Updated on 2024/10/02

写真b

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

  • Research Interests
  • Astrophysics

  • Campus Career*
    • 4 2023 - Present 
      College of Science   Department of Physics   Senior Specially Appointed Professor
    • 4 2023 - Present 
      Graduate School of Science   Master's Program in Physics   Senior Specially Appointed Professor
    • 4 2023 - Present 
      Graduate School of Science   Doctoral Program in Physics   Senior Specially Appointed Professor
    • 4 2001 - 3 2023 
      College of Science   Department of Physics   Professor
    • 4 2005 - 3 2023 
      Graduate School of Science   Master's Program in Physics   Professor
    • 4 2005 - 3 2023 
      Graduate School of Science   Doctoral Program in Physics   Professor

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    Research Areas

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

    Research History

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

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

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

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

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    • 4 1995 - 3 1996 
      Osaka University   School of Science

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    • 4 1985 - 3 1995 
      Osaka University   School of Science

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    Education

    • 4 1982 - 3 1985 
      Osaka University   Graduate School of Science

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      Country: Japan

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    • 4 1980 - 3 1982 
      Osaka University

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    • - 3 1980 
      Osaka University   Faculty of Science

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      Country: Japan

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    Committee Memberships

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

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    • 6 2021 - 5 2023 
      Astronomical Society of Japan   Director

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      Committee type:Academic society

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

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      Committee type:Academic society

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

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      Committee type:Academic society

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

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      Committee type:Academic society

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

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      Committee type:Academic society

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

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      Committee type:Academic society

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    Papers

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

          3 2024

    • 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

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

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      Language:English   Publishing type:Research paper (international conference proceedings)   Publisher: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 )   4 2021

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      Publishing type:Research paper (scientific journal)  

      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   13 12 2020

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      Publishing type:Research paper (international conference proceedings)   Publisher: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   13 12 2020

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      Publishing type:Research paper (international conference proceedings)   Publisher: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   6 2020

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      Publishing type:Research paper (scientific journal)   Publisher: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   31 7 2019

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

      DOI: 10.3847/1538-4357/ab2b3d

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

    • 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 )   6 9 2018

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      Publishing type:Research paper (scientific journal)   Publisher: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 Peer-reviewed

      Hitomi Collaboration

      PASJ70 ( 3 )   3 4 2018

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

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

      DOI: 10.1093/pasj/psy027

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

      Hitomi Collaboration

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

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

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    • Ground calibration of the Astro-H (Hitomi) soft x-ray spectrometer Peer-reviewed

      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

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

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

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

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

      DOI: 10.1117/1.JATIS.4.1.011208

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

      Yuki Yoshida, Shunji Kitamoto, Akio Hoshino

      ASTROPHYSICAL JOURNAL849 ( 2 )   11 2017

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

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

      DOI: 10.3847/1538-4357/aa9023

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

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

      NATURE551 ( 7681 ) 478 - +   11 2017

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

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

      DOI: 10.1038/nature24301

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

      Juri Sugimoto, Shunji Kitamoto, Tatehiro Mihara, Masaru Matsuoka

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

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

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

      DOI: 10.1093/pasj/psx028

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

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

      ASTROPHYSICAL JOURNAL LETTERS837 ( 1 ) L15 - L23   3 2017

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

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

      DOI: 10.3847/2041-8213/aa61fa

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

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

      ASTROPHYSICAL JOURNAL838 ( 1 ) 30 - 44   3 2017

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

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

      DOI: 10.3847/1538-4357/aa6301

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

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

      NATURE535 ( 7610 ) 117 - +   7 2016

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

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

      DOI: 10.1038/nature18627

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

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

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

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

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

      DOI: 10.1093/pasj/psw004

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    • 21pCD-11 Status of the Soft X-ray Spectrometer (SXS) onboard ASTRO-H

      Tashiro M. S., Mitsuda k., Yamasaki N., Takei Y., Tsujimoto M., Ogawa M., Koyama S., Sakai K., Sugita H., Sato Y., Shinozaki, Okamoto A., Fujimoto R., Ohashi T., Ishisaki Y., Ezoe Y., Yamada S., Seta H., Terada Y., Kitamoto S., Hoshino A., Tamagawa T., Ishikawa K., Noda H., Sato K., Ota N., Sawada M., Mitsuishi I., Murakami M., Murakami H., Iyomoto N., 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 team

      Meeting Abstracts of the Physical Society of Japan71   509 - 509   2016

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      Language:Japanese   Publisher:The Physical Society of Japan (JPS)  

      DOI: 10.11316/jpsgaiyo.71.1.0_509

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    • In-orbit performance of the Soft X-ray Spectrometer (SXS) onboard ASTRO-H (Hitomi)

      Fujimoto R., Mitsuda K., Yamasaki N. Y., Takei Y., Tsujimoto M., Ogawa M., Koyama S., Ishikawa K., Sugita H., Sato Y., Shinozaki K., Okamoto A., Ohashi T., Ishisaki Y., Ezoe Y., Yamada S., Seta H., Tashiro M. S., Terada Y., Kitamoto S., Hoshino A., Tamagawa T., Sato K., Sawada M., Noda H., Mitsuishi I., Murakami H., Ota N., Iyomoto N., Murakami M., 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., ASTRO-H SXS team

      Meeting Abstracts of the Physical Society of Japan71   367 - 367   2016

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      Language:Japanese   Publisher:The Physical Society of Japan  

      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   1 1 2016

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

      DOI: 10.1117/12.2232933

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

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

      SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY9905   2016

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

      We present the overall design and performance of the Astro-H (Hitomi) Soft X-Ray Spectrometer (SXS). The instrument uses a 36-pixel array of x-ray microcalorimeters at the focus of a grazing-incidence x-ray mirror Soft X-Ray Telescope (SXT) for high-resolution spectroscopy of celestial x-ray sources. The instrument was designed to achieve an energy resolution better than 7 eV over the 0.3-12 keV energy range and operate for more than 3 years in orbit. The actual energy resolution of the instrument is 4-5 eV as demonstrated during extensive ground testing prior to launch and in orbit. The measured mass flow rate of the liquid helium cryogen and initial fill level at launch predict a lifetime of more than 4 years assuming steady mechanical cooler performance. Cryogen-free operation was successfully demonstrated prior to launch. The successful operation of the SXS in orbit, including the first observations of the velocity structure of the Perseus cluster of galaxies, demonstrates the viability and power of this technology as a tool for astrophysics.

      DOI: 10.1117/12.2232509

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

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

      SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY9905   2016

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

      We summarize all the in-orbit operations of the Soft X-ray Spectrometer (SXS) onboard the ASTRO-H (Hitomi) satellite. The satellite was launched on 2016/02/17 and the communication with the satellite ceased on 2016/03/26. The SXS was still in the commissioning phase, in which the setups were progressively changed. This article is intended to serve as a reference of the events in the orbit to properly interpret the SXS data taken during its short life time, and as a test case for planning the in-orbit operation for future micro-calorimeter missions.

      DOI: 10.1117/12.2231784

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

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

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

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

      DOI: 10.1093/mnras/stu2516

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    • 23pDK-4 Development status of Soft X-ray Spectrometer (SXS) onboard ASTRO-H (VI)

      Ishisaki K., Mitsuda K., Yamasaki N., Takei Y., Tsujimoto M., Ogawa M., Sugita H., Sato Y., Shinozaki K., Okamoto A., Fujimoto R., Ohashi T., Ezoe Y., Yamada S., Konami S., Tashiro M., Terada Y., H. Seta H. Seta, Kitamoto S., Hoshino A., Tamagawa T., Ishikawa K., Noda H., Sato K., Ota N., Sawada M., Mitsuishi I., Murakami M., Murakami H., Iyomoto N., 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 team

      Meeting Abstracts of the Physical Society of Japan70   471 - 471   2015

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      Language:Japanese   Publisher:The Physical Society of Japan (JPS)  

      DOI: 10.11316/jpsgaiyo.70.1.0_471

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    • 24aDJ-8 Long-term variation in the hard state and the soft state of Cygnus X-1 observed by MAXI

      Mihara T., Sugimoto J., Kitamoto S., Matsuoka M., Sugizaki M., Negoro H., Nakahira S.

      Meeting Abstracts of the Physical Society of Japan70   500 - 500   2015

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      Language:Japanese   Publisher:The Physical Society of Japan (JPS)  

      DOI: 10.11316/jpsgaiyo.70.1.0_500

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

      Umezu Rika, Kitamoto Shunji, Murakami Hiroshi

      REVIEW OF SCIENTIFIC INSTRUMENTS85 ( 7 )   7 2014

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

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

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

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

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

      DOI: 10.1093/pasj/psu019

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    • 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

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      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

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      Language:English   Publishing type:Research paper (international conference proceedings)   Publisher: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 Peer-reviewed

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

      SPACE TELESCOPES AND INSTRUMENTATION 2014: ULTRAVIOLET TO GAMMA RAY9144   2014

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

      We present the development status of the Soft X-ray Spectrometer (SXS) onboard the ASTRO-H mission. The SXS provides the capability of high energy-resolution X-ray spectroscopy of a FWHM energy resolution of < 7eV in the energy range of 0.3 - 10 keV. It utilizes an X-ray micorcalorimeter array operated at 50 mK. The SXS microcalorimeter subsystem is being developed in an EM-FM approach. The EM SXS cryostat was developed and fully tested and, although the design was generally confirmed, several anomalies and problems were found. Among them is the interference of the detector with the micro-vibrations from the mechanical coolers, which is the most difficult one to solve. We have pursued three different countermeasures and two of them seem to be effective. So far we have obtained energy resolutions satisfying the requirement with the FM cryostat.

      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 Peer-reviewed

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

      Astrophysical Journal Letters769 ( 1 )   20 5 2013

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

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

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

      Todoroki Shotaro, Kitamoto Shunji, Yoshida Yuki, Murakami Hiroshi

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

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      Language:English   Publisher: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 Peer-reviewed

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

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

    • X-Ray Inerferometer with a X-Ray Beamsplitter Peer-reviewed

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

      SPACE TELESCOPES AND INSTRUMENTATION 2012: ULTRAVIOLET TO GAMMA RAY8443   2012

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      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 Peer-reviewed

      Todoroki Shotaro, Kitamoto Shunji, Murakami Hiroshi

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

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    • Suzaku Observations of Six Early Type Stars Peer-reviewed

      Kitamoto Shunji, Yoshida Masaki, Shimizu Yusuke, Murakami Hiroshi

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

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

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

      PASJ63 ( SP3 ) S873 - S878   12 2011

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

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

      PASJ2011 ( SP3 ) S729 - S783   12 2011

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

      Yoshida, Masaki, Kitamoto, Shunji, Murakami, Hiroshi

      PASJ2011 ( SP3 ) S717 - S728   12 2011

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    • A New X-ray Interferometer Peer-reviewed

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

      Proceedings of SPIE - The International Society for Optical Engineering8147   2011

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      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 Peer-reviewed

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

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

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

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

      DOI: 10.1093/pasj/62.5.1249

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

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

      CRYOGENICS50 ( 9 ) 488 - 493   9 2010

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

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

      DOI: 10.1016/j.cryogenics.2010.02.004

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    • 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   2 2010

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      Language:English   Publishing type:Research paper (international conference proceedings)   Publisher:Japan Aerospace Exploration Agency (JAXA)  

      The 3rd Suzaku international Conference "Energetic Cosmos : from Suzaku to ASTRO-H" (June 29-July 2, 2009. Grand Park Otaru Hotel), Otaru, Hokkaido JapanWe have developed the X-ray CCD camera system for the Soft X-ray Imager (SXI) which will be launched as focal plane detectors of X-ray telescope onboard the Japanese 6th X-ray astronomical satellite, Astro-H. The X-ray CCD is 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). The X-ray CCD is affected by large doses of extreme ultraviolet (EUV) radiation from Earth sun-lit atmosphere (airglow) in orbit. To evaluate the performance of polyimide that cut off EUV, we measured the EUV transmission of both OBL and OBF at various energy range between 15 - 72 eV by utilizing beam line located at the Photon Factory in High Energy Accelerator Research Organization (KEK-PF) in this March and June, and obtained the EUV transmission to be 3% at 41 eV which is as same as expected transmission from the designed thickness of polyimide layer.Meeting sponsors: The University of Tokyo, The Institute of Physical and Chemical Research, The Japan Society for the Promotion of ScienceNumber of authors: 22

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

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

      Proceedings of the 3rd Suzaku Conference ( 9 ) 414 - 415   2 2010

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      Language:English   Publishing type:Research paper (international conference proceedings)   Publisher:Japan Aerospace Exploration Agency (JAXA)  

      The 3rd Suzaku international Conference "Energetic Cosmos : from Suzaku to ASTRO-H" (June 29-July 2, 2009. Grand Park Otaru Hotel), Otaru, Hokkaido JapanWe report the XIS calibration on the data taken with the 2 x 2 mode and window option and the current status of the XIS Non-X-ray Background (NXB) database. The 2 x 2 mode and window option are useful for bright source observations to avoid telemetry saturation and event pile-up. The NXB database provides the best-estimated NXB spectrum for any specific observations obtained with the standard mode (Normal-Clock with no Window or Burst and 5 x 5(sub -) (3 x 3(sub -) Editing mode). The data taken with the 2 x 2 mode in the "SCI-off" era are fully calibrated, and there is no practical difference from those taken with the standard mode. A calibration study for the data taken with the 2 x 2 mode in the "SCI-on" era is on-going. The calibration for the data taken with the window option was significantly improved in the HEASOFT 6.6.2 released at 2009 April 1st. In the comparison with the standard-mode data, the gain difference around 6 keV becomes less than 10 and 15 eV in XIS 0,3 and XIS 1, respectively. We have been updating the NXB database every half a year. There is no drastic change in the light curves, but steady approximately 4 % year(sup -1) level increase and decrease are found in those of XIS 0,3 and XIS 1, respectively.Meeting sponsors: The University of Tokyo, The Institute of Physical and Chemical Research, The Japan Society for the Promotion of ScienceNumber of authors: 25

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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   2 2010

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

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

      DOI: 10.1063/1.3294330

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    • Imaging Experiment of an Adaptive Optics with a Normal-Incident EUV Telescope Peer-reviewed

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

      Proceedings of SPIE - The International Society for Optical Engineering7803   2010

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      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 Peer-reviewed

      H. Murakami, S. Kitamoto

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

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

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      Language:English   Publishing type:Research paper (international conference proceedings)   Publisher: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 Peer-reviewed

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

      SPACE TELESCOPES AND INSTRUMENTATION 2010: ULTRAVIOLET TO GAMMA RAY7732   2010

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

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

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

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

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

      DOI: 10.1117/12.856909

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

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

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

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

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

      DOI: 10.1093/pasj/61.4.629

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

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

      ASTRONOMICAL JOURNAL137 ( 5 ) 4160 - 4168   5 2009

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

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

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

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

      ASTROPHYSICAL JOURNAL LETTERS697 ( 1 ) L54 - L57   5 2009

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      We report the detection of superhard (&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 Peer-reviewed

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

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

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

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

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      Language:English   Publishing type:Research paper (international conference proceedings)   Publisher: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 Peer-reviewed

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

      Proceedings of SPIE - The International Society for Optical Engineering7435   2009

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

      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 Peer-reviewed

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

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

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

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

      DOI: 10.1093/pasj/61.sp1.S69

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    • The X-ray microcalorimeter on the NeXT mission

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

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

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

      DOI: 10.1117/12.787952

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

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

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

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

      The black-hole binary Cygnus X-1 was observed for 17 ks with the Suzaku X-ray observatory in 2005 October, while it was in a low/hard state with a 0.7-300 keV luminosity of 4.6 x 10(37) ergs(-1). The XIS and HXD spectra, spanning 0.7-400 keV, were reproduced successfully, incorporating a cool accretion disk and a hot Comptonizing corona. The corona is characterized by an electron temperature of similar to 100 keV, and two optical depths of similar to 0.4 and similar to 1.5, which account for the softer and harder continua, respectively. The disk has an innermost temperature of similar to 0.2keV, and is thought to protrude half way into the corona. The disk not only provides seed photons to the Compton cloud, but also produces a soft spectral excess, a mild reflection hump, and a weakly broadened iron line. A comparison with the Suzaku data on GRO J1655-40 reveals several interesting spectral differences, which can mostly be attributed to inclination effects, assuming that the disk has a flat geometry while the corona is grossly spherical. An intensity-sorted spectroscopy indicates that the continuum becomes less Comptonized when the source flares up on time scales of 1-200 s, while the underlying disk remains unchanged.

      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   24 4 2008

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

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

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

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

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

      We report on the detection of a transient X-ray source toward the Small Magellanic Cloud (SMC) using the X-ray Imaging Spectrometer (XIS) on board the Suzaku telescope. The source was detected at the edge of the XIS image during a routine observation of the calibration source 1E0102.2-7219, a supernova remnant in the SMC. We constrained the source position using ray-tracing simulations. No such transient source was found at the position in the other Suzaku observations, nor in all of the available archived images of other X-ray missions for the last similar to 28 years. The XIS spectrum can be explained by a single blackbody with a temperature of similar to 72 eV, and an interstellar extinction of similar to 4.9 x 10(20) H atoms cm(-2), consistent with the value to the SMC. An additional absorption edge at similar to 0.74 keV was also confirmed, which is presumably due to absorption by helium-like oxygen ions. Assuming that the source is at the distance of the SMC, the X-ray luminosity in the 0.2-2.0 keV band is similar to 10(37) erg s(-1) and the radius of the source is similar to 10(8) cm. The XIS light curve shows about a two-fold decline in X-ray flux during the 24 ks observation. Together with the archived data, the X-ray flux in the burst is at least three-orders of magnitude brighter than the undetected quiescent level. All of these properties are often seen among supersoft sources (SSSs). We conclude that the transient source is another example of SSS in the SMC.

      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

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

      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 Peer-reviewed

      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

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

      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

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      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 Peer-reviewed

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

      Proceedings of SPIE - The International Society for Optical Engineering7015   2008

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      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 Peer-reviewed

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

      Advances in Space Research41 ( 3 ) 411 - 415   2008

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      SN 1006 is one of the supernova remnants (SNRs) with relatively low-temperature electrons, considering the young age of just 1000 years. We carried out SN 1006 mapping observations with the X-ray Imaging Spectrometers (XIS) and the Hard X-ray Detector (HXD) onboard Suzaku, the fifth Japanese X-ray satellite. Thanks to the excellent spectral resolution of XIS in the soft X-ray band, H-like and He-like oxygen emission lines were clearly detected, and we could make a map of the line intensity, and as well as a flux and the photon index of nonthermal component. We found that these parameters have spatial dependences from region to region in the SNR; the north region is bright in nonthermal, while dim in thermal; the east region is bright in both nonthermal and thermal; the inner region shows dim nonthermal and bright thermal emission. The photon index is the smallest in the north region. © 2007.

      DOI: 10.1016/j.asr.2007.03.055

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

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

      Publications of the Astronomical Society of Japan60 ( SPEC. ISS. 1 ) S69 - S83   2008

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

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

      ASTROPHYSICAL JOURNAL672 ( 1 ) 516 - 523   1 2008

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

      The transient X-ray binary pulsar A0535+262 was observed with Suzaku on 2005 September 14 when the source was in the declining phase of the August-September minor outburst. The similar to 103 s X-ray pulse profile was strongly energy dependent, with a double-peaked profile in the soft X-ray energy band (&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   9 2007

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      The X-ray Imaging Spectrometers (XIS) on-board Suzaku is an X-ray CCD camera system that has features of low background, good energy resolution, and high quantum efficiency (QE) at 0.2-12 keV band. However, an unexpected degradation of the QE at low energies (< 1 keV) has emerged since November 2005. Some contaminants are considered to be adsorbed on the Optical Blocking Filter (OBF) for each sensor and cause the degradation. A suspected contamination source is rubber used in the shock absorber of the satellite gyro. For the recovery of the QE, we now design to remove the contaminants by increasing the OBF temperature. Before the on-board bakeout is performed, we need to confirm on the ground that it does not cause a serious damage to the OBF. In order to reproduce the on-board contamination, we adsorbed the contaminant of ∼ 160 μg cm-2 from the rubber on a spare OBF and a Thermoelectric Quartz Crystal Microbalance simultaneously, which are cooled down to -40 °C. Although unexpected wrinkles appeared on the OBF surface during the adsorption and they remained through the subsequent bakeout, we could not find any tears on it. In addition, we estimated the desorption rate at -15 °C to be ∼ 5 μg cm-2 per day. In our presentation, we also discuss the expected effect by the on-board bakeout based on these results.

      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

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      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

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      Language:English   Publisher:Progress of Theoretical Physics  

      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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      Other Link: http://dl.ndl.go.jp/info:ndljp/pid/10886569

    • Millenium study of SN 1006 with suzaku Peer-reviewed

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

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

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      Publishing type:Research paper (international conference proceedings)  

      SN 1006 is the milestone of understanding the acceleration mechanism of cosmic rays, and this year is the millennium year for the remnant. We carried out SN 1006 mapping observations with the X-ray Imaging Spectrometers (XIS) onboard Suzaku satellite. Thanks to the excellent spectral response of XIS, K emission lines from highly ionized oxygen were clearly resolved. The intensity maps of these lines have been made additional to the intensity and photon index maps of the nonthermal component. We discovered that regions with strong and hard nonthermal component has weak thermal emission. The north rim of the SNR has the hardest nonthermal component. These facts might have information of efficient cosmic ray acceleration and background plasma.

      DOI: 10.1143/PTPS.169.142

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

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

      Advances in Space Research40 ( 10 ) 1485 - 1490   2007

    • Orbital calibration of the XIS Peer-reviewed

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

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

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

      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.

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

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

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

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

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

      DOI: 10.1093/pasj/59.sp1.S23

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

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

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

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

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

      DOI: 10.1093/pasj/59.sp1.S151

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

      Norimasa Yamamoto, Haruko Takano, Shunji Kitamoto, Takayoshi Kohmura

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

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

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

      DOI: 10.1093/pasj/59.1.237

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    • The X-ray observatory Suzaku

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

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

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

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

      DOI: 10.1093/pasj/59.sp1.S1

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

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

      ASTROPHYSICAL JOURNAL648 ( 2 ) L139 - L142   9 2006

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

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

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    • 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

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      Publishing type:Research paper (international conference proceedings)  

      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 Peer-reviewed

      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

    • 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

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      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 Peer-reviewed

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

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

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      We give overview and the current status of the development of the Soft X-ray Imager (SXI) onboard the NeXT satellite. SXI is a back-illuminated supportless CCD (a combination of "back-illuminated CCD" and "supportless CCD") whose imaging area and the supportless region are 42 × 42mm2 and 30mmφ respectively. The goal of the thickness of the depletion layer is 300μm, which enables us to cover the energy range of 0.3 - 25 keV. The evaluation model 'CCD-NeXT1' with the size of 24 × 48mm2 shows no performance change due to the thinning process. The test model of P-channel CCD was confirmed to have high quantum efficiency above 10 keV with an equivalent depletion layer of 300m.

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

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

      European Space Agency, (Special Publication) ESA SP622 ( 622 SP ) 325 - 332   2006

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      The Galactic black-hole binary GRO J1655-40 was observed with Suzaku on 2005 September 22-23, for a gross time span of similar to 1 day. The source was detected over a wide and continuous energy range of 0.7-300 keV, with an intensity of similar to 50 mCrab in the 1.5 - 12 keV band. At an assumed distance of 3.2 kpc, the 0.7-300 keV luminosity is calculated to be similar to 4.4 x 10(36) ergs s(-1). The source was in a typical low/hard state, since its overall spectrum was dominated by a power-law component with a photon index of similar to 1.7. The source intensity gradually decreased by 20% during the observation, involving little spectral changes above similar to 3 keV. However, at softer energies, the amplitude of variability was somewhat enhanced. This indicates the presence of an independent soft component. The spectra in the hard energy band reveal a high-energy spectral cutoff, with an e-folding energy of similar to 200 keV which is suggested to be higher than those observed from typical black hole binaries in the low/hard state.

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      Other Link: 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   1 1 2006

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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

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      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 Peer-reviewed

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

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

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      Astro-E2 is the fifth Japanese X-ray astronomical satellite and will be launched in 2005. The Astro-E2 X-ray Imaging Spectrometers (XISs) consist of four sets of X-ray CCD cameras. Each CCD camera has an imaging area of 1024×1024 pixels and covers a region of 18′×18′ on the sky combined with an X-ray Telescope. One XIS will utilize back-side illuminated (BI) CCDs, and the other three will be equipped with front-side illuminated (FI) CCDs. The BI CCD has a higher quantum efficiency than the FI CCD below 2 keV, while the FI CCD is more sensitive to X-rays above 5 keV than the BI CCD. Both types of the CCDs have nearly the same energy resolution (full-width at half-maximum (FWHM)=∼130eV at 6 keV). All four cameras have a charge injection capability and 55Fe calibration sources, and we can correct the change of the gain and recover the degradation of the energy resolution due to radiation damage caused by cosmic rays. The sensors are cooled to -90°C to minimize thermal noise in orbit. The low temperature is also helpful to reduce the influence of the radiation damage. © 2005 Elsevier B.V. All rights reserved.

      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 Peer-reviewed

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

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

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      We give an overview, the current status and future plan of the development of the Soft X-ray Imager (SXI) onboard the NeXT (Non-thermal Energy eXploration Telescope) satellite proposed to be launched around 2010. The SXI is a back-illuminated supportless CCD (a combination of "back-illuminated CCD" and "supportless CCD") whose imaging area size and the supportless region are 42mm×42mm and 30mmφ, respectively. The goal of the depletion layer of the CCD is 300μm, which enable us to cover the X-ray energy range of 0.5-20 keV. The first test model of the supportless CCD shows no performance change due to the thinning process of the CCD. We have already started processing the evaluation model 'CCD-NeXT1', which will be completed at the end of 2004. We are also studying the camera system, the focal plane assembly including thermal electric cooler (TEC) and electronics as well as the CCD chip. © 2005 Published by Elsevier B.V.

      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   1 1 2005

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

      北本 俊二

      Physica, E29   505 - 509   1 1 2005

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    • Soft 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

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      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   1 1 2004

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    • X-ray time variation of GRS 1915+105

      Y Ohkawa, S Kitamoto, T Kohmura

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

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

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

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

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

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

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

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

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

      S. Kitamoto

      NIMA505.683-687   4 2003

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    • 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

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      Language:English   Publishing type:Research paper (international conference proceedings)   Publisher: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   1 1 2003

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    • Lunar X-ray spectrometer experiment on the selene mission Peer-reviewed

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

      Advances in Space Research30 ( 8 ) 1909 - 1914   2002

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      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 Peer-reviewed

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

      Advances in Space Research29 ( 8 ) 1237 - 1242   2002

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      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   1 1 2002

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

      Kentaro Terada, Shunji Kitamoto, Hitoshi Negoro, Sayuri Iga

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

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

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

      DOI: 10.1093/pasj/54.4.609

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

      北本 俊二

      放射光 ( 4 ) 19 - 28   1 1 2002

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

      AKH Kong, PA Charles, E Kuulkers, S Kitamoto

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

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

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

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    • Evaluations of domestic X-ray CCDs with XIS analog electronics Peer-reviewed

      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

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      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 Peer-reviewed

      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

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

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

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

      DOI: 10.1086/323848

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

      北本 俊二

      NIMA   191 - 199   1 1 2001

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

      北本 俊二

      ApJ ( 554 ) 528 - 533   1 1 2001

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    • 「あすか」が見た星形成領域と若い星

      北本 俊二

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

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

      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

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      Language:English   Publishing type:Research paper (international conference proceedings)   Publisher: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 Peer-reviewed

      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

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher: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 Peer-reviewed

      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

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

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

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      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

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

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

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    • Soft X-ray response of a CCD with a grating spectrometer Peer-reviewed

      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   10 1999

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher: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 Peer-reviewed

      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   10 1999

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher: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   9 1999

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

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      Language:English   Publishing type:Research paper (international conference proceedings)   Publisher: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 Peer-reviewed

      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

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

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

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      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 Peer-reviewed

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

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

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    • 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   1 8 1998

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher: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   3 1998

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher: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 Peer-reviewed

      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   2 1998

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher: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 Peer-reviewed

      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

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

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      Language:English   Publisher:The Japan Society of Applied Physics  

      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

      Jpn J Appl Phys36 ( 5 ) 2906 - 2911   15 5 1997

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      Language:English   Publisher:The Japan Society of Applied Physics  

      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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      Other Link: 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

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      Language:English   Publishing type:Research paper (international conference proceedings)   Publisher: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   20 3 1995

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

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher: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 Peer-reviewed

      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

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher: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   3 1993

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      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 Peer-reviewed

      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

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      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 Peer-reviewed

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

      Astrophysical Journal389 ( 2 ) 676 - 684   20 4 1992

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      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 Peer-reviewed

      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

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      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 Peer-reviewed

      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

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher: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 Peer-reviewed

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

      ASTROPHYSICAL JOURNAL383 ( 2 ) 784 - 807   12 1991

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher: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   12 1991

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher: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 Peer-reviewed

      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   10 11 1991

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher: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 )   10 7 1991

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      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

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher: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 )   20 12 1990

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      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   1 10 1990

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

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      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

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      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

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      Language:English   Publishing type:Research paper (scientific journal)  

      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 Peer-reviewed

      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

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

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    • DELAYED HARD X-RAYS FROM CYGNUS X-1 Peer-reviewed

      S MIYAMOTO, S KITAMOTO, K MITSUDA, T DOTANI

      NATURE336 ( 6198 ) 450 - 452   12 1988

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

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    • TRANSIENT DIPS OF CYGNUS X-1 OBSERVED FROM TENMA Peer-reviewed

      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

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

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    • 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

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    • Concept of the X-ray Astronomy Recovery Mission

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

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

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      © 2018 SPIE. The ASTRO-H mission was designed and developed through an international collaboration of JAXA, NASA, ESA, and the CSA. It was successfully launched on February 17, 2016, and then named Hitomi. During the in-orbit verification phase, the on-board observational instruments functioned as expected. The intricate coolant and refrigeration systems for soft X-ray spectrometer (SXS, a quantum micro-calorimeter) and soft X-ray imager (SXI, an X-ray CCD) also functioned as expected. However, on March 26, 2016, operations were prematurely terminated by a series of abnormal events and mishaps triggered by the attitude control system. These errors led to a fatal event: the loss of the solar panels on the Hitomi mission. The X-ray Astronomy Recovery Mission (or, XARM) is proposed to regain the key scientific advances anticipated by the international collaboration behind Hitomi. XARM will recover this science in the shortest time possible by focusing on one of the main science goals of Hitomi,&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 Peer-reviewed

      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

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      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 Peer-reviewed

      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

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      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 X-ray spectrum of Cyg X-3 in ultra-soft state with MAXI, XRT and Swift

      Mihara Tatehiro, Matsuoka Masaru, Nakajima Motoki, Sugizaki Mutsumi, Nakahira Satoshi, Kitamoto Shunji, Kotani Taro

      Meeting abstracts of the Physical Society of Japan69 ( 2 ) 36 - 36   22 8 2014

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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   5 3 2014

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

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

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

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

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

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

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    • Physics Education Today : The Seventh (2011) Junior Session in the 66th Annual Meeting of JPS

      Kitamoto Shunji, Matsuo Masayuki

        67 ( 6 ) 406 - 408   6 2012

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    • As a Chairman of Division Committee

      KITAMOTO Shunji

        67 ( 4 ) 225 - 225   5 4 2012

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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   3 2012

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      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   6 1 2012

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    • Soft X-ray response of the X-ray CCD camera directly coated with Optical Blocking Layer Peer-reviewed

      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

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      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 Peer-reviewed

      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

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

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

      Meeting Abstracts of the Physical Society of Japan67 ( 0 ) 119 - 119   2012

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    • Report on the Symposium "Utilization of Nuclear Energy and Future Energy Strategies from View Points of Physicists"

      AIHARA Hiroaki, KITAMOTO Shunji

        66 ( 10 ) 783 - 784   5 10 2011

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      Physical Society of Japan held an urgent symposium, in order to discuss the utilization of nuclear power and future energy problem, with members of the society and related scientists. We make a brief report of its contents.

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    • Report on the Symposium "Utilization of Nuclear Energy and Future Energy Strategies from View Points of Physicists"

      AIHARA Hiroaki, KITAMOTO Shunji

        66 ( 10 ) 783 - 784   5 10 2011

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      Physical Society of Japan held an urgent symposium, in order to discuss the utilization of nuclear power and future energy problem, with members of the society and related scientists. We make a brief report of its contents.

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

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

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

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

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

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

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    • 26aGS-13 Discovery of Non-thermal X-ray Emission from Classical Novae

      Takei Dai, Tsujimoto Masahiro, Kitamoto Shunji

      Meeting abstracts of the Physical Society of Japan66 ( 1 ) 111 - 111   3 3 2011

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    • 26aGS-13 Discovery of Non-thermal X-ray Emission from Classical Novae

      Takei Dai, Tsujimoto Masahiro, Kitamoto Shunji

      Meeting abstracts of the Physical Society of Japan66 ( 1 ) 111 - 111   3 3 2011

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

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

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

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    • X線天文衛星ASTRO‐H搭載X線CCD(SXI)の紫外線対策

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

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

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    • ASTRO‐H衛星搭載X線用CCDの可視光・紫外線遮光対策

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

      PFシンポジウム要旨集28th   88   2011

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    • すざく衛星搭載XISのOBFの破れの評価

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

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

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

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

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

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    • 宇宙X線用CCDの赤外線遮光対策

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

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

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    • The Fifth (2009) Junior Session in the 65th Annual Meeting of JPS

      KITAMOTO Shunji, NAMIKI Masatoshi

      Butsuri65 ( 5 ) 356 - 358   5 5 2010

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

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

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

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

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

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

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

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

      Meeting Abstracts of the Physical Society of Japan65 ( 0 ) 83 - 83   2010

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    • すざく衛星搭載X線CCDカメラXISのP‐sumモードの較正

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

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

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

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

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

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    • 10pSD-4 X-ray Polarimeter with a Transmission Multilayer

      Kitamoto Shunji, Murakami Hiroshi, Shishido Youichi, Saito Kousuke, Watanabe Takeshi, Kanai Jun'ichi, Takenaka Eri, Nagasaki Kenta, Takei Dai, Morii Mikio

      Meeting abstracts of the Physical Society of Japan64 ( 2 ) 35 - 35   18 8 2009

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

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

      Meeting abstracts of the Physical Society of Japan64 ( 2 ) 31 - 31   18 8 2009

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

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

      Meeting abstracts of the Physical Society of Japan64 ( 1 ) 92 - 92   3 3 2009

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

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

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

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

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

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

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    • 22pSH-6 Suzaku Observations of Cyg X-1 in the Low-Hard state (II)

      Makishima K., Yamada S., Takahashi H., Kubota A., Dotani T., Ebisawa K., Kitamoto S., Negoro H., Ueda Y., Yamaoka K.

      Meeting abstracts of the Physical Society of Japan63 ( 2 ) 89 - 89   25 8 2008

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    • 「すざく」搭載X線CCDカメラ(XIS)の時刻付けの較正

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

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

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    • Spektr-RG衛星搭載X線カロリメータ分光装置SXC

      藤本龍一, 大橋隆哉, 石崎欣尚, 江副祐一郎, 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, 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

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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

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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

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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

      Publications of the Astronomical Society of Japan59 ( 6 ) 1141 - 1151   25 12 2007

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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   21 8 2007

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    • NeXT衛星搭載X線CCDカメラSXIシステム開発の現状

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

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

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    • 「すざく」ファーストライト:X線CCDカメラXIS

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

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

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

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

      Meeting Abstracts of the Physical Society of Japan61 ( 0 ) 77 - 77   2006

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

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

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

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      We give overview and the current status of the development of the Soft X-ray Imager (SXI) onboard the NeXT satellite. SXI is an X-ray CCD camera placed at the focal plane detector of the Soft X-ray Telescopes for Imaging (SXT-I) onboard NeXT. The pixel size and the format of the CCD is 24 × 24μm (IA) and 2048 × 2048 × 2 (IA+FS). Currently, we have been developing two types of CCD as candidates for SXI, in parallel. The one is front illumination type CCD with moderate thickness of the depletion layer (70 ∼ 100μm) as a baseline plan. The other one is the goal plan, in which we develop back illumination type CCD with a thick depletion layer (200 ∼ 300μm). For the baseline plan, we successfully developed the proto model 'CCD-NeXT1' with the pixel size of 12μm × 12μm and the CCD size of 24mm × 48mm. The depletion layer of the CCD has reached 75 ∼ 85μm. The goal plan is realized by introduction of a new type of CCD 'P-channel CCD', which collects holes in stead of electrons in the common 'N-channel CCD'. By processing a test model of P-channel CCD we have confirmed high quantum efficiency above 10 keV with an equivalent depletion layer of 300μm. A back illumination type of P-channel CCD with a depletion layer of 200μm with aluminum coating for optical blocking has been also successfully developed. We have been also developing a thermo-electric cooler (TEC) with the function of the mechanically support of the CCD wafer without standoff insulators, for the purpose of the reduction of thermal input to the CCD through the standoff insulators. We have been considering the sensor housing and the onboard electronics for the CCD clocking, readout and digital processing of the frame date.

      DOI: 10.1117/12.670649

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    • Astro‐E2衛星の現状:X線CCD検出器(XIS)

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

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

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    • 24pXK-6 Development of a New Radiation Detector Utilizing Carbon Nanotube as Anode

      Kotani T., Kawai N., Chiba S., Kitamoto S.

      Meeting abstracts of the Physical Society of Japan60 ( 1 ) 89 - 89   4 3 2005

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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   5 1 2005

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

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

      日本天文学会年会講演予稿集2004   256   2004

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

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

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

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      The NeXT mission has been proposed to study high-energy non-thermal phenomena in the universe. The high-energy response of the super mirror will enable us to perform the first sensitive imaging observations up to 80 keV. The focal plane detector, which combines a fully depleted X-ray CCD and a pixelated CdTe detector, will provide spectra and images in the wide energy range from 0. 5 keV to 80 keV. In the soft gamma-ray band upto ∼ 1 MeV, a narrow field-of-view Compton gamma-ray telescope utilizing several tens of layers of thin Si or CdTe detector will provide precise spectra with much higher sensitivity than present instruments. The continuum sensitivity will reach several x 10-8 photons/s/keV/cm2 in the hard X-ray region and a few × 107 photons/s/keV/cm2 in the soft γ-ray region.

      DOI: 10.1117/12.551500

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    • Development of an Ultra High Angler Resolution X-ray Telescope 2

      Kitamoto S., Yamamoto N., Kohmura T., Sekiguchi H., Suga K., Takano H., Saitoh H., Ueda Y., Itoh M., X-mas Team

      Meeting abstracts of the Physical Society of Japan58 ( 1 ) 95 - 95   6 3 2003

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    • Development of an Ultra High Angular Resolution X-ray Telescope : Measurement and Correction of Wave Front from the Main Mirror

      Yamamoto N., Kitamoto S., Komura T., Sekiguchi H., Suga K., Takano H., Saito H., Ueda Y., Ito Masayuki, X-mas team

      Meeting abstracts of the Physical Society of Japan58 ( 1 ) 95 - 95   6 3 2003

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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   9 1 2003

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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   9 1 2003

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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

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    • ASTRO‐EII搭載のCCDカメラXIS(I)

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

      日本天文学会年会講演予稿集2003   231   2003

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    • Devolopment of an Ultra High Precision X-ray Telescope I

      Kitamoto S., Sekiguchi H., Suga K., Kohmura T., Yamamoto N., Saito H., Takano H., Uewda Y., Itoh M., X-mas Team

      Meeting abstracts of the Physical Society of Japan57 ( 2 ) 84 - 84   13 8 2002

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    • X-ray Observation of X-ray Binary Pulsar Centaurus X-3 with RXTE

      Kohmura Takayoshi, Kitamoto Sunji

      Meeting abstracts of the Physical Society of Japan57 ( 2 ) 74 - 74   13 8 2002

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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   1 3 2002

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

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

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

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      We report on design updates for the XIS (X-ray Imaging Spectrometer) on-board the Astro-E2 satellite. Astro-E2 is a recovery mission of Astro-E, which was lost during launch in 2000. Astro-E2 carries a total of 5 X-ray telescopes, 4 of which have XIS sensors as their focal plane detectors. Each XIS CCD camera covers a field of view of 19 × 19 arcmin in the energy range of 0.4-12 keV. The design of the Astro-E2 XIS is basically the same as that for Astro-E, but some improvements will be implemented. These are (1) CCD charge injection capability. (2) a revised heat-sink assembly, and (3) addition of a 55Fe radio-isotope on the door. Charge injection may be used to compensate for and calibrate radiation-induced degradation of the CCD charge transfer efficiency. This degradation is expected to become significant after a few year's operation in space. The new heat-sink assembly is expected to increase the mechanical reliability and cooling capability of the XIS sensor. The new radio-isotope on the door will provide better calibration data. We present details of these improvements and summarize the overall design of the XIS.

      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   11 1 2001

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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   11 1 2001

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    • XIS読み出し回路を用いた国産CCDの性能評価(II)

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

      日本天文学会年会講演予稿集2001   267   2001

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    • 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   3 2000

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      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

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      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

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    • 25pSD-12 The X-ray Detectors and the Calibration System for the MAXI Mission

      TOMIDA H, MATSUOKA M, TORII K, SUGIZAKI M, UENO S, TSUNEI H, MIYATA E, HAYASHIDA K, KITAMOTO S, AKUTSU D, MORI K, YOSHITA K, YAMAUCHI M, KAWAI N, YOSHIDA A, MIHARA T, SHIRASAKI Y, SAKURAI I, NEGORO H

      Meeting abstracts of the Physical Society of Japan54 ( 2 ) 83 - 83   13 9 1999

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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   13 9 1999

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    • 30p-XJ-6 Soft X-Ray Response of the CCD Camera(XIS)for the ASTRO-E Mission

      Syouho M., Katayama H., Katayama K., Kohmura T., Tsunemi H., Kitamoto S., Hayashida K., Miyata E., Hashimotodani K., Koyama K., Ricker G., Bautz M.W., Foster R., Kissel S., Dotani T., Team XIS

      Meeting abstracts of the Physical Society of Japan54 ( 1 ) 362 - 362   15 3 1999

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    • 28a-YK-9 MAXI test detector and X-ray calibration facility

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

      Meeting abstracts of the Physical Society of Japan54 ( 1 ) 76 - 76   15 3 1999

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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

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      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

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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

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      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

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      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   11 1998

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      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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    • Soft X-Ray Response of the CCD Camera (XIS) for the ASTRO-E Mission

      SYOUHO M., KATAYAMA H., KATAYAMA K., KOHMURA T., TSUNEMI H., KITAMOTO S., HAYASHIDA K., MIYATA E., HASHIMOTODANI K., KOYAMA K., RICKER G., BAUTZ M.W, FOSTER R., DOUTANI T., XIS-TEAM

      Meeting abstracts of the Physical Society of Japan53 ( 2 ) 83 - 83   5 9 1998

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    • Quantumn Efficiency of the CCD Camera (XIS) for the ASTRO-E Mission

      KATAYAMA H., SYOUHO M., KOHMURA K., KATAYAMA K., TSUNEMI H., KITAMOTO S., HAYASHIDA K., MIYATA E., HASHIMOTODANI K., KOYAMA K., RICKER G., BAUTZ M.W, FOSTER R., XIS-TEAM

      Meeting abstracts of the Physical Society of Japan53 ( 2 ) 83 - 83   5 9 1998

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    • MAXI(Monitor of All-sky X-ray lmage)on International Space Station(II)

      KAWAI N., MATSUOKA M., YOSHIDA A., MIHARA T., KOTANI T., NEGORO H., RUBIN Brad, KUBO H., SHIRASAKI Y., TSUNEMI H., KITAMOTO S., HAYASHIDA K., MIYATA E., TORII K., HASHIMOTODANI K., YOSHITA K., YAMAUCHI M.

      Meeting abstracts of the Physical Society of Japan53 ( 1 ) 81 - 81   10 3 1998

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    • Reports of Soft X-Ray Response of the Proto-Type CCD Camera(XIS) for The ASTRO-E Mission

      KOHMURA T., KATAYAMA K., ASAKURA R., TSUNEMI H., KITAMOTO S., HAYASHIDA K., MIYATA E., HASHIMOTODANI K., RICKER G.R., XIS-TEAM

      Meeting abstracts of the Physical Society of Japan53 ( 1 ) 80 - 80   10 3 1998

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

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

      日本天文学会年会講演予稿集1998   181   1998

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

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

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

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

      M Akiyama, K Ohta, T Yamada, Y Ueda, T Takahashi, M Sakano, T Tsuru, B Boyle

      ASTRONOMISCHE NACHRICHTEN319 ( 188 ) 465 - 466   1998

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      DOI: 10.1002/asna.2123190127

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

      KAMADO Yasuhide, KITAMOTO Shunji, MIYAMOTO Sigenori

      Publications of the Astronomical Society of Japan49 ( 5 ) 589 - 605   25 10 1997

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    • 23p-J-13 MAXI(Monitor of All-sky X-ray Image) on International Space Station

      Mihara T., Matsuoka M., Kawai N., Yoshida A., Kotani T., Negoro H., Rubin B., Shimizu H.M., Tsunemi H., Kitamoto S., Hayashida K., Miyata E., Hashimotodani K., Yoshita K., Yamauchi M.

      Meeting abstracts of the Physical Society of Japan52 ( 2 ) 84 - 84   2 9 1997

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    • Astro‐E搭載用X線CCDカメラ(XIS)の開発 II

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

      日本天文学会年会講演予稿集1997   184   1997

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    • ASCA Observation of Cygnus OB2 Association

      KITAMOTO Shunji, MUKAI Koji

      Publications of the Astronomical Society of Japan48 ( 6 ) 813 - 818   1 12 1996

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    • 8a-C-2 Measurement of Quantum Efficiency of a CCD for Direct X-Ray Detection

      Kitamoto S., Tsunemi H., Hayashida K., Miyata E., Hashimotodani K., Ohno Y., Sumi Y., Koyama K., Yamamoto K., Miyaguchi K.

      Abstracts of the meeting of the Physical Society of Japan. Sectional meeting1996 ( 1 ) 168 - 168   13 9 1996

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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.

      Publications of the Astronomical Society of Japan48 ( 3 ) 425 - 440   25 6 1996

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

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

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

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    • 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   1 1996

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      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   10 6 1995

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    • 衛星搭載用X線CCDカメラの開発 (II)

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

      日本天文学会年会講演予稿集1995   226   1995

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    • ASTRO‐E搭載用X線CCDカメラ(XIS)の開発

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

      日本天文学会年会講演予稿集1995   224   1995

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    • 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   12 1994

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      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   1 5 1994

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    • 31p-YW-1 Study of the plasma around CygX-3 observed with ASCA satellite

      Kitamoto Shunji, Kawashima Kenji, Megoro Hitoshi, Nagase Fumiaki, White N.E

      Abstracts of the meeting of the Physical Society of Japan. Annual meeting49 ( 1 ) 173 - 173   16 3 1994

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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

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      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   8 1992

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      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   5 1992

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      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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    • Iron Emission Line from Cygnus X-3

      Kitamoto S., Yamashita K., Nakamura H.

        1990 ( 1 ) 92 - 92   12 9 1990

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    • A Jet Model for X-ray Star GX339-4

      Miyamoto S., Kitamoto S.

        1990 ( 1 ) 92 - 92   12 9 1990

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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   6 1990

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

      KITAMOTO S.

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

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    • 13p-C-3 Phase lag structure of the X-rays from Cyg X-1 and GX 339-4

      Miyamoto Sigenori, Kitamoto Shunji, Kimura Kazuhiro

        1989 ( 1 ) 87 - 87   12 9 1989

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

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

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    • Time Variation of the X-rays from Cygnus X-1 : Hard X-ray Time Lag

      MIYAMOTO Sigenori, KITAMOTO Shunji

        23   77 - 94   3 1989

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      Cygnus X-1 has long been known as a the black hole candidate, whose X-ray flux shows rapid variability on many time scales. Its X-rays have long been considered to be due to inverse Compton scattering of low energy photons by a high temperature plasma clound of 10^8&acd;10^9K situated near the black hole. In this case, time variations of high energy X-rays are expected to be delayed with respect to those of lower energy X-rays. Complex cross spectrum analysis of Cygnus X-1 data taken with the large area proportional counters (LAC) onboard Ginga revealed that the time delay of the high energy X-rays with respect to the lower energy X-rays increases from about 2 msec to several sec for periods from 0.1 sec to 300 sec. This result is inconsistent with the inverse Compton scattering model of Cygnus X-1. The time lag is different in its sign from those in the low mass (QPO) X-ray stars which contain neutron stars. This seems to be explained by the fact that the X-ray emitting plasma is heating up near the black hole and disappears suddenly into the black hole. The phase lag always showed similar time behavior even if the energy ranges and observing times were different, and its characteristic time constants were about 0.1 sec, 3 sec and 10 sec.

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    • The Observation of a Bright X-Ray Nova, GS2000+25,Discovered with The ASM

      TSUNEMI Hiroshi, KITAMOTO Shunji, OKAMURA Sadanori, ROUSSEL-DUPRE Diane

        23   29 - 37   3 1989

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      Language:Japanese   Publisher:Japan Aerospace Exploration Agency  

      We report here the discovery with the All Sky Monitor Detector on board the GINGA satellite of the X-ray transient, GS2000+25,which appeared in the constellation Vulpecula on 23 April, 1988. The maximum observed intensity was 12 Crab (1-6keV). Two stars in the X-ray error box appeared to increase from the epoch of the Palomar Observatory Sky Survey; one of these was confirmed to be the counterpart by optical spectra and radio measurements. The X-ray spectrum and light curve during the decay phase shows that it belongs to a class of ultra-soft sources which include black hole candidates like A 0620-00. A detailed comparison with A 0620-00 supports the identification of GS2000+25 as a possible new black hole candidate.

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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 - &   2 1989

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      Language:English   Publisher: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   11 1988

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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   16 9 1988

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      Language:Japanese   Publisher:一般社団法人日本物理学会  

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    • Application of Multilayer Reflectors to X-Ray Optic System for Cosmic X-Ray Observation

      YMASHITA Koujun, TSUNEMI Hiroshi, KITAMOTO Shunji, HATSUKADE Isamu, MIYAKE Akira, UENO Yoshihiro

        21   31 - 45   3 1988

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      Language:Japanese   Publisher:Japan Aerospace Exploration Agency  

      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.

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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   16 9 1987

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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   16 9 1987

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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   12 9 1986

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

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

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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   10 9 1984

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      Language:Japanese   Publisher:一般社団法人日本物理学会  

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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   12 3 1984

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      Language:Japanese   Publisher:一般社団法人日本物理学会  

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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   14 9 1982

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      Language:Japanese   Publisher:一般社団法人日本物理学会  

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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   14 9 1981

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      Language:Japanese   Publisher:一般社団法人日本物理学会  

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    Books and Other Publications

    • 宇宙まるごとQ&A

      北本俊二, 原田知広, 亀田真吾( Role: Joint author)

      理工図書  2 2021 

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    • 最新 宇宙学

      北本 俊二( Role: Joint author ,  第10章)

      裳華房  1 1 2004 

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      Language:Japanese Book type:Other

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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-

      ( Role: Other)

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

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      Language:Japanese Book type:Other

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    • 天体現象3Dシミュレーションソフト:太陽系大紀行

      ( Role: Other)

      講談社  4 2003 

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      Language:Japanese Book type:Other

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    • X線天文学で学ぶ物理の世界

      北本 俊二( Role: Other)

      メディア教育開発センター  1 1 2002 

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      Language:Japanese Book type:Other

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    • 宇宙スペクトル博物館<X線編>見えない星空への招待

      ( Role: Other)

      裳華房  4 1999 

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      Language:Japanese Book type:Other

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    • X線でさぐるブラックホール

      ( Role: Other)

      裳華房ポピュラーサイエンス  4 1998 

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      Language:Japanese Book type:Other

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    • The Hot Universe

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

      Springer  1998 

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    Professional Memberships

    • 1983 - Present 
      日本物理学会

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    • 1983 
      Th Astronomical Society of Japan

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    •  
      International Astronomical Union

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    Works

    • 回折限界X線望遠鏡の性能評価 Other

      4 2004
      -
      4 2005

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      Work type:Other  

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

      4 2002
      -
      4 2003

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    Research Projects

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

      科学研究費補助金 

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      4 2001 - Present

      Grant type:Competitive

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    • 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

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      4 2022 - 3 2025

      Grant number:22K03678

      Grant amount:\1170000 ( Direct Cost: \900000 、 Indirect Cost:\270000 )

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    • 銀河団の暗黒物質の直接測定の可能性の研究

      日本学術振興会  科学研究費助成事業 

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      4 2013 - 3 2015

      Grant type:Competitive

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    • 新型エックス線管長系の試作研究

      科学研究費助成事業 

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      4 2010 - 3 2012

      Grant type:Competitive

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

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

      日本学術振興会  科学研究費助成事業 

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      4 2007 - 3 2010

      Grant type:Competitive

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    • 多層膜と電荷結合素子の組み合わせによるエックス線偏光計の開発

      科学研究費助成事業 

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      4 2007 - 3 2009

      Grant type:Competitive

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    • Application of Space Database to Space Science Education

      Japan Society for the Promotion of Science  Grants-in-Aid for Scientific Research 

      NAGASE Fumiaki, EBISAWA Ken, KITAMOTO Syunji, YOSHIDA Atsumasa, MATSUZAKI Keiichi, TAMURA Takayuki, YAJI Kentaro, UNO Shinichiro, MATSUSHITA Kyoko, TSUBOI Yoko, HIRABAYASHI Hisashi, TSUJIMOTO Kunihiro, BAMBA Aya, MURAKAMI Hiroshi, KUBOTA Aya, IIZUKA Ryo, FURUTA Yutaka, HAYASHI Souichi, AYABE Syunji, YOSHIDA Kiyonori, NOGUCHI Satoru, KAWABATA Yoshiaki, MIYAWAKI Ryousuke, SAWADA Sayoko, IWAMOTO Hitomi, YOSHIDA Tessei, BABA Akitoshi, SUGAWARA Yasuharu, TOTSUKA Shota, ASAOKA Ikuko, SHINOHARA Hideo, YAGIHASHI Nobuyoshi, UZAWA Akiko, KUSUNOKI Shingo

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      2007 - 2009

      Grant number:19300270

      Grant amount:\12480000 ( Direct Cost: \9600000 、 Indirect Cost:\2880000 )

      We produced a teaching course material for young students to learn about high energy phenomena in space, using archival database obtained from high energy astronomical satellites. The teaching material consists of two parts ; the first part is a pamphlet of introduction to high energy astrophysics, history of X-ray astronomy, instruments and satellites for high energy observations, and guidance of the topics treated in this course. The second part is the main body of the course, distributed as a CD, which gives data analysis manual and discussion on the results for each scientific topic. This course includes scientific topics such as early type stars, supernova remnants, neutron stars, black-holes, dark-mater in clusters of galaxies. The CD includes both the data and software to be used for the analysis, thus readers can learn space science themselves using this CD on their own PCs.

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

      文部科学省  科学研究費助成事業 

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      4 2005 - 3 2007

      Grant type:Competitive

      公募

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    • 回折限界X線望遠鏡の性能評価

      JAXA  受託研究(一般受託研究) 

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      4 2004 - 3 2007

      Grant type:Competitive

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    • Studies on x-ray emission mechanisms of stars by a collisional-radiative model including effects of radiation transfer

      Japan Society for the Promotion of Science  Grants-in-Aid for Scientific Research 

      YAMAMOTO Norimasa, KOHMURA TAKAYOSHI, KITAMOTO SHUNJI, SHIBAZAKI NORIAKI

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      2004 - 2006

      Grant number:16540221

      Grant amount:\3100000 ( Direct Cost: \3100000 )

      Our research goal is to elucidate X-ray emission mechanisms of stars. To accomplish our study, at first we developed a new collisional-radiative model of stellar wind from stars including the radiation transfer. Next we applied our stellar wind model to the observed X-ray spectral lines with X-ray satellites to reveal the X-ray emitted region around stars, the density of the stellar wind, the temperature of the stellar wind, and so on.
      The result of our study is as follows.
      (1) Developments of a high precise collisional-radiative model of various helium-like (C, N, O, Ne, Mg, Si, S) ions. Inclusions of radiation transfer by Monte Carlo method are at a stage of a toy model.
      (2) Developments of a collisional-radiative model on KLM-shell Fe ions and applications to laboratory plasma. The model for Fe ions was applied to helical plasmas (large helical device (LHD) at the National Institute for Fusion Science) for highly precise modeling.
      (3) Constructions of a Doppler model including three components, the doppler shift derived from a velocity distribution of stellar winds, absorptions by mediums in stellar winds, and filling factors.
      (4) Analysis of early type stars obtained with X-ray satellites (Chandra and XMM-Newton) by the doppler model, and discussions of X-ray emission regions around stars. Furthermore X-ray emission spectra of stars by Suzaku satellite (launched in 2005) were analyzed. We obtained that x-ray emission regions of zeta-pup are near a star, on the other hand these of tau-sco are far from a star (Yamamoto et al.2007).
      We plan as follows, more precise analysis of x-ray emission spectra, a development from current toy model to a practical radiation transfer model, researches of practical non-equilibrium plasma model. Then, astronomical plasmas and solar plasmas are analyzed by the model.

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    • 見えない信号をキャッチせよ

      民間財団等  日産財団 

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      4 2004 - 3 2005

      Grant type:Competitive

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

      文部科学省  科学研究費助成事業 

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      4 2003 - 3 2005

      Grant type:Competitive

      公募

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    • ブラックホールの直接観測を目指した超高分解能X線望遠鏡の開発

      日本宇宙フォーラム  受託研究(一般受託研究) 

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      4 2003 - 3 2004

      Grant type:Competitive

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    • X線光学における能動光学系の応用

      科学研究費助成事業 

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      4 2002 - 3 2004

      Grant type:Competitive

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    • X線によるマゼラン星雲の星形成

      科学研究費助成事業 

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      4 1998 - 3 2002

      Grant type:Competitive

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    • 画素の小さなCCDの開発研究

      科学研究費助成事業 

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      4 1996 - 3 2001

      Grant type:Competitive

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    • 高効率・高分散X線分光器の開発研究

      日本学術振興会  科学研究費助成事業 

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      4 1997 - 3 1999

      Grant type:Competitive

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    • X-ray Astronomy Study with the ASCA Satellite

      Japan Society for the Promotion of Science  Grants-in-Aid for Scientific Research 

      NAGASE Fumiaki, TANAKA Yasuo, ISHIDA Manabu, TAKAHASHI Tadayiki, MITSUDA Kazuhisa, INOUE Hajime

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      1996 - 1998

      Grant number:08044103

      Grant amount:\9100000 ( Direct Cost: \9100000 )

      The purpose of this project is to perform observations and operations of ASCA in a collaboration between Japan and the United States of America, and to obtain scientific results from the X-ray observations on the X-ray binaries including compact objects, supernova remnants, active galactic nuclei, clusters of galaxies and the cosmic X-ray background. ASCA is the fourth Japanese X-ray satellite which was constructed in a collaboration between Japan and the U.S.A., and it was launched on February 20, 1993. The results of this project are summarized below :
      (1)We had national meetings and Japan-U.S.A.international meetings every year to select observation targets from the proposals, and discuss the organization of observation and operation of the satellite.
      (2)We examined the performance of the instruments onboard the satellite and provided the calibration database of the response of the instruments, including a time-dependent degradation of the performance of instruments.
      (3)We continuosly updated various software programs for data analysis, and produced an archival database for the convenience of international users.
      (4)We analyzed data from our own observations, and discussed the results with our partner country. These scientific results were presented at the international conferences and were published in academic journals.
      (5)All of the archival data were released to the scientists around the world with well-organized formats when the period of exclusive use by the owners expired.
      Because of the support by this grant-in-aid, we were able to perform well the ASCA observations and operations under the collaboration between Japan and the U.S.A.We obtained remarkable scientific results from the ASCA observations in various fields of X-ray astronomy.

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    • Development of an X-ray Poralimeter Using Direct X-ray Imaging CCD with Position, Energy and Time Resolution

      Japan Society for the Promotion of Science  Grants-in-Aid for Scientific Research 

      TSUNEMI Hiroshi, YAMAMOTO Kohei, HAYASHIDA Kiyoshi, KITAMOTO Syunji

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      1995 - 1996

      Grant number:07554002

      Grant amount:\21100000 ( Direct Cost: \21100000 )

      The purpose of this research project is to improve not only the fundamental properties of X-ray CCD but also as an X-ray polarimeter. The research group consists of the member s in Hamamatsu photnonics (HPK) and the members in Osaka university. According to the specification determined by all the members, the CCD chips were fabricated at HPK,and the university side operated and examined those chips.
      Several kinds of CCD chips using different material and production methods have been made. We got eventually energy resolution of 140 eV for 5.9 keV X-rays with a CCD chip of which pixel size is 12 mum and pixel number is 512x512. Although the resolution was 160 eV at the end of the first year in the research term, reduction of the dark current by 1/50 lead to the better resolution. Using high registivity material, we got a CCD chip of which depletion layr is as thick as 20 mum.
      University side activities include the development of CCD operation and evaluation ; 1) spectrometer system for measuing the CCD detection efficiency for 0.4-2.2keV X-rays, 2) CCD drive clock to suppress spurious charge noise, 3) high speed read-out system using DSP,4) simulation code for X-ray absorption and charge collection process within CCD.Adding these, we invented a novel method for measuring detection efficiency for sub-pixel size structure by employing a mesh in front of the CCD chip. We also measured polarization degree of the X-ray beam from a laboratory X-ray generator. CCD chips with pixel size of 6 mum, which should be effective for X-ray polarimetry, were started to fabricate. The polarimeter-capability of those small pixel size CCD will be measured within the year of 1997.

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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

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      1995 - 1995

      Grant number:07222208

      Grant amount:\1700000 ( Direct Cost: \1700000 )

      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 - 1994

      Grant number:06233214

      Grant amount:\1600000 ( Direct Cost: \1600000 )

      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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    • X-Ray Astronomy Study with the Astro-D Satellite

      Japan Society for the Promotion of Science  Grants-in-Aid for Scientific Research 

      NAGASE Fumiaki, DOTANI Takayasu, ISHIDA Manabu, KII Tsuneo, ITOH Masayuki, MATSUOKA Masaru, SHIBAZAKI Noriaki, OHASHI Takaya, KUNIEDA Hideyo, TAWARA Yujuru, KITAMOTO Shunji, MIHARA Tatehiro, TANAKA Yasuo, CANIZARES C., RICKER G., TSURU Takeshi, AWAKI Hisamitsu, KAWAI Nobuyuki, YOSHIDA Atsumasa, SERLEMITSOS P., HAYASHIDA Kiyoshi, BREON S., EBISAWA Ken, VOLZ S.v., KELLEY R., HELFAND D., MCCAMMON, TSUNEMI Hiroshi, MAKISHIMA Kazuo, MITSUDA Kazuhisa, MURAKAMI Toshiaki, KOYAMA Katsuji, YAMASHITA Koujun, OGAWARA Yoshiaki, MIYAMOTO Shigenori, MUSHOTZKY R., MAKINO Fumiyashi, HOLT S., INOUE Hajime

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      1992 - 1994

      Grant number:04044167

      Grant amount:\11600000 ( Direct Cost: \11600000 )

      ASCA (ASTRO-D), the fourth X-ray astronomy satellite of ISAS,was successfully launched on February 20,1993. It carries nested thin-foil X-ray mirrors providing a large effective area over a wide energy range from 0.5 to 10keV.A set of CCD cameras and imaging gas scintillation proportional counters are placed on the focal plane. ASCA is a high-throughput imaging and spectroscopic X-ray observatory with these instruments.
      An extensive collaboration between Japanese and U.S.scientists has been carried out in the joint developments of the X-ray telescopes, the X-ray CCD cameras, and computer software. It is continuing in the maintenance and the in-flight calibration of the instruments, and also in the data analysis and the following scientific activities.
      ASCA is an X-ray astronomy observatory which is, for the first time, capable of performing imaging and spectroscopic observations simultaneously over a wide energy range 0.5-10keV.The ASCA instruments cover the most important energy band for plasma diagnostics, because all the K-lines and the K-absorption edges from oxygen through iron at various ionization stages lie within this band. The CCD camera of ASCA can resolve all major lines individually. Motion of plasma of the order or greater than 1000km/s can be measured significantly from Doppler shift of the line energies. These capabilities of ASCA allow diagnostics of accreting matter around such compact objects as neutron stars and black holes. Spatially-resolved spectroscopy with ASCA also provides powerful means for the investigations of extended plasmas in supernova remnants, galaxies, and clusters of galaxies.
      The key elements of ASCA are succesfully working in orbit. ASCA has already obtained several remarkable scientific results. Most of them are due to the Japan-US collaboration with the help of this International Scientific Research Program as A Grant-in Aid for Scientific Research.

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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

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      1993 - 1993

      Grant number:05242214

      Grant amount:\2500000 ( Direct Cost: \2500000 )

      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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    • High Energy Transient Experiment

      Japan Society for the Promotion of Science  Grants-in-Aid for Scientific Research 

      MATSUOKA Masaru, HATSUKADE Isamu, TAKAGISHI Kunio, KITAMOTO Shunji, TSUNEMI Hiroshi, KOHNO Tsuyoshi, IMAI Takashi, YAMAUCHI Makoto, YOSHIDA Atsumasa, KAWAI Nobuyuki, RICKER George, FENIMORE Wdward E.

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      1991 - 1993

      Grant number:03044162

      Grant amount:\6000000 ( Direct Cost: \6000000 )

      It has become increasingly apparent that origin of cosmic gamma-ray bursts (CGBs) can only be determined by identifying burster counterparts in other energy ranges. To date, slightly over half a dozen CGBs have positions determined to 10 square arc-minutes or better. Although the burst and transient experiment on the Gamma-Ray Observatory are greatly increasing the number of known burst sources and provide fundamentally new information on their distribution over the sky, the accuracy of source locations it provides to be at best in the -1 degree range. Infrared, optical and soft X-ray searches have not revealed any convincing candidates for these CGBs. Even apart from the important information which such observations convey about the physics of CGB sources, they can in principle serve the important function of bridging the gap between the relatively large (-several arc-minutes in size) gamma-ray error boxes and the very small (-a few arc-seconds in size) boxes needed to conduct deep optical searches (> 25th magnitude) for the exceedingly faint quiescent burster counterparts. For all searches to date, questions concerning possible proper motion, the association between the putative optical and gamma-ray emission and the time structure of the optical transient event, remain unanswered. The high energy transient experiment project was internationally organized to reach an integrated approach to resolving these and other fundamental questions about CGBs and other astronomical transients.
      Considering these situations, this project promotes the international specific satellite which contains three scientific instruments ; an omnidirectional gamma-ray spectrometer (France-CESR), a wide-field X-ray monitor (Japan- RIKEN), and an ultraviolet transient camera array. (USA-MIT) This satellite is scheduled to be launched by NASA Pegasus rocket in April-May, 1995. We have to communicate various information internationally to promote this satellite. We have meetings and do tests to adjust collaboration and interfaces of instruments.

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    • Study of Hard X-rays and gamma -rays from AGN's aboard Balloons

      Japan Society for the Promotion of Science  Grants-in-Aid for Scientific Research 

      KAMAE Tsuneyoshi, BRAGA J., DUROUCHOUX P., MICHAELSON P., SADOULET B., EDBERG T., CORREA R., WEISKOPF M., TAKAHASHI Yoshiyuki, NOMACHI Masaharu, IKEDA Hirokazu, OHTA Shigeo, AKIYAMA Hiromitsu, YAMAGAMI Takamasa, YAJIMA Nobuyuki, TAKAHASHI Tadayuki

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      1991 - 1993

      Grant number:03041022

      Grant amount:\30000000 ( Direct Cost: \30000000 )

      We have been developing a new hard X-ray/Gamma-ray(40keV - 800keV)detector, Welcome-1. Its characteristic is the low-background counts, which is very important factor of the balloon or satellite-borne detector. The detector utilizes the well-type phoswich counter and the compound-eye configuration. Based on the experience with the Welcome -1 detector launched from Brazil, we have improved the detector. In order to obtain higher sensitivity along the line we have pursued, we have reduced the background by narrowing the opening angle of the detector and replacing the main scintillation detector from GSO to Nal.
      We performed the balloon-borne experiment at Sanriku, Japan on June 5, 1993. Dr. Tim Edberg was invited as a co-investigator. We observed Crab Nebuula/Pulsar for three hours. Signal to noise ration at the energy range from 50keV to 150 keV exceeds 1.5 in which the flux from the source is reduced to 1/3 by tghe air-attenuation. This S/N ration is the highest among the hard X-ray detectors launched so far. In order to discuss, the feasibility and possible procedures for the future collaborative balloon campaign, we went abroad and discussed with the chair person at several institutes.

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    • An Basic Study for a Transmission Grating with Reduced 0th Order Light

      Japan Society for the Promotion of Science  Grants-in-Aid for Scientific Research 

      KITAMOTO Sunji

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      1991 - 1992

      Grant number:03804009

      Grant amount:\1600000 ( Direct Cost: \1600000 )

      A new transmission grating is developed. So far crystals and gratings have been used fro a dispersive elements in spectrometers for X-rays. The crystals provide high spectral resolution, but the observation effeciency for a certain energy band is small. The reflective gratings have a good efficiency near the brazed wave length. But in order to apply it for the X-rays above 2 ke V a large area is required. The transmission grating is one of the most interesting device for the spectrometer for X-rays above 2 keV. However, the big disadvantage of the transmission grating is its inefficiency into the dispersed light (10.13% for each first order). One of the reason of the inefficiency is that the braze-angle could not be introduced for a transmission grating.
      In this research, I introduce a new idea for the transmission grating in order to improve the efficiency to the first order light. The introduction of one reflection in the transmission grating can resemble a braze-angle, and make the 0th order light reduced, and the first order light emphasized. Computer simulation demonstrated these performances. Furthermore, experiments using a visible light also showed the grate advantage of this new transmission grating.

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    • Japan-U. K. Collaboration in X-ray Astronomy Research with the Scientific Satellite "Ginga"

      Japan Society for the Promotion of Science  Grants-in-Aid for Scientific Research 

      TANAKA Yasuo, TAHARA Yuzuru, KUNIEDA Hideyo, ITOH Masayuki, DOTANI Tadayasu, MITSUDA Kazuhisa, KII Tsuneo, TSUNEMI Hiroshi, SHIBAZAKI Noriaki, MAKISHIMA Kazuo, MURAKAMI Toshio, INOUE Hajime, NAGASE Fumiaki, MATSUOKA Masasu, KOYAMA Katsuji, YAMASHITA Koujun, OGAWARA Yoshiki, MIYAMOTO Shigenori, MAKINO Fumiyoshi, HAYASHIDA Kiyoshi, KITAMOTO Shunji, COOKE B. A., WATSON M. G., WARWICK R. S., STEWART G. S., OHASHI Takaya, KAWAI Nobuyuki, POUNDS K. A., TURNER M. J. L, YOSHIDA Atsumasa, ISHIDA Manabu, TENNANT A., MCHARDY I., WILLIAMS R., CRUISE M., PATCHET B., MASON K. O., MUKAI K., FABIAN A.

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      1989 - 1991

      Grant number:01044145

      Grant amount:\10800000 ( Direct Cost: \10800000 )

      The fiscal year of 1991 has become the end of mission life of the Ginga satellite, which stayed in the orbit for 4 years and 9 months since the launch on February 5 1987. The orbit of Ginga continued to decay, until October 30 1991 when the last contact was made with the satellite. It is believed that Ginga re-entered the atmosphere on November 1 or so. Under these circumstances, two scientists from Japan visited the United Kingdom on three occasions, and two UK scientists visited Japan on three occasions as well. Principal results of collaboration in the present fiscal year include the following three items.
      (1)The scientists from, both parties closely collaborated on the Ginga operation during the last phase of its mission life. In particular, the Large Area Proportional Counter, a UK-Japan joint experiment serving as the main instrument of Ginga, has been calibrated in detail to demonstrate that its performance stayed constant during the entire mission life.
      (2)The entire Ginga data are stored both in Japan and UK, and will continue to be of precious scientific valuable for the entire world. Discussion was therefore made to establish an appropriate scheme to make these archival data open to public, especially to scientists of other countries.
      (3)Joint data analysis was made on several research topics, followed by preparations of joint papers. The topics include cosmic X-ray background, active galactic nuclei, X-ray pulsars, X-ray emitting white dwarfs, and so on.

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    • A Long term time variation of the X-rays from binary X-ray stars.

      Japan Society for the Promotion of Science  Grants-in-Aid for Scientific Research 

      MIYAMOTO Sigenori, KITAMOTO Shunji, TSUNEMI Hiroshi

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      1988 - 1989

      Grant number:63540197

      Grant amount:\1100000 ( Direct Cost: \1100000 )

      Time variation of X-rays from binary X-ray stars are observed with the all sky monitor, (ASM) and the large area counters (LAC) onboard GINGA. With ASM we found more than 13 so-called X-ray novas. Among these, there are GS2000+25 and GS2023+338, which seem to be black hole candidates because of their time variations and energy spectra of X-rays. We also studied the X-ray time variations of Cygnus X-1 and GX339-4, which were also black hole candidates.
      We discovered GS2023+25 on 26th April 1989. Its whole behavior from the appearance to the disappearance was very similar to the black hole candidate X- ray star AO620-00.
      GS2023+338 was discovered on 21st May 1989. This source showed very large, short and long term time variations up to the factor of about 500 before 1st of June. After this time, this source showed rapid time variations which was very similar to those of Cygnus X-1 in its low state. The power density spectrum and the lag time structure of its time variations were similar to those of Cygnus X-1.
      Cygnus X-1 was observed with LAC, and we found the structure of the time lag of the time variations can not be explained by the Compton scattering model, which had been assumed to explain the energy spectrum of this source. We also found there were two characteristic time constants of about 0.2 sec and 0.7 sec, with which we could reproduce the power density spectrum and phase lag structure of X-rays from this source.
      We found there existed very high state in GX339-4 from the observation with ASM. We also observed this source with LAC and found the phase lag structure could be explained by the existence of the Compton scattering cloud of the size of about 2 10^9cm. Based on this fact we proposed a jet model which can explain the energy spectrum and the phase lag structure of this source.

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    • A Research for High Efficiency X-Ray Spectrometers Using Multilayers

      Japan Society for the Promotion of Science  Grants-in-Aid for Scientific Research 

      KITAMOTO Shunji, YAMASHITA Koujun

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      1987 - 1988

      Grant number:62540190

      Grant amount:\1700000 ( Direct Cost: \1700000 )

      For a high efficiency X-ray spectrometer, we introduced a new method using etalon. Multilayers have a merit which can be freely designed the structure. Inserting a spacer between regularly piled layers, we can make a etalon. Furthermore, we can control the characteristics of the reflectivity of etalon, changing the thickness of the spacer. Using suitable etalons, we can get a fourier transformed signals of the X-ray spectrum and we can reconstruct the X-ray spectrum with inverse fourier transforms of the signals. We showed the validity of this method by a computer simulation.
      To get a basic data of the multilayers, we fabricated various thickness multilayers consisting of Ni and C, and evaluated the reflectivity. We found that it is difficult to make a high reflectivity multilayers with the thickness of less than 100A and found that its cause is roughness of the layers of about 10A (r.m.s). On the basis of this results, we fabricated etalons consisting Ni and C and evaluated the characteristics of reflectivity using characteristic X-rays and synchrotron orbital radiators. We found that the etalons have a roughly designed characteristics.
      We also developed a position sensitive proportional counter and evaluated its characteristics. We found that our position sensitive proportional counter has about 2 mm position resolution and 18% energy resolution for 5.9 keV X-rays. It is possible to make a high efficiency X-ray spectrometer using our position sensitive proportional counter and etalons.

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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

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      1987 - 1987

      Grant number:62041110

      Grant amount:\3600000 ( Direct Cost: \3600000 )

      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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    • Application of Multilayer Reflectors to Spectroscopic and Instruments for Cosmic X-Ray Observation

      Japan Society for the Promotion of Science  Grants-in-Aid for Scientific Research 

      YAMASHITA Koujun, KITAMOTO Shunji, TSUNEMI Hiroshi, MIYAMOTO Shigenori

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      1985 - 1987

      Grant number:60420004

      Grant amount:\31300000 ( Direct Cost: \31300000 )

      Development of multilayer reflectors makes it possible to apply to the grazing and normal incidence X-ray optic system for the comsic 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 geometrical configuration. The normal incidence X-ray telescope is attainable in the energy range below 0.4keV, though the sensitive energy hand is limited by Bragg condition estimated form 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 an electro beam evaporation in method ultrahigh vacuum. Material combinations are Mo/C, Mo/Si and Ni/C with 5-20 layer pairs and the layer thickness of 36-100A. 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 the Bragg angle of the reflection order with four characteristic X-rays of Cu-K<alpha>(1.54A), Si-K<alpha> (7.13A), Al-K<alpha>(8.34A), C-K<alpha>(44.7A). Further investigations are carried out with the monochromatized synchrotron radiation in 14-250A band at Photon Factory, National Laboratory for High Energy Physics, and at UVSOR, Institute for Molecular Science. The peak reflectivity of Cu-K<alpha> is obtained to be 80% for Mo/C in the grazing incidence and that of <lambda>160A to be more than 30% for Mo/Si in the near normal incidence.

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    • 軟X線光学、軟X線検出器

      科学研究費補助金 

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      Grant type:Competitive

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    • X線分光測定装置

      北本俊二

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      Applicant:JST

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

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