 翔馬, 牛山 薫, 金子 健太, 北本 俊二, 村上 弘志

      日本物理学会講演概要集65 ( 0 ) 83 - 83   2010年

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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   2009年8月20日

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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   2009年8月20日

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    • 10pSD-4 透過型多層膜を使ったX線偏光計の開発(X線・γ線,宇宙線・宇宙物理領域)

      北本 俊二, 村上 弘志, 宍戸 洋一, 齋藤 恒介, 渡邊 岳史, 金井 純一, 竹中 恵理, 長崎 健太, 武井 大, 森井 幹雄

      日本物理学会講演概要集64 ( 2 ) 35 - 35   2009年8月18日

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    • 10aSD-11 ASTRO-H搭載 精密軟X線分光装置SXSの開発の現状(II)(X線・γ線,宇宙線・宇宙物理領域)

      藤本 龍一, 佐藤 浩介, 満田 和久, 山崎 典子, 竹井 洋, 辻本 匡弘, 杉田 寛之, 佐藤 洋一, 篠崎 慶亮, 大橋 隆哉, 石崎 欣尚, 江副 祐一郎, 村上 正秀, 田代 信, 寺田 幸功, 玉川 徹, 三原 建弘, 川原田 円, 山口 弘悦, 北本 俊二, 村上 弘志, Kelley R.L, Kilbourne C.A, Porter F.S, McCammon D, den Herder J.-W, ASTRO-II SXSチーム

      日本物理学会講演概要集64 ( 2 ) 31 - 31   2009年8月18日

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    • 28pSH-5 ASTRO-H衛星搭載マイクロカロリメータSXSの開発(28pSH X線・γ線,宇宙線・宇宙物理領域)

      竹井 洋, 満田 和久, 山崎 典子, 辻本 匡弘, 篠崎 慶亮, 杉田 寛之, 佐藤 洋一, 藤本 龍一, 佐藤 浩介, 大橋 隆哉, 石崎 欣尚, 江副 祐一郎, 村上 正秀, 田代 信, 寺田 幸功, 玉川 徹, 三原 建弘, 川原田 円, 山口 弘悦, 北本 俊二, 村上 弘志, 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チーム

      日本物理学会講演概要集64 ( 1 ) 92 - 92   2009年3月3日

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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

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

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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   2009年2月20日

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    • 22pSH-6 「すざく」衛星によるLow-Hard状態におけるCygX-1の観測(II)(22pSH X線・γ線,宇宙線・宇宙物理領域)

      牧島 一夫, 山田 真也, 高橋 弘充, 久保田 あや, 堂谷 忠靖, 海老沢 研, 北本 俊二, 根来 均, 上田 佳宏, 山岡 和貴

      日本物理学会講演概要集63 ( 2 ) 89 - 89   2008年8月25日

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    • 「すざく」搭載X線CCDカメラ(XIS)の時刻付けの較正

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

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    • Spektr-RG衛星搭載X線カロリメータ分光装置SXC

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      日本天文学会年会講演予稿集2008   2008年

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    • NeXTとSpektr-RG衛星のX線カロリメータによる銀河団の観測計画

      藤本龍一, 満田和久, 山崎典子, 篠崎慶亮, 竹井洋, 中川貴雄, 杉田寛之, 佐藤洋一, 大橋隆哉, 石崎欣尚, 江副祐一郎, 村上正秀, 田代信, 北本俊二, 玉川徹, 川原田円, 三原建弘, KELLEY R. L., KILBOURNE C. A., PORTER F. S., MCCAMMON D., DEN HERDER J.-W.

      日本天文学会年会講演予稿集2008   2008年

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    • NeXT,Spectrum-RG衛星搭載X線マイクロカロリメータ用冷凍機の開発

      篠崎慶亮, 満田和久, 山崎典子, 竹井洋, 中川貴雄, 杉田寛之, 佐藤洋一, 藤本龍一, 大橋隆哉, 石崎欣尚, 江副祐一郎, 村上正秀, 田代信, 北本俊二, 玉川徹, 川原田円, 三原建弘, 平林誠之, 金尾憲一, 吉田誠至, KELLEY R., KILBOURNE C., PORTER F. S., MCCAMMON D., DEN HERDER Jan-Willem

      日本天文学会年会講演予稿集2008   2008年

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

      Yamauchi Shigeo, Nakagawa Yoshio, Sudoh Keisuke, KITAMOTO Shunji

      PASJ : publications of the Astronomical Society of Japan59 ( 6 ) 1141 - 1151   2007年12月25日

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      記述言語:英語   出版者・発行元:Astronomical Society of Japan  

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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 - 106   2007年8月21日

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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   2006年8月20日

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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   2006年2月20日

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    • 23pSH-4 「すざく」衛星によるブラックホール連星系GRO J1655-40の観測(23pSH X線・γ線,宇宙線・宇宙物理領)

      高橋 弘充, 大貫 宏祐, 高橋 忠幸, 海老沢 研, 堂谷 忠靖, 伊藤 健, 国分 紀秀, 牧島 一夫, 並木 雅章, 小谷 太郎, Parmr Arvind, 水野 恒史, Done Chris, 「すざく」チーム, 深沢 泰司, 須藤 敬輔, 荻田 喬行, 北本 俊二, 久保田 あや, 山岡 和貴, 上田 佳宏

      日本物理学会講演概要集61 ( 0 ) 77 - 77   2006年

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    • Soft X-ray Imager (SXI) onboard the NeXT satellite 査読有り

      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年

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      記述言語:英語  

      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   2005年8月20日

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    • 24pXK-6 カーボン・ナノチューブを用いる放射線検出器の開発(X線衛星装置開発,宇宙線・宇宙物理)

      小谷 太郎, 河合 誠之, 千葉 茂人, 北本 俊二

      日本物理学会講演概要集60 ( 1 ) 89 - 89   2005年3月4日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

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    • 木舟正, 『宇宙高エネルギー粒子の物理学=宇宙線・ガンマ線天文学』, 培風館, 東京, 2004, vi+206p, 21.5×14.5cm, 本体3,500円(新物理学シリーズ34)[学生・大学院向,専門書]

      北本 俊二

      日本物理學會誌60 ( 1 ) 60 - 61   2005年1月5日

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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年

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    • Wide band X-ray Imager (WXI) and Soft Gamma-ray Detector (SGD) for the NeXT Mission 査読有り

      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年

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      記述言語:英語  

      DOI: 10.1117/12.551500

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    • 29aSL-13 超高角度分解能 X 線望遠鏡の開発研究 2

      北本 俊二, 山本 則正, 幸村 孝由, 関口 宏之, 須賀 一治, 高野 晴子, 齋藤 晴江, 上田 佳宏, 伊藤 真之, X-masチーム

      日本物理学会講演概要集58 ( 1 ) 95 - 95   2003年3月6日

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    • 29aSL-12 超高角度分解能 X 線望遠鏡の開発研究 : 反射鏡の形状測定と形状制御

      山本 則正, 北本 俊二, 幸村 孝由, 関口 宏之, 須賀 一治, 高野 晴子, 齋藤 晴江, 上田 佳宏, 伊藤 真之, X-masチーム

      日本物理学会講演概要集58 ( 1 ) 95 - 95   2003年3月6日

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    • 超高精度X線望遠鏡計画(X-mas Project)

      高野 晴子, 北本 俊二, 幸村 孝由

      宇宙科学シンポジウム3   485 - 488   2003年1月9日

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    • NeXT搭載ハイブリッドカメラ:CCD検出器

      堂谷 忠靖, 尾崎 正伸, 北本 俊二

      宇宙科学シンポジウム3   131 - 134   2003年1月9日

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      記述言語:日本語   出版者・発行元:宇宙科学研究所  

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    • Astro-E2衛星搭載X線CCDカメラの可視光遮断フィルターの特性 II

      幸村孝由, 北本俊二, 須賀一治, 山本則正, 斎藤晴江, 高野晴子, 林田清, 江の口英之, 白庄司貴之, 田原譲, 古沢彰浩, 田中武

      日本天文学会年会講演予稿集2003   2003年

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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年

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    • 16aRA-3 超高角度分解能X線望遠鏡の開発研究 I(X線,宇宙線)

      北本 俊二, 関口 宏之, 須賀 一治, 幸村 孝由, 山本 則正, 斉藤 晴江, 高野 晴子, 上田 佳宏, 伊藤 真之, X-masチーム

      日本物理学会講演概要集57 ( 2 ) 84 - 84   2002年8月13日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

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    • 15aRA-3 RXTE衛星を用いたX線連星パルサーケンタウルス座X-3のX線観測(X線,宇宙線)

      幸村 孝由, 北本 俊二

      日本物理学会講演概要集57 ( 2 ) 74 - 74   2002年8月13日

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    • 27aXD-8 X線CCDカメラ用可視光遮断フィルターの特性評価

      北本 俊二, 須賀 一治, 小澤 栄治, 鈴木 一真, 加藤 理紗, 立花 祐輔, 辻 佑介, 小金井 謙, 林田 清, 幸村 孝由, 片山 晴善, 中島 雄介, 江の口 英之

      日本物理学会講演概要集57 ( 1 ) 76 - 76   2002年3月1日

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    • X-ray imaging spectrometer (XIS) on board Astro-E2 査読有り

      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年

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      記述言語:英語  

      DOI: 10.1117/12.461313

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    • 超高角分解能X線望遠鏡衛星計画

      北本 俊二, 林田 清, 宮田 恵美

      宇宙科学シンポジウム1   109 - 116   2001年1月11日

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    • ASTRO-E2搭載用X線CCDカメラ(XIS:X-ray Imaging Spectrometer)

      片山 晴善, 常深 博, 北本 俊二

      宇宙科学シンポジウム1   319 - 322   2001年1月11日

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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年

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    • Ginga all-sky monitor observations of Cygnus X-1

      S Kitamoto, W Egoshi, S Miyamoto, H Tsunemi, JC Ling, WA Wheaton, B Paul

      ASTROPHYSICAL JOURNAL531 ( 1 ) 546 - 552   2000年3月

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      記述言語:英語   出版者・発行元:IOP PUBLISHING LTD  

      We report 1-20 keV monitoring of the black hole candidate Cyg X-l by the Ginga ah-sky monitor (ASM), in 339 observations spanning from 1987 February to 1991 October. Cyg X-l was in the X-ray low state in the entire 4.5 yr period. Flux modulation at the 5.6 days orbital period was observed dearly (if we assume no periodic variation, reduced chi(2) value is 7.1) in the low-energy (1-2.1 keV) band. In the higher energy band, the modulation amplitude was small and less significant. The 1-2.1 keV folded light curve is a smooth function of the 5.6 days phase. These facts suggest that the modulation is caused by the orbital variation in the column density of photoelectrically absorbing circumstellar matter, as might be expected from the wind of the companion O9.7 Iab star, HDE 226868. The analysis of the spectral modulation suggests that the absorbing wind is not homogeneous. The similar to 300 days periodicity, reported previously by the Vela 5B investigators, was studied. Approximately 150 days periodicity, rather than similar to 300 days, was suggested in our data. Also, a broad peak around similar to 210-230 days period was found in both the power spectral density and the epoch-folding analysis. These periodicities seem to be unstable in their periods. The time-averaged 1-20 keV spectrum from the Ginga ASM alone can be characterized by a power law. However, the combined spectrum measured by Ginga in the 1-20 keV range and by the Solar Maximum Mission (SMM) hard X-ray and burst spectrometer (HXRBS), in the 25-400 keV range in 1987-1988 would require a more complex model, such as the unsaturated Comptonization model.

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    • Characteristics around oxygen and silicon K absorption edges of a charge-coupled-device

      K Mori, M Shouho, H Katayama, S Kitamoto, H Tsunemi, K Hayashida, E Miyata, M Ohta, T Kohmura, K Koyama, MW Bautz, R Foster, S Kissel

      X-RAY OPTICS, INSTRUMENTS, AND MISSIONS III4012   539 - 547   2000年

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      記述言語:英語   出版者・発行元:SPIE-INT SOC OPTICAL ENGINEERING  

      We measure various spectral response characteristics around the oxygen and silicon K absorption edges of a Charge-Coupled-Devise (CCD) X-ray detector used in the X-ray Imaging Spectrometer (XIS) developed for the ASTRO-E mission. We have evaluated X-ray Absorption Fine Structure (XAFS) around oxygen K edge in detail. A strong absorption peak of 45% is confirmed just above the oxygen Kedge and an oscillatory structure follows whose amplitude decreases from 20% at the edge to less than 1% at 0.9 keV. We also show XAFS and discuss on a change of the response function around the silicon K edge. The discontinuity of the signal pulse height at the silicon K edge is less than 1.8 eV. We determine the thickness of silicon, silicon dioxide, and silicon nitride in the dead layer using the depth of the absorption edge.

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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年

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    • 25pSD-12 国際宇宙ステーション搭載全天X線モニター(MAXI)用検出器と較正用X線ビームライン

      冨田 洋, 松岡 勝, 鳥居 研一, 杉崎 睦, 上野 史郎, 常深 博, 宮田 恵美, 林田 清, 北本 俊二, 阿久津 大介, 森 浩二, 吉田 久美, 山内 誠, 河合 誠之, 吉田 篤正, 三原 健弘, 白崎 裕治, 桜井 郁也, 根来 均

      日本物理学会講演概要集54 ( 2 ) 83 - 83   1999年9月13日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

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    • 25pSD-5 X線観測衛星ASTRO-Eに搭載するCCDカメラ(XIS)の較正報告(I)

      森 浩二, 幸村 孝由, 片山 晴善, 荘保 信, 大田 基在, 常深 博, 北本 俊二, 林田 清, 宮田 恵美, 小山 勝二, 堂谷 忠晴, RICKER G., BAUTZ M.W., FOSTER R., KISSEL S.

      日本物理学会講演概要集54 ( 2 ) 81 - 81   1999年9月13日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

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    • 30p-XJ-6 ASTRO-E搭載X線CCDカメラ(XIS)の較正結果報告

      荘保 信, 片山 晴善, 片山 和典, 幸村 孝由, 常深 博, 北本 俊二, 林田 清, 宮田 恵美, 橋本谷 磨志, 小山 勝二, Ricker G., Bautz M.W., Foster R., Kissel S., 堂谷 忠靖, Team XIS

      日本物理学会講演概要集54 ( 1 ) 362 - 362   1999年3月15日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

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    • 28a-YK-9 MAXI試作検出器とX線較正施設

      桜井 郁也, 松岡 勝, 河合 誠之, 吉田 篤正, 三原 建弘, 小谷 太郎, 根来 均, 白崎 祐治, 松本 浩典, 並木 雅章, 常深 博, 北本 俊二, 林田 清, 宮田 恵美, 吉田 久美, 橋本 康明, 鳥居 研一, 山内 誠, 鎌江 稔員

      日本物理学会講演概要集54 ( 1 ) 76 - 76   1999年3月15日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

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    • Soft X-ray response of the CCD camera (XIS)

      M Shouho, H Katayama, K Katayama, T Kohmura, H Tsunemi, S Kitamoto, K Hayashida, E Miyata, K Hashimotodani, K Koyama, G Ricker, MW Bautz, R Foster, S Kissel

      ASTRONOMISCHE NACHRICHTEN320 ( 4-5 ) 382 - 382   1999年

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      記述言語:英語   出版者・発行元:WILEY-V C H VERLAG GMBH  

      Soft X-ray response of the CCD camera (XIS, X-ray Imaging Spectrometer), which will be aboard the Astro-E satellite, was investigated for the monochromatic;X-rays in the 0.25-2.2 keV. Detailed pulse-height distribution was examined particularly for O-K line, where significant low-energy tail was found. With the aid of Monte Carlo simulation we found that the photons absorbed in the channel stop was responsible for the component.

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    • Soft X-ray quantum efficiency of the CCD camera for the Astro-E

      T Kohmura, K Katayama, H Katayama, M Shouho, H Tsunemi, S Kitamoto, K Hayashida, E Miyata, K Hashimotodani, K Koyama, G Ricker, MW Bautz, R Foster, S Kissel

      ASTRONOMISCHE NACHRICHTEN320 ( 4-5 ) 373 - 373   1999年

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      記述言語:英語   出版者・発行元:WILEY-V C H VERLAG GMBH  

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    • Calibration of the x-ray CCD camera (XIS) for the ASTRO-E in the soft x-ray band

      H Katayama, M Shouho, T Kohmura, K Katayama, M Ohta, H Tsunemi, S Kitamoto, K Hayashida, E Miyata, K Yoshita, K Koyama, G Ricker, MW Bautz, R Foster, S Kissel, J Doty

      EUV, X-RAY, AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY X3765   721 - 728   1999年

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      記述言語:英語   出版者・発行元:SPIE-INT SOC OPTICAL ENGINEERING  

      The ASTRO-E X-ray Imaging Spectrometers (XISs) consists of four sets of X-ray CCD camera for the ASTRO-E mission. The XISs have been calibrated at Osaka University: KJ oto University, ISAS and MIT. The calibration experiment. at, Osaka focuses on the soft, X-ray response of the XIS (from 0.25 to 2.2 keV).
      The calibration of the XIS Flight Model (XIS FM) has been performed since: August 1998. We measured the signal-pulse height, the energy resolution and the quantum efficiency of the XIS as a function of energy of which are essential to construct the response function of the XIS. The detailed shape of the pulse-height-distribution, are also investigated.
      We also constructed a numerical simulator of the XIS, which tracks the physical processes in the CCD so as to reproduce the measured data. With a help of this simulator, we propose a model for the pulse-height-distribution of the XIS for single energy incident X-rays. The model consists of four components; two Gaussians, a constant, plus a triangle-shape component.

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    • Quantum efficiency measurement of the X-ray CCD camera (XIS) for the ASTRO-E mission in the soft X-ray band

      T Kohmura, K Katayama, H Katayama, M Shouho, H Tsunemi, S Kitamoto, K Hayashida, E Miyata, M Ohtani, M Ohta, K Yoshita, K Koyama, G Ricker, MW Bautz, R Foster, S Kissel

      EUV, X-RAY, AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY X3765   588 - 596   1999年

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      記述言語:英語   出版者・発行元:SPIE-INT SOC OPTICAL ENGINEERING  

      We report the X-ray quantum efficiency of the XIS (X-ray Imaging Spectrometer) in the soft. X-ray band between 0.5 keV and 2.2 keV. We also report the X-ray and optical transmission of the OBF(Optical Blocking Filter). We obtained the quantum efficiency of the XIS of similar to 0.25 at 0.53 keV (O K alpha) and similar to 0.9 at 1.74 keV (Si K alpha). We also obtained the X-ray transmission of similar to 0.65 at O K alpha and optical transmission below 5x10(-5) in the range 400-950nm.

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    • Measurement of quantum efficiency of a charge coupled device

      K Hashimotodani, T Toneri, S Kitamoto, H Tsunemi, K Hayashida, E Miyata, M Ohtani, R Asakura, K Katayama, T Kohmura, J Hiraga, H Katayama, M Shoho, K Kinugasa, T Imayoshi, Y Sumi, Y Ohono

      REVIEW OF SCIENTIFIC INSTRUMENTS69 ( 11 ) 3746 - 3750   1998年11月

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      記述言語:英語   出版者・発行元:AMER INST PHYSICS  

      We report a measurement of the quantum efficiency of a charge coupled device (CCD) with a simple method and report a resultant quantum efficiency in the energy range from 0.47 to 9 keV. The CCD is a front side illuminated device and is fabricated by Hamamatsu Photonics K.K. The quantum efficiency for 4.5 keV x rays is 11% for the single pixel events, 33% for the spectroscopic events, and 60% for flux mode operation. We present the quantum efficiency as a function of the energy. (C) 1998 American Institute of Physics. [S0034-6748(98)02911-6].

      DOI: 10.1063/1.1149173

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    • 4a-E-5 X線観測衛星ASTRO-Eに搭載するCCDカメラ(XIS)の応答関数構築

      荘保 信, 片山 晴善, 片山 和典, 幸村 孝由, 常深 博, 北本 俊二, 林田 清, 宮田 恵美, 橋本谷 麿志, 小山 勝二, RICKER G., BAUTZ M.W, FOSTER R., 堂谷 忠靖, XIS-Team

      日本物理学会講演概要集53 ( 2 ) 83 - 83   1998年9月5日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

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    • 4a-E-4 X線観測衛星ASTRO-Eに搭載するCCDカメラ(XIS)の量子効率

      片山 晴善, 荘保 信, 幸村 孝由, 片山 和典, 常深 博, 北本 俊二, 林田 清, 宮田 恵美, 橋本谷 麿志, 小山 勝二, RICKER G., BAUTZ M.W, FOSTER R., XIS-eam

      日本物理学会講演概要集53 ( 2 ) 83 - 83   1998年9月5日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

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    • 2a-J-8 国際宇宙ステーション搭載全天X線監視装置MAXI(II)

      河合 誠之, 松岡 勝, 吉田 篤正, 三原 建弘, 小谷 太郎, 根来 均, RUBIN Brad, 窪 秀利, 白崎 祐治, 常深 博, 北本 俊二, 林田 清, 宮田 恵美, 鳥居 研一, 橋本谷 磨志, 吉田 久美, 山内 誠

      日本物理学会講演概要集53 ( 1 ) 81 - 81   1998年3月10日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

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    • 2a-J-6 X線観測衛星Astro-Eに搭載するCCDカメラ(XIS)の2.2keV以下のX線に対する応答

      幸村 孝由, 片山 和典, 朝倉 励子, 常深 博, 北本 俊二, 林田 清, 宮田 恵美, 橋本谷 麿志, RICKER G.R., XIS-TEAM

      日本物理学会講演概要集53 ( 1 ) 80 - 80   1998年3月10日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

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    • ASTRO‐E搭載X線CCDカメラ(XIS)EM動作試験報告

      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年

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      記述言語:日本語  

      J-GLOBAL

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    • Soft X-ray response of the proto-type CCD camera (XIS) for Astro-E 査読有り

      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年

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      記述言語:英語  

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    • Optical follow-up observations of the ASCA Large Sky Survey 査読有り

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

      HOT UNIVERSE319 ( 188 ) 465 - 466   1998年

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      記述言語:日本語  

      DOI: 10.1002/asna.2123190127

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    • Time Variation of X-Rays from GX 5-1

      Kamado Yasuhide, Kitamoto Shunji, Miyamoto Shigenori

      PASJ : publications of the Astronomical Society of Japan49 ( 5 ) 589 - 605   1997年10月25日

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      記述言語:英語   出版者・発行元:Astronomical Society of Japan  

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    • 23p-J-13 国際宇宙ステーション搭載全天X線監視装置MAXI

      三原 建弘, 松岡 勝, 河合 誠之, 吉田 篤正, 小谷 太郎, 根来 均, Rubin B., 清水 裕彦, 常深 博, 北本 俊二, 林田 清, 宮田 恵美, 橋本谷 麿志, 吉田 久美, 山内 誠

      日本物理学会講演概要集52 ( 2 ) 84 - 84   1997年9月2日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

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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年

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    • ASCA Observation of Cygnus OB2 Association

      Kitamoto Shunji, Mukai Koji

      PASJ : publications of the Astronomical Society of Japan48 ( 6 ) 813 - 818   1996年12月1日

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      記述言語:英語   出版者・発行元:Astronomical Society of Japan  

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    • 8a-C-2 X線直接撮像型CCDのX線検出効率の測定

      北本 俊二, 常深 博, 林田 清, 宮田 恵美, 橋本谷 磨志, 大野 喜明, 鷲見 裕一郎, 小山 勝二, 山本 晃永, 宮口 和久, 川嶋 健治, 今吉 拓哉, 戸練 景, 藤原 哉, 鶴 剛, 栗木 久光

      日本物理学会講演概要集. 秋の分科会1996 ( 1 ) 168 - 168   1996年9月13日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

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    • X-Ray Spectroscopy of Centaurus X-3 with ASCA over an Eclipse

      Ebisawa Ken, Day Charles S.R., Kallman Timothy R., NAGASE Fumiaki, KOTANI Taro, KAWASHIMA Kenji, KITAMOTO Shunji, WOO Jonathan W.

      PASJ : publications of the Astronomical Society of Japan48 ( 3 ) 425 - 440   1996年6月25日

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      記述言語:英語   出版者・発行元:Astronomical Society of Japan  

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    • X線偏光撮像分光計画

      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   1996年3月

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      J-GLOBAL

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    • Long-term behavior of centaurus X-3 observed with the all sky monitor on board Ginga

      H Tsunemi, S Kitamoto, Tamura, I

      ASTROPHYSICAL JOURNAL456 ( 1 ) 316 - 319   1996年1月

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      記述言語:英語   出版者・発行元:UNIV CHICAGO PRESS  

      The long-term X-ray light curve of Centaurus X-3 and its pulse-period history, which were obtained by the All Sky Monitor on board the Ginga satellite from 1987 February to 1991 October, are presented. The pulse-period history shows a monotonic spin-up overlapping a roughly sinusoidal wave structure with a period of 9.23 +/- 0.14 yr. The observed light curve shows no correlation with the spin-up history. Since Cen X-3 is considered to be a disk-fed X-ray pulsar, the mass accretion affects the pulse period by means of angular-momentum transfer onto the neutron star. In the absence of a correlation between the light curve and pulse period, we conclude that the observed intensity does not represent the mass accretion rate.

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    • ACCRETION DISK STRUCTURE AND BRANCH BEHAVIOR OF CYGNUS X-2

      HIRANO Akira, KITAMOTO Shunji, YAMADA Tatsuya.T, MINESHIGE Shin, FUKUE Jun

      The Astrophysical Journal446   350 - 356   1995年6月10日

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      記述言語:英語   出版者・発行元:The American Astronomical Society  

      A new analysis of the branch behavior of Cygnus X-2 is presented, applying a new disk model with a free parameter of a radial temperature gradient, q = -d log T/d log r, for the spectral fitting. We find that the spectral fitting is significantly improved for about one third of data and that the derived q-value changes from 0.67 to 0.85 in accordance with the spectral evolution from the horizontal branch (HB) to the flaring branch (FB) via the normal branch (NB). Two positive and negative correlations are found between the inner disk radius (R_in) and q, and between R_in and the inner disk temperature (T_in). Possible new interpretations regarding the branch behavior of C_yg X-2 are discussed based on these results.

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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年

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      J-GLOBAL

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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年

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    • IRON LINE INTENSITY VARIATIONS OF HERCULES-X-1 OVER THE PULSE PHASE AND THE 35-DAY CYCLE

      CS CHOI, F NAGASE, F MAKINO, T DOTANI, S KITAMOTO, S TAKAHAMA

      ASTROPHYSICAL JOURNAL437 ( 1 ) 449 - 457   1994年12月

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      記述言語:英語   出版者・発行元:UNIV CHICAGO PRESS  

      We have studied the iron line intensity variation of Her X-l over its characteristic periodicities such as the pulse period of 1.24 s, the orbital period of 1.7 days, and the long-term period of 35 days, with Ginga observations made from 1989 April to June. From an analysis of the pulse phase-resolved spectra obtained from the MAIN HIGH state of Her X-l, we discover that the line flux modulates from (4.3 +/- 1.9) x 10(-3) to (1.0 +/- 0.3) x 10(-2) photons cm(-2) s(-1) (the average 7.5 x 10(-3) cm(-2) s(-1)) during the pulse period. We also find that the line flux modulation is consistent with that of soft X-rays below 1 keV observed by previous authors. From the study of the orbital phase and the 35 day cycle dependences, we see the following facts: (1) the line flux observed during the high intensity state of Her X-l does not depend significantly on the orbital phase of 0.2-0.9, while the flux is almost invisible during the eclipse, (2) the pattern of the iron line flux modulation along the 35 day cycle is very similar to that of the continuum X-ray flux. With the line pulsations and the solid angle required to explain the equivalent width of the line in the MAIN HIGH state, we deduce that the extent of reprocessing site is less than 10(10) cm. Based on the similarity of the modulation pattern between the line flux and the continuum flux along the 35 day cycle, and the equivalent width change, we suggest that the line flux variation is mainly due to occultation of the reprocessing site by an accretion disk rather than to a change of reprocessing site; some line flux, very small compared with the MAIN HIGH line flux, from an additional site may be responsible for the equivalent width change.

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    • TIME-DEPENDENT DISK ACCRETION IN X-RAY NOVA MUSCAE 1991

      MINESHIGE Shin, HIRANO Akira, KITAMOTO Shunji, YAMADA Tatsuya.T, FUKUE Jun

      The Astrophysical Journal426   308 - 312   1994年5月1日

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      記述言語:英語   出版者・発行元:The American Astronomical Society  

      We propose a new model for X-ray spectral fitting of binary black hole candidates. In this model, it is assumed that X-ray spectra are composed of a Comptonized blackbody (hard component) and a disk blackbody spectra (soft component), in which the temperature gradient of the disk, q = -d log T/d log r, is left as a fitting parameter. With this model, we have fitted X-ray spectra of X-ray Nova Muscae 1991 obtained by Ginga. The fitting shows that a hot cloud, which Compton up-scatters soft photons from the disk, gradually shrank and became transparent after the main peak. The temperature gradient turns out to be fairly constant and is q ~ 0.75, the value expected for a Newtonian disk model. To reproduce this value with a relativistic disk model, a small inclination angle, i ~ 0°-15°, is required. It seems, however, that the q-value temporarily decreased below 0.75 at the main flare, and q increased in a transient fashion at the second peak (or the reflare) occurring ~70 days after the main peak. Although statistics are poor, these results, if real, would indicate that the disk brightening responsible for the main and secondary peaks are initiated in the relatively inner portions of the disk.

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    • 31p-YW-1 「あすか」が観測したCygX-3近傍のプラズマの状態

      北本 俊二, 川島 健治, 根来 均, 長瀬 文昭, White N.E

      日本物理学会講演概要集. 年会49 ( 1 ) 173 - 173   1994年3月16日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

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    • X-RAY-OBSERVATION OF THE JOVIAN IMPACTS OF COMET SHOEMAKER-LEVY-9

      K TERADA, H NEGORO, K HAYASHIDA, S KITAMOTO, H TSUNEMI, H OYA, T ONO, A MORIOKA, Y TAWARA, T MUKAI, M HOSHINO, T TERASAWA

      EARTH MOON AND PLANETS66 ( 1 ) 75 - 81   1994年

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      記述言語:英語   出版者・発行元:KLUWER ACADEMIC PUBL  

      An ASCA observation of the Jovian impact of the comet Shoemaker-Levy 9 is reported. Four impacts of H, L, Q1 and R were observed and four impacts of B, C, G, and Q2 were observed within 60 minutes after their impacts. No significant flaring of X-ray emission was observed. Upper limit X-ray fluxes of 90 % confidence level, averaged 5 minutes just after the impacts, were 2.4 x 10(-13) erg sec(-1) cm(-2), 3.5 X 10(-13) erg sec(-1) cm(-2), 1.6 X 10(-13) erg sec(-1) cm(-2) and 2.9 x 10(-13) erg sec(-1) cm(-2) for the impacts of H, L, Q1 and R, respectively, in the 0.5(0.7 for H and Q1)-10 keV energy range. However, a hint of X-ray enhancement around Jupiter from July 17 to July 19 was detected with about 2 similar to 6 x 10(-14) erg sec(-1) cm(-2) in the 0.5-10 keV energy range.

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    • DISCOVERY AND X-RAY-PROPERTIES OF GS-1124-683 (=NOVA MUSCAE)

      S KITAMOTO, H TSUNEMI, S MIYAMOTO, K HAYASHIDA

      ASTROPHYSICAL JOURNAL394 ( 2 ) 609 - 614   1992年8月

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      記述言語:英語   出版者・発行元:UNIV CHICAGO PRESS  

      A bright X-ray nova: GS 1124-683 was discovered by the All Sky Monitor (ASM) on board Ginga on 1991 January 8. X-ray properties observed with the ASM from 1991 January 5 to the end of August are presented. The observed spectra were roughly described by a two-component model consisting of a power-law (a hard X-ray) and a disk-blackbody or a blackbody (a soft X-ray) component. In its rising phase, the hard X-ray component appeared first and the soft X-ray component followed with increase of the temperature and the emission area. After the maximum, the intensity of the energy range 1-6 keV decayed exponentially with a time constant of 31.2 +/- 0.1 days, whereas the hard component fell off more rapidly with a time constant of approximately 13 days. The state where the hard component has an appreciable fraction of the energy flux can be recognized as a very high state, which is observed in GX 339-4. With the decay of the hard X-ray component, GS 1124-683 would transfer to the so-called high state. The decay of the soft component can be interpreted to be due to the decrease of temperature of the soft X-ray component. On 70 days after the maximum, a hump of the intensity was observed. About 140 days after the maximum the spectrum becomes hard and would change into the so-called low state. Similar behaviors are observed from two ultrasoft transient sources, A0620-00 and GS 2000+25, therefore such behaviors are considered to be common for bright ultrasoft transient sources.

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    • X-RAY-SPECTRUM AND TIME-VARIATION OF X1850-087 IN THE GLOBULAR-CLUSTER NGC-6712

      S KITAMOTO, H TSUNEMI, D ROUSSELDUPRE

      ASTROPHYSICAL JOURNAL391 ( 1 ) 220 - 227   1992年5月

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      記述言語:英語   出版者・発行元:IOP PUBLISHING LTD  

      We observed the energy spectrum and the time variation of the X-rays from X1850-087 in the globular cluster NGC 6712 with the Large Area Counter on board Ginga. The luminosity of X1850-087, when we observed it, was 1.3 x 10(36) (D/6.8 kpc)2 ergs s-1. The X-ray energy spectrum can be represented by a single power-law type spectrum with a photon index of 2.3, with an interstellar absorption of less than 10(21) H atoms cm-2. A model consisting of disk blackbody and radiation from the neutron star requires an unphysically small inner-disk-radius and a small emission region on the neutron star surface where allowances have been made for the difference between the color temperature and the effective temperature. On the other hand, a model where the main X-ray formation mechanism is Compton scattering indicates that the plasma, which is responsible for Compton scattering, becomes thin and hot in the low accretion rate state. No significant periodic variation was detected, but a significant variation below 1 Hz was found, which is similar to a high-frequency noise observed in the island state of the atoll sources.

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    • 30a-SC-12 白鳥座X-3からの鉄輝線

      北本 俊二, 山下 広順, 中村 浩

      秋の分科会講演予稿集1990 ( 1 ) 92 - 92   1990年9月12日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

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    • 30a-SC-13 X線星 GX339-4 のJet Model

      宮本 重徳, 北本 俊二

      秋の分科会講演予稿集1990 ( 1 ) 92 - 92   1990年9月12日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

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    • X線新星とブラックホ-ル候補 (ぎんが特集)

      常深 博, 北本 俊二, 井上 一

      天文月報83 ( 6 ) p161 - 163   1990年6月

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      記述言語:日本語   出版者・発行元:日本天文学会  

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    • X-Ray Spectrum and Iron Line Emission from Cygnus X-1

      Kitamoto Shunji

      Publications of the Astronomical Society of Japan42 ( 1 ) p85 - 97   1990年3月

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      記述言語:英語   出版者・発行元:Astronomical Society of Japan  

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    • 13p-C-3 CYG X-1, GX339-4よりのX線の位相遅れの構造

      宮本 重徳, 北本 俊二, 木村 和宏

      秋の分科会講演予稿集1989 ( 1 ) 87 - 87   1989年9月12日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

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    • Scattered X-Ray Halo and Transient Dips of Cygnus X-1

      Kitamoto Shunji, Miyamoto Sigenori, Yamamoto Toshiko

      Publications of the Astronomical Society of Japan41 ( 1 ) p81 - 95   1989年3月

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      記述言語:英語   出版者・発行元:Astronomical Society of Japan  

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    • CYGNUS X-1 よりの X 線の時間変動 : 硬い X 線の時間変動の遅れ

      宮本 重徳, 北本 俊二

      宇宙科学研究所報告. 特集23   77 - 94   1989年3月

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      記述言語:日本語   出版者・発行元:宇宙航空研究開発機構  

      白鳥座X-1(Cygnus X-1)は, ブラックホール候補と考えられている。その一つの特徴は, X線の強度がいろいろな時間尺度で非常に激しく変動していることである。これまで, 観測されるX線は低エネルギーの光子がブラックホールの近くにある高温(約1億度から10億度)のプラズマで逆コンプトン散乱されてできたものであると, 考えられてきた。その場合, 高エネルギー側のX線の時間変動は, 低エネルギー側のそれに比べて, 遅れが生じると期待される。我々は, 『ぎんが』に搭載された大面積比例計数管(LAC)により白鳥座X-1を観測し, その時系列データをクロス スペクトルの方法で解析を行った。その結果, 高エネルギー側のX線は, 低エネルギー側のX線に比べて遅れており, その遅れの時間は, 0.1秒周期の周波数成分における約2ミリ秒から, 300秒周期の周波数成分における数秒までほぼ直線的に増加していることをつきとめた。この時間の遅れの周波数依存性は, 逆コンプトン散乱のモデルとは矛盾するものである。白鳥座X-1では, 高エネルギー側のX線に遅れが見られるが, 準周期的振動(QPO)を示す低質量X線連星系(中性子星を含む)で観測される低周波雑音(LFN)では, 低エネルギー側のX線に遅れが見られる。この違いは, 白鳥座X-1は, ブラックホールを含むため, X線を放射しているプラズマが, ブラックホールに落ちるにつれて高温になり, やがてブラックホールに落ちて消えてしまうという描像で説明されるかも知れない。また, 我々は白鳥座X-1の観測時期, エネルギーバンドにかかわらず, 時間の遅れは0.1秒, 3秒, 10秒に特徴的構造がある事を発見した。

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    • ASM の発見した X 線新星 GS2000+25 とその観測

      常深 博, 北本 俊二, 岡村 定矩, ROUSSEL-DUPRE Diane

      宇宙科学研究所報告. 特集23   29 - 37   1989年3月

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      記述言語:日本語   出版者・発行元:宇宙航空研究開発機構  

      1988年4月23日に『ぎんが』搭載のASMが, 銀河面から約3度離れたこぎつね座にX線新星を発見し, GS2000+25と名付けた。その後増光し, 最大強度は12クラブ(1&acd;6keV)に達した。光学観測から, パロマ-星図と比べて増光している二個の星が検出された。その後, その内の一個がX線新星の光学天体であることが光のスペクトルと電波の観測から分かった。X線のスペクトルからは, この新星がA0620-00に代表されるようないわゆるウルトラソフトX線新星であることが示された。GS2000+25とA0620-00との詳細な比較から, GS2000+25も有力なブラックホール侯補であることが分かった。

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    • DISCOVERY OF A BRIGHT X-RAY NOVA, GS-2000+25

      H TSUNEMI, S KITAMOTO, S OKAMURA, D ROUSSELDUPRE

      ASTROPHYSICAL JOURNAL337 ( 2 ) L81 - &   1989年2月

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      記述言語:英語   出版者・発行元:UNIV CHICAGO PRESS  

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    • AN X-RAY OUTBURST FROM 4U 0115+63 IN 1987 FEBRUARY MARCH

      H TSUNEMI, S KITAMOTO

      ASTROPHYSICAL JOURNAL334 ( 1 ) L21 - L23   1988年11月

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      記述言語:英語   出版者・発行元:UNIV CHICAGO PRESS  

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    • 4p-G-3 こぎつね座に出現した大変明るいX線新星の観測

      北本 俊二, 常深 博

      秋の分科会講演予稿集1988 ( 1 ) 89 - 89   1988年9月16日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

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    • 多層膜反射鏡の宇宙 X 線観測器への応用

      山下 広順, 常深 博, 北本 俊二, 廿日出 勇, 三宅 明, 上野 良弘

      宇宙科学研究所報告. 特集21   31 - 45   1988年3月

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      記述言語:日本語   出版者・発行元:宇宙航空研究開発機構  

      Development of multilayer reflectors makes it possible to apply to the grazing and normal incidence X-ray optic system for the cosmic X-ray observation in 0.1-10keV region. For the grazing incidence X-ray telescope, multilayer reflectors have an advantage to make larger the glancing angle and to extend the energy range up to 10keV in the fixed configuration. The normal incidence X-ray telescope is attainable in the energy range below 0.4keV, though the sensitive energy band is limited by Bragg condition estimated from the layer thickness and the number of layer pairs. Multilayers are also useful optical elements to fabricate the X-ray spectrometer and polarimeter. We are fabricating multilayer reflectors with electron beam evaporation method in ultra-high vacuum. Material combinations are Mo/C, Mo/Si and Ni/C with 5-20 layer pairs and the layer thickness of 31-100A. They are deposited on flat and figured substrates of float glass and superpolished glass with the surface roughness of 2-3A (rms). Multilayers thus fabricated are evaluated by measuring the reflectivity, the wavelength resolution and Bragg angle with three characteristic X-rays of Cu-Kα(1.54A), Si-Kα(7.13A) and C-Kα(44.7A). Further investigations are carried out with the monochromatized synchrotron radiation in 14-250A band. The peak reflectivity of Cu-Kα is obtained to be 80% for Mo/C in the grazing incidence and that of λ160A to be more than 30% for Mo/Si in near normal incidence.

      CiNii Article

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    • 26p-A-6 多層膜反射鏡のX線望遠鏡への応用

      山下 広順, 常深 博, 北本 俊二, 廿日 出勇, 上野 良弘

      秋の分科会講演予稿集1987 ( 2 ) 394 - 394   1987年9月16日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

      CiNii Article

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    • 30a-B-9 低バックグラウンドガス蛍光比例計算管の開発

      宮本 重徳, 木村 和宏, 斎藤 誠, 常深 博, 北本 俊二

      秋の分科会講演予稿集1987 ( 1 ) 61 - 61   1987年9月16日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

      CiNii Article

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    • 8p-E-7 白鳥産X1のDip中の星間ダストによる散乱成分

      北本 俊二

      秋の分科会講演予稿集1986 ( 1 ) 107 - 107   1986年9月12日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

      CiNii Article

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    • The Transient X-Ray Source 4U 1543-47 Observed from Tenma

      Kitamoto Shunji

      Publications of the Astronomical Society of Japan36 ( 4 ) p799 - 806   1985年1月

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      記述言語:英語   出版者・発行元:Astronomical Society of Japan  

      CiNii Article

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    • 1a-EE-3 宇宙X線源CygX-3の4.8時間周期変動

      北本 俊二, 宮本 重徳, 松井 渉, 天馬観測班

      秋の分科会講演予稿集1984 ( 1 ) 95 - 95   1984年9月10日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

      CiNii Article

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    • 4p-BA-10 「てんま」によるSNRのX線スペクトルの観測

      常深 博, 北本 俊二, 山下 広順, 宮本 重徳, てんま観測班

      年会講演予稿集39 ( 1 ) 138 - 138   1984年3月12日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

      CiNii Article

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    • 30a-A-3 高精度位置検出型比例計数管の開発

      北本 俊二

      年会講演予稿集37 ( 1 ) 81 - 81   1982年9月14日

      詳細を見る

      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

      CiNii Article

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    • 1p-SE-10 新しい読み出し方式による位置検出型比例計数管の製作

      北本 俊二, 常深 博, 村井 秀夫, 津野 克彦, 宮本 重徳, 山下 広順

      秋の分科会講演予稿集1981 ( 1 ) 102 - 102   1981年9月14日

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      記述言語:日本語   出版者・発行元:一般社団法人日本物理学会  

      CiNii Article

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    ▼全件表示

    書籍等出版物

    • 宇宙まるごとQ&A

      北本俊二, 原田知広, 亀田真吾( 担当: 共著)

      理工図書  2021年2月 

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    • 最新 宇宙学

      北本 俊二( 担当: 共著 ,  範囲: 第10章)

      裳華房  2004年1月1日 

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      記述言語:日本語 著書種別:その他

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    • 物理学実験―大阪大学理学部物理学科・物理学実験テキスト-

      ( 担当: その他)

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

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      記述言語:日本語 著書種別:その他

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    • 天体現象3Dシミュレーションソフト:太陽系大紀行

      ( 担当: その他)

      講談社  2003年4月 

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      記述言語:日本語 著書種別:その他

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    • X線天文学で学ぶ物理の世界

      北本 俊二( 担当: その他)

      メディア教育開発センター  2002年1月1日 

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      記述言語:日本語 著書種別:その他

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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

      ( 担当: その他)

      裳華房  1999年4月 

      詳細を見る

      記述言語:日本語 著書種別:その他

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    • X線でさぐるブラックホール

      ( 担当: その他)

      裳華房ポピュラーサイエンス  1998年4月 

      詳細を見る

      記述言語:日本語 著書種別:その他

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    • The Hot Universe

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

      Springer  1998年 

      詳細を見る

    ▼全件表示

    所属学協会

    • 1983年 - 現在 
      日本物理学会

      詳細を見る

    • 1983年 
      日本天文学会

      詳細を見る

    •  
      International Astronomical Union

      詳細を見る

    Works(作品等)

    • 回折限界X線望遠鏡の性能評価 その他

      2004年4月
      -
      2005年4月

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      作品分類:その他  

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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 その他

      2002年4月
      -
      2003年4月

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      作品分類:その他  

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    共同研究・競争的資金等の研究

    • 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 

      詳細を見る

      2001年4月 - 現在

      資金種別:競争的資金

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    • ブラックホール候補天体からのX線放射の半世紀にわたる長期変動の研究

      日本学術振興会  科学研究費助成事業 

      北本 俊二

      詳細を見る

      2022年4月 - 2025年3月

      課題番号:22K03678

      配分額:1170000円 ( 直接経費:900000円 、 間接経費:270000円 )

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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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      2013年4月 - 2015年3月

      資金種別:競争的資金

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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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      2010年4月 - 2012年3月

      資金種別:競争的資金

      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 

      詳細を見る

      2007年4月 - 2010年3月

      資金種別:競争的資金

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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 

      詳細を見る

      2007年4月 - 2009年3月

      資金種別:競争的資金

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    • 科学衛星観測データベースの宇宙科学教育への活用

      日本学術振興会  科学研究費助成事業 

      長瀬 文昭, 海老沢 研, 北本 俊二, 吉田 篤正, 松崎 恵一, 田村 隆幸, 矢治 健太郎, 宇野 伸一郎, 松下 恭子, 坪井 陽子, 平林 久, 辻本 匡弘, 馬場 彩, 村上 弘志, 久保田 あや, 飯塚 亮, 古田 豊, 林 壮一, 綾部 俊二, 吉田 清典, 野口 語, 川端 啓明, 宮脇 亮介, 沢田 紗衣子, 岩本 ひとみ, 吉田 鉄生, 馬場 亮輔, 菅原 泰晴, 戸塚 晃太, 朝岡 育子, 篠原 秀雄, 八木橋 伸佳, 鵜沢 明子, 楠 進吾

      詳細を見る

      2007年 - 2009年

      課題番号:19300270

      配分額:12480000円 ( 直接経費:9600000円 、 間接経費:2880000円 )

      科学衛星により主にX線領域で観測された宇宙・天体の高エネルギー現象に係る観測データベースを利用して、宇宙科学の学習教材を作成した。教材はX線天文学の特徴・発展の歴史・観測手段等を簡単に解説し、本教材の各章で取り扱う学習課題を概説した解説書と、星の誕生と終焉、中性子星・ブラックホールなどの特異天体、銀河団と暗黒物質などを学習課題として取り上げ、解析実習を誘導し結果を考察させるCD-ROM版の指導書で構成される。そのCDには解析実習用に集約されたデータおよび解析実習に必要なソフトウェアーを搭載しており、パソコンを保有している読者はこのCDを使って自立して学習が出来る。

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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 

      詳細を見る

      2005年4月 - 2007年3月

      資金種別:競争的資金

      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) 

      詳細を見る

      2004年4月 - 2007年3月

      資金種別:競争的資金

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    • 輻射輸送を考慮した衝突輻射モデルによる星のX線放射機構の解明

      日本学術振興会  科学研究費助成事業 

      山本 則正, 幸村 孝由, 北本 俊二, 柴崎 徳明

      詳細を見る

      2004年 - 2006年

      課題番号:16540221

      配分額:3100000円 ( 直接経費:3100000円 )

      本研究課題は、1978年の発見以来長年謎であった星からのX線放射機構を解明することである。既存のX線天文衛星で観測した星のエネルギースペクトルに対し、我々が構築した輻射輸送まで考慮したプラズマの衝突輻射モデルを適用し、星からのX線放射機構を解明するというアプローチで研究を遂行した。
      我々の研究成果として、次の4つが挙げられる。
      (1)実験室プラズマから得たサテライト線を含むエネルギースペクトルに対し、我々が構築した輻射輸送まで考慮したプラズマの衝突輻射モデルを適用することで、より高精度な各元素のヘリウム様イオンの衝突輻射モデル開発を行った。ただし、輻射輸送などの効果の取り入れは、モンテカルロ法でのトイモデルの段階であり、今後天体プラズマヘの適用には更に改良をする必要がある。
      (2)実験室プラズマの適応を行い、鉄イオンの衝突輻射モデルの開発を行った。具体的には、我々が構築した衝突輻射モデルと、核融合科学研究所の大型ヘリカル装置で得られら高温プラズマのエネルギースペクトルなどとを比較し、モデルの高精度化を行った。
      (3)X線天文衛星で観測した星のエネルギースペクトルの輝線の解析のため、星風のドップラーモデルを開発した。このドップラーモデルは、星風中で放射されたX線が、星風自身によって吸収されるというモデルである。
      (4)米国のChandra衛星、欧州のXMM-Newton衛星によるX線の輝線に対し、星風のドップラーモデルを適用させ、早期型星からのX線放射領域を決定した。今後は、2005年に打ち上げられた日本のX線天文衛星「すざく」で観測する早期型星などの解析も進める予定である。
      上記の成果に加えて、今後の計画として、天体プラズマのX線スペクトル解析をさらに進める必要がある。またトイモデル段階である輻射輸送モデルを発展させ、プラズマの運動の効果を取り入れるなどして、非平衡プラズマにも適用可能なプラズマの輻射輸送モデルの開発を行っていく。また天体プラズマ・太陽プラズマの輝線の解析を進めていく予定である。

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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 

      詳細を見る

      2004年4月 - 2005年3月

      資金種別:競争的資金

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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 

      詳細を見る

      2003年4月 - 2005年3月

      資金種別:競争的資金

      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) 

      詳細を見る

      2003年4月 - 2004年3月

      資金種別:競争的資金

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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 

      詳細を見る

      2002年4月 - 2004年3月

      資金種別:競争的資金

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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 

      詳細を見る

      1998年4月 - 2002年3月

      資金種別:競争的資金

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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 

      詳細を見る

      1996年4月 - 2001年3月

      資金種別:競争的資金

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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 

      詳細を見る

      1997年4月 - 1999年3月

      資金種別:競争的資金

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    • 「あすか」衛星によるX線天文学の観測的研究

      日本学術振興会  科学研究費助成事業 

      長瀬 文昭, 田中 靖郎, 石田 学, 高橋 忠幸, 満田 和久, 井上 一, 宇野 伸一郎, HOLT S., 伊藤 真之, SERLEMITSOS P., 松岡 勝, 北本 俊二, WHITE N.E., 林田 清, MADJSKI G., 田原 譲, CANIZARES C., 大橋 隆哉, MUSHOTZKY R., 紀伊 恒男, PETER R., 国枝 秀世, 山内 茂雄, 堂谷 忠靖, 村上 敏夫, 常深 博, 牧島 一夫, 小山 勝二, 山下 広順, 三原 建弘, 小川原 嘉明, 吉田 篤正, 槙野 文命, HUGHES J., 宮田 恵美, 鶴 剛, 粟木 久光, 石崎 欣尚, 藤本 龍一, 上田 佳宏, 根来 均, 田代 信, 河合 誠之, RICKER G., HELFAND D., MCCAMMON D.

      詳細を見る

      1996年 - 1998年

      課題番号:08044103

      配分額:9100000円 ( 直接経費:9100000円 )

      「あすか」は、日米共同で製作されたX線天文衛星であり、1993年2月に打ち上げられた。そして、その後の観測運用も両国の緊密な協力によって遂行されている。これまで衛星は順調に運用され、装置は正常に稼し、所期の性能を発揮しており、試験観測・公募観測とも順調に行われてきた。本研究の目的はこの衛星の観測・運営を日米協力の下で行い、中性子星やブラックホールを含むX線連星や、超新星残骸、活動的銀河核、銀河団等からのX線放射、宇宙X線背景放射等の研究を行うことであった。この目的に沿って研究を進め次の各項目に述べる成果を挙げた。
      (1) 専門科学者グループの会合を定期的に開催し、観測計画の評価・ターゲットの選択、衛星の運用、適切な検出器較正等の衛星観測運営上の基本方針について討議をおこなった。
      (2) X線望遠鏡および各測定装置の精密な較正を行うとともに、各検出器の諸特性・応答関数の時間変化を明らかにし、すべての観測に対し正確な解析を可能とした。
      (3) データ解析ソフトウエアーの改良・拡充、科学データの編集、管理を両国研究者が協力し且つ継続的におこなった。
      (4) 観測から得られたデータを共同で解析、討議を行って、その科学的成果をまとめた。さらにこれらの得られた成果を各種国際学会・研究集会において発表し、また学術専門誌に公表した。
      (5) 観測者の占有期間を過ぎたデータを統一的に編集・管理し、またその観測記録を整備して、これらの観測記録、アーカイブデータを広く公開し、世界中の研究者の使用の便に供した。
      特に、「あすか」によるX線観測では、その高感度、高帯域、高分光撮像特性により、宇宙論研究に重大な寄与をするX線背景放射の解明、遠方のクエーサーや原始銀河からのX線放射の発見、銀河団の進化および暗黒物質の解明、活動銀河核、ブラックホール天体、ジェット天体、強磁場中性子星等の特異天体の解明、激変星、高温白色わい星、超新星残骸等における高温プラズマ状態の研究等において重要な成果を得ることが出来た。これら「あすか」の成果は国際的にも高く評価されている。以上、本研究課題に対する科学研究費補助金により、国際協力の下での「あすか」衛星の観測・運営が円滑に行われ、また十分な科学的成果を挙げることが出来た。

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    • 位置,エネルギー,時間分解能を持つ直接X線撮像型CCDを使ったX線偏光計の開発

      日本学術振興会  科学研究費助成事業 

      常深 博, 山本 晃永, 林田 清, 北本 俊二

      詳細を見る

      1995年 - 1996年

      課題番号:07554002

      配分額:21100000円 ( 直接経費:21100000円 )

      本研究の目標は、X線CCDの基本性能の向上とともに、X線偏光検出能力の向上にあった。研究は、大学側のメンバーと浜松ホトニクス社のメンバーの共同でなされた。双方の協議によりCCD素子の仕様を決定した上で、実際の素子製作は浜松ホトニクス社の施設において行い、大学側ではCCD素子の動作、評価試験を担当した。
      1年目は、2年目を通じて数種類のCCD素子が素材、製作方法を変えて製作された。ピクセルサイズ12ミクロン、画素数512x512のCCD素子に関しては、5.9keVのX線に対する分解能140eVを得るにいたった。1年目の終わりに160eVであったのがここまで向上したのには暗電流を1/50に抑えられたことが利いている。また、高抵抗の素子を使用した素子で、空乏層厚が20ミクロンに達したことも確認した。
      大学側ではCCDの動作方法、評価方法の改良を行った。具体的には、1) 0.4keV-2.2keVの連続分散光を利用した検出効率測定システム,2)スプリアス電荷によるノイズを抑えるためのCCDドライブ方法、3) DSPを利用した高速データ取得システム、4) CCD内部でのX線吸収、電荷収集過程のシュミレーションコードがある。また、全く新たな測定方法としてCCDの前面にCCDのピクセルサイズとほぼ同じピッチのメッシュをおいて測定することで、サブピクセルの構造による検出効率の違いを測定できる方法を考察し、実際に実験で実証した。さらに、実験室内のX線発生装置からの連続X線の偏光度を測定し、管電圧を調整することで50%程度の偏光度のX線が容易に得られることを示した。偏光検出に有利なピクセルサイズ6ミクロンのCCD素子の製作も開始されたが、実際にX線偏光検出能力の測定にはいたらなかった。平成9年度に実験を引き続き行う予定である。

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    • 早期型星のX線放射機構の研究

      日本学術振興会  科学研究費助成事業 

      北本 俊二

      詳細を見る

      1995年 - 1995年

      課題番号:07222208

      配分額:1700000円 ( 直接経費:1700000円 )

      X線天文衛生「あすか」で4個のO型星ζ-Ori, δ-Ori, λ-Ori, ζ-PupからのX線を観測した。そして、各々の星から、高階電離したマグネシウムや珪素からの輝線を発見した。これより、O型星からのX線は熱的な起源をもつことを明らかにした。この結果を根拠にX線が光学的に薄い高温プラズマからの放射であると仮定して、X線放射のモデルと輝線の強度から、酸素、ネオン、マグネシウム、珪素、硫黄、鉄の組成比を見積もることに成功した。その結果、それらの元素組成比は、硫黄を除いて、いわゆる宇宙組成の約1/3以下で、とくに、鉄に関しては約1/10以下である事がわかった。これら、重元素の相対組成比は大質量星の爆発であるII型超新星で作られる元素組成比とたいへん良く似ている。このことから、O型星はII型超新星によって汚染されたガスから作られた事が示唆される。
      また、O型星の元素組成比がいわゆる宇宙組成比より重元素が少ないということは、次のような大問題を含んでいる。O型星のような早期型星はその年齢がせいぜい1千万年であるから、O型星を形成する元となったガスは、1千万年前のわれわれの銀河系内にあったガスである。O型星のような早期型星の表面のガスはほぼ星が形成された時のガスのままであるか、または、星内部の核融合反応によって生成された重元素によりさらに汚染されているはずである。X線は星風か、表面のコロナから放射されているはずであるから、X線で決めた重元素比は、星表面物質の重元素比を表わしている。すなわち、我々の結果は、1千年前の我々銀河系のガスがいわゆる宇宙組成比よりもはるかに少ない重元素しか含まなかった事を示唆している。

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    • 白鳥座X-3のX線発生機構の研究

      日本学術振興会  科学研究費助成事業 

      北本 俊二

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      1994年 - 1994年

      課題番号:06233214

      配分額:1600000円 ( 直接経費:1600000円 )

      研究目標は、白鳥座X-3のまわりで繰り広げられているたいへん強いX線と濃いガスの相互作用を解明するために、白鳥座X-3のまわりではどのような電離状態が達成されているか明らかにすることである。研究成果は以下のとうりである。「あすか」により白鳥座X-3の観測を行いそのエネルギースペクトルにはMg,Si,S,Ar,Ca,Feの輝線が大変強いことを発見した。これは、まさにX線とガスとの相互作用の結果と考えられる。さらに、鉄輝線は3本の輝線(H状イオン、He状イオン、ほぼ中性のイオンからの輝線)に分解することが出来た。また、H状及びHe状イオンからの輝線は公転周期に従ってその強度も等価幅も変動しており、しかもそれは、連続成分の変動とはまったく違った変動を示している。これは、輝線の放射機構と連続成分の放射機構が違っていることを意味する。また、「あすか」によりX線強度が少し違う状態で2度目の観測を行った。両者を比べることにより、少なくとも鉄輝線に関しては明らかな違いがあり、特に強度が弱くなると電離状態が低いと思われるイオンからの輝線が強くなっていることが明らかになった。これより、イオンの電離状態はX線の強度に強く依存することがわかった。公転周期の解析により、周りのガスの密度が推定することができ、X線の強度とガスの密度から、電離状態等を計算することができ、ほぼ観測とあうことを確認した。

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    • 科学衛星Astro-DによるX線天文学の観測的研究

      日本学術振興会  科学研究費助成事業 

      長瀬 文昭, 田中 靖郎, 堂谷 忠靖, 石田 学, 紀伊 恒男, 伊藤 真之, 松岡 勝, 柴崎 徳明, 大橋 隆哉, 国枝 秀世, 田原 譲, 北本 俊二, 三原 建弘, 田中 靖郎, CANIZARES C., RICKER G., 鶴 剛, 粟木 久光, 河合 誠之, 吉田 篤正, SERLEMITSOS アール, 林田 清, BREON S., 海老沢 研, VOLZ S.V., KELLEY R., HELFAND D., MCCAMMON D., 常深 博, 牧島 一夫, 満田 和久, 村上 敏明, 小山 勝二, 山下 広順, 小川原 嘉明, 宮本 重徳, MUSHOTZKY R., 槇野 文命, HOLT S., 井上 一, SERLEMITSOS R., 川口 淳一郎, 中川 道夫, 藤本 光昭, 長瀬 文昭, 松尾 弘毅, 上杉 邦憲, WANG B., FEIGELSON E., GRAFFAGNINO V., REYNOLDS C., 羽部 朝男, GEHRELS N., FABBIANO G., SERLEMITSOS, RICKER G, 山内 茂雄, 池辺 靖

      詳細を見る

      1992年 - 1994年

      課題番号:04044167

      配分額:11600000円 ( 直接経費:11600000円 )

      「あすか」(Astro-D)は、1993年2月に打ち上げれられ、わが国4番目のX線天文衛星となった。この衛星は0.5-10keVの広いエネルギー帯をカバーし、史上最高の感度でX線天体の撮影を行うと共に、世界で初めてX線CCDによる精密X線分光を行う高性能X線天文台である。「あすか」の性能はX線天文学を飛躍的に進めるものと国際的に注目されている、X線天体は極めて多岐に亘り、殆どあらゆる種類の天体がX線天文学の対象となっている。特に銀河系では中性子星やブラックホールのX線連星、超新星残骸等、銀河外では、銀河団、クェーサー等の活動銀河中心核、更に遠方からのX線背景放射が重要課題である。
      この衛星に搭載されている観測装置は日米共同で製作された。打ち上げ前には、装置の設計・製作・試験・較正・調整を、打ち上げ直後には装置の較正・調整を共同で行ってきた。さらに、定常観測に入ってからは、装置の性能の正確な把握や正しいデータ解析のツールの提供等でも共同で作業を行うとともに、その成果を最大限に挙げるために、観測計画の打ち合わせ、ソフトウエア開発、観測結果の処理、解析等の各過程で両国の研究者が協力して作業を行ってきた。これらの作業のための日米研究者の移動は、主に、本科学研究費によって行われた。これら日米協力に基づく「あすか」がもたらしたいくつかの成果を以下にまとめる。
      ・「あすか」が打ち上がって40日もたたないうちに近傍銀河M81に発生したSN1993Jからは、ドイツのX線天文衛星ROSATとほぼ同時にX線を検出した。発生して1週間ほどの超新星からX線を検出したのは今回がはじめてである。
      ・超新星の爆発で飛び散った物質が星間物質と衝突して光っている超新星残骸について、「あすか」のすぐれた分光特性による新しい学問的展開がひらかれている。
      ・ガンマ線バーストと呼ばれる特異な現象の発生源をはじめて既知の天体との同定に成功し、この現象の原因の解明に大きな貢献をした。
      ・われわれの銀河系の中心部や円盤部を満たす高温ガスからのX線の分光的研究が進み、従来の予想では理解し難い事実があきらかになりつつある。
      ・楕円銀河、銀河群、銀河団といった宇宙の大きな構造物をとりまく高温ガスの分光学的研究が進み、これらのガス中の重元素量が一貫して少ないという、新しい考え方の導入を迫る事実があきらかになってきた。また、これらの構造物を構成する暗黒物質の分布や量についても新しい知見が得られつつある。
      ・遠方の銀河団をつかった宇宙の大きさを決める研究も、「あすか」の広い波長範囲の分光を行える能力をつかって、着々と成果をあげつつある。
      ・活動銀河の中心にある大質量ブラックホールのごく近傍からのものとおもわれる鉄の輝線構造をはじめて発見し、ブラックホール近傍での物質流につき貴重な情報をもたらしている。この中心核を取り巻く比較的遠方の物質や分布の物理状態についても「あすか」のすぐれた分光性能により新しい事実が次々と明らかになってきている。
      ・宇宙X線背景放射の研究も、「あすか」の波長範囲の広さを利用して、宇宙のはて近い遠方の宇宙初期の原始天体を探る研究がはじまりつつある。
      以上のように、本科学研究費補助金の援助のもと、「あすか」を用いた日米の研究者による共同研究は大きな成果をあげている。

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    • X線ラインスペクトルを用いたX線天体におけるX線放射過程の研究

      日本学術振興会  科学研究費助成事業 

      宮本 重徳, 林田 清, 北本 俊二

      詳細を見る

      1993年 - 1993年

      課題番号:05242214

      配分額:2500000円 ( 直接経費:2500000円 )

      ブラックホール候補星GS1124-683と中性子星X線星GX5-1からのX線のエネルギースペクトルと時間変動の関係を研究した。GS1124-683のHigh Stateに於けるX線は、巾関数型のパワースペクトルの時間変動を持つ降着円盤からの成分と、ローレンツ関数型のパワースペクトルの時間変動を示す高エネルギー成分から構成されていることが解った。大雑把には、それぞれの成分は独自の大きさを持ち、観測されるX線は二つの成分の独立な和として解釈出来るが、高エネルギー成分の割合が多くなると降着円盤成分の時間変動は大きくなる傾向がある。Low Stateでは、X線はHigh State時に比べて大きな時間変動を示す巾関数型のエネルギースペクトルを持つ。二つの状態で、クロススペクトルから求めたエネルギーバンド間の時間の遅れの様子も違う。GX5-1からのX線もGS1124-683のHigh Stateと同様に、巾関数型で大きさもGS1124-683とほぼ同じパワースペクトルの時間変動を持つ降着円盤からの成分と、ローレンツ関数型のパワースペクトルの時間変動を示す高エネルギー成分(おそらく中性子星表面からの成分)から構成されていることが解った。
      「あすか」により白鳥座X-3の観測を行い輝線スペクトルについて、かつて無い精度でその振舞いを調べた。鉄輝線は3本の輝線(H状イオン、He状イオン、ほぼ中性のイオンからの輝線)に分解することが出来た。また、H状及びHe状イオンからの輝線は公転周期に従ってその強度も等価幅も変動しており、しかもそれは、連続成分の変動とはまったく違った変動を示している。これは、輝線の放射機構と連続成分の放射機構が違っていることを意味する。

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    • 高エネルギー・トランジェント天体観測実験

      日本学術振興会  科学研究費助成事業 

      松岡 勝, 廿日出 勇, 高岸 邦夫, 北本 俊二, 常深 博, 河野 毅, 今井 喬, 山内 誠, 吉田 篤正, 河合 誠之, FENIMORE Edw, RICKER Georg, EDWORD E.Fen, GEORGE R.Ric

      詳細を見る

      1991年 - 1993年

      課題番号:03044162

      配分額:6000000円 ( 直接経費:6000000円 )

      高エネルギー・トランジェント天体の研究のため日・米・仏・伊の国際共同研究を行ってきた。このため共同で小型の衛星を製作しX線,紫外線,ガンマ線で同時にトランジェント天体を観測する。日本の担当はX線観測装置を製作することであるが,紫外線観測装置(米国),ガンマ線観測装置(フランス)及び衛星全体のシステムと調整するため,米国で4回,日本で2回の会合をもった。会議の目的と成果は大きく分けて次の3つである。
      (1)高エネルギー・トランジェント天体の研究の現状の把握と共同研究で開発している衛星に反影させる。
      高エネルギー・トランジェント天体として最重要なものはガンマ線バーストである。このガンマ線バーストの空間分布,エネルギースペクトルを調整しこれからの衛星計画の観測精度,感度,ソフトウェア開発について討議した。この結果を現在進行中の共同開発の衛星に反影させた。
      (2)共同開発中の衛星に関するソフトウェアについて討議する。
      ソフトウェアは,衛星に搭載するソフトウェアとデータ受信した後に処理するソフトウェアである。これらを科学的成果が最大に引き出せるアルゴリズムを討議した。
      (3)各国が担当した衛星搭載装置のインターフェースを確認するための試験を行う。
      日・米・仏の各国が開発した衛星搭載装置を米国に持ちより,機械的及び電気的なインターフェース試験を行った。図面上で製作した装置は大きな間違いなく合わせることができた。
      本研究費の補助のためスムーズにすすめられたハードウェアの研究成果を以下に記す。
      (1)搭載用の回路の製作後,パルサーを使った試験を行い,16系統の信号処理回路について詳細なデータを取得した。更に,回路の温度試験は衛星環境の条件に從い遂行した。
      (2)搭載する位置検知型X線検出器の製作を行い,予備器も含め試験用X線ビームを使って詳細な試験を行った。この試験は搭載用の回路をとおし行った。この結果エネルギー分解能,位置分解能ともに初期の目的を達成できた。ただし,検出器の信頼性については引き続き試験し,スペア検出器の用意をすることとした。
      (3) HETE衛星のための日本側担当機器,X線観測装置の搭載機器を米国に持ち込み衛星全体の組み上げ試験を行った。電気的、機械的なインターフェースは若干の手直しを除き無事終えることができた。インターフェースのチェックは日・米・仏の協力で行った。
      (4)上記のような搭載機器の個々の試験は平成4年12月までにほぼ終え平成5年1-3月まではX線観測装置全体を組み上げ1気圧中での熱サイクル試験,振動・衝撃試験,熱真空試験を行っている。若干の手直しを行って3月末には完成する予定である。
      (5)宮崎大学での衛星データ受信のための基礎工事を行った。また,米国とのインターネットワークの試験を行っている。
      (6)トランジェント天体に関する国内外の権威者によるワークショップを米国とわが国で行った。ガンマ線バーストの起源の謎は深まるばかりである。一方国内の共同研究者とは,本研究に関連したシンポジウムを開催してガンマ線バーストの現状の把握とガンマ線バースト発生のモデルを討議した。シンポジウムは,(1)ガンマ線バーストの観測と理論,(2)軟ガンマ線バースト源の「あすか」衛星による観測結果,(3)ガンマ線バーストの空間分布の宇宙論的意義,(4)ガンマ線バーストのモデル,(5)暗黒物質とガンマ線バースト将来計画,などについて討議し,本研究計画に有効に反影させることができた。

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    • 気球による活動銀河核等からの硬X線・ガンマ線の調査研究

      日本学術振興会  科学研究費助成事業 

      釜江 常好, BRAGA J., DUROUCHOUX P, MICHAELSON P, SADOULET B., EDBERG T., CORREA R., WEISKOPF M., 高橋 義幸, 能町 正治, 池田 博一, 太田 茂雄, 秋山 弘光, 山上 隆正, 矢島 信之, 高橋 忠幸, E Santos, C Abrahao, R Correa, J Braga, J Grunsfeld, V Kirchhoff, M Weisskopf, P Michaelson, 北本 俊二, 中川 道夫, 河合 誠之, 藤本 真克, 村上 敏夫, CORREA Ricar, 柳田 昭平, 常深 博, 藤井 正美

      詳細を見る

      1991年 - 1993年

      課題番号:03041022

      配分額:30000000円 ( 直接経費:30000000円 )

      本研究はハップル望遠鏡、GRO,Astro-Dなどでの研究の進展にも対応しつつ、北天(アメリカ)・南天(ブラジル)でAGNや銀河中心SN1987A等の天体を随時観測することで銀河の誕生のメカニズム、超新星とその残骸について研究を進めるのが目的である。平成3、4年度に取得したデータを解析した結果、検出器の改良、方向制御の改良を行うことにより、気球実験でもアメリカのGRO衛星を上回る結果を得ることができるという確信を持った。そのために平成5年度はデータの解析を続けると共に、検出器の改良および、気球を用いた高度40Kmでの試験実験を国内で行った。カニ星雲は、1054年に観測された超新星爆発の残骸である。その中にあるカニパルサーは1968年に発見され、33msという高度で自転する中性子星であることが知られている。以来、ラジオ波から高エネルギーγ線にいたるまで幅広いエネルギーの領域での観測が精力的に行われてきたがその放射メカニズムの解明にはいたっていない。パルス波形は、どのエネルギー領域でも同じ位相の似通った二つ山を示す。しかし、その二つ山の中間の領域における輻射-以後、インターパルスと呼ぶ-は、硬X線/γ線領域でのみ強くなることが知られている。
      われわれは、この硬X線/γ線領域でのインターパルスに注目し、カニパルサーの観測実験を行った。また、われわれの検出器は高感度であるため、他の様々な検出器での観測で報告されているラインについて、そして、短期時間変動について、新たな知見が得られるものと期待された。
      気球実験は三陸大気球観測所でおこなった。われわれは、1989年から1991年の間、ブラジルで、硬X線/γ線領域の天体観測をWelcome-1(mk1)検出器を用いて行ってきた。今回、日本で放球するにあたり、大幅な改良、変更を行い、Welcome-1(mk2)検出器を開発した。この実験には日本で気球実験を行う手法の確率、そして、次期衛星搭載予定のWelcome-2の開発のための基礎データの取得という目的もあった。
      場所の移動により、近いという多大な恩恵を受けたが、重量制限、観測時間の減少、海上回収というデメリットもあった。重量制限のために、検出器の面積は減らさざるをえなかった。そこで、われわれは、低バックグランド化により高感度化させることを試み、短時間観測でも有意な結果をえようとした。また、海上回収のために新たに防水カバーを開発した。低バックグランド化の改良の一つとして、開口角からのバックグランドの混入を減らすべく、検出器の視野を以前の1/4にした。そのため、高安定度の達成が期待出来る。リアクションホイールとよじれ戻しモーターを用いた方位制御方式を採用し、容易に機能の変更ができる柔軟な姿勢制御システムを構築した。
      われわれが取得したデータは、日本のぎんが衛星やアメリカのGRO衛星の中間のエネルギー範囲のデータであり、互いに相補的な役割を果たす。本年度は研究者を派遣し、平成4年度に行った解析を更に発展させるために、アメリカやヨーロッパの研究者と協力してGRO衛星や他の気球実験のデータの解析を行うと共に将来の共同観測に向けて、具体的な協議を行った。
      特に、U.C.Berkeley校で、同様の実験を行っている、Tin Edberg博士を招聘し、三陸での実験を最初から最後まで協力して行った。これはU.C.のグループにとって、今後のアメリカでの実験を行う際に非常に大きなknowhowとなる。

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    • 0次光を除いた透過型グレーティングの基礎研究

      日本学術振興会  科学研究費助成事業 

      北本 俊二

      詳細を見る

      1991年 - 1992年

      課題番号:03804009

      配分額:1600000円 ( 直接経費:1600000円 )

      X線領域で使う分光素子として結晶や回折格子を使った分光器はこれまでも使われてきた。結晶を使ったものは一般に分解能は良いが広い波長バンドを分光するには効率が悪い。また,反射型回折格子は,数keV以上のエネルギー領域で使うためには,分散角が小さいにもかかわらず,たいへん斜入射光学系で使用する必要があり,0次光による悪影響がどうしても出てしまうことや,大きなものを作成するのが困難であるという問題がある。そこで数keVあたりのX線を分光するためには透過型の回折格子が有望となる。ところが,X線領域で使う透過型回折格子の場合,反射型で使われるブレーズ角の考えが導入できないために,分光された光である1次光への効率が悪いという欠点がある。
      そこで,この研究の於て,1回反射を使った透過型の回折格子を考案した。そうすることによって,あたかもブレーズ角を持った透過型回折格子が可能である。この考えを元に計算機による数値実験を行なった。そして,試作した新しい回折格子と,マイクロチャンネルプレートを回折格子として使用して,それ等を可視光を使って実験的に評価した。その結果新しい考えを導入した透過型回折格子は,0次光を小さく1次光を強くすることが可能であることを確かめた。この考えを基に新しいタイプのX線用透過型回折格子を作成すれば,宇宙X線観測用としてたいへん有望な装置を開発できる。

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    • 科学衛星「ぎんが」によるX線天文学日英協同研究

      日本学術振興会  科学研究費助成事業 

      田中 靖郎, 田原 譲, 国枝 秀世, 伊藤 真之, 堂谷 忠靖, 満田 和久, 紀伊 恒男, 常深 博, 柴崎 徳明, 牧島 一夫, 村上 敏夫, 井上 一, 長瀬 文昭, 松岡 勝, 小山 勝二, 山下 広順, 小川原 嘉明, 宮本 重徳, 槙野 文命, MUKAI K., FABIAN A., PATCHET B., MASON K.O., TENNANT A., 北本 俊二, 林田 清, CRUISE M., WILLIAMS R., STEWART G.S., WARWICK R.S., WATSON M.G., COOKE B.A., 河合 誠之, 吉田 篤正, POUNDS K.A., TURNER M.J.L, MCHARDY I., 大橋 隆哉

      詳細を見る

      1989年 - 1991年

      課題番号:01044145

      配分額:10800000円 ( 直接経費:10800000円 )

      本研究では、わが国の科学衛星「ぎんが」を用い、3年間にわたって日英共同によるX線天文学の研究を行なってきた。これは「ぎんが」の主観測装置である大面積比例計数管(LAC)が、英国(主としてレスタ-大学)と日本の緊密な国際協力により実現した装置であるという経緯に基づいている。この間、「ぎんが」は大きな故障なしに観測を続け、予想をはるかに上回る多くの成果を挙げたが、次第に軌道高度を下げ、惜しくも1991年11月1日頃に大気圏に再突入し4年9か月のミッションライフを閉じた。以下ではこの間の研究実績を、総論と各論に分けて述べる。
      【総論】
      日英科学者は本研究を通じて頻繁に往来し、緊密に協力しつつ、衛星の運用、搭載装置の較正やメンテナンス、観測計画の立案、デ-タの配分や管理などにあたってきた。また実際に「ぎんが」を用いて多くの共同観測を行ない、共同でデ-タを解析し、多くの共著論文を仕上げてきた。
      これらの共同研究は、日英双方がこれまで独自に蓄積してきた技術や経験を交換する、貴重な機会を与えてくれることになった。さらに、同じ観測デ-タを日英それぞれで解析し結果を詳しくつき合わせることにより、研究成果の信頼性を大きく高めることができ、ひいては「ぎんが」の学術的意義を広くかつ深くする上で、資するところが極めて大であった。得られた主要な学術的成果は、各論の部分で述べる。
      幸い「ぎんが」は、世界のX線天文学の最前線を大きく推し進めるプロジェクトとして、高い国際的評価を獲得した。その一因として、「ぎんが」が多くの外国人研究者の利用に供されてきたことが挙げられるが、そのさい本研究が呼び水として重要な役割を果たしたことも忘れてはならないであろう。
      以上をまとめると、本研究により日英双方のこの研究分野に、大きなメリットがもたらされた。さらに本研究にもとづく国際協力により、国際的な学術研究に対し大きな貢献が成し遂げられた。
      【学術的成果の各論】
      (1)宇宙X線背景放射:宇宙X線背景放射は、X線天文学の最大の謎の一つであり、宇宙の進化の鍵を握っていると考えられている。本研究では、宇宙の遠方におけるX線天体の数密度を巧妙な方法で求め、宇宙X線背景放射に対するそれらの寄与を推定した。また2keV以上のエネルギ-範囲で多くのクェ-サ-のX線スペクトルを初めて測定し、宇宙X線背景放射のスペクトルとは明確に異なることを示した。この結果、クェ-サ-など既知の天体の重ね合わせだけで宇宙X線背景放射を説明することは難しく、未知の宇宙初原天体が存在する可能性が残った。
      (2)活動銀河核の性質:クェ-サ-、セイファ-ト銀河などの活動銀河は、中心核に極めて激しい活動をもつ。本研究では多くのクェ-サ-を観測し、X線スペクトルの変動、スペクトルと電波強度の関係などを調べた。観測結果の多くは、シンクロトロン放射機構あるいはシンクロトロン自己コプトン機構により説明でき、活動銀河核が巨大ブラックホ-ルであるという考えを支持している。2個のクェ-サ-からは初めて鉄輝線が検出され、また多くのセイファ-ト銀河では中心核を濃い物質が取り巻いていることが発見された。このように活動銀河核の環境についても多くの情報が得られた。
      (3)銀河系内のX線天体の観測:X線パルサ-やX線バ-スタ-など、中性子星を含むX線天体について、多くの共同観測が行なわれた。X線パルサ-から非周期的な変動を発見したのは、その成果の一例である。X線を放射する白色わい星については特に緊密な日英共同研究が行なわれた結果、X線放射機構やその自転変調の仕組みが明らかになり、この研究分野に大きな進展をつけ加えた。いくつかの星のコロナの観測も日英共同で行なわれ、極めて温度の高い成分があること、鉄輝線が理論値より弱い場合があること、などが分かった。

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    • X線連星の長時間変動の研究

      日本学術振興会  科学研究費助成事業 

      宮本 重徳, 北本 俊二, 常深 博

      詳細を見る

      1988年 - 1989年

      課題番号:63540197

      配分額:1100000円 ( 直接経費:1100000円 )

      『ぎんが』衛星に搭載したオ-ルスカイモニタ-(ASM)及び大面積比例計数管(I.A.C)の観測によりX線連星の時間変動を研究した。ASMによりいわゆるX線新星を13例以上発見し、その内GS2000+25及びGS2023+338はブラックホ-ル候補と考えられるものである。又、Cyg X-1及びGX339-4をI.A.Cにより観測しその時間変動を調べた。
      GS2000+25は、1988年5月26日に発見した。その出現と消滅にいたるX線強度変化は、ブラックホ-ル候補天体のA0620-00に酷似している。
      GS2023+338は、1989年5月21日に発見した。この天体は、5月21日から6月1日迄は、秒から日のオ-ダ-の時間スケ-ルで、強度がファクタ-500にも増減する激しい時間変動を示した。その後は、Cyg X-1のlow stateに於ける様な短時間変動が残り、激しい長時間変動は影を潜めた。この比較的静かな時期のパワ-密度スペクトル、時間変化の遅れの構造は、Cyg X-1に良く似ていることを見いだした。
      Cyg x-1のI.ACによる観測デ-タを詳しく調べることにより、時間変動の遅れはCompton散乱モデルでは説明できないことを見いだした。又、位相遅れ対フ-リエ周期相関図で2つ山構造があることを見付けた。これと観測されたパワ-密度スペクトルとを併せ検討することにより、Cyg X-1の時間変動に約0.7秒と0.2秒の2つの特性時間が存在することを見つけた。これらの位相遅れの構造は、1983年の『てんま』衛星による観測の時でもほぼ同じである。
      GX339-4でvery high stateが存在することをASMの観測より見つけた。このstateでは、X線の時間遅れ-フ-リエ周期の構造が、約210^9cmコンプトン散乱雲によるとして説明可能である事が分かった。このことは、Cyg X-1のlow stateとは全く異なっており、very high stateでは、Jetが存在しているというモデルを検討している。

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    • 多層膜分光素子による宇宙X線観測用高効率分光器の開発研究

      日本学術振興会  科学研究費助成事業 

      北本 俊二, 高木 伸, 山下 廣順

      詳細を見る

      1987年 - 1988年

      課題番号:62540190

      配分額:1700000円 ( 直接経費:1700000円 )

      高効率X線分光器を開発するにあたり、広いエネルギー帯にわたって高い反射率を示す多層膜を使用することは有望である。しかしながら、高分解能を兼ね備えた高効率の分光器を開発するためには、工夫が必要である。そこで、我々は、エタロンを使用した新しい型の分光器を考案した。規則的に積層した多層膜の間にスペーサーを入れることによりエタロンを作成することができる。また、そのスペーサーの厚さをコントロールすることによりエタロンの反射特性をある程度自由に変えることができる。適当なエタロンの組合せにより、X線のエネルギースペクトルのフーリエ変換した形の信号を取得することができる。こうして取得したデータを逆フーリエ変換することにより元のエネルギースペクトルを再現できる。このことは、計算機シミュレーションによっても確かめた。次に、実際にエタロンを作成するための基礎的なデータを得るために、いろいろな層の厚さのNi/Cの多層膜を作成し、特性X線、及び、シンクロトロン放射光を使用して、反射率を測定した。その結果、層の厚さ(2d)が、100〓以下では、高い反射率の多層膜を作成することは難しく、その原因は、層の粗さ(rms)が、およそ10〓であると考えて良いことを示した。そのデータを基にして、実際にNi/Cのエタロンを作成し、特性X線、及び、シンクロトロン放射光で、反射率を測定した。その結果、ほぼ設計通りのエタロンが作成できていることを確認した。また、エタロンで反射させたX線を検出するための位置検出型比例計数管を作成し、その性能評価を行った。その結果、ほぼ20cmにわたって、5_09keVの特性X線で、約2mmの位置分解能と、約18%以下のエネルギー分解能が達成されていることを確かめた。この作成したエタロンと位置検出型比例計数管を組み合わせることにより、高効率X線用分光器が作成可能である。

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    • 科学衛星Astro-C(ぎんが)による日英共同X線観測調査

      日本学術振興会  科学研究費助成事業 

      田中 晴郎, 渡辺 鉄哉, 河合 誠之, 北本 俊二, 大橋 隆哉, 国枝 秀世, 常深 博, 満田 和久, 田原 譲, 井上 一, 村上 敏夫, 杉岡 勝, 牧島 一夫, 小山 勝二, 長瀬 文昭, 山下 広順, 小川原 嘉明, 宮本 重徳, 小田 稔

      詳細を見る

      1987年 - 1987年

      課題番号:62041110

      配分額:3600000円 ( 直接経費:3600000円 )

      この研究の目的は日英双方のX線天文学グループが経験と技術を併せて,〓界最大規模の大面積比例計数管を製作Astro-C(ぎんが)に搭載しX線天体の精密観測による研究を行うことである. ぎんがは昭和62年2月打ち上げられ性能評価,調整作業も無事完了したので,次は日英科学者が共同して多くの観測成果を挙げることがこれからの目的である.
      宇宙科学研究所のX線天文衛星「ぎんが」は昭和62年2月5日に打ち上げられ,順調に働いている. この衛星の主観測装置である大面積比例計数管は日本と英国のLeicester大学,Rutherford Appsleton研究所のグループとの共同で製作したものであり,これまでで〓界最高のX線集光面積を持つものである.
      打ち上げ以来,昭和62年9月まで,軌道上での性能評価,較正及び解析ソフトウェアの開発等を日英共同で行った. この目的のため「かに星雲」その他標準となるX線源の観測を行い,それを日英双方で解析を行い,両者のソフトウェアの互換性のチェックを行うと共に,最適性能を得るよう観測装置の微調整を行った.
      9月以降は個々の科学者からの観測申込を日英双方から募集し,選択されたものについて観測を行っている. 多数の応募があったため,2度の日英会合で調整を計った. 11月には初期成果の検討会を宇宙研で開催し, (宇宙圏研究会),英国側から数名が参加した.
      「ぎんが」の性能を反映して,多くの優れた成果が得られつつある. 日英共同の観測については,論文を作成するため結果の検討,討議が必要であり,この為の科学者の相互訪門が行れた. 数編の日英共著の論文がまとまりつつあり,間もなく学会誌に発表される運びである.
      これ迄に,多くのX線星について周期的変化(パルサー),準周期変動,不規測変動スペクトル等について詳しく調べられた他,特異X線星SS433の構造を調べる手掛りとなる新しい知見が得られた. 又, 新しいX線源の発見と共に,超遠方の活動銀河核のスペクトルや強度変化等についてこれまでにない高精度の観測結果が次々に生まれている. 更に,大マゼラン星雲に出現した超新星については最新のデーターを全〓界に提供している. 将来も引き続き,日英科学者による密接な共同研究を続けることを双方が強く希望している.

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    • 多層膜反射鏡を用いた宇宙X線の分光結像観測装置の開発研究

      日本学術振興会  科学研究費助成事業 

      山下 廣順, 北本 俊二, 常深 博, 宮本 重徳

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      1985年 - 1987年

      課題番号:60420004

      配分額:31300000円 ( 直接経費:31300000円 )

      多層膜反射鏡はX線全反射鏡とブラッグ結晶の特長を併せ持った新しい型のX線光学素子であり, 分光, 結像性能の優れた宇宙X線観測装置への応用を目ざしてその基礎研究を行ってきた. 斜入射型X線望遠鏡に用いる場合には焦点距離を変えずに有効面積(口径)の増大, エネルギー帯域の拡大を図ることができる. 更に0.4keV以下のエネルギー領域では光学望遠鏡と同様な直入射型X線望遠鏡が可能になるし, X線分光素子・偏光子にも応用できる.
      我々は超高真空電子ビーム蒸着装置によって, Mo/C, Mo/si, Ni/Cの組合せで2d値が60〜200A, 積層数5〜30組の多層膜を作製した. これらの多層膜はCu-Kα(1.54A), Si-Kα(7.13A)Ab-Kα(8.34A), C-Kα(44.7A)の特性X線を用いて反射率, エネルギー分解能ブラッグ角を測定することによって性能評価された. 更に高工研フォトンファクトリ, 分子研UVSORのシンクロトロン放射光を用いて, 14〜250Aの波長域で同様な測定を行った. その結果Mo/C, (2d=160A, N=10)ではCu-Kαに対して80%, Ni/C(2d=72A, N=20)ではC-Kαに対して10%, Mo/si, (2d=190A, N=20)では123〜170Aの波長域で30%以上のピーク反射率を得た. 特にMo/Siの球面鏡を製作し, 直入射型X線望遠鏡として十分な性能をもつことが確かめられた. 又シンクロトロン放射光によって45°入射のX線偏光子としての有用性も確認された. これらの結果をもとに昭和65年度のロケット観測を目指して多層膜反射鏡を用いたX線望鏡の製作を始めている. 多層膜反射鏡の応用範囲は広く, X線顕微鏡, 放射光ビームラインX線光学系, プラズマ計測用X線光学系等があり, 多くの研究者から関心が寄せられている.
      今後の課題として膜厚の薄膜化, 波長帯域の拡大があり, 薄膜物性とも関連して更なる発展が期待される.

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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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      資金種別:競争的資金

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    産業財産権

    • X線分光測定装置

      北本俊二

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      出願人:JST

      出願番号:平成10年特許願第248718  出願日:1998年9月2日

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