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  2. Keiichi Matsuzaki

Keiichi Matsuzaki

  (松崎 恵一)

Profile Information

Affiliation
Japan Aerospace Exploration Agency
J-GLOBAL ID
202001007325831201
researchmap Member ID
R000009366

Research Interests

 8

Papers

 34
  • MIURA Akira, MATSUZAKI Keiichi, ISHIDA Takayuki, TANAKA Masamitsu, INOUE Koji
    JAXA Research and Development Report: Journal of Space Science Informatics Japan, JAXA-RR-22-009(12) 31-40, Feb 28, 2023  Peer-reviewed
    This paper describes a method of interactive visualization for explaining the behavior of Single Flux Quantum (SFQ) circuits, a kind of logic circuit based on the principle of superconductivity. For the space exploration in the future, there has been an idea to develop devices based on SFQ circuits onboard spacecraft. SFQ circuits are expected to have extremely low power consumption and high computational speed during operation. On the other hand, since the principle of SFQ circuits is greatly different from that of logic circuits of semiconductor devices such as CPUs and memories, visualization tools for understanding such type of circuits are expected to be useful. In this paper we developed an interactive visualization application for SFQ circuits using JavaScript libraries including WebGL-based APIs and discussed issues as well as prospects.
  • Nishimura Kayoko, Matsuzaki Keiichi, Shimokawa Yuki, Yatagai Hiroshi, Miyano Yoshikazu
    JAXA Research and Development Report: Journal of Space Science Informatics Japan, JAXA-RR-14-009(4) 1-13, Mar 31, 2015  Peer-reviewedCorresponding author
  • Yoshino Akira, Inada Kuriko, Matsuzaki Keiichi, Yamauchi Chisato
    JAXA Research and Development Report: Journal of Space Science Informatics Japan, JAXA-RR-14-009(4) 105-125, Mar 31, 2015  Peer-reviewed
    DARTS (http://darts.jaxa.jp/) is a scientific data archive system which provides data of scientific satellites launched by JAXA, and is developed and maintained by Center for Science-satellite Operation and Data Archive (C-SODA) in ISAS/JAXA. We have developed a web interface with search function to provide 2 dimensional image data (all-sky map) obtained from all sky survey observation of infrared astronomy satellite “AKARI”. The all-sky map is composed of many image files which are arranged like as tiles to cover whole celestial sphere and each image occupies a region about several square degrees. This search function is intended to return all image files in the region designated by a user, if they are overlapped with the region. To realize such a search, we adopt a method that each image is divided into a large number of small rectangular areas and then the center of each area is represented by an orthogonal coordinate system to register in the database. This method has the advantages that other external libraries to divide the celestial area such as HEALPix are not needed, and that both celestial poles is not treated as a singular point, and that high-speed search for arbitrary coordinate system can be obtained. To reduce the costs of development and maintenance, we apply the mechanism of AKARI catalogue search to this search function using PHP and PostgreSQL.
  • Nishimura Kayoko, Matsuzaki Keiichi, Miyazawa Hideyuki, Takaki Ryoji, Yamashita Miwako, Miyano Yoshikazu, Fukuda Seisuke, Baba Hajime, Nagamatsu Hiroyuki, Yamada Takahiro
    JAXA Research and Development Report: Journal of Space Science Informatics Japan, JAXA-RR-13-010(3) 17-26, Mar 31, 2014  Peer-reviewedCorresponding author
    GSTOS is Generic Spacecraft Test and Operations Software applied for test and operation system of future ISAS (Institute of Space and Aeronautical Science) spacecraft based on database SIB2 (Spacecraft Information Base version 2). SIB2/GSTOS-1 is a project to provide SIB2/GSTOS for SPRINT-A, ASTRO-H, Bepi/MMO. This paper describes goal, achievement relative to typical test and operation system for former ISAS spacecraft, development status and tasks for the future of SIB2/GSTOS-1.
  • Y. Katsukawa, K. Ichimoto, Y. Suematsu, H. Hara, R. Kano, T. Shimizu, K. Matsuzaki
    SOLAR PHYSICS AND SPACE WEATHER INSTRUMENTATION V, 8862, 2013  Peer-reviewed
    We present a design progress of the Solar UV-Vis-IR Telescope (SUVIT) aboard the next Japanese solar mission SOLAR-C. SUVIT has an aperture diameter of similar to 1.4 m for achieving spectro-polarimetric observations with spatial and temporal resolution exceeding the Hinode Solar Optical Telescope (SOT). We have studied structural and thermal designs of the optical telescope as well as the optical interface between the telescope and the focal plane instruments. The focal plane instruments are installed into two packages, filtergraph and spectrograph packages. The spectropolarimeter is the instrument dedicated to accurate polarimetry in the three spectrum windows at 525 nm, 854 nm, and 1083 nm for observing magnetic fields at both the photospheric and chromospheric layers. We made optical design of the spectrograph accommodating the conventional slit spectrograph and the integral field unit (IFU) for two-dimensional coverage. We are running feasibility study of the IFU using fiber arrays consisting of rectangular cores.
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Misc.

 20
  • 成影典之, 岡光夫, 深沢泰司, 松崎恵一, 渡辺伸, 坂尾太郎, 萩野浩一, 三石郁之, 水野恒史, 篠原育, 川手朋子, 下条圭美, 高棹真介, 金子岳史, 田辺博士, 上野宗孝, 高橋忠幸, 高島健, 太田方之
    日本天文学会年会講演予稿集, 2022, 2022  
  • 成影典之, 岡光夫, 深沢泰司, 松崎恵一, 渡辺伸, 坂尾太郎, 萩野浩一, 三石郁之, 水野恒史, 篠原育, 川手朋子, 下条圭美, 高棹真介, 金子岳史, 田辺博士, 上野宗孝, 高橋忠幸, 高島健, 太田方之
    日本天文学会年会講演予稿集, 2021, 2021  
  • Noriyuki Narukage, Mitsuo Oka, Yasushi Fukazawa, Keiichi Matsuzaki, Shin Watanabe, Taro Sakao, Kouichi Hagino, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Iku Shinohara, Masumi Shimojo, Shinsuke Takasao, Hiroshi Tanabe, Munetaka Ueno, Tadayuki Takahashi, Takeshi Takashima, Masayuki Ohta
    Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray, Dec 13, 2020  
  • Makoto S. Tashiro, Hironori Maejima, Kenichi Toda, Richard L. Kelley, Lillian Reichenthal, Leslie Hartz, Robert Petre, Brian J. Williams, Matteo Guainazzi, Elisa Costantini, Ryuichi Fujimoto, Kiyoshi Hayashida, Joy Henegar-Leon, Matt Holland, Yoshitaka Ishisaki, Caroline Kilbourne, Mike Loewenstein, Kyoko Matsushita, Koji Mori, Takashi Okajima, F. Scott Porter, Gary Sneiderman, Yoh Takei, Yukikatsu Terada, Hiroshi Tomida, Hiroya Yamaguchi, Shin Watanabe, Hiroki Akamatsu, Yoshitaka Arai, Marc Audard, Hisamitsu Awaki, Iurii Babyk, Aya Bamba, Nobutaka Bando, Ehud Behar, Thomas Bialas, Rozenn Boissay-Malaquin, Laura Brenneman, Greg Brown, Edgar Canavan, Meng Chiao, Brian Comber, Lia Corrales, Renata Cumbee, Cor de Vries, Jan-Willem den Herder, Johannes Dercksen, Maria Diaz-Trigo, Michael DiPirro, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Carlo Ferrigno, Yutaka Fujita, Yasushi Fukazawa, Akihiro Furuzawa, Luigi Gallo, Nathalie Gorter, Martin Grim, Liyi Gu, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, David Hawthorn, Katsuhiro Hayashi, Natalie Hell, Junko Hiraga, Edmund Hodges-Kluck, Takafumi Horiuchi, Ann Hornschemeier, Akio Hoshino, Yuto Ichinohe, Sayuri Iga, Ryo Iizuka, Manabu Ishida, Naoki Ishihama, Kumi Ishikawa, Kosei Ishimura, Tess Jaffe, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Steven Kenyon, Mark Kimball, Takao Kitaguti, Shunji Kitamoto, Shogo Kobayashi, Akihide Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Muzi Li, Tom Lockard, Yoshitomo Maeda, Maxim Markevitch, Connor Martz, Hironori Matsumoto, Keiichi Matsuzaki, Dan McCammon, Brian McLaughlin, Brian McNamara, Joseph Miko, Eric Miller, Jon Miller, Kenji Minesugi, Shinji Mitani, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Hideto Nakamura, Kazuhiro Nakazawa, Chikara Natsukari, Kenichiro Nigo, Yusuke Nishioka, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Mina Ogawa, Takaya Ohashi, Masahiro Ohno, Masayuki Ohta, Atsushi Okamoto, Naomi Ota, Masanobu Ozaki, Stephane Paltani, Paul Plucinsky, Katja Pottschmidt, Michael Sampson, Takahiro Sasaki, Kosuke Sato, Rie Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Yasuko Shibano, Maki Shida, Megumi Shidatsu, Shuhei Shigeto, Keisuke Shinozaki, Peter Shirron, Aurora Simionescu, Randall Smith, Kazunori Someya, Yang Soong, Keisuke Sugawara, Yasuharu Sugawara, Andy Szymkowiak, Hiromitsu Takahashi, Toshiaki Takeshima, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Hiroyuki Uchida, Yuusuke Uchida, Hideki Uchiyama, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Tomomi Watanabe, Michael Wittheof, Rob Wolfs, Shinya Yamada, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Keiichi Yanagase, Tahir Yaqoob, Susumu Yasuda, Tessei Yoshida, Nasa Yoshioka, Irina Zhuravleva
    Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray, Dec 13, 2020  
  • Hironori Maejima, Lorella Angelini, Elisa Costantini, Mark R. Edison, Jan-Willem den Herder, Yoshitaka Ishisaki, Kyoko Matsushita, Koji Mori, Matteo Guainazzi, Richard L. Kelley, Kenichi Toda, Lillian S. Reichenthal, James V. Lobell, Robert Petre, Ryuichi Fujimoto, Martin Grim, Kiyoshi Hayashida, Stéphane Paltani, Gary A. Sneiderman, Yoh Takei, Yukikatsu Terada, Hiroshi Tomida, Makoto S. Tashiro, Hiroki Akamatsu, Yoshitaka Arai, Hisamitsu Awaki, Iurii 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, 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 Kitaguti, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Shu Koyama, Aya Kubota, Maurice A. Leutenegger, Tom Lockard, Mike Loewenstein, Yoshitomo Maeda, Lynette Marbley, Maxim Markevitch, Hironori Matsumoto, Keiichi Matsuzaki, Dan McCammon, Brian McNamara, Joseph Miko, Eric Miller, Jon Miller, Kenji Minesugi, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Hideyuki Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Hideto Nakamura, Shinya Nakashima, Kazuhiro Nakazawa, Chikara Natsukari, Kenichiro Nigo, Yusuke Nishioka, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Mina Ogawa, Takaya Ohashi, Masahiro Ohno, Masayuki Ohta, Takashi Okajima, Atsushi Okamoto, Michitaka Onizuka, Naomi Ota, Masanobu Ozaki, Paul Plucinsky, F. Scott Porter, Katja Pottschmidt, Kosuke Sato, Rie Sato, Makoto Sawada, Hiromi Seta, Ken Shelton, Yasuko Shibano, Maki Shida, Megumi Shidatsu, Peter Shirron, Aurora Simionescu, Randall Smith, Kazunori Someya, Yang Soong, Yasuharu Suagawara, Andy Szymkowiak, Hiromitsu Takahashi, Toru Tamagawa, Takayuki Tamura, Takaaki Tanaka, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Hiroyuki Uchida, Hideki Uchiyama, Yoshihiro Ueda, Shinichiro Uno, Thomas Walsh, Shin Watanabe, Brian Williams, Rob Wolfs, Michael Wright, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Y. Yamasaki, Shigeo Yamauchi, Makoto Yamauchi, Keiichi Yanagase, Tahir Yaqoob, Susumu Yasuda, Nasa Yoshioka, Jaime Zabala, Zhuravleva Irina, Yutaka Fujita
    Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray, 10699, Jul 6, 2018  
    © 2018 SPIE. The ASTRO-H mission was designed and developed through an international collaboration of JAXA, NASA, ESA, and the CSA. It was successfully launched on February 17, 2016, and then named Hitomi. During the in-orbit verification phase, the on-board observational instruments functioned as expected. The intricate coolant and refrigeration systems for soft X-ray spectrometer (SXS, a quantum micro-calorimeter) and soft X-ray imager (SXI, an X-ray CCD) also functioned as expected. However, on March 26, 2016, operations were prematurely terminated by a series of abnormal events and mishaps triggered by the attitude control system. These errors led to a fatal event: the loss of the solar panels on the Hitomi mission. The X-ray Astronomy Recovery Mission (or, XARM) is proposed to regain the key scientific advances anticipated by the international collaboration behind Hitomi. XARM will recover this science in the shortest time possible by focusing on one of the main science goals of Hitomi,"Resolving astrophysical problems by precise high-resolution X-ray spectroscopy".1 This decision was reached after evaluating the performance of the instruments aboard Hitomi and the mission's initial scientific results, and considering the landscape of planned international X-ray astrophysics missions in 2020's and 2030's. Hitomi opened the door to high-resolution spectroscopy in the X-ray universe. It revealed a number of discrepancies between new observational results and prior theoretical predictions. Yet, the resolution pioneered by Hitomi is also the key to answering these and other fundamental questions. The high spectral resolution realized by XARM will not offer mere refinements; rather, it will enable qualitative leaps in astrophysics and plasma physics. XARM has therefore been given a broad scientific charge: "Revealing material circulation and energy transfer in cosmic plasmas and elucidating evolution of cosmic structures and objects". To fulfill this charge, four categories of science objectives that were defined for Hitomi will also be pursued by XARM; these include (1) Structure formation of the Universe and evolution of clusters of galaxies; (2) Circulation history of baryonic matters in the Universe; (3) Transport and circulation of energy in the Universe; (4) New science with unprecedented high resolution X-ray spectroscopy. In order to achieve these scientific objectives, XARM will carry a 6 × 6 pixelized X-ray micro-calorimeter on the focal plane of an X-ray mirror assembly, and an aligned X-ray CCD camera covering the same energy band and a wider field of view. This paper introduces the science objectives, mission concept, and observing plan of XARM.
  • Asai Ayumi, Hara Hirohisa, Watanabe Tetsuya, Imada Shinsuke, Kamio Suguru, Matsuzaki Keiichi, Sakao Taro, Narukage Noriyuki, Hinode EIS team
    Meeting Abstracts of the Physical Society of Japan, 64 202-202, 2009  
  • HARA Hirohisa, WATANABE Tetsuya, MATSUZAKI Keiichi, HARRA Louise K., CULHANE J. Leonard, CARGILL Peter, MARISKA John T., DOSCHEK George A.
    Publications of the Astronomical Society of Japan, 60(2) 275-284, Apr 25, 2008  
  • DERE Kenneth P., DOSCHEK George A., MARISKA John T., HANSTEEN Viggo H., HARRA Louise K., MATSUZAKI Keiichi, THOMAS Roger J.
    Publications of the Astronomical Society of Japan, 59(3) S721-S726, Nov 30, 2007  
  • MATSUZAKI Keiichi, HARA Hirohisa, WATANABE Tetsuya, DERE Kenneth P., BROWN Charles M., CULHANE Len
    Publications of the Astronomical Society of Japan, 59(3) S683-S689, Nov 30, 2007  
  • T. Kosugi, K. Matsuzaki, T. Sakao, T. Shimizu, Y. Sone, S. Tachikawa, T. Hashimoto, K. Minesugi, A. Ohnishi, T. Yamada, S. Tsuneta, H. Hara, K. Ichimoto, Y. Suematsu, M. Shimojo, T. Watanabe, S. Shimada, J. M. Davis, L. D. Hill, J. K. Owens, A. M. Title, J. L. Culhane, L. K. Harra, G. A. Doschek, L. Golub
    SOLAR PHYSICS, 243(1) 3-17, Jun, 2007  
    The Hinode satellite (formerly Solar-B) of the Japan Aerospace Exploration Agency's Institute of Space and Astronautical Science (ISAS/JAXA) was successfully launched in September 2006. As the successor to the Yohkoh mission, it aims to understand how magnetic energy gets transferred from the photosphere to the upper atmosphere and results in explosive energy releases. Hinode is an observatory style mission, with all the instruments being designed and built to work together to address the science aims. There are three instruments onboard: the Solar Optical Telescope (SOT), the EUV Imaging Spectrometer (EIS), and the X-Ray Telescope (XRT). This paper provides an overview of the mission, detailing the satellite, the scientific payload, and operations. It will conclude with discussions on how the international science community can participate in the analysis of the mission data.
  • Uno Shinichiro, Kameyama Tetsuya, Horihata Masaki, Asano Norihisa, Ebisawa Ken, Tamura Takayuki, Kasaba Yasumasa, Shinohara Iku, Miyashita Yukinaga, Miura Akira, Matsuzaki Keiichi, Murakami Hiroshi, Furuzawa Fumie
    Journal of social and information sciences, Nihon Fukushi University, 10 1-9, Mar 30, 2007  
    We report on the current status of our astronomical data sonification project. This project aims to sonify astronomical data, that is, to convert a visual medium into an audio medium for both scientists and the visually impaired. We hope that sonification can lead to a new way of conceptualizing scientific data. The primary sources of the data used for this project come from Japanese satellites dedicated to X-ray astronomy and geophysics. This project is performed in collaboration with Nihon Fukushi University and the Center for Planning and Information Systems (PLAIN center) of the Japan Aerospace Exploration Agency (JAXA) Institute of Space and Astronautical Science (ISAS). Our project began in March 2006. Since this time we have sonified astronomical data sets, including data from X-ray pulsars, and have published these results. In this paper we also discuss future plans for the project, as well as its implications for visually impaired scientists and public.
  • 坂東貴政, 鹿野良平, 古徳純一, 下条圭美, 坂尾太郎, 松崎恵一, 常田佐久
    日本天文学会年会講演予稿集, 2007, 2007  
  • S Osone, K Makishima, K Matsuzaki, Y Ishisaki, Y Fukazawa
    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, 54(3) 387-392, Jun, 2002  
    An X-ray study was made to examine whether some part of the soft X-ray background is coming from hot gas in the Local Group. For this purpose, four consecutive pointings were made with ASCA toward a sky region between M 31 and M 33, which is close to the direction of the center of the Local Group. By comparing the X-ray surface brightness in this sky direction with that in another blank sky region near the north equatorial pole, an upper limit on any soft excess X-ray background was determined to be 2.8 x 10(-9) erg cm(-2) s(-1) sr(-1) with a 90% confidence level statistical error. Assuming an optically-thin thermal bremsstrahlung energy spectrum (Raymond-Smith model) for a temperature of 1 keV and a beta-model electron density distribution for a core radius of 100 kpc for the X-ray halo., the upper limit of the central plasma density was obtained to be 1.3 x 10(-4) cm(-3). The plasma column density is too low to contribute significantly to the observed quadrupole anisotropy in the cosmic microwave background.
  • M Sugizaki, K Mitsuda, H Kaneda, K Matsuzaki, S Yamauchi, K Koyama
    ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 134(1) 77-102, May, 2001  
    The X-ray emission from the central region of the Galactic plane, \l\ less than or similar to 45 degrees and \b\ less than or similar to 0.degrees4, was studied in the 0.7-10 keV energy band with a spatial resolution of similar to3' with the Advanced Satellite for Cosmology and Astrophysics (ASCA) observatory. We developed a new analysis method for the ASCA data to resolve discrete sources from the extended Galactic ridge X-ray emission (GRXE). We successfully resolved 163 discrete sources with an X-ray flux down to 10(-12.5) ergs cm(-2) s(-1) and determined the intensity variations of the GRXE as a function of the Galactic longitude with a spatial resolution of about 1 degrees. The longitudinal intensity variation in the energy band above 4 keV, for which there is little absorption in the Galactic plane, shows a large enhanced feature within \l\ less than or similar to 30 degrees. This suggests a strong enhancement ment of X-ray emissivity of the GRXE inside the 4 kpc arm of the Galaxy. Searches for identifications of the resolved X-ray sources with cataloged X-ray sources and optical stars show that the 66% are unidentified. Spectral analysis of each source shows that a large number of the unidentified sources have hard X-ray spectra obscured by the Galactic interstellar medium. We classified the sources into several groups by the flux, the hardness and the softness of the spectra, and performed further detailed analysis for the spectra summed within each group. Possible candidates of X-ray origins of these unidentified sources are discussed based on the grouping spectral analysis. Also, we derived the log N-log S relations of the resolved sources in the energy bands below and above 2 keV separately. The log N-log S relation of the Galactic X-ray sources above 2 keV was obtained for the first time with this study. It is represented by a power-law with an index of -0.79 +/- 0.07 after correction for the contribution of extragalactic X-ray sources. This flat power-law relation suggests that the spatial distribution of the X-ray sources should have an armlike structure in which the solar system is included. The integrated surface brightness of the resolved sources is about 10% of the total GRXE in both energy bands. The approximately 90% of the emission remaining is still unresolved.
  • SEKIMOTO Yutaro, MATSUZAKI Keiichi, KAMAE Tuneyoshi, TATEMATSU Ken'ichi, YAMAMOTO Satoshi, UMEMOTO Tomofumi
    Publications of the Astronomical Society of Japan, 52(5) L31-L35, Oct 25, 2000  
  • M Sugizaki, K Matsuzaki, H Kaneda, S Yamauchi, K Mitsuda
    ASTRONOMISCHE NACHRICHTEN, 320(4-5) 383-383, 1999  
  • K. Matsuzaki, Y. Sekimoto, T. Kamae, S. Yamamoto, K. Tatematsu, T. Umemoto
    Astronomische Nachrichten, 320(4-5) 323-323, 1999  Peer-reviewed
  • Mutsumi Sugizaki, Fumiaki Nagase, Ken'ichi Torii, Kenzo Kinugasa, Tatsuhiko Asanuma, Keiichi Matsuzaki, Katsuji Koyama, Shigeo Yamauchi
    Publications of the Astronomical Society of Japan, 49(5) L25-L30, 1997  
    During a galactic-plane survey with ASCA in 1996 September, we detected a relatively bright, soft source at R.A. = 17h8m46.s6, DEC. = -40°9′27″ (J2000), and discovered an 11-s X-ray pulsation from the source. This source has been identified with the ROSAT source 1RXS J170849.0-400910. From a timing analysis of the source, we obtained a barycentric pulse period of P = 10.99759±0.00005 s with a broad sinusoidal shape of a pulse fraction of ∼ 30%. The energy spectrum in the 0.8-10 keV region is very soft, and can be fitted by a power-law model with a photon index of 3.5 and an absorption column density of 1.8 × 1022 cm-2. The observed pulse-phase-averaged flux in the range 0.8-10 keV is 4.3 × 10-11 erg cm-2 s-1, which corresponds to 1.7 × 10-10 erg cm-2 s-1 after correcting for soft X-ray absorption. During an observation interval of about 14 hr, neither a significant change in the pulsation period, nor a significant variation in the phase-averaged flux was detected. From these X-ray properties, we suggest that this newly discovered X-ray pulsar might be a member of a small subgroup of "anomalous" X-ray pulsars with a period close to 6-9 s.
  • Kazuo Makishima, Makoto Tashiro, Ken Ebisawa, Hajime Ezawa, Yasushi Fukazawa, Shuichi Gunji, Masaharu Hirayama, Eriko Idesawa, Yasushi Ikebe, Manabu Ishida, Yoshitaka Ishisaki, Naoko Iyomoto, Tsuneyoshi Kamae, Hidehiro Kaneda, Ken'ichi Kikuchi, Yoshiki Kohmura, Hidetoshi Kubo, Kyoko Matsushita, Keiichi Matsuzaki, Tatehiro Mihara, Ken'ichiro Nakagawa, Takaya Ohashi, Yoshitaka Saito, Yutaro Sekimoto, Tadayuki Takahashi, Takayuki Tamura, Takeshi Tsuru, Yoshihiro Ueda, Noriko Y. Yamasaki
    Publications of the Astronomical Society of Japan, 48(2) 171-189, 1996  Peer-reviewed
    The in-orbit performance and calibration of the Gas Imaging Spectrometer (GIS), located on the focal plane of the X-ray astronomy satellite ASCA, are described. An extensive in-orbit calibration has confirmed its basic performance, including a position resolution of 0.6 mm (FWHM) and an energy resolution of 7.8% (FWHM), both at 6 keV. When combined with the X-ray telescope, the GIS sensitivity range becomes 0.7-10 keV. The in-orbit non X-ray background of the GIS has been confirmed to be as low as (5-9) × 10-4 c s-1 cm-2 keV-1 over the 1-10 keV range. The long-term detector gain has been stable within a few % for nearly 3 years. Extensive observations of the Crab Nebula and other sources have provided accurate calibrations of the position response, photometric capability, dead time, and timing accuracy of the GIS. Furthermore, the overall energy response, including the temporal and positional gain variations and the absolute gain scale, has been calibrated to ∼ 1%. Thus, the GIS is working as an all-round cosmic X-ray detector, capable of X-ray imagery, fine X-ray spectroscopy, X-ray photometry with a flux dynamic range covering more than 5 orders of magnitude, and fast X-ray photometry with a time resolution up to 60 μs.
  • Hidehiro Kaneda, Hajime Ezawa, Masaharu Hirayama, Tsuneyoshi Kamae, Hidetoshi Kubo, Keiichi Matsuzaki, Kazuo Makishima, Takanori Ohtsuka, Yoshitaka Saito, Yutaro Sekimoto, Tadayuki Takahashi, Takayuki Tamura
    Proceedings of SPIE - The International Society for Optical Engineering, 2518 85-95, 1995  Peer-reviewed
    The ASTRO-E satellite is scheduled for launch in 2000 by the Institute of Space and Astronautical Science (ISAS). In this paper the design and performance of the hard x ray detector (HXD) developed for ASTRO-E are described. The HXD is a combination of YAP/BGO phoswich scintillators and silicon PIN diodes covering a wide energy band of 10 - 700 keV. The detector background is reduced down to several times 10 -6c/s/cm 2/keV, and the sensitivity of the HXD is more than one order of magnitude higher than any other past missions in the range of a few 10 keV to several 100 keV. Thus ASTRO-E HXD is expected to achieve an extreme high performance for detecting cosmic hard x rays and low-energy gamma rays. Astrophysics to be explored with the HXT are expected to be extremely widespread and rich.

Major Presentations

 38
  • Naoko Ogawa, Shintaro Nakajima, Takanobu Shimada, Masanobu Ozaki, Keiichi Matsuzaki, Miyuki Arai, Takahiro Owaki, Takamitsu Oyama, Takane Imada
    Oct 19, 2023, The Japan Society for Aeronautical and Space Sciences
    This paper shows the system design and development status of the data handling system, ISC(DH), for the Martian Moons eXploration (MMX) mission. ISC(DH) consists of SMU (Spacecraft Management Unit), MDP (Mission Data Processor) and PDCU (Power Distribution Control Unit). System overviews and configuration are described.
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Research Projects

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