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  2. Ryuichi Fujimoto

Ryuichi Fujimoto

  (藤本 龍一)

Profile Information

Affiliation
Professor, Department of Space Astronomy and Astrophysics, Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency
Professor, Graduate Institute for Advanced Studies, The Graduate University for Advanced Studies (SOKENDAI)
Visiting Professor, School of Science, Tokyo Institute of Technology
Degree
Ph. D.(The University of Tokyo)
master's degree(The University of Tokyo)
Researcher number
20280555
ORCID ID
 https://orcid.org/0000-0002-2374-7073
J-GLOBAL ID
200901095989600566
researchmap Member ID
1000363020

I have been developing cryogenic high-resolution X-ray microcalorimeter spectrometers onboard X-ray astronomy satellite. It was achieved as the Resolve instrument onboard XRISM, which was launched in September, 2023.

Here are research themes I can provide. (1) Analyze high-resolution X-ray spectroscopy data obtained by XRISM satellite, and research motion of the hot gas in clusters of galaxies, in order to understand the formation of the large-scale structures of the Universe. (2) Conduct experimental studies, in anticipation of LiteBIRD mission, that aims for observing the polarization of the cosmic microwave background radiation.

Message to students: Through the research, develop an understanding of specific natural phenomena, and also learn the process to reach fundamental physics laws that underlie the complex phenomena, together with experimental and/or analytical methods.

Research Interests

 6

Research Areas

 2

Research History

 8
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Education

 4

Committee Memberships

 2

Awards

 2

Papers

 155
  • Seiji Yoshida, Masahito Isshiki, Ken'ichi Kanao, Shoji Tsunematsu, Kiyomi Otsuka, Syou Mizunuma, Yoh Takei, Akio Hoshino, Ryuichi Fujimoto, Yuichiro Ezoe, Kosuke Sato, Michael DiPirro, Peter Shirron
    Cryogenics, 139 103831-103831, Apr, 2024  Peer-reviewed
  • Hasebe, T., Imamura, R., Tsujimoto, M., Awaki, H., Chiao, M.P., Fujimoto, R., Hartz, L.S., Kilbourne, C.A., Sneiderman, G.A., Takei, Y., Yasuda, S.
    Journal of Astronomical Telescopes, Instruments, and Systems, 9(1) 14003-14003, 2023  
  • K. Sato, N. Y. Yamasaki, M. Ishida, Y. Maeda, K. Mitsuda, Y. Ishisaki, Y. Fujita, Y. Ezoe, I. Mitsuishi, Y. Tawara, K. Osato, N. Kawai, K. Matsushita, D. Nagai, K. Yoshikawa, R. Fujimoto, T. G. Tsuru, N. Ota, S. Yamada, Y. Ichinohe, Y. Uchida, Y. Nakashima
    Journal of Low Temperature Physics, 209(5-6) 971-979, Dec, 2022  
  • Kosuke Sato, Noriko Y. Yamasaki, Shinya Yamada, Ikuyuki Mitsuishi, Yuto Ichinohe, Hajime Omamiuda, Yuusuke Uchida, Kazuhisa Mitsuda, Daisuke Nagai, Kohji Yoshikawa, Ken Osato, Kyoko Matsushita, Yutaka Fujita, Yoshitaka Ishisaki, Yuichiro Ezoe, Manabu Ishida, Yoshitomo Maeda, Nobuyuki Kawai, Ryuichi Fujimoto, Takeshi G. Tsuru, Naomi Ota, Yuki Nakashima
    Space Telescopes and Instrumentation 2022: Ultraviolet to Gamma Ray, 12181, Aug 31, 2022  
  • Takashi Hasebe, Ryuta Imamura, Masahiro Tsujimoto, Hisamitsu Awaki, Meng P. Chiao, Ryuichi Fujimoto, Leslie S. Hartz, Gary A. Sneiderman, Yoh Takei, Susumu Yasuda
    Proceedings of SPIE - The International Society for Optical Engineering, 12181, 2022  
    Resolve is a payload hosting an x-ray microcalorimeter detector operated at 50 mK in the X-Ray Imaging and Spectroscopy Mission (XRISM), which is currently under development by an international collaboration and is planned to be launched in 2023. One of the technical concerns is the micro-vibration interference to the sensitive microcalorimeter detector by the spacecraft bus components. We verified this in a series of the ground tests in 2021–2022, the results of which are reported here. We defined the micro-vibration interface between the spacecraft and the Resolve instrument. In the instrument-level test, we tested the flight-model hardware against the interface level by injecting micro-vibration using vibrators and evaluated the instrument response using the 50 mK stage temperature stability, the ADR magnet current consumption rate, and the detector noise spectra. We found the strong responses when injecting micro-vibration at ∼200, 380, and 610 Hz. In the former two cases, the beat among the injected frequency and the cryocooler frequency harmonics are also observed in the detector noise spectra. In the spacecraft-level test, we measured the acceleration and the instrument responses with and without suspending the entire spacecraft. The reaction wheels and the inertial reference units, two major sources of micro-vibration among the bus components, were operated. We found that the observed Resolve responses are within acceptable levels.
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Misc.

 129
  • Maeda, Y., Ebara, M., Fujimoto, R., Hayashi, T., Inoue, H., Ishisaki, Y., Mori, H., Okada, S., Suzuki, K., Uchiyama, Y., Serlemitsos, P.J., Soong, Y., Chan, K.-W., Okajima, T., Lehan, J.P., Itoh, K., Itoh, A., Yokoyama, Y., Itoh, Y., Nakamura, R., Ishida, M., Hayakawa, A., Inoue, C., Okuma, S., Kubota, R., Suzuki, M., Osawa, T., Yamashita, K., Kunieda, H., Tawara, Y., Ogasaka, Y., Furuzawa, A., Tamura, K., Shibata, R., Haba, Y., Naitou, M., Misaki, K., Iizuka, R.
    Progress of Theoretical Physics Supplement, (169) 322-325, 2007  
    We present the in-flight performance of the X-ray telescopes (XRTs) onboard Suzaku. The imaging capability is significantly improved over the ASCA XRT, which had half-power diameters of 3'.6, to 1'.8-2'.3 for all four XRT-I modules. Contemporaneous fits of a power law to all the XIS spectra of the Crab Nebula taken at the two standard observing positions (XIS/HXD-default positions) gives a flux consistent with that obtained by Toor & Seward (1974) to within〜2%. The pre-collimator on the top of each XRT module successfully reduces the intensity of the stray light from the 20' and 50'-off directions down to the level of pre-flight expectations. We also present the thermal wobbling of the satellite. The wobbling causes the alignment error between the XRT-XIS system and the attitude and orbit control system. The wobbling of the alignment is as large as〜1arcmin. In the currently processed data, the absolute coordinate also has systematic uncertainty of up to〜1arcmin.
  • Tsuru, T.G., Ozawa, M., Hyodo, Y., Matsumoto, H., Koyama, K., Awaki, H., Fujimoto, R., Griffiths, R., Kilbourne, C., Matsushita, K., Mitsuda, K., Ptak, A., Ranalli, P., Yamasaki, N.Y.
    Publications of the Astronomical Society of Japan, 59(1 SPEC. ISS.) S269-S282, 2007  
    The extended X-ray emission from &#039;the Cap&#039; region located 11&#039; (11.6 kpc)<br /> above the disk of the starburst galaxy M82 has been observed with Suzaku and<br /> XMM-Newton. Owing to the good energy resolution and the large collecting area<br /> of the XIS on Suzaku, combined with similar properties of the EPIC instrument<br /> on XMM-Newton, we have clearly detected K-shell emission lines from O VII, O<br /> VIII, Ne X, Mg XI, Mg XII and the Fe-L complex. Two optically-thin thermal<br /> plasma components are required to fit the observed X-ray spectra. We have<br /> determined the metal abundances of O, Ne, Mg, Si and Fe in this region for the<br /> first time. Their metal abundance ratios agree well with those of metal-poor<br /> stars and the model prediction of metals synthesized by type-II supernovae, but<br /> they are not consistent with the metallicities of type-Ia supernovae. This<br /> result is support for the idea that the origin of the metals in the Cap is<br /> type-II supernovae explosions occurring in the starburst regions in the M82<br /> galaxy. We discuss the possible contribution from sputtered dust grains to the<br /> metals in the Cap. An emission line consistent with the C VI transition of n=4<br /> to 1 at 0.459 keV is marginally detected, although it is not statistically<br /> significant at the 99% confidence level; the presence of this line would<br /> suggest charge-exchange processes in the Cap.
  • KANAO Ken-ichi, OTSUKA Kiyomi, TSUNEMATSU Shoji, NARASAKI Katsuhiro, MITSUDA Kazuhisa, FUJIMOTO Ryuichi
    The Symposium on Stirlling Cycle, 2006(10) 73-74, Oct 19, 2006  
    Cryogenic cooling is useful to most detectors in astronomical and atmospheric observation for improving the sensitivity and reducing the background noise. Recently cryocoolers are often adopted as cooling devices. This paper describes a single stage Stirling cryocooler. It is designed, manufactured and tested for space borne mission. The typical cooling power is 2W at 80K with 50W input. The cooler on the X-ray telescope satellite "Suzaku" was launched July 2005. It is operating over 1 year without any trouble. On the other hand, a cooler achieved 50,000 hour operation in the lifetime test on the ground. Same type coolers will be launched on the lunar explorer and the Venus orbiter of Japan
  • 田和憲明, 林田清, 山口弘悦, 竹井洋, 藤本龍一, 海老沢研, 中澤知洋, 石崎欣尚, 水野恒史, 深澤泰司
    日本天文学会年会講演予稿集, 2006 254, Aug 20, 2006  
  • 田和 憲明, 林田 清, 山口 弘悦, 竹井 洋, 藤本 龍一, 海老沢 研, 中澤 知洋, 石崎 欣尚, 水野 恒史, 深澤 泰司
    日本物理学会講演概要集, 61(2) 76-76, Aug 18, 2006  
  • Fujimoto Ryuichi, Mitsuda Kazuhisa, Takei Yoh, McCammon Dan, Bauer Michael, Porter F. Scott, Ishisaki Yoshitaka, the Suzaku team
    Meeting abstracts of the Physical Society of Japan, 61(2) 72-72, Aug 18, 2006  
  • Takei Y, Mitsuda K, Fujimoto R, Ohashi T, Henry J.Patrick, Tamura T, Yamasaki N.Y
    Meeting abstracts of the Physical Society of Japan, 61(1) 87-87, Mar 4, 2006  
  • T. Ohashi, M. Ishida, S. Sasaki, Y. Ishisaki, K. Mitsuda, N. Y. Yamasaki, R. Fujimoto, Y. Takei, Y. Tawara, A. Furuzawa, Y. Suto, Y. Yoshikawa, H. Kawayara, N. Kawai, T. G. Tsuru, K. Matsushita, T. Kitayama
    Space Telescopes and Instrumentation II: Ultraviolet to Gamma Ray, Pts 1 and 2, 6266(No.) G2660-G2660, 2006  
    We present our proposal for a small X-ray mission DIOS (Diffuse Intergalactic Oxygen Surveyor), consisting of a 4-stage X-ray telescope and an array of TES microcalorimeters, cooled with mechanical coolers, with a total weight of about 400 kg. The mission will perform survey observations of warm-hot intergalactic medium using OVII and OVIII emission lines, with the energy coverage up to 1.5 keV. The wide field of view of about 50' diameter, superior energy resolution close to 2 eV FWHM, and very low background will together enable us a wide range of science for diffuse X-ray sources. We briefly describe the design of the satellite, performance of the subsystems and the expected results.
  • 江副祐一郎, 輿石真樹, 吉野友崇, 三田信, 藤本龍一, 山崎典子, 満田和久, 藤森玉行, 大島泰, 石崎欣尚, 大橋隆哉, 高野貴之, 前田龍太郎
    応用物理学関係連合講演会講演予稿集, 53rd(1), 2006  
  • Yoshino T., Yoshida K., Hagihara T., Ishisaki Y., Morita U., Sato K., Mitsuda K., Yamasaki N., Fujimoto R.
    Meeting abstracts of the Physical Society of Japan, 60(2) 36-36, Aug 19, 2005  
  • J. Cottam, K. R. Boyce, G. V. Brown, G. V. Brown, R. Fujimoto, T. Furusho, Y. Ishisaki, R. L. Kelley, C. A. Kilbourne, D. McCammon, K. Mitsuda, U. Morita, F. S. Porter, T. Saab, Y. Takai, M. Yamamoto
    AIP Conference Proceedings, 774 379-382, Jun 13, 2005  
    The XRS microcalorimeter will be launched in 2005 as part of the Astro-E2 mission. It will cover the energy band from 0.3 to 10 keV with a nearly constant energy resolution of 6.0 eV and a peak effective area of 200 cm 2 at 1.5 keV. The XRS will provide unprecedented throughput and resolving power, particularly at high energies. Detailed spectral features in the Fe K region will be resolved for the first time, providing access to spectroscopic diagnostics for a wide range of astrophysical objects. In this presentation we will describe the XRS instrument, details of its spectral performance, and how it compares to the current high-resolution instruments on the Chandra and XMM-Newton observatories. © 2005 American Institute of Physics.
  • Fujimoto R., Furusho T., Ishisaki Y., Takei Y., Morita U., Yamamoto M., Ota N., Yamasaki N., Mitsuda K., Boyce K. R., Brown G., Cottam J., Kelley R. L., Kilbourne C. A., McCammon D., Porter S., XRS team
    Meeting abstracts of the Physical Society of Japan, 60(1) 90-90, Mar 4, 2005  
  • Furusho Tae, Fujimoto Ryuichi, Mitsuda Kazuhisa, Tamura Takayuki, Ishisaki Yoshitaka, Ohashi Takaya, Kelley Richard L, XRS team
    Meeting abstracts of the Physical Society of Japan, 60(1) 209-209, Mar 4, 2005  
  • 古庄 多恵, 藤本 龍一, 満田 和久
    宇宙科学シンポジウム, 5 654-657, Jan 6, 2005  
  • 星野晶夫, 篠崎慶亮, 石崎欣尚, 森田うめ代, 佐藤浩介, 山川善之, 藤森玉行, 大島泰, 大橋隆哉, 満田和久, 山崎典子, 藤本龍一, 三原健弘, 田中啓一
    日本天文学会年会講演予稿集, 2005, 2005  
  • 満田 和久, 山崎 典子, 藤本 龍一
    宇宙科学シンポジウム, 4 39-42, Jan 8, 2004  
  • 藤本 龍一, 満田 和久, 山崎 典子
    宇宙科学シンポジウム, 4 101-104, Jan 8, 2004  
  • 石崎欣尚, 森田うめ代, 篠崎慶亮, 佐藤浩介, 大橋隆哉, 満田和久, 山崎典子, 藤本龍一, 古庄多恵, 大島泰, 竹井洋
    日本天文学会年会講演予稿集, 2004, 2004  
  • Suto, Y., Yoshikawa, K., Yamasaki, N.Y., Mitsuda, K., Fujimoto, R., Furusho, T., Ohashi, T., Ishida, M., Sasaki, S., Ishisaki, Y., Tawara, Y., Furuzawa, A.
    Journal of the Korean Physical Society, 45(SUPPL.), 2004  
    Approximately 30 to 50 percent of the total baryons in the present universe is supposed to take the form of wa arm/hot intergalactic medium (WHIM) whose X-ray continuum emission is very weak. In order to carry out a direct and homogeneous survey of elusive cosmic missing baryons, we propose a dedicated soft-X-ray mission, DIOS (Diffuse Intergalactic Oxygen Surveyor). The unprecedented energy resolution (∼ 2eV) of the XSA (X-ray Spectrometer Array) on-board DIOS enables us to identify WHIM with gas temperatures T = 106-7K and overdensity δ= 10-100 located at z &lt; 0.3 through emission lines of OVII and OVIII. DIOS, which will hopefully be launched in several years time, promises to open a new window of detection and characterization of cosmic missing baryons and to provide yet another important and complementary tool to trace the large-scale structure of the universe.
  • Fujimoto, R., Takei, Y., Tamura, T., Mltsuda, K., Yamasaki, N.Y., Shibata, R., Ohashi, T., Ota, N., Audley, M.D., Kelley, R.L., Kilbourne, C.A.
    Publications of the Astronomical Society of Japan, 56(5) L29-L34-L34, 2004  
  • IZUMI T., KUDO H., SATO H., ARAKAWA T., KOBAYASHI H., OHTSUKA S., MORI K., SHOJI S., HONMA N., MITSUDA K., YAMASAKI N., FUJIMOTO R., IYOMOTO N., OHSHIMA Y., JIGEN K., TAKEI Y., ICHITSUBO T., FUJIMORI T., YOSHIDA K., ISHISAKI Y, MORITA U., KOGA T., SHINOSAKI K., SATO H., TAKAI M., KURODA Y., OHNISHI M., GOTO M., BEPPU F.
    2003(1) 19-24, Sep 19, 2003  
  • Fujimoto R, Mitsuda K, Yamasaki Y, Ohashi T, Ishisaki Y, Kelley R. L, Stahle C. K, Furusho T, McCammon D, Astro-E, XRS team
    Meeting abstracts of the Physical Society of Japan, 58(1) 86-86, Mar 6, 2003  
  • Iyomoto N, Ichitsubo T, Mitsuda K, Yamasaki N, Fujimoto R, Oshima Y, Futamoto K, Takei Y, Fujimori T, Miyazaki T, Ohashi T, Ishisaki Y, Morita U, Sato K, Koga T, Tanaka K, Morooka T, Nakayama S, Chinone K
    Meeting abstracts of the Physical Society of Japan, 58(1) 94-94, Mar 6, 2003  
  • 藤本 龍一, 満田 和久, 山崎 典子
    宇宙科学シンポジウム, 3 499-502, Jan 9, 2003  
  • 満田 和久, 山崎 典子, 藤本 龍一
    宇宙科学シンポジウム, 3 127-130, Jan 9, 2003  
  • H Kudo, T Nakamura, T Arakawa, S Ohtsuka, T Izumi, S Shoji, H Sato, H Kobayashi, K Mori, T Homma, T Osaka, K Mitsuda, NY Yamasaki, R Fujimoto, N Iyomoto, T Oshima, K Futamoto, Y Takei, T Ichitsubo, T Fujimori, Y Ishisaki, U Morita, T Koga, K Sato, T Ohashi, Y Kuroda, M Onishi, K Otake
    NANOTECH 2003, VOL 1, 1 436-439, 2003  
    An x-ray microcalorimeter is a promising x-ray spectrometer for its extremely good energy resolution and its good detecting efficiency. We are developing an x-ray microcalorimeter for high energy resolution x-ray imaging application. The energy resolution of 43eV(FWHM) at 5.9keV is obtained with our x-ray microcalorimeter. The intrinsic performance of our x-ray microcalorimeter was estimated to be 10.4eV(FWHM) at 5.9keV. This value is more than 10 times better than that of the 2 WORKING PRINCIPLES conventional x-ray CCD.
  • H Kudo, T Nakamura, T Arakawa, S Ohtsuka, T Izumi, S Shoji, H Sato, H Kobayashi, K Mori, T Homma, T Osaka, K Mitsuda, NY Yamasaki, R Fujimoto, N Iyomoto, T Oshima, K Futamoto, Y Takei, T Ichitsubo, T Fujimori, Y Ishisaki, U Morita, T Koga, K Sato, T Ohashi, Y Kuroda, M Onishi, K Otake
    BOSTON TRANSDUCERS'03: DIGEST OF TECHNICAL PAPERS, VOLS 1 AND 2, 1108-1111, 2003  
    An x-ray microcalorimeter is a noble x-ray spectrometer that can be used for photon counting with a high energy resolution comparable to the gratings. A 2x2 x-ray microcalorimeter array was fabricated and tested. Due to the purpose of imaging application, we have applied so-called 'mushroom-shaped' x-ray microabsorber fabricated using two-step exposure and electrodeposition process. The energy resolution of 180eV(FWHM) at 5.9keV was obtained with the first prototype of the x-ray microcalorimeter array using Sri microabsorber. By using Bi absorber, it is,estimated that the energy resolution can be improved up to 4.5eV.
  • Takei Y., Fujimori T., Ishisaki Y., Koga T., Sato K., Ohashi T., Kudo H., Sato H., Nakamura T., Kobayashi H., Arakawa T., Morita U., Otsuka S., Izumi T., Mori K., Shoji S., Honma T., Osaka T., Tanaka K., Morooka T., Nakayama T., Chinone K., Mitsuda K., Kuroda Y., Onishi M., Ichitubo T., Iyomoto N., Fujimoto R., Yamasaki N., Futamoto K., Oshima T.
    Meeting Abstracts of the Physical Society of Japan, 58(1) 94-94, 2003  
  • 森田うめ代, 石崎欣尚, 古賀丈雄, 佐藤浩介, 大橋隆哉, 伊予本直子, 竹井洋, 市坪太郎, 満田和久, 山崎典子, 藤本龍一, 大島泰, 二元和朗, 藤森玉行, TERRACOL S. F., 宮崎利行, FRIEDRICH S., 田中啓一, 師岡利光, 中山哲, 茅根一夫
    日本天文学会年会講演予稿集, 2003, 2003  
  • 伊予本直子, 市坪太郎, 満田和久, 山崎典子, 藤本龍一, 大島泰, 二元和朗, 竹井洋, 藤森玉行, 宮崎利行, 石崎欣尚, 古賀丈雄, 森田うめ代, 佐藤浩介, 大橋隆哉, 田中啓一, 師岡利光, 中山哲, 茅根一夫
    日本天文学会年会講演予稿集, 2003, 2003  
  • 古賀丈雄, 森田うめ代, 石崎欣尚, 佐藤浩介, 大橋隆哉, 伊予本直子, 市坪太郎, 満田和久, 山崎典子, 藤本龍一, 大島泰, 二元和朗, 竹井洋, 藤森玉行, 庄子習一, 工藤寛之, 中村友亮, 荒川貴博, 泉俊光, 大塚真一郎, 逢坂哲彌, 本間敬之, 佐藤裕崇, 小林秀臣, 森健太郎, 黒田能克, 大西光延, 後藤雅也
    日本天文学会年会講演予稿集, 2003, 2003  
  • 古賀丈雄, 森田うめ代, 石崎欣尚, 佐藤浩介, 大橋隆哉, 伊予本直子, 市坪太郎, 満田和久, 山崎典子, 藤本龍一, 大島泰, 二元和朗, 竹井洋, 藤森玉行, 庄子習一, 工藤寛之, 中村友亮, 荒川貴博, 泉俊光, 大塚真一郎, 逢坂哲彌, 本間敬之, 佐藤裕崇, 小林秀臣, 森健太郎, 黒田能克, 大西光延, 後藤雅也, 別府史章
    日本天文学会年会講演予稿集, 2003, 2003  
  • 穴吹直久, 藤本龍一, 井上一, 中川貴雄
    日本天文学会年会講演予稿集, 2003, 2003  
  • TSURUDOME Takehisa, KANAO Kenichi, HASEBE Tsuginori, NARASAKI Katsuhiro, HIRABAYASHI Masayuki, YOSHIDA Seiji, MITSUDA Kazuhisa, FUJIMOTO Ryuichi
    67 185-185, Oct 30, 2002  
  • KANAO Ken-ichi, HASEBE Tsuginori, TSURUDOME Takehisa, NARASAKI Katsuhiro, HIRABAYASHI Masayuki, YOSHIDA Seiji, MITSUDA Kazuhisa, FUJIMOTO Ryuichi
    67 184-184, Oct 30, 2002  
  • Sato K., Morita U., Koga T., Ishisaki Y., Ohashi T., Takei Y., Ichitsubo T., Fujimori T., Futamoto K., Oshima Y., Iyomoto N., Fujimoto R., Yamasaki N.Y., Mitsuda K.
    Meeting abstracts of the Physical Society of Japan, 57(2) 85-85, Aug 13, 2002  
  • 伊予本 直子, 満田 和久, 藤本 龍一, 大島 泰, 二元 和朗, 竹井 洋, 宮崎 利行, 大橋 隆哉, 山崎 典子, 石崎 欣尚, 広池 哲平, 森田 うめ代, 中山 哲
    日本物理学会講演概要集, 57(1) 81-81, Mar 1, 2002  
  • 広池 哲平, 二元 和朗, 竹井 洋, 工藤 寛之, 佐藤 裕崇, 中村 友亮, 小林 秀臣, 庄子 習一, 本間 敬之, 逢坂 哲彌, 黒田 能克, 大橋 隆哉, 大西 光延, 後藤 雅也, 田中 啓一, 師岡 利光, 中山 哲, 茅根 一夫, 山崎 典子, 石崎 欣尚, 森田 うめ代, 満田 和久, 藤本 龍一, 伊予本 直A, 大島 泰
    日本物理学会講演概要集, 57(1) 81-81, 2002  
  • 森田うめ代, 大橋隆哉, 山崎典子, 石崎欣尚, 広池哲平, 満田和久, 藤本龍一, 伊予本直子, 大島泰, 二元和朗, 竹井洋, 田中啓一, 師岡利光, 中山哲, 茅根一夫
    日本天文学会年会講演予稿集, 2002, 2002  
  • 森田うめ代, 石崎欣尚, 佐藤浩介, 古賀丈雄, 大橋隆哉, 山崎典子, 満田和久, 藤本龍一, 伊予本直子, 大島泰, 竹井洋, 市坪太郎, 藤森玉行, 二元和朗
    日本天文学会年会講演予稿集, 2002, 2002  
  • 石崎欣尚, 森田うめ代, 佐藤浩介, 古賀丈雄, 大橋隆哉, 山崎典子, 満田和久, 藤本龍一, 伊予本直子, 大島泰, 竹井洋, 市坪太郎, 藤森玉行, 二元和朗
    日本天文学会年会講演予稿集, 2002, 2002  
  • 市坪太郎, 伊予本直子, 満田和久, 藤本龍一, 大島泰, 二元和朗, 竹井洋, 藤森玉行, 宮崎利行, 大橋隆哉, 山崎典子, 石崎欣尚, 森田うめ代, 佐藤浩介, 古賀丈雄, 田中啓一, 師岡利光, 中山哲, 茅根一夫
    日本天文学会年会講演予稿集, 2002, 2002  
  • 古賀丈雄, 石崎欣尚, 森田うめ代, 佐藤浩介, 大橋隆哉, 山崎典子, 満田和久, 藤本龍一, 伊予本直子, 大島泰, 竹井洋, 市坪太郎, 藤森玉行, 二元和朗, 田中啓一, 師岡利光, 中山哲, 茅根一夫
    日本天文学会年会講演予稿集, 2002, 2002  
  • 穴吹直久, 藤本龍一, 米徳大輔, 中川貴雄, 井上一
    日本天文学会年会講演予稿集, 2002, 2002  
  • 満田 和久, 国枝 秀世, 藤本 龍一
    宇宙科学シンポジウム, 2 375-378, Nov 19, 2001  
  • 伊予本 直子, 満田 和久, 藤本 龍一, 大島 泰, 二元 和朗, 竹井 洋, 大橋 隆哉, 山崎 典子, 石崎 欣尚, 広池 哲平, 森田 うめ代, 工藤 寛之, 佐藤 裕崇, 中村 友亮, 小林 秀臣, 庄子 習一, 本間 敬之, 逢坂 哲彌, 黒田 能克, 大西 光延, 後藤 雅也
    日本物理学会講演概要集, 56(2) 47-47, Sep 3, 2001  
  • Hiroike T., Futamoto K., Takei Y., Kudo H., Hirotaka S., Nakamura T., Kobayashi H., Shoji S., Homma K., Osaka T., Kuroda Y., Ohashi T., Onishi M., Goto M., Yamasaki N., Ishisaki Y., Morita U., Mitsuda K., Fujimoto R., Iyomoto N., Oshima Y.
    Meeting Abstracts of the Physical Society of Japan, 56 48-48, 2001  
  • 石崎欣尚, 影井智宏, 大橋隆哉, 山崎典子, 久志野彰寛, 広池哲平, 宮崎利行, 大島泰, 満田和久, 藤本龍一, 伊予本直子, AUDLEY M. D., 山崎正裕, 二元和朗, 庄子習一, 工藤寛之, 横山雄一
    日本天文学会年会講演予稿集, 2001, 2001  
  • 二元和朗, 山崎正裕, 満田和久, 藤本龍一, 伊予本直子, 宮崎利行, 大島泰, AUDLEY M. D., 石崎欣尚, 影井智宏, 広池哲平, 大橋隆哉, 山崎典子, 庄子習一, 工藤寛之, 横山雄一
    日本天文学会年会講演予稿集, 2001, 2001  
  • 竹井洋, 満田和久, 藤本龍一, 伊豫本直子, 大島泰, 二元和朗, 森田うめ代, 広池哲平, 大橋隆哉, 山崎典子, 石崎欣尚, 庄子習一, 工藤寛之, 田中啓一, 師岡利光, 中山哲, 茅根一夫
    日本天文学会年会講演予稿集, 2001, 2001  

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