Curriculum Vitaes

Masahiro Tsujimoto

  (辻本 匡弘)

Profile Information

Affiliation
Assistant professor, Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency
Degree
博士(理学)(Mar, 2003, 京都大学)
修士(理学)(Mar, 2000, 京都大学)

Contact information
tsujimoto.masahirojaxa.jp
Researcher number
10528178
ORCID ID
 https://orcid.org/0000-0002-9184-5556
J-GLOBAL ID
201801010256574610
Researcher ID
ABC-6667-2020
researchmap Member ID
B000296937

External link

Papers

 218
  • Frederick S. Porter, Caroline A. Kilbourne, Meng P. Chiao, Renata S. Cumbee, Megan E. Eckart, Ryuichi Fujimoto, Yoshitaka Ishisaki, Yoshiaki Kanemaru, Richard L. Kelley, Maurice A. Leutenegger, Yoshitomo Maeda, Misaki Mizumoto, Kosuke Sato, Makoto Sawada, Gary A. Sneiderman, Yoh Takei, Masahiro Tsujimoto, Yuusuke Uchida, Tomomi Watanabe, Shinya Yamada
    Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray, 56-56, Aug 21, 2024  
  • Takayuki Hayashi, Rozenn Boissay-Malaquin, Keisuke Tamura, Takashi Okajima, Megan E. Eckart, Maurice A. Leutenegger, Tahir Yaqoob, Michael Loewenstein, Richard L. Kelley, Frederick S. Porter, Caroline A. Kilbourne, Meng P. Chiao, Gary A. Sneiderman, Renata S. Cumbee, Yoshitaka Ishisaki, Ryuichi Fujimoto, Masahiro Tsujimoto, Makoto Sawada, Toshiki Sato, Yoshitomo Maeda, Manabu Ishida, Lia Corrales, Eric Miller, Aysegul Tumer, Hiromitsu Takahashi, Laura Brenneman, Yoshiaki Kanemaru, Misaki Mizumoto, Maxim Markevitch, Matteo Guainazzi
    Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray, 58-58, Aug 21, 2024  
  • Megan E. Eckart, Gregory V. Brown, Meng P. Chiao, Renata S. Cumbee, Ryuichi Fujimoto, Natalie Hell, Akio Hoshino, Yoshitaka Ishisaki, Richard L. Kelley, Steven J. Kenyon, Caroline A. Kilbourne, Shunji Kitamoto, Maurice A. Leutenegger, Thomas E. Lockard, Michael Loewenstein, Edward W. Magee, Misaki Mizumoto, Frederick S. Porter, Kosuke Sato, Makoto Sawada, Chintan D. Shah, Russell F. Shipman, Gary A. Sneiderman, Yoh Takei, Masahiro Tsujimoto, Cor P. de Vries, Tomomi Watanabe, Michael C. Witthoeft, Rob Wolfs, Shinya Yamada, Tahir Yaqoob
    Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray, 62-62, Aug 21, 2024  
  • Russell F. Shipman, Shunji Kitamoto, Rob Wolfs, Elisa Costantini, Megan E. Eckart, Carlo Ferrigno, Ludovic Genolet, Nathalie Q. S. Gorter, Martin Grim, Jan-Willem A. den Herder, Caroline A. Kilbourne, Maurice A. Leutenegger, Erik van der Meer, Misaki Mizumoto, Frederick S. Porter, Stéphane Paltani, Makoto Sawada, Simon Strotmann, Masahiro Tsujimoto, Cor P. de Vries
    Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray, 225-225, Aug 21, 2024  
  • Yuto Mochizuki, Masahiro Tsujimoto, Caroline A. Kilbourne, Megan E. Eckart, Yoshitaka Ishisaki, Yoshiaki Kanemaru, Maurice . Leutenegger, Misaki Mizumoto, Frederick S. Porter, Kosuke Sato, Makoto Sawada, Shinya Yamada
    Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray, 233-233, Aug 21, 2024  

Misc.

 26
  • 植松令太, 石野宏和, 桜井雄基, 松村知岳, 高久諒太, HOANG Thuong, 辻本匡弘, 富永愛侑, 富永愛侑, MATSUDA F., 小栗秀悟
    日本物理学会講演概要集(CD-ROM), 78(2), 2023  
  • 堂谷忠靖, 関本裕太郎, 辻本匡弘, 小栗秀悟, 松田フレドリック, 永田竜, 篠崎慶亮, 小田切公秀, 綿貫一也, 高倉隼人, 富永愛侑, 中野遼, 増村亮, 羽澄昌史, DE HAAN Tijmen, 長谷川雅也, 長崎岳人, 加藤晶大, 片山伸彦, 松村知岳, 桜井雄基, 長谷部孝, GHIGNA Tommaso, 杉山真也, 高久諒太, 星野百合香, 石野宏和, STEVER Samantha, 小松国幹, 高瀬祐介, 長野佑哉, 鹿島伸悟, 小松英一郎
    日本天文学会年会講演予稿集, 2021, 2021  
  • 堂谷忠靖, 篠崎慶亮, 関本裕太郎, 高倉隼人, 辻本匡弘, 長谷部孝, 満田和久, 永田竜, 羽澄昌史, 南雄人, 片山伸彦, 桜井雄基, 菅井肇, 高倉理, 松村知岳, 石野宏和, 魚住聖, 鹿島伸悟, 小松英一郎
    日本天文学会年会講演予稿集, 2020, 2020  
  • 堂谷忠靖, 関本裕太郎, 篠崎慶亮, 辻本匡弘, 小栗秀悟, 長谷部孝, 永田竜, 羽澄昌史, 南雄人, 長谷川雅也, DE HAAN Tijmen, 長崎岳人, 片山伸彦, 松村知岳, 桜井雄基, 今田大皓, 石野宏和, STEVER Samantha Lynn, 鹿島伸悟, 小松英一郎
    宇宙科学技術連合講演会講演集(CD-ROM), 64th, 2020  
  • 関本裕太郎, 堂谷忠靖, 篠崎慶亮, 高倉隼人, 辻本匡弘, 長谷部孝, 満田和久, 永田竜, 羽澄昌史, 南雄人, 片山伸彦, 桜井雄基, 菅井肇, 高倉理, 松村知岳, 石野宏和, 魚住聖, 鹿島伸悟, 小松英一郎, 今田大皓
    日本天文学会年会講演予稿集, 2019, 2019  
  • 関本裕太郎, 堂谷忠靖, 篠崎慶亮, 高倉隼人, 辻本匡弘, 長谷部孝, 満田和久, 永田竜, 羽澄昌史, 南雄人, 宇都宮真, 片山伸彦, 桜井雄基, 菅井肇, 高倉理, 松村知岳, 石野宏和, 魚住聖, 鹿島伸悟, 小松英一郎, 今田大皓
    日本天文学会年会講演予稿集, 2019, 2019  
  • 石崎欣尚, 江副祐一郎, 山田真也, 一戸悠人, 藤本龍一, 竹井洋, 安田進, 石田学, 山崎典子, 前田良知, 辻本匡弘, 飯塚亮, 小山志勇, 野田博文, 玉川徹, 澤田真理, 佐藤浩介, 北本俊二, 星野晶夫, BROWN G. V., ECKART M., HAYASHI T., KELLEY R. L., KILBOURNE C. A., LEUTENEGGER M. A., MORI H., OKAJIMA T., PORTER F. S., SOONG Y., MCCAMMON D., SZYMKOWIAK A. E.
    日本天文学会年会講演予稿集, 2017, 2017  
  • 一戸悠人, 飯塚亮, 井上翔太, 上田周太朗, 太田直美, 北山哲, 佐藤浩介, 田中桂悟, 田村隆幸, 辻本匡弘, 藤本龍一, 前田良知
    日本天文学会年会講演予稿集, 2017, 2017  
  • 上田周太朗, 飯塚亮, 一戸悠人, 井上翔太, 太田直美, 北山哲, 佐藤浩介, 田中桂悟, 田村隆幸, 辻本匡弘, 藤本龍一, 前田良知
    日本天文学会年会講演予稿集, 2017, 2017  
  • Mitsuda K., Yamasaki N., Takei Y., Tsujimoto M., Ogawa M., Sugita H., Sato Y., Shinozaki K., Okamoto A., Ohashi T., Ishisaki Y., Ezoe Y., Mitsuishi I., Fujimoto R., Hoshino A., Tashiro M., Terada Y., Kitamoto S., Murakami H., Seta H., Tamagawa T., Yamada S., Sato K., Ota N., Sawada M., Iyomoto N., Murakami M., Kelley R. L., Kilbourne C. A., Porter F. S., Sneiderman G. A., Boyce K. R., DiPirro M. J., Shirron P. J., Gendreau K. C., Brown G. V., McCammon D., Szymkowiak A., den Herder J.-W., de Vries C., Costantini E., Akamatsu H., Paltani S., Pohl M.
    Meeting abstracts of the Physical Society of Japan, 68(1) 133-133, Mar 26, 2013  
  • Mitsuda Kazuhisa, Yamasaki Noriko, Takei Yoh, Tsujimoto Masahiro, Ogawa Mina, Sugita Hiroyuki, Sato Yoichi, Shinozaki Keisuke, Okamoto Atsushi, Ohashi Takaya, Ishisaki Yoshitaka, Ezoe Yuichiro, Mitsuishi Ikuyuki, Fujimoto Ryuichi, Hoshino Akio, Tashiro Makoto, Terada Yukikatu, Kitamoto Shunji, Murakami Hiroshi, Seta Hiromi, Tamagawa Toru, Yamada Shinya, Sato Kosuke, Ota Naomi, Sawada Makoto, Iyomoto Naoko, Murakami Masahide, Kelley R. L., Kilbourne C. A., Porter F. S., Sneidermann G. A., Boyce K. R., DiPirro M. J., Shirron P. J., Gentreau K. C., Brown G. V., McCammon D., Szymkowiak A., den Herder J.-W., de Vries C., Costantini E., Akamatsu H., Paltani S., Pohl M., ASTRO-H SXS Team
    Meeting abstracts of the Physical Society of Japan, 68(1) 133-133, Mar 26, 2013  
  • J. W. Den Herdera, D. Bagnali, S. Bandler, M. Barbera, X. Barcons, D. Barret, P. Bastia, M. Bisotti, K. Boyce, C. Cara, M. Ceballos, L. Corcione, B. Cobo, L. Colasanti, J. De Plaa, M. DiPirro, W. B. Doriese, Y. Ezoe, R. Fujimoto, F. Gatti, L. Gottardi, P. Guttridge, R. Den Hartog, I. Hepburn, R. Kelley, K. Irwin, Y. Ishisaki, C. Kilbourne, P. A J, De Korte, J. Van, Der Kuur, S. Lotti, C. Macculi, K. Mitsuda, T. Mineo, L. Natalucci, T. Ohashi, M. Page, S. Paltani, E. Perinati, L. Piro, C. Pigot, F. S. Porter, G. Rauw, L. Ravera, E. Renotte, J. L. Sauvageot, C. Schmid, S. Sciortino, P. Shirron, Y. Takei, G. Torrioli, M. Tsujimoto, L. Valenziano, D. Willingale, C. De Vries, H. Van Weers, J. Wilms, N. Y. Yamasaki
    Proceedings of SPIE - The International Society for Optical Engineering, 8443, Dec 1, 2012  
    one of the instruments on the Advanced Telescope for High-Energy Astrophysics (Athena) which was one of the three missions under study as one of the L-class missions of ESA, is the X-ray Microcalorimeter Spectrometer (XMS). This instrument, which will provide high-spectral resolution images, is based on X-ray micro-calorimeters with Transition Edge Sensor (TES) and absorbers that consist of metal and semi-metal layers and a multiplexed SQUID readout. The array (32 x 32 pixels) provides an energy resolution of < 3 eV. Due to the large collection area of the Athena optics, the XMS instrument must be capable of processing high counting rates, while maintaining the spectral resolution and a low deadtime. In addition, an anti-coincidence detector is required to suppress the particle-induced background. Compared to the requirements for the same instrument on IXO, the performance requirements have been relaxed to fit into the much more restricted boundary conditions of Athena. In this paper we illustrate some of the science achievable with the instrument. We describe the results of design studies for the focal plane assembly and the cooling systems. Also, the system and its required spacecraft resources will be given. © 2012 SPIE.
  • H. Seta, H. Seta, M. S. Tashiro, Y. Ishisaki, M. Tsujimoto, M. Tsujimoto, Y. Shimoda, S. Takeda, S. Yamaguchi, K. Mitsuda, R. Fujimoto, R. Fujimoto, Y. Takei, R. L. Kelley, K. R. Boyce, C. A. Kilborne, C. A. Kilborne, F. S. Porter, J. J. Miko, J. J. Miko, K. Masukawa, K. Matsuda
    Proceedings of SPIE - The International Society for Optical Engineering, 8443, Dec 1, 2012  
    We present the development status of the Pulse Shape Processor (PSP), which is the on-board digital electronics responsible for the signal processing of the X-ray microcalorimeter spectrometer instrument (the Soft X-ray Spectrometer; SXS) for the ASTRO-H satellite planned to be launched in 2014. We finished the design and fabrication for the engineering model, and are currently undertaking a series of performance verification and environmental tests. In this report, we summarize the results obtained in a part of the tests completed in the first half of this year. © 2012 SPIE.
  • Mitsuda Kazuhisa, Yamasaki Noriko, Takei Yoh, Tsujimoto Masahiro, Ogawa Mina, Sugita Hiroyuki, Sato Yoichi, Shinozaki Keisuke, Okamoto Atsushi, Ohashi Takaya, Ishisaki Yoshitaka, Ezoe Yuichiro, Fujimoto Ryuichi, Hoshino Akio, Tashiro Makoto, Terada Yukikatsu, Kitamoto Shunji, Murakami Hiroshi, Tamagawa Toru, Sato Kosuke, Ota Naomi, Murakami Masahide, Kelley R.L., Kilbourne C.A., Porter F.S., Snedermann G.A., Boyce K.R., DiPirro M.J., Shirron P.J., Gentreau K.C., Brown G.V., McCammon D., Szymkowiak A., Herder J.-W. den, Vries C. de, Costantini E., Paltani S., Pohl M.
    Meeting abstracts of the Physical Society of Japan, 67(1) 141-141, Mar 5, 2012  
  • 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 Proceedings, 1427 247-248, Mar, 2012  
  • Takei Dai, Tsujimoto Masahiro, Kitamoto Shunji
    Meeting abstracts of the Physical Society of Japan, 66(1) 111-111, Mar 3, 2011  
  • Shimoda Y., Seta H., Tashiro M., Terada Y., Yasuda T., Takeda S., Ishisaki Y., Abe Y., Tsujimoto M., Mitsuda K., Boyce Kevin, Matsuda K., Masukawa K.
    Meeting abstracts of the Physical Society of Japan, 66(1) 121-121, Mar 3, 2011  
  • Matsuta Keiko, Dotani Tadayasu, Ozaki Masanobu, Bamba Aya, Tsujimoto Masahiro, Tsuru Takeshi G., Matsumoto Hironori, Hayashida Kiyoshi, Tsunemi Hiroshi, XIS team
    (9) 412-413, Feb 26, 2010  
    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 current status of the timing calibration of the X-ray Imaging Spectrometer (XIS) on board Suzaku. The XIS is designed to be flexible enough and can be operated in various clocking modes. Since the absolute timing accuracy of the Hard X-ray Detector (HXD) was calibrated to be better than 360 microseconds, we calibrated the XIS timing accuracy referring to the HXD data. We employed Hercules X-1 and Cygnus X-1 for the calibration taking into account of the energy dependence of their time variations. We found no significant offset in the XIS time assignment in the normal mode (with burst/window options), whereas a marginal offset of 30 +/- 16 ms was found in the Parallel-Sum mode.Meeting sponsors: The University of Tokyo, The Institute of Physical and Chemical Research, The Japan Society for the Promotion of Science
  • 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
    (9) 414-415, Feb 26, 2010  
    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
  • Hiromi Seta, Makoto S. Tashiro, Yukikatsu Terada, Yuya Shimoda, Kaori Onda, Yoshitaka Ishisaki, Masahiro Tsujimoto, Toshishige Hagihara, Yoh Takei, Kazuhisa Mitsuda, Kevin R. Boyce, Andrew E. Szymkowiak
    AIP Conference Proceedings, 1185 278-281, Dec 1, 2009  
    A digital signal processing system for the X-ray microcalorimeter array (SXS) is being developed for the next Japanese X-ray astronomy satellite, ASTRO-H. The SXS digital signal processing system evaluates each pulse by an optimal filtering process. For the ASTRO-H project, we decided to employ digital electronics hardware, which includes a digital I/O board based upon FPGAs, and a separate CPU board. It is crucially important for the FPGA to be able to detect the presence of an "secondary" pulses on the tail of an initial pulse. In order to detect the contaminating pulses, we have developed a new finite impulse response filter, to compensate for the undershoot in the derivative. By employing the filter it is possible for FPGA to detect the secondary pulse very close the first pulse, and to reduce the load of the CPU in the secondary pulse searching process. © 2009 American Institute of Physics.
  • 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 Japan, 64(2) 31-31, Aug 18, 2009  
  • 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 team
    Meeting abstracts of the Physical Society of Japan, 64(1) 92-92, Mar 3, 2009  
  • Seta Hiromi, Tashiro Makoto, Terada Yukikatsu, Onda Kaori, Shimoda Yuuya, Ishisaki Yoshitaka, Takei Yoh, Mitsuda Kazuhisa, ASTRO-H SXS team
    Meeting abstracts of the Physical Society of Japan, 64(1) 93-93, Mar 3, 2009  
  • IMANISHI Kensuke, TSUJIMOTO Masahiro, KOYAMA Katsuji
    57(9) 638-645, Sep 5, 2002  
    Protostars, the first stage of stellar evolution, are born in a dense core of a molecular cloud with temperature of about 10 K. X-rays can be emitted from a high temperature plasma of 10^6-10^8K, hence may not be expected from protostars. Nature, however, is much more imaginative than we are. The Japanese X-ray satellite ASCA found X-rays from a few protostars. The US satellite Chandra successively found that X-rays are common in most of the young stars. Many protostars show flare-like events similar to our sun, hence the X-rays are attributable to solar type magnetic activities. The X-ray work should finally lead to our deep understanding of the evolution and structure of young stars and planets. This paper overviews the pioneering results in the unique waveband, the X-ray.
  • M Kohno, K Imanishi, A Bamba, M Tsujimoto, H Murakami, T Tsuru, K Koyama
    X-RAY AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY XII, 4497 149-157, 2002  Peer-reviewed
    We study the relation between diffusion and loss of charge produced in X-ray CCDs with the fitting method. We obtain the extent and the pulse height of each X-ray event in a CCD by a two-dimensional image-fitting the charge distribution of the event. For the monochromatic X-rays, we find that the event with small extent keeps all the charge produced, while that with larger extent than a certain value loses some part of the produced charge as a function of extent. The result suggests that the event with a small extent is produced by an X-ray absorbed in the depletion layer. On the other hand, the event with large extent corresponds to an X-ray absorbed in the field-free region. We develop two new methods which enable us to derive the relation between the extent of an event and the absorption depth. One is performed by illuminating well calibrated monochromatic X-ray source. The other is realized by using with two monochromatic X-rays and enables us to measure the thickness of the CCD depletion layer without calibrating absolute flux of the monochromatic X-rays.
  • M Tsujimoto, H Murakami, K Hamaguchi, TG Tsuru, H Awaki, K Koyama
    X-RAY AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY XI, 4140 470-477, 2000  Peer-reviewed
    CCDs can function as the X-ray spectrometer by counting the number of electrons created by the ionization of semiconductor atoms following the photoelectric absorption of a X-ray photon. In order to measure the incident X-ray energy correctly, we have to sum up all the electrons split over several pixels, thus the grade method is conventionally used. We will discuss the possible alternative to this method the fitting method -, which has several advantages over the grade method. By applying this method to the data taken with our CCD chip, we will show that the fitting method can improve the quantum efficiency, is appliable to the analysis of polarized X-ray events, and gives us insights on the structure of CCDs.

Research Projects

 7