2021/06/22 更新

写真b

イチノヘ ユウト
一戸 悠人
ICHINOHE Yuto
*大学が定期的に情報更新している項目(その他は、researchmapの登録情報を転載)
所属*
理学部 物理学科
職名*
助教
学位
博士(理学) ( 東京大学 ) / 修士(理学) ( 東京大学 )
担当科目*
学内職務経歴*
  • 2018年4月 - 現在 
    理学部   物理学科   助教
 

研究分野

  • 自然科学一般 / 天文学

  • 自然科学一般 / 素粒子、原子核、宇宙線、宇宙物理にする理論

経歴

  • 2018年4月 - 現在 
    立教大学   理学部 物理学科   助教

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  • 2016年4月 - 2018年3月 
    首都大学東京   理工学研究科   日本学術振興会特別研究員

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学歴

  • - 2016年3月 
    東京大学   理学系研究科   物理学専攻

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    国名: 日本国

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  • - 2016年3月 
    東京大学   理学系研究科   物理学専攻

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    国名: 日本国

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  • - 2016年3月 
    東京大学   理学系研究科   物理学専攻

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    国名: 日本国

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  • - 2013年3月 
    東京大学   理学系研究科   物理学専攻

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    国名: 日本国

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  • - 2011年3月 
    東京大学   理学部   物理学科

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    国名: 日本国

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受賞

  • 2013年5月  
    KEK測定器開発室  第3回測定器開発・優秀修士論文賞 
     
    一戸悠人

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    受賞区分:国内学会・会議・シンポジウム等の賞 

    受賞国:日本国

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論文

  • CAMELOT: design and performance verification of the detector concept and localization capability

    Masanori Ohno, Norbert Werner, András Pál, Jakub Řípa, Gabór Galgóczi, Norbert Tarcai, Zsolt Várhegyi, Yasushi Fukazawa, Tsunefumi Mizuno, Hiromitsu Takahashi, Koji Tanaka, Nagomi Uchida, Kento Torigoe, Kazuhiro Nakazawa, Teruaki Enoto, Hirokazu Odaka, Yuto Ichinohe, Zsolt Frei, László Kiss

    Proc. SPIE 10699, Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray   2018年7月6日

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

    DOI: 10.1117/12.2313228

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  • CAMELOT: Cubesats Applied for MEasuring and LOcalising Transients mission overview

    Norbert Werner, Jakub Řípa, András Pál, Masanori Ohno, Norbert Tarcai, Kento Torigoe, Koji Tanaka, Nagomi Uchida, László Mészáros, Gabór Galgóczi, Yasushi Fukazawa, Tsunefumi Mizuno, Hiromitsu Takahashi, Kazuhiro Nakazawa, Zsolt Várhegyi, Teruaki Enoto, Hirokazu Odaka, Yuto Ichinohe, Zsolt Frei, László Kiss

    Proc. SPIE 10699, Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray   2018年7月6日

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

    DOI: 10.1117/12.2313764

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  • Super DIOS: future x-ray spectroscopic mission to search for dark baryons

    T. Ohashi, Y. Ishisaki, Y. Ezoe, S. Yamada, R. Hayakawa, K. Nunomura, K. Sato, Y. Tawara, I. Mitsuishi, K. Ohtsuka, K. Mitsuda, N. Y. Yamasaki, T. Kikuchi, T. Hayashi, H. Muramatsu, Y. Nakashima, N. Ota, K. Osato, Y. Ichinohe, M. E. Eckart, S. R. Bandler, R. L. Kelley, C. A. Kilbourne

    Proc. SPIE 10699, Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray   2018年7月6日

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

    DOI: 10.1117/12.2313122

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

    Hitomi Collaboration, including Yuto Ichinohe

    Publications of the Astronomical Society of Japan70 ( 3 ) 38   2018年6月1日

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    記述言語:英語   掲載種別:研究論文(学術雑誌)  

    DOI: 10.1093/pasj/psy027

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  • Super DIOS: Future X-ray Spectroscopic Mission to Search for Dark Baryons 査読有り

    S. Yamada, T. Ohashi, Y. Ishisaki, Y. Ezoe, Y. Ichinohe, S. Kitazawa, K. Kosaka, R. Hayakawa, K. Nunomura, K. Mitsuda, N. Y. Yamasaki, T. Kikuchi, T. Hayashi, H. Muramatsu, Y. Nakashima, Y. Tawara, I. Mitsuishi, Y. Babazaki, D. Seki, K. Otsuka, M. Ishihara, K. Osato, N. Ota, M. Tomariguchi, D. Nagai, E. Lau, K. Sato, the DIOS team

    Journal of Low Temperature Physics   1 - 8   2018年4月24日

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    記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Springer New York LLC  

    The updated program of the future Japanese X-ray satellite mission Diffuse Intergalactic Oxygen Surveyor (DIOS), called as Super DIOS, is planned to search for dark baryons in the form of warm–hot intergalactic medium (WHIM) with high-resolution X-ray spectroscopy. The mission will detect redshifted emission lines from OVII, OVIII and other ions, leading to an overall understanding of the physical nature and spatial distribution of dark baryons as a function of cosmological timescale. We have started the conceptual design of the satellite and onboard instruments, focusing on the era of 2030s. The major change will be an improved angular resolution of the X-ray telescope. Super DIOS will have a 10-arcsec resolution, which is an improvement by a factor of about 20 over DIOS. With this resolution, most of the contaminating X-ray sources will be separated, and the level of the diffuse X-ray background will be much reduced after subtraction of point sources. This will give us higher sensitivity to map out the WHIM in emission.

    DOI: 10.1007/s10909-018-1918-z

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  • Neural network-based preprocessing to estimate the parameters of the X-ray emission of a single-temperature thermal plasma 査読有り

    Y. Ichinohe, S. Yamada, N. Miyazaki, S. Saito

    Monthly Notices of the Royal Astronomical Society475 ( 4 ) 4739 - 4744   2018年4月21日

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

    We present data preprocessing based on an artificial neural network to estimate the parameters of the X-ray emission spectra of a single-temperature thermal plasma. The method finds appropriate parameters close to the global optimum. The neural network is designed to learn the parameters of the thermal plasma (temperature, abundance, normalization and redshift) of the input spectra. After training using 9000 simulated X-ray spectra, the network has grown to predict all the unknown parameters with uncertainties of about a fewper cent. The performance dependence on the network structure has been studied. We applied the neural network to an actual high-resolution spectrum obtained with Hitomi. The predicted plasma parameters agree with the known best-fitting parameters of the Perseus cluster within uncertainties of ≲10 per cent. The result shows that neural networks trained by simulated data might possibly be used to extract a feature built in the data. This would reduce human-intensive preprocessing costs before detailed spectral analysis, and would help us make the best use of the large quantities of spectral data that will be available in the coming decades.

    DOI: 10.1093/mnras/sty161

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  • Resolve Instrument on X-ray Astronomy Recovery Mission (XARM) 査読有り

    Y. Ishisaki, Y. Ezoe, S. Yamada, Y. Ichinohe, R. Fujimoto, Y. Takei, S. Yasuda, M. Ishida, N. Y. Yamasaki, Y. Maeda, M. Tsujimoto, R. Iizuka, S. Koyama, H. Noda, T. Tamagawa, M. Sawada, K. Sato, S. Kitamoto, A. Hoshino, G. V. Brown, M. E. Eckart, T. Hayashi, R. L. Kelley, C. A. Kilbourne, M. A. Leutenegger, H. Mori, T. Okajima, F. S. Porter, Y. Soong, D. McCammon, A. E. Szymkowiak, The XARM Resolve Team

    Journal of Low Temperature Physics   1 - 5   2018年4月19日

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    記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Springer New York LLC  

    The X-ray Astronomy Recovery Mission (XARM) is a recovery mission of ASTRO-H/Hitomi, which is expected to be launched in Japanese Fiscal Year of 2020 at the earliest. The Resolve instrument on XARM consists of an array of 6 × 6 silicon-thermistor microcalorimeters cooled down to 50 mK and a high-throughput X-ray mirror assembly with the focal length of 5.6 m. Hitomi was launched into orbit in February 2016 and observed several celestial objects, although the operation of Hitomi was terminated in April 2016. The soft X-ray spectrometer (SXS) on Hitomi demonstrated high-resolution X-ray spectroscopy of ~ 5 eV FWHM in orbit for most of the pixels. The Resolve instrument is planned to mostly be a copy of the Hitomi SXS and soft X-ray telescope designs, though several changes are planned based on the lessons learned from Hitomi. We report a brief summary of the SXS performance and the status of the Resolve instrument.

    DOI: 10.1007/s10909-018-1913-4

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  • HITOMI (ASTRO-H) X-ray astronomy satellite 査読有り

    Tadayuki Takahashi, Motohide Kokubun, Kazuhisa Mitsuda, Richard L. Kelley, Takaya Ohashi, Felix Aharonian, Hiroki Akamatsu, Fumie Akimoto, Steven W. Allen, Naohisa Anabuki, Lorella Angelini, Keith Arnaud, Makoto Asai, Marc Audard, Hisamitsu Awaki, Magnus Axelsson, Philipp Azzarello, Chris Baluta, Aya Bamba, Nobutaka Bando, Marshall W. Bautz, Thomas Bialas, Roger Blandford, Kevin Boyce, Laura W. Brenneman, Gregory V. Brown, Esra Bulbul, Edward M. Cackett, Edgar Canavan, Maria Chernyakova, Meng P. Chiao, Paolo S. Coppi, Elisa Costantini, Steve O' Dell, Michael DiPirro, Chris Done, Tadayasu Dotani, John Doty, Ken Ebisawa, Megan E. Eckart, Teruaki Enoto, Yuichiro Ezoe, Andrew C. Fabian, Carlo Ferrigno, Adam R. Foster, Ryuichi Fujimoto, Yasushi Fukazawa, Stefan Funk, Akihiro Furuzawa, Massimiliano Galeazzi, Luigi C. Gallo, Poshak Gandhi, Kirk Gilmore, Margherita Giustini, Andrea Goldwurm, Liyi Gu, Matteo Guainazzi, Daniel Haas, Yoshito Haba, Kouichi Hagino, Kenji Hamaguchi, Ilana M. Harrus, Isamu Hatsukade, Takayuki Hayashi, Katsuhiro Hayashi, Kiyoshi Hayashida, Jan Willem Den Herder, Junko S. Hiraga, Kazuyuki Hirose, Ann Hornschemeier, Akio Hoshino, John P. Hughes, Yuto Ichinohe, Ryo Iizuka, Hajime Inoue, Yoshiyuki Inoue, Kazunori Ishibashi, Manabu Ishida, Kumi Ishikawa, Kosei Ishimura, Yoshitaka Ishisaki, Masayuki Itoh, Masachika Iwai, Naoko Iwata, Naoko Iyomoto, Chris Jewell, Jelle Kaastra, Tim Kallman, Tsuneyoshi Kamae, Erin Kara, Jun Kataoka, Satoru Katsuda, Junichiro Katsuta, Madoka Kawaharada, Nobuyuki Kawai, Taro Kawano, Shigeo Kawasaki, Dmitry Khangulyan, Caroline A. Kilbourne, Mark Kimball

    Journal of Astronomical Telescopes, Instruments, and Systems4 ( 2 )   2018年4月

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    記述言語:英語   掲載種別:研究論文(学術雑誌)  

    © The Authors. The Hitomi (ASTRO-H) mission is the sixth Japanese x-ray astronomy satellite developed by a large international collaboration, including Japan, USA, Canada, and Europe. The mission aimed to provide the highest energy resolution ever achieved at E > 2 keV, using a microcalorimeter instrument, and to cover a wide energy range spanning four decades in energy from soft x-rays to gamma rays. After a successful launch on February 17, 2016, the spacecraft lost its function on March 26, 2016, but the commissioning phase for about a month provided valuable information on the onboard instruments and the spacecraft system, including astrophysical results obtained from first light observations. The paper describes the Hitomi (ASTRO-H) mission, its capabilities, the initial operation, and the instruments/spacecraft performances confirmed during the commissioning operations for about a month.

    DOI: 10.1117/1.JATIS.4.2.021402

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  • Design and performance of Soft Gamma-ray Detector onboard the Hitomi (ASTRO-H) satellite 査読有り

    Hiroyasu Tajima, Shin Watanabe, Yasushi Fukazawa, Roger Blandford, Teruaki Enoto, Andrea Goldwurm, Kouichi Hagino, Katsuhiro Hayashi, Yuto Ichinohe, Jun Kataoka, Junichiro Katsuta, Takao Kitaguchi, Motohide Kokubun, Philippe Laurent, François Lebrun, Olivier Limousin, Grzegorz M. Madejski, Kazuo Makishima, Tsunefumi Mizuno, Kunishiro Mori, Takeshi Nakamori, Toshio Nakano, Kazuhiro Nakazawa, Hirofumi Noda, Hirokazu Odaka, Masanori Ohno, Masayuki Ohta, Shinya Saito, Goro Sato, Rie Sato, Shinichiro Takeda, Hiromitsu Takahashi, Tadayuki Takahashi, Takaaki Tanaka, Yasuyuki Tanaka, Yukikatsu Terada, Hideki Uchiyama, Yasunobu Uchiyama, Kazutaka Yamaoka, Yoichi Yatsu, Daisuke Yonetoku, Takayuki Yuasa

    Journal of Astronomical Telescopes, Instruments, and Systems4 ( 2 )   2018年4月1日

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

    Hitomi (ASTRO-H) was the sixth Japanese X-ray satellite that carried instruments with exquisite energy resolution of &lt
    7 eV and broad energy coverage of 0.3 to 600 keV. The Soft Gamma-ray Detector (SGD) was the Hitomi instrument that observed the highest energy band (60 to 600 keV). The SGD design achieves a low background level by combining active shields and Compton cameras where Compton kinematics is utilized to reject backgrounds coming from outside of the field of view. A compact and highly efficient Compton camera is realized using a combination of silicon and cadmium telluride semiconductor sensors with a good energy resolution. Compton kinematics also carries information for gamma-ray polarization, making the SGD an excellent polarimeter. Following several years of development, the satellite was successfully launched on February 17, 2016. After proper functionality of the SGD components were verified, the nominal observation mode was initiated on March 24, 2016. The SGD observed the Crab Nebula for approximately two hours before the spacecraft ceased to function on March 26, 2016. We present concepts of the SGD design followed by detailed description of the instrument and its performance measured on ground and in orbit.

    DOI: 10.1117/1.JATIS.4.2.021411

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  • Glimpse of the highly obscured HMXB IGR J16318−4848 with Hitomi 査読有り

    Hitomi Collaboration, including Yuto Ichinohe

    Publications of the Astronomical Society of Japan70 ( 2 ) 17   2018年3月1日

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    記述言語:英語   掲載種別:研究論文(学術雑誌)  

    DOI: 10.1093/pasj/psx154

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  • Hitomi observations of the LMC SNR N 132 D: Highly redshifted X-ray emission from iron ejecta 査読有り

    Hitomi Collaboration, including Yuto Ichinohe

    Publications of the Astronomical Society of Japan70 ( 2 ) 16   2018年3月1日

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    記述言語:英語   掲載種別:研究論文(学術雑誌)  

    DOI: 10.1093/pasj/psx151

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  • Hitomi X-ray studies of giant radio pulses from the Crab pulsar 査読有り

    Felix Aharonian, Hiroki Akamatsu, Fumie Akimoto, Steven W. Allen, Lorella Angelini, Marc Audard, Hisamitsu Awaki, Magnus Axelsson, Aya Bamba, Marshall W. Bautz, Roger Blandford, Laura W. Brenneman, Gregory V. Brown, Esra Bulbul, Edward M. Cackett, Maria Chernyakova, Meng P. Chiao, Paolo S. Coppi, Elisa Costantini, Jelle De Plaa, Cor P. De Vries, 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, L. E.E. Shiu-Hang, Maurice A. Leutenegger, Olivier O. Limousin, 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

    Publications of the Astronomical Society of Japan70 ( 2 ) 15   2018年3月1日

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    記述言語:英語   掲載種別:研究論文(学術雑誌)  

    © The Author(s) 2017. Published by Oxford University Press on behalf of the Astronomical Society of Japan. To search for giant X-ray pulses correlated with the giant radio pulses (GRPs) from the Crab pulsar, we performed a simultaneous observation of the Crab pulsar with the X-ray satellite Hitomi in the 2-300 keV band and the Kashima NICT radio telescope in the 1.4-1.7 GHz band with a net exposure of about 2 ks on 2016 March 25, just before the loss of the Hitomi mission. The timing performance of the Hitomi instruments was confirmed to meet the timing requirement and about 1000 and 100 GRPs were simultaneously observed at the main pulse and inter-pulse phases, respectively, and we found no apparent correlation between the giant radio pulses and the X-ray emission in either the main pulse or inter-pulse phase. All variations are within the 2 σ fluctuations of the X-ray fluxes at the pulse peaks, and the 3 σ upper limits of variations of main pulse or inter-pulse GRPs are 22% or 80% of the peak flux in a 0.20 phase width, respectively, in the 2-300 keV band. The values for main pulse or inter-pulse GRPs become 25% or 110%, respectively, when the phase width is restricted to the 0.03 phase. Among the upper limits from the Hitomi satellite, those in the 4.5-10 keV and 70-300 keV bands are obtained for the first time, and those in other bands are consistent with previous reports. Numerically, the upper limits of the main pulse and inter-pulse GRPs in the 0.20 phase width are about (2.4 and 9.3) × 10−11 erg cm−2, respectively. No significant variability in pulse profiles implies that the GRPs originated from a local place within the magnetosphere. Although the number of photon-emitting particles should temporarily increase to account for the brightening of the radio emission, the results do not statistically rule out variations correlated with the GRPs, because the possible X-ray enhancement may appear due to a >0.02% brightening of the pulse-peak flux under such conditions.

    DOI: 10.1093/pasj/psx083

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  • Search for thermal X-ray features from the Crab nebula with the Hitomi soft X-ray spectrometer 査読有り

    Hitomi Collaboration, including Yuto Ichinohe

    Publications of the Astronomical Society of Japan70 ( 2 ) 14   2018年3月1日

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    記述言語:英語   掲載種別:研究論文(学術雑誌)  

    DOI: 10.1093/pasj/psx072

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  • Hitomi observation of radio galaxy NGC 1275: The first X-ray microcalorimeter spectroscopy of Fe-Kα line emission from an active galactic nucleus 査読有り

    Hitomi Collaboration, including Yuto Ichinohe

    Publications of the Astronomical Society of Japan70 ( 2 ) 13   2018年3月1日

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    記述言語:英語   掲載種別:研究論文(学術雑誌)  

    DOI: 10.1093/pasj/psx147

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  • Atomic data and spectral modeling constraints from high-resolution X-ray observations of the Perseus cluster with Hitomi 査読有り

    Hitomi Collaboration, including Yuto Ichinohe

    Publications of the Astronomical Society of Japan70 ( 2 ) 12   2018年3月1日

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    記述言語:英語   掲載種別:研究論文(学術雑誌)  

    DOI: 10.1093/pasj/psx156

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  • Temperature structure in the Perseus cluster core observed with Hitomi 査読有り

    Hitomi Collaboration, including Yuto Ichinohe

    Publications of the Astronomical Society of Japan70 ( 2 ) 11   2018年3月1日

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    記述言語:英語   掲載種別:研究論文(学術雑誌)  

    DOI: 10.1093/pasj/psy004

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  • Measurements of resonant scattering in the Perseus Cluster core with Hitomi SXS 査読有り

    Hitomi Collaboration, including Yuto Ichinohe

    Publications of the Astronomical Society of Japan70 ( 2 ) 10   2018年3月1日

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    記述言語:英語   掲載種別:研究論文(学術雑誌)  

    DOI: 10.1093/pasj/psx127

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  • Atmospheric gas dynamics in the Perseus cluster observed with Hitomi 査読有り

    Hitomi Collaboration, including Yuto Ichinohe as the first corresponding author

    Publications of the Astronomical Society of Japan70 ( 2 ) 9   2018年3月1日

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    記述言語:英語   掲載種別:研究論文(学術雑誌)  

    DOI: 10.1093/pasj/psx138

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  • CAMELOT - Concept study and early results for onboard data processing and GPS-based timestamping

    András Pál, László Mészáros, Norbert Tarcai, Norbert Werner, Jakub Řípa, Masanori Ohno, Kento Torigoe, Koji Tanaka, Nagomi Uchida, Gabór Galgóczi, Yasushi Fukazawa, Tsunefumi Mizuno, Hiromitsu Takahashi, Kazuhiro Nakazawa, Zsolt Várhegyi, Teruaki Enoto, Hirokazu Odaka, Yuto Ichinohe, Zsolt Frei, László Kiss

    arXiv   2018年

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    記述言語:英語  

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  • Performance study of a large CsI(Tl) scintillator with an MPPC readout for nanosatellites used to localize gamma-ray bursts 査読有り

    Kento Torigoe, Yasushi Fukazawa, Gabór Galgóczi, Tsunefumi Mizuno, Kazuhiro Nakazawa, Masanori Ohno, András Pál, Hiromitsu Takahashi, Koji Tanaka, Norbert Tarcai, Nagomi Uchida, Norbert Werner, Teruaki Enoto, Zsolt Frei, Yuto Ichinohe, László Kiss, Hirokazu Odaka, Jakub Řípa, Zsolt Várhegyi

    Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment   2018年

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    記述言語:英語   掲載種別:研究論文(学術雑誌)  

    DOI: 10.1016/j.nima.2018.08.039

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  • Multiwavelength study of X-ray luminous clusters in the Hyper Suprime-Cam Subaru Strategic Program S16A field 査読有り

    Keita Miyaoka, Nobuhiro Okabe, Takao Kitaguchi, Masamune Oguri, Yasushi Fukazawa, Rachel Mandelbaum, Elinor Medezinski, Yasunori Babazaki, Atsushi J. Nishizawa, Takashi Hamana, Yen-Ting Lin, Hiroki Akamatsu, I-Non Chiu, Yutaka Fujita, Yuto Ichinohe, Yutaka Komiyama, Toru Sasaki, Motokazu Takizawa, Shutaro Ueda, Keiichi Umetsu, Jean Coupon, Chiaki Hikage, Akio Hoshino, Alexie Leauthaud, Kyoko Matsushita, Ikuyuki Mitsuishi, Hironao Miyatake, Satoshi Miyazaki, Surhud More, Kazuhiro Nakazawa, Naomi Ota, Kousuke Sato, David Spergel, Takayuki Tamura, Masayuki Tanaka, Manobu M Tanaka, Yousuke Utsumi

    Publications of the Astronomical Society of Japan70 ( SP1 ) S22   2018年1月1日

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

    We present a joint X-ray, optical, and weak-lensing analysis for X-ray luminous galaxy clusters selected from the MCXC (Meta-Catalog of X-Ray Detected Clusters of Galaxies) cluster catalog in the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) survey field with S16A data. As a pilot study for a series of papers, we measure hydrostatic equilibrium (HE) masses using XMM-Newton data for four clusters in the current coverage area out of a sample of 22 MCXC clusters. We additionally analyze a non-MCXC cluster associated with one MCXC cluster. We show that HE masses for the MCXC clusters are correlated with cluster richness from the CAMIRA catalog, while that for the non-MCXC cluster deviates from the scaling relation. The mass normalization of the relationship between cluster richness and HE mass is compatible with one inferred by matching CAMIRA cluster abundance with a theoretical halo mass function. The mean gas mass fraction based on HE masses for the MCXC clusters is (fgas) = 0.125 ± 0.012 at spherical overdensity Δ = 500, which is ∼80%-90% of the cosmic mean baryon fraction, Ωb/Ωm,measured by cosmicmicrowave background experiments. We find that themean baryon fraction estimated from X-ray and HSC-SSP optical data is comparable to Ωb/Ωm. A weak-lensing shear catalog of background galaxies, combined with photometric redshifts, is currently available only for three clusters in our sample. Hydrostatic equilibrium masses roughly agree with weak-lensing masses, albeit with large uncertainty. This study demonstrates that further multi wave length study for a large sample of clusters using X-ray, HSC-SSP optical, and weak-lensing data will enable us to understand cluster physics and utilize cluster-based cosmology.

    DOI: 10.1093/pasj/psx132

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  • Concept of X-ray Astronomy Recovery Mission

    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, Stephane Paltani, Kyoko Matsushita, Koji Mori, Gary Sneiderman, Yoh Takei, Yukikatsu Terada, Hiroshi Tomida, Hiroki Akamatsu, Lorella Angelini, 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, 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, Tom Lockard, Mike Loewenstein, Yoshitomo Maeda, Lynette Marbley, Maxim Markevitch, Connor Martz, 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 Sugawara, 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 Yamasaki, Shigeo Yamauchi, Makoto Yamauchi, Keiichi Yanagase, Tahir Yaqoob, Susumu Yasuda, Nasa Yoshioka, Jaime Zabala, Irina Zhuravleva

    SPACE TELESCOPES AND INSTRUMENTATION 2018: ULTRAVIOLET TO GAMMA RAY10699   2018年

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

    The 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 x 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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  • Solar abundance ratios of the iron-peak elements in the Perseus cluster 査読有り

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

    NATURE551 ( 7681 ) 478 - +   2017年11月

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

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

    DOI: 10.1038/nature24301

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  • An azimuthally resolved study of the cold front in Abell 3667 査読有り

    Y. Ichinohe, A. Simionescu, N. Werner, T. Takahashi

    MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY467 ( 3 ) 3662 - 3676   2017年6月

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

    The microphysical properties, such as effective viscosity and conductivity, of the weakly magnetized intergalactic plasma are not yet well known. We investigate the constraints that can be placed by an azimuthally resolved study of the cold front in Abell 3667 using similar to 500 ks archival Chandra data. We find that the radius of the interface fluctuates with position angle and the morphology of the interface is strikingly similar to recent numerical simulations of inviscid gas-stripping. We find multiple edges in the surface brightness profiles across the cold front as well as azimuthal variations, which are consistent with the presence of Kelvin-Helmholtz instabilities (KHIs) developing along the cold front. They indicate that the characteristic length-scale of KHI rolls is around 20-80 kpc. This is the first observational indication of developing KHIs along a merger cold front in a galaxy cluster. Based on the KHI scenario, we estimated the upper limit of the intracluster medium effective viscosity. The estimated value of mu less than or similar to 200 g cm(-1) s(-1) is at most 5 per cent of the isotropic Spitzer-like viscosity. The observed apparent mixing towards the outer edges away from the tip of the front provides an additional evidence for suppressed viscosity.

    DOI: 10.1093/mnras/stx280

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  • Hitomi Constraints on the 3.5 keV Line in the Perseus Galaxy Cluster 査読有り

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

    ASTROPHYSICAL JOURNAL LETTERS837 ( 1 ) L15   2017年3月

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

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

    DOI: 10.3847/2041-8213/aa61fa

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  • Beamline test of a transition-edge-sensor spectrometer in preparation for kaonic-atom measurements 査読有り

    Hashimoto, T., Bazzi, M., Bennett, D.A., Berucci, C., Bosnar, D., Curceanu, C., Doriese, W.B., Fowler, J.W., Fujioka, H., Guaraldo, C., Parnefjord Gustafsson, F., Hayakawa, R., Hayano, R.S., Hays-Wehle, J.P., Hilton, G.C., Hiraiwa, T., Ichinohe, Y., Iio, M., Iliescu, M., Ishimoto, S., Ishisaki, Y., Itahashi, K., Iwasaki, M., Ma, Y., Noda, H., Noumi, H., O'Neil, G.C., Ohnishi, H., Okada, S., Outa, H., Piscicchia, K., Reintsema, C.D., Sada, Y., Sakuma, F., Sato, M., Schmidt, D.R., Scordo, A., Sekimoto, M., Shi, H., Sirghi, D., Sirghi, F., Suzuki, K., Swetz, D.S., Tanida, K., Tatsuno, H., Tokuda, M., Uhlig, J., Ullom, J.N., Yamada, S., Yamazaki, T., Zmeskal, J.

    IEEE Transactions on Applied Superconductivity27 ( 4 )   2017年

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    記述言語:英語   掲載種別:研究論文(学術雑誌)  

    DOI: 10.1109/TASC.2016.2646374

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  • Study of the polarimetric performance of a Si/CdTe semiconductor Compton camera for the Hitomi satellite 査読有り

    Junichiro Katsuta, Ikumi Edahiro, Shin Watanabe, Hirokazu Odaka, Yusuke Uchida, Nagomi Uchida, Tsunefumi Mizuno, Yasushi Fukazawa, Katsuhiro Hayashi, Sho Habata, Yuto Ichinohe, Takao Kitaguchi, Masanori Ohno, Masayuki Ohta, Hiromitsu Takahashi, Tadayuki Takahashi, Shin'ichiro Takeda, Hiroyasu Tajima, Takayuki Yuasa, Masayoshi Itou

    NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT840   51 - 58   2016年12月

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

    Gamma-ray polarization offers a unique probe into the geometry of the y-ray emission process in celestial objects. The Soft Gamma-ray Detector (SGD) onboard the X-ray observatory Hitomi is a SVCdTe Compton camera and is expected to be an excellent polarimeter, as well as a highly sensitive spectrometer due to its good angular coverage and resolution for Compton scattering. A beam test of the final-prototype for the SGD Compton camera was conducted to demonstrate its polarimetric capability and to verify and calibrate the Monte Carlo simulation of the instrument. The modulation factor of the SGD prototype camera, evaluated for the inner and outer parts of the CdTe sensors as absorbers, was measured to be 0.649-0.701 (inner part) and 0.637-0.653 (outer part) at 122.2 keV and 0.610-0.651 (inner part) and 0.564-0.592 (outer part) at 194.5 keV at varying polarization angles with respect to the detector. This indicates that the relative systematic uncertainty of the modulation factor is as small as similar to 3%.

    DOI: 10.1016/j.nima.2016.09.057

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  • Development and verification of signal processing system of avalanche photo diode for the active shields onboard ASTRO-H 査読有り

    M. Ohno, T. Kawano, I. Edahiro, H. Shirakawa, N. Ohashi, C. Okada, S. Habata, J. Katsuta, Y. Tanaka, H. Takahashi, T. Mizuno, Y. Fukazawa, H. Murakami, S. Kobayashi, K. Miyake, K. Ono, Y. Kato, Y. Furuta, Y. Murota, K. Okuda, Y. Wada, K. Nakazawa, T. Mimura, J. Kataoka, Y. Ichinohe, Y. Uchida, M. Katsuragawa, H. Yoneda, G. Sato, R. Sato, M. Kawaharada, A. Harayama, H. Odaka, K. Hayashi, M. Ohta, S. Watanabe, M. Kokubun, T. Takahashi, S. Takeda, M. Kinoshita, K. Yamaoka, H. Tajima, Y. Yatsu, H. Uchiyama, S. Saito, T. Yuasa, K. Makishima

    NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT831   410 - 414   2016年9月

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

    The hard X-ray Imager and Soft Gamma-ray Detector onboard ASTRO-H demonstrate high sensitivity to hard X-ray (5-80 keV) and soft gamma-rays (60-600 keV), respectively. To reduce the background, both instruments are actively shielded by large, thick Bismuth Germanate scintillators. We have developed the signal processing system of the avalanche photodiode in the BGO active shields and have demonstrated its effectiveness after assembly in the flight model of the HXI/SGD sensor and after integration into the satellite. The energy threshold achieved is about 150 keV and anti-coincidence efficiency for cosmic -ray events is almost 100%. Installed in the BGO active shield, the developed signal processing system successfully reduces the room background level of the main detector. (C) 2016 Elsevier B.V. All rights reserved.

    DOI: 10.1016/j.nima.2016.04.063

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  • Suzaku observations of a shock front tracing the western edge of the giant radio halo in the Coma Cluster 査読有り

    Yuusuke Uchida, Aurora Simionescu, Tadayuki Takahashi, Norbert Werner, Yuto Ichinohe, Steven W. Allen, Ondrej Urban, Kyoko Matsushita

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN68 ( SP1 ) S20   2016年6月

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

    We present the results of new Suzaku observations of the Coma Cluster, the X-ray brightest, nearby, merging system hosting a well-studied, typical giant radio halo. It has been previously shown that, on the western side of the cluster, the radio brightness shows a much steeper gradient compared to other azimuths. XMM-Newton and Planck revealed a shock front along the southern half of the region associated with this steep radio gradient, suggesting that the radio emission is enhanced by particle acceleration associated with the shock passage. Suzaku demonstrates for the first time that this shock front extends northwards, tracing the entire length of the western edge of the Coma radio halo. The shock is detected both in the temperature and X-ray surface brightness distributions and has a Mach number of around M similar to 1.5. The locations of the surface brightness edges align well with the edge of the radio emission, while the obtained temperature profiles seem to suggest shocks located 125-185 kpc further out in radius. In addition, the shock strengths derived from the temperature and density jumps are in agreement when using extraction regions parallel to the radio halo edge, but become inconsistent with each other when derived from radial profiles centered on the Coma Cluster core. It is likely that, beyond mere projection effects, the geometry of the shock is more complex than a front with a single, uniform Mach number and an approximately spherically symmetric shape.

    DOI: 10.1093/pasj/psv126

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  • X-ray substructure in clusters of galaxies and its implications for the physics of the intergalactic plasma

    Yuto Ichinohe

        2016年3月23日

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    記述言語:英語   掲載種別:学位論文(博士)  

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  • Development and in-orbit performance of all-sky monitoring function of BGO active shield of the soft gamma-ray detector onboard Hitomi

    Masanori Ohno, Yasushi Fukazawa, Tsunefumi Mizuno, Hiromitsu Takahashi, Takao Kitaguti, Yasuyuki Tanaka, Jun'ichiro Katsuta, Takafumi Kawano, Hiroyuki Shirakawa, Ikumi Edahiro, Sho Habata, Chiho Okada, Norie Ohashi, Koji Tanaka, Tadayuki Takahashi, Motohide Kokubun, Shin Watanabe, Goro Sato, Masayuki Ohta, Koichi Hagino, Rie Sato, Kunishiro Mori, Yusuke Uchida, Miho Katsuragawa, Ryota Tomaru, Hiroki Yoneda, Kazuhiro Nakazawa, Shunsuke Torii, Soki Sakurai, Makoto Sasano, Hidetoshi Nishida, Shogo

    7 years of MAXI: monitoring X-ray Transients, held 5-7 December 2016 at RIKEN   2016年

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

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  • In-flight performance of the Soft Gamma-ray Detector (SGD) onboard Hitomi

    Yasushi Fukazawa, Hiroyasu Tajima, Shin Watanabe, Roger Blandford, Teruaki Enoto, Andrea Goldwurm, Kouichi Hagino, Katsuhiro Hayashi, Yuto Ichinohe, Jun Kataoka, Junichiro Katsuta, Takao Kitaguchi, Motohide Kokubun, Philippe Laurent, François Lebrun, Olivier Limousin, M. Madejski, Kazuo rzegorz Makishima, Tsunefumi Mizuno, Kunishiro Mori, Takeshi Nakamori, Toshio Nakano, Kazuhiro Nakazawa, Hirofumi Noda, Hirokazu Odaka, Masanori Ohno, Masayuki Ohta, Shinya Saito, Goro Sato, Rie Sato, Shi

    7 years of MAXI: monitoring X-ray Transients, held 5-7 December 2016 at RIKEN   2016年

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

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  • Localization of Gamma-ray Bursts with BGO Active Shield of the Soft Gamma-ray Detector and Hard X-ray Imager onboard Hitomi

    Koji Tanaka, Masanori Ohno, Yasushi Fukazawa, Tsunefumi Mizuno, Hiromitsu Takahashi, Takao Kitaguti, Yasuyuki Tanaka, Jun'ichiro Katsuta, Takafumi Kawano, Hiroyuki Shirakawa, Ikumi Edahiro, Sho Habata, Chiho Okada, Norie Ohashi, Tadayuki Takahashi, Motohide Kokubun, Shin Watanabe, Goro Sato, Masayuki Ohta, Koichi Hagino, Rie Sato, Kunishiro Mori, Yusuke Uchida, Miho Katsuragawa, Ryota Tomaru, Hiroki Yoneda, Kazuhiro Nakazawa, Shunsuke Torii, Soki Sakurai, Makoto Sasano, Hidetoshi Nishida, Shogo

    7 years of MAXI: monitoring X-ray Transients, held 5-7 December 2016 at RIKEN   2016年

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

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  • Deep Chandra observation and numerical studies of the nearest cluster cold front in the sky 査読有り

    N. Werner, J. A. ZuHone, I. Zhuravleva, Y. Ichinohe, A. Simionescu, S. W. Allen, M. Markevitch, A. C. Fabian, U. Keshet, E. Roediger, M. Ruszkowski, J. S. Sanders

    MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY455 ( 1 ) 846 - 858   2016年1月

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

    We present the results of a very deep (500 ks) Chandra observation, along with tailored numerical simulations, of the nearest, best resolved cluster cold front in the sky, which lies 90 kpc (19 arcmin) to the north-west of M87. The northern part of the front appears the sharpest, with a width smaller than 2.5 kpc (1.5 Coulomb mean free paths; at 99 per cent confidence). Everywhere along the front, the temperature discontinuity is narrower than 4-8 kpc and the metallicity gradient is narrower than 6 kpc, indicating that diffusion, conduction and mixing are suppressed across the interface. Such transport processes can be naturally suppressed by magnetic fields aligned with the cold front. Interestingly, comparison to magnetohydrodynamic simulations indicates that in order to maintain the observed sharp density and temperature discontinuities, conduction must also be suppressed along the magnetic field lines. However, the northwestern part of the cold front is observed to have a non-zero width. While other explanations are possible, the broadening is consistent with the presence of Kelvin-Helmholtz instabilities (KHI) on length-scales of a few kpc. Based on comparison with simulations, the presence of KHI would imply that the effective viscosity of the intracluster medium is suppressed by more than an order of magnitude with respect to the isotropic Spitzer-like temperature dependent viscosity. Underneath the cold front, we observe quasi-linear features that are similar to 10 per cent brighter than the surrounding gas and are separated by similar to 15 kpc from each other in projection. Comparison to tailored numerical simulations suggests that the observed phenomena may be due to the amplification of magnetic fields by gas sloshing in wide layers below the cold front, where the magnetic pressure reaches similar to 5-10 per cent of the thermal pressure, reducing the gas density between the bright features.

    DOI: 10.1093/mnras/stv2358

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  • SERENDIPITOUS DISCOVERY OF AN EXTENDED X-RAY JET WITHOUT A RADIO COUNTERPART IN A HIGH-REDSHIFT QUASAR 査読有り

    A. Simionescu, L. Stawarz, Y. Ichinohe, C. C. Cheung, M. Jamrozy, A. Siemiginowska, K. Hagino, P. Gandhi, N. Werner

    ASTROPHYSICAL JOURNAL LETTERS816 ( 1 ) L15   2016年1月

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

    A recent Chandra observation of the nearby galaxy cluster Abell 585 has led to the discovery of an extended X-ray jet associated with the high-redshift background quasar B3 0727+ 409, a luminous radio source at redshift z = 2.5. This is one of only few examples of high-redshift X-ray jets known to date. It has a clear extension of about 12", corresponding to a projected length of similar to 100 kpc, with a possible hot spot located 35" from the quasar. The archival high resolution Very Large Array maps surprisingly reveal no extended jet emission, except for one knot about 1"4 from the quasar. The high X-ray to radio luminosity ratio for this source appears consistent with the alpha(1 + z)(4) amplification expected from the inverse Compton radiative model. This serendipitous discovery may signal the existence of an entire population of similar systems with bright X-ray and faint radio jets at high redshift, a selection bias that must be accounted for when drawing any conclusions about the redshift evolution of jet properties and indeed about the cosmological evolution of supermassive black holes and active galactic nuclei in general.

    DOI: 10.3847/2041-8205/816/1/L15

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  • The first demonstration of the concept of "narrow-FOV Si/CdTe semiconductor Compton camera" 査読有り

    Yuto Ichinohe, Yuusuke Uchida, Shin Watanabe, Ikumi Edahiro, Katsuhiro Hayashi, Takafumi Kawano, Masanori Ohno, Masayuki Ohta, Shin'ichiro Takeda, Yasushi Fukazawa, Miho Katsuragawa, Kazuhiro Nakazawa, Hirokazu Odaka, Hiroyasu Tajima, Hiromitsu Takahashi, Tadayuki Takahashi, Takayuki Yuasa

    NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT806   5 - 13   2016年1月

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

    The Soft Gamma-ray Detector (SGD), to be deployed on board the ASTRO-H satellite, has been developed to provide the highest sensitivity observations of celestial sources in the energy band of 60-600 keV by employing a detector concept which uses a Compton camera whose field-of-view is restricted by a EGO shield to a few degree (narrow-FOV Compton camera). In this concept, the background from outside the FOV can be heavily suppressed by constraining the incident direction of the gamma ray reconstructed by the Compton camera to be consistent with the narrow FOV. We, for the first time, demonstrate the validity of the concept using background data taken during the thermal vacuum test and the low-temperature environment test of the flight model of SGD on ground. We show that the measured background level is suppressed to less than 10% by combining the event rejection using the anti-coincidence trigger of the active EGO shield and by using Compton event reconstruction techniques. More than 75% of the signals from the field-of-view are retained against the background rejection, which clearly demonstrates the improvement of signal-to-noise ratio. The estimated effective area of 22.8 cm(2) meets the mission requirement even though not all of the operational parameters of the instrument have been fully optimized yet. (C) 2015 Elsevier B.V. All rights reserved.

    DOI: 10.1016/j.nima.2015.09.081

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  • The soft gamma-ray detector (SGD) onboard ASTRO-H

    Shin Watanabe, Hiroyasu Tajima, Yasushi Fukazawa, Roger Blandford, Teruaki Enoto, Andrea Goldwurm, Kouichi Hagino, Katsuhiro Hayashi, Yuto Ichinohe, Jun Kataoka, Junichiro Katsuta, Takao Kitaguchi, Motohide Kokubun, Philippe Laurent, Francois Lebrun, Olivier Limousin, Grzegorz M. Madejski, Kazuo Makishima, Tsunefumi Mizunoe, Kunishiro Mori, Takeshi Nakamori, Toshio Nakano, Kazuhiro Nakazawa, Hirofumi Noda, Hirokazu Odaka, Masanori Ohno, Masayuki Ohta, Shinya Saito, Goro Sato, Rie Sato, Shin'ichiro Takeda, Hiromitsu Takahashi, Tadayuki Takahashi, Takaaki Tanaka, Yasuyuki Tanaka, Yukikatsu Terada, Hideki Uchiyama, Yasunobu Uchiyama, Kazutaka Yamaoka, Yoichi Yatsu, Daisuke Yonetoku, Takayuki Yuasa

    SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY9905   2016年

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

    The Soft Gamma-ray Detector (SGD) is one of science instruments onboard ASTRO-H (Hitomi) and features a wide energy band of 60-600 keV with low backgrounds. SGD is an instrument with a novel concept of "Narrow field-of-view" Compton camera where Compton kinematics is utilized to reject backgrounds which are inconsistent with the field-of-view defined by the active shield. After several years of developments, the flight hardware was fabricated and subjected to subsystem tests and satellite system tests. After a successful ASTRO-H (Hitomi) launch on February 17, 2016 and a critical phase operation of satellite and SGD in-orbit commissioning, the SGD operation was moved to the nominal observation mode on March 24, 2016. The Compton cameras and BGO-APD shields of SGD worked properly as designed. On March 25, 2016, the Crab nebula observation was performed, and, the observation data was successfully obtained.

    DOI: 10.1117/12.2231962

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  • The ASTRO-H (Hitomi) X-ray astronomy satellite

    Tadayuki Takahashi, Motohide Kokubun, Kazuhisa Mitsuda, Richard Kelley, Takaya Ohashi, Felix Aharonian, Hiroki Akamatsu, Fumie Akimoto, Steve Allen, Naohisa Anabuki, Lorella Angelini, Keith Arnaud, Makoto Asai, Marc Audard, Hisamitsu Awaki, Magnus Axelsson, Philipp Azzarello, Chris Baluta, Aya Bamba, Nobutaka Bando, Marshall Bautz, Thomas Bialas, Roger Blandford, Kevin Boyce, Laura Brenneman, Greg Brown, Esra Bulbul, Edward Cackett, Edgar Canavan, Maria Chernyakova, Meng Chiao, Paolo Coppi, Elisa Costantini, Jelle De Plaa, Jan Willem Den Herder, Michael DiPirro, Chris Done, Tadayasu Dotani, John Doty, Ken Ebisawa, Megan Eckart, Teruaki Enoto, Yuichiro Ezoe, Andrew Fabian, Carlo Ferrigno, Adam Foster, Ryuichi Fujimoto, Yasushi Fukazawa, Akihiro Furuzawa, Massimiliano Galeazzi, Luigi Gallo, Poshak Gandhi, Kirk Gilmore, Margherita Giustini, Andrea Goldwurm, Liyi Gu, Matteo Guainazzi, Daniel Haas, Yoshito Haba, Kouichi Hagino, Kenji Hamaguchi, Atsushi Harayama, Ilana Harrus, Isamu Hatsukade, Takayuki Hayashi, Katsuhiro Hayashi, Kiyoshi Hayashida, Junko Hiraga, Kazuyuki Hirose, Ann Hornschemeier, Akio Hoshino, John Hughes, Yuto Ichinohe, Ryo Iizuka, Yoshiyuki Inoue, Hajime Inoue, Kazunori Ishibashi, Manabu Ishida, Kumi Ishikawa, Kosei Ishimura, Yoshitaka Ishisaki, Masayuki Itoh, Naoko Iwata, Naoko Iyomoto, Chris Jewell, Jelle Kaastra, Timothy Kallman, Tuneyoshi Kamae, Erin Kara, Jun Kataoka, Satoru Katsuda, Junichiro Katsuta, Madoka Kawaharada, Nobuyuki Kawai, Taro Kawano, Shigeo Kawasaki, Dmitry Khangulyan, Caroline Kilbourne, Mark Kimball, Ashley King

    Proceedings of SPIE - The International Society for Optical Engineering9905   2016年

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

    © 2016 SPIE. The Hitomi (ASTRO-H) mission is the sixth Japanese X-ray astronomy satellite developed by a large international collaboration, including Japan, USA, Canada, and Europe. The mission aimed to provide the highest energy resolution ever achieved at E > 2 keV, using a microcalorimeter instrument, and to cover a wide energy range spanning four decades in energy from soft X-rays to gamma-rays. After a successful launch on 2016 February 17, the spacecraft lost its function on 2016 March 26, but the commissioning phase for about a month provided valuable information on the on-board instruments and the spacecraft system, including astrophysical results obtained from first light observations. The paper describes the Hitomi (ASTRO-H) mission, its capabilities, the initial operation, and the instruments/spacecraft performances confirmed during the commissioning operations for about a month.

    DOI: 10.1117/12.2232379

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  • A UNIFORM CONTRIBUTION OF CORE-COLLAPSE AND TYPE Ia SUPERNOVAE TO THE CHEMICAL ENRICHMENT PATTERN IN THE OUTSKIRTS OF THE VIRGO CLUSTER 査読有り

    A. Simionescu, N. Werner, O. Urban, S. W. Allen, Y. Ichinohe, I. Zhuravleva

    ASTROPHYSICAL JOURNAL LETTERS811 ( 2 ) L25   2015年10月

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

    We present the first measurements of the abundances of a-elements (Mg, Si, and S) extending out beyond the virial radius of a cluster of galaxies. Our results, based on Suzaku Key Project observations of the Virgo Cluster, show that the chemical composition of the intracluster medium is consistent with being constant on large scales, with a flat distribution of the Si/Fe, S/Fe, and Mg/Fe ratios as a function of radius and azimuth out to 1.4 Mpc (1.3 r(200)). Chemical enrichment of the intergalactic medium due solely to core-collapse supernovae (SNcc) is excluded with very high significance; instead, the measured metal abundance ratios are generally consistent with the solar value. The uniform metal abundance ratios observed today are likely the result of an early phase of enrichment and mixing, with both SNcc and SNe Ia contributing to the metal budget during the period of peak star formation activity at redshifts of 2-3. We estimate the ratio between the number of SNe Ia and the total number of supernovae enriching the intergalactic medium to be between 12% and 37%, broadly consistent with the metal abundance patterns in our own Galaxy or with the SN Ia contribution estimated for the cluster cores.

    DOI: 10.1088/2041-8205/811/2/L25

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  • Prospect for future MeV gamma-ray active galactic nuclei population studies 査読有り

    Yoshiyuki Inoue, Yasuyuki T. Tanaka, Hirokazu Odaka, Atsushi Takada, Yuto Ichinohe, Shinya Saito, Shin'ichiro Takeda, Tadayuki Takahashi

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN67 ( 4 ) 76   2015年8月

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

    While the X-ray, GeV gamma-ray, and TeV gamma-ray skies have been extensively studied, the MeV gamma-ray sky has not yet been well investigated since the Imaging Compton Telescope (COMPTEL) scanned the sky about two decades ago. In this paper, we investigate the prospects for active galactic nuclei population studies with future MeV gamma-ray missions using recent spectral models and luminosity functions of Seyferts and flat-spectrum radio quasars (FSRQs). Both of them are plausible candidates for the origins of the cosmic MeV gamma-ray background. If the cosmic MeV gamma-ray background radiation is dominated by non-thermal emission from Seyferts, a sensitivity of 10(-12) erg cm(-2) s(-1) is required to detect several hundred Seyferts in the entire sky. If FSRQs make up the cosmic MeV gamma-ray background, a sensitivity of similar to 4x10(-12) erg cm(-2) s(-1) is required to detect several hundred FSRQs following the recent FSRQ X-ray luminosity function. However, based on the latest FSRQ gamma-ray luminosity function, with which FSRQs can explain up to similar to 30% of the MeV background, we can expect several hundred FSRQs even with a sensitivity of 10(-11) erg cm(-2) s(-1), which is almost the same as the sensitivity goal of the next-generation MeV telescopes.

    DOI: 10.1093/pasj/psv043

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  • A portable Si/CdTe Compton camera and its applications to the visualization of radioactive substances 査読有り

    Shin'ichiro Takeda, Atsushi Harayama, Yuto Ichinohe, Hirokazu Odaka, Shin Watanabe, Tadayuki Takahashi, Hiroyasu Tajima, Kei Genba, Daisuke Matsuura, Hiroshi Ikebuchi, Yoshikatsu Kuroda, Tetsuya Tomonaka

    NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT787   207 - 211   2015年7月

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

    Gamma-ray imagers with the potential for visualizing the distribution of radioactive materials are required in the fields of astrophysics, medicine, nuclear applications, and homeland security. Based on the technology of the Si/CdTe Compton camera, we have manufactured the first commercial Compton camera for practical use Through field tests in Fukushima, we demonstrated that the camera is capable of hot spot detection and the evaluation of radioactive decontamination. (C) 2014 Elsevier B.V. All rights reserved.

    DOI: 10.1016/j.nima.2014.11.119

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  • The growth of the galaxy cluster Abell 85: mergers, shocks, stripping and seeding of clumping 査読有り

    Y. Ichinohe, N. Werner, A. Simionescu, S. W. Allen, R. E. A. Canning, S. Ehlert, F. Mernier, T. Takahashi

    MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY448 ( 3 ) 2971 - 2986   2015年4月

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

    We present the results of deep Chandra, XMM-Newton and Suzaku observations of the nearby galaxy cluster Abell 85, which is currently undergoing at least two mergers, and in addition shows evidence for gas sloshing which extends out to r approximate to 600 kpc. One of the two infalling subclusters, to the south of the main cluster centre, has a dense, X-ray bright cool core and a tail extending to the south-east. The northern edge of this tail is strikingly smooth and sharp (narrower than the Coulomb mean free path of the ambient gas) over a length of 200 kpc, while towards the south-west the boundary of the tail is blurred and bent, indicating a difference in the plasma transport properties between these two edges. The thermodynamic structure of the tail strongly supports an overall north-westward motion. We propose, that a sloshing-induced tangential, ambient, coherent gas flow is bending the tail eastwards. The brightest galaxy of this subcluster is at the leading edge of the dense core, and is trailed by the tail of stripped gas, suggesting that the cool core of the subcluster has been almost completely destroyed by the time it reached its current radius of r approximate to 500 kpc. The surface-brightness excess, likely associated with gas stripped from the infalling southern subcluster, extends towards the south-east out to at least r(500) of the main cluster, indicating that the stripping of infalling subclusters may seed gas inhomogeneities. The second merging subcluster appears to be a diffuse non-cool-core system. Its merger is likely supersonic with a Mach number of approximate to 1.4.

    DOI: 10.1093/mnras/stv217

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  • The Si/CdTe semiconductor Compton camera of the ASTRO-H Soft Gamma-ray Detector (SGD) 査読有り

    Shin Watanabe, Hiroyasu Tajima, Yasushi Fukazawa, Yuto Ichinohe, Shin'ichiro Takeda, Teruaki Enoto, Taro Fukuyama, Shunya Furui, Kei Genba, Kouichi Hagino, Atsushi Harayama, Yoshikatsu Kuroda, Daisuke Matsuura, Ryo Nakamura, Kazuhiro Nakazawa, Hirofumi Noda, Hirokazu Odaka, Masayuki Ohta, Mitsunobu Onishi, Shinya Saito, Goro Sato, Tamotsu Sato, Tadayuki Takahashi, Takaaki Tanaka, Atsushi Togo, Shinji Tomizuka

    NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT765   192 - 201   2014年11月

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

    The Soft Gamma-ray Detector (SGD) is one of the instrument payloads onboard ASTRO-H, and will cover a wide energy band (60-600 key) at a background level 10 times better than instruments currently in orbit. The SGD achieves low background by combining a Compton camera scheme with a narrow field-of-view active shield. The Compton camera in the SGD is realized as a hybrid semiconductor detector system which consists of silicon and cadmium telluride (CcITe) sensors. The design of the SGD Compton camera has been finalized and the final prototype, which has the same configuration as the flight model, has been fabricated for performance evaluation. The Compton camera has overall dimensions of 12 cm x 12 cm x 12 cm, consisting of 32 layers of Si pixel sensors and 8 layers of CdTe pixel sensors surrounded by 2 layers of CcITe pixel sensors. The detection efficiency of the Compton camera reaches about 15% and 3% for 100 keV and 511 keV gamma rays, respectively. The pixel pitch of the Si and CdTe sensors is 3.2 mm, and the signals from all 13,312 pixels are processed by 208 ASlCs developed for the SGD. Good energy resolution is afforded by semiconductor sensors and low noise ASlCs, and the obtained energy resolutions with the prototype Si and CciTe pixel sensors are 1020 keV (RNHM) at 60 keV and 1.6-2.5 keY (RNHN1) at 122 keV, respectively. This results in good background rejection capability due to better constraints on Compton kinematics. Compton camera energy resolutions achieved with the final prototype are 6.3 keY (RNHN1) at 356 keV and 10.5 keV (ENVHM) at 662 keV, which satisfy the instrument requirements for the SGD Compton camera (better than 2%) Moreover, a low intrinsic background has been confirmed by the background measurement with the final prototype. (C) 2014 Elsevier B.V. All rights reserved.

    DOI: 10.1016/j.nima.2014.05.127

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  • ASTRO-H White Paper - Plasma Diagnostic and Dynamics of the Galactic Center Region

    K. Koyama, J. Kataoka, M. Nobukawa, H. Uchiyama, S. Nakashima, F. Aharonian, M. Chernyakova, Y. Ichinohe, K. K. Nobukawa, Y. Maeda, H. Matsumoto, H. Murakami, C. Ricci, L. Stawarz, T. Tanaka, T. G. Tsuru, S. Watanabe, S. Yamauchi, T. Yuasa, for the ASTRO-H, Science Working Group

    arXiv   2014年

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    記述言語:英語  

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  • Development and calibration of Fine Collimators for the ASTRO-H Soft Gamma-ray Detector

    T. Mizuno, D. Kimura, Y. Fukazawa, S. Furui, K. Goto, T. Hayashi, S. K. Kawabata, T. Kawano, Y. Kitamura, H. Shirakawa, T. Tanabe, K. Makishima, K. Nakajima, K. Nakazawa, T. Fukuyama, Y. Ichinohe, K. Ishimura, M. Ohta, T. Sato, T. Takahashi, Y. Uchida, S. Watanabe, K. Ishibashi, K. Sakanobe, H. Matsumoto, T. Miyazawa, H. Mori, M. Sakai, H. Tajima

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

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

    The Soft Gamma-ray Detector (SGD) is a Si/CdTe Compton telescope surrounded by a thick BGO active shield and is scheduled to be onboard the ASTRO-H satellite when it is launched in 2015. The SGD covers the energy range from 40 to 600 keV with high sensitivity, which allows us to study nonthermal phenomena in the universe. The SGD uses a Compton camera with the narrow field-of-view (FOV) concept to reduce the non-Xray background (NXB) and improve the sensitivity. Since the SGD is essentially a nonimaging instrument, it also has to cope with the cosmic X-ray background (CXB) within the FOV. The SGD adopts passive shields called "fine collimators" (FCs) to restrict the FOV to <= 0.6 degrees for low-energy photons (<= 100 keV), which reduces contamination from CXB to less than what is expected due to NXB. Although the FC concept was already adopted by the Hard X-ray Detector onboard Suzaku, FCs for the SGD are about four times larger in size and are technically more difficult to operate. We developed FCs for the SGD and confirmed that the prototypes function as required by subjecting them to an X-ray test and environmental tests, such as vibration tests. We also developed an autocollimator system, which uses visible light to determine the transmittance and the optical axis, and calibrated it against data from the X-ray test. The acceptance tests of flight models started in December 2013: five out of six FCs were deemed acceptable, and one more unit is currently being produced. The activation properties were studied based on a proton-beam test and the results were used to estimate the in-orbit NXB.

    DOI: 10.1117/12.2054649

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  • Sub-MeV all sky survey with a compact Si/CdTe Compton telescope

    Nakazawa, Kazuhiro, Takahashi, Tadayuki, Watanabe, Shin, Ichinohe, Yuto, Takeda, Shin'ichiro, Enoto, Teruaki, Fukazawa, Yasushi, Kamae, Tuneyoshi, Kokubun, Motohide, Makishima, Kazuo, Mitani, Takefumi, Mizuno, Tsunefumi, Nomachi, Masaharu, Tajima, Hiroyasu, Takashima, Takeshi, Tamagawa, Toru, Terada, Yukikatsu, Tashiro, Makoto, Uchiyama, Yasunobu, Yoshimitsu, Tetsuo

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

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

    Recent progress in wide field of view or all-sky observations such as Swift/BAT hard X-ray monitor and Fermi GeV gamma-ray observatory has opened up a new era of time-domain high energy astro-physics addressing new insight in, e.g., particle acceleration in the universe. MeV coverage with comparable sensitivity, i.e. 1 similar to 10 mCrab is missing and a new MeV all-sky observatory is needed. These new MeV mission tend to be large, power-consuming and hence expensive, and its realization is yet to come. A compact sub-MeV (0.2-2 MeV) all-sky mission is proposed as a path finder for such mission. It is based on a Si/CdTe semiconductor Compton telescope technology employed in the soft gamma-ray detector onboard ASTRO-H, to be launched in to orbit on late 2015. The mission is kept as small as 0.5 x 0.5 x 0.4 m(3), 150 kg in weight and 200 W in power in place of the band coverage above a few MeV, in favor of early realization as a sub-payload to other large platforms, such as the international space station.

    DOI: 10.1117/12.2055422

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  • ASTRO-H衛星搭載軟ガンマ線検出器におけるコンプトン再構成アルゴリズムの開発

    一戸悠人

        2013年3月25日

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    記述言語:日本語   掲載種別:学位論文(修士)  

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  • Study of event reconstruction algorithm for a large-scale Si/CdTe multilayer Compton camera

    Yuto Ichinohe, Shin'ichiro Takeda, Hirokazu Odaka, Shin Watanabe, Taro Fukuyama, Masayuki Ohta, Tadayuki Takahashi, Kazuhiro Nakazawa, Hiroyasu Tajima, Yasushi Fukazawa, Takaaki Tanaka

    Nuclear Science Symposium and Medical Imaging Conference (NSS/MIC)   2013年

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

    DOI: 10.1109/NSSMIC.2013.6829409

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  • High-resolution Compton cameras based on Si/CdTe double-sided strip detectors 査読有り

    Hirokazu Odaka, Yuto Ichinohe, Shin'ichiro Takeda, Taro Fukuyama, Koichi Hagino, Shinya Saito, Tamotsu Sato, Goro Sato, Shin Watanabe, Motohide Kokubun, Tadayuki Takahashi, Mitsutaka Yamaguchi, Takaaki Tanaka, Hiroyasu Tajima, Kazuhiro Nakazawa, Yasushi Fukazawa

    NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT695   179 - 183   2012年12月

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

    We have developed a new Compton camera based on silicon (Si) and cadmium telluride (CdTe) semiconductor double-sided strip detectors (DSDs). The camera consists of a 500-mu m-thick Si-DSD and four layers of 750-mu m-thick CdTe-DSDs all of which have common electrode configuration segmented into 128 strips on each side with pitches of 250 mu m. In order to realize high angular resolution and to reduce size of the detector system, a stack of DSDs with short stack pitches of 4 mm is utilized to make the camera. Taking advantage of the excellent energy and position resolutions of the semiconductor devices, the camera achieves high angular resolutions of 4.5 degrees at 356 key and 3.5 degrees at 662 keV. To obtain such high resolutions together with an acceptable detection efficiency, we demonstrate data reduction methods including energy calibration using Compton scattering continuum and depth sensing in the CdTe-DSD. We also discuss imaging capability of the camera and show simultaneous multi-energy imaging. (C) 2012 Elsevier B.V. All rights reserved.

    DOI: 10.1016/j.nima.2011.12.061

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  • Applications and imaging techniques of a Si/CdTe Compton gamma-ray camera 査読有り

    Shin'ichiro Takeda, Yuto Ichinohe, Kouichi Hagino, Hirokazu Odaka, Takayuki Yuasa, Shin-nosuke Ishikawa, Taro Fukuyama, Shinya Saito, Tamotsu Sato, Goro Sato, Shin Watanabe, Motohide Kokubun, Tadayuki Takahashi, Mitsutaka Yamaguchi, Hiroyasu Tajima, Takaaki Tanaka, Kazuhiro Nakazawa, Yasushi Fukazawa, Takashi Nakano

    PROCEEDINGS OF THE 2ND INTERNATIONAL CONFERENCE ON TECHNOLOGY AND INSTRUMENTATION IN PARTICLE PHYSICS (TIPP 2011)37   859 - 866   2012年

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

    By using a new Compton camera consisting of a silicon double-sided strip detector (Si-DSD) and a CdTe double-sided strip detector (CdTe-DSD), originally developed for the ASTRO-H satellite mission, an experiment involving imaging radioisotopes was conducted to study their feasibility for hotspot monitoring. In addition to the hotspot imaging already provided by commercial imaging systems, identification of various radioisotopes is possible thanks to the good energy resolution obtained by the semiconductor detectors. Three radioisotopes of Ba-133 (356 keV), Na-22 (511 keV) and Cs-137 (662 keV) were individually imaged by applying event selection in the energy window and the gamma-ray images were correctly overlapped by an optical picture. Detection efficiency of 1.68 x10(-4) (effective area : 1.7 x10(-3) cm(2)) and angular resolution of 3.8 degrees were obtained by stacking five detector modules for a 662 keV gamma ray. The higher detection efficiency required in specific use can be achieved by stacking more detector modules. (C) 2012 Published by Elsevier B.V. Selection and/or peer review under responsibility of the organizing committee for TIPP 11.

    DOI: 10.1016/j.phpro.2012.04.096

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  • Imaging and spectral performance of CdTe double-sided strip detectors for the Hard X-ray Imager onboard ASTRO-H

    Kouichi Hagino, Hirokazu Odaka, Goro Sato, Shin Watanabe, Shin'ichiro Takeda, Motohide Kokubun, Taro Fukuyama, Shinya Saito, Tamotsu Sato, Yuto Ichinohe, Tadayuki Takahashi, Toshio Nakano, Kazuhiro Nakazawa, Kazuo Makishima, Hiroyasu Tajima, Takaaki Tanaka, Kazunori Ishibashi, Takuya Miyazawa, Michito Sakai, Karin Sakanobe, Hiroyoshi Kato, Shunya Takizawa, Kentaro Uesugi

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

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

    The imaging and spectral performance of CdTe double-sided strip detectors (CdTe-DSDs) was evaluated for the ASTRO-H mission. The charcterized CdTe-DSDs have a strip pitch of 0.25 mm, an imaging area of 3.2 cm x 3.2 cm and a thickness of 0.75 mm. The detector was successfully operated at a temperature of -20 degrees C and with an applied bias voltage of 250 V. By using two-strip events as well as one-strip events for the event reconstruction, a good energy resolution of 2.0 keV at 59.5 keV and a sub-strip spatial resolution was achieved. The hard X-ray and gamma-ray response of CdTe-DSDs is complex due to the properties of CdTe and the small pixel effect. Therefore, one of the issues to investigate is the response of the CdTe-DSD. In order to investigate the spatial dependence of the detector response, we performed fine beam scan experiments at SPring-8, a synchrotron radiation facility. From these experiments, the depth structure of the electric field was determined as well as properties of carriers in the detector and successfully reproduced the experimental data with simulated spectra.

    DOI: 10.1117/12.926052

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  • Concept of a small satellite for sub-MeV & MeV all sky survey: the CAST mission

    Nakazawa, Kazuhiro, Takahashi, Tadayuki, Ichinohe, Yuto, Takeda, Shin'ichiro, Tajima, Hiroyasu, Kamae, Tuneyoshi, Kokubun, Motohide, Takashima, Takeshi, Tashiro, Makoto, Tamagawa, Toru, Terada, Yukikatsu, Nomachi, Masaharu, Fukazawa, Yasushi, Makishima, Kazuo, Mizuno, Tsunefumi, Mitani, Takefumi, Yoshimitsu, Tetsuo, Watanabe, Shin

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

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

    MeV and sub-MeV energy band from similar to 200 keV to similar to 2 MeV contains rich information of high-energy phenomena in the universe. The CAST (Compton Telescope for Astro and Solar Terrestrial) mission is planned to be launched at the end of 2010s, and aims at providing all-sky map in this energy-band for the first time. It is made of a semiconductor Compton telescope utilizing Si as a scatterer and CdTe as an absorber. CAST provides all-sky sub-MeV polarization map for the first time, as well. The Compton telescope technology is based on the design used in the Soft Gamma-ray Detector (SGD) onboard ASTRO-H, characterized by its tightly stacked semiconductor layers to obtain high Compton reconstruction efficiency. The CAST mission is currently planned as a candidate for the small scientific satellite series in ISAS/JAXA, weighting about 500 kg in total. Scalable detector design enables us to consider other options as well. Scientific outcome of CAST is wide. It will provide new information from high-energy sources, such as AGN and/or its jets, supernova remnants, magnetors, black-hole and neutron-star binaries and others. Polarization map will tell us about activities of jets and reflections in these sources, as well. In addition, CAST will simultaneously observe the Sun, and depending on its attitude, the Earth.

    DOI: 10.1117/12.926164

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▼全件表示

MISC

  • 超広角コンプトンカメラによる放射性物質分布の可視化 招待有り

    高橋忠幸, 武田伸一郎, 渡辺伸, 一戸悠人, 田島宏康, 黒田能克, 池淵博, 玄蕃恵, 松浦大介

    放射線39 ( 4 )   2014年

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    記述言語:日本語   掲載種別:記事・総説・解説・論説等(学術雑誌)  

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講演・口頭発表等

  • Atmospheric gas dynamics in the Perseus cluster observed with Hitomi 招待有り 国際会議

    Yuto Ichinohe

    SnowCluster 2018 - The Physics of Galaxy Clusters  2018年3月18日 

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    記述言語:英語   会議種別:口頭発表(招待・特別)  

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  • X線観測で探る銀河団ガスの物理 招待有り

    一戸悠人

    国立天文台談話会  2017年12月8日 

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    記述言語:日本語   会議種別:公開講演,セミナー,チュートリアル,講習,講義等  

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  • X線スペクトル解析と機械学習

    一戸悠人

    ASTRO-AI 第1回研究会  2017年9月25日 

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    記述言語:日本語   会議種別:口頭発表(一般)  

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  • Hitomi SXS view of the gas motions in the core of the Perseus cluster 招待有り 国際会議

    Yuto Ichinohe

    The power of X-ray spectroscopy  2017年9月6日 

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    記述言語:英語   会議種別:口頭発表(招待・特別)  

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  • Gas motions in the Perseus galaxy cluster observed with Hitomi 国際会議

    Yuto Ichinohe, the Hitomi collaboration

    The X-ray Universe 2017  2017年6月6日 

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    記述言語:英語   会議種別:口頭発表(一般)  

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  • An azimuthally resolved study of the cold front in Abell 3667 国際会議

    Yuto Ichinohe

    Physics of the Intra-Cluster Medium 2017  2017年4月3日 

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    記述言語:英語   会議種別:口頭発表(一般)  

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  • 「ひとみ」によるペルセウス座銀河団のガス速度測定: (1) 速度構造

    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, 辻元匡弘, 藤本龍一, 前田良知, および「ひとみ」コラボレーション

    日本天文学会2017年春季年会  2017年3月15日 

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    記述言語:日本語   会議種別:ポスター発表  

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  • Perseus velocity team status report 招待有り 国際会議

    Yuto Ichinohe on behalf of the, Perseus velocity team

    16th ASTRO-H science meeting  2017年2月13日 

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    記述言語:英語   会議種別:口頭発表(一般)  

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  • 衝突銀河団 Abell 85 のガス運動と相互作用

    一戸悠人, N. Werner, A. Simionescu, S. W. Allen, R. E. A. Canning, S. Ehlert, F. Mernie, 高橋忠幸

    日本天文学会 2015 年秋季年会  2015年9月9日 

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    記述言語:日本語   会議種別:口頭発表(一般)  

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  • Complex gas structures and interaction in Abell 85 国際会議

    Yuto Ichinohe

    Astroparticle View of Galaxy Clusters  2015年3月24日 

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    記述言語:英語   会議種別:口頭発表(一般)  

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  • An Iterative Energy Calibration Method for Large-scale Semiconductor Multilayer Compton Cameras 国際会議

    Yuto Ichinohe, Hirokazu Odaka, Shin’ichiro Takeda, Shin Watanabe, Tadayuki Takahashi, Hiroyasu Tajima, Daisuke Matsuura, Kei Genba, Yoshikatsu Kuroda

    IEEE Nuclear Science Symposium and Medical Imaging Conference  2014年11月8日 

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    記述言語:英語   会議種別:口頭発表(一般)  

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  • Gas motions in Abell 85 国際会議

    Yuto Ichinohe, N. Werner, A. Simionescu, S. W. Allen, R. E. A. Canning, S. Ehlert, F. Mernier, T. Takahashi

    Workshop "ICM Inhomogeneities in the Intracluster Plasma"  2014年7月28日 

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    記述言語:英語   会議種別:口頭発表(一般)  

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  • Complex gas dynamics during the hierarchical growth of the galaxy cluster Abell 85 国際会議

    Yuto Ichinohe

    KIPAC Tea Talk  2014年6月13日 

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    記述言語:英語   会議種別:公開講演,セミナー,チュートリアル,講習,講義等  

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  • Study of Event Reconstruction Algorithm for a Large-Scale Si/CdTe Multilayer Compton Camera 国際会議

    Yuto Ichinohe, Shin'ichiro Takeda, Hirokazu Odaka, Shin Watanabe, Taro Fukuyama, Masayuki Ohta, Tadayuki Takahashi, Kazuhiro Nakazawa, Hiroyasu Tajima, Yasushi Fukazawa, Takaaki Tanaka

    IEEE Nuclear Science Symposium and Medical Imaging Conference  2013年10月27日 

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    記述言語:英語   会議種別:口頭発表(一般)  

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  • ASTRO-H 衛星搭載軟ガンマ線検出器におけるコンプトン再構成アルゴリズムの開発 招待有り

    一戸悠人

    日本物理学会 2013年秋季大会  2013年9月20日 

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    記述言語:日本語   会議種別:口頭発表(招待・特別)  

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  • Search for Cosmic Gamma-ray Lines Using ASTRO-H SGD 国際会議

    Yuto Ichinohe

    4th ASTRO-H Summer School  2013年9月5日 

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    記述言語:英語   会議種別:ポスター発表  

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  • ASTRO-H 衛星搭載軟ガンマ線検出器 (SGD) におけるイベント処理アルゴリズムの研究

    一戸悠人, 武田伸一郎, 小高裕和, 佐藤有, 萩野浩一, 齋藤新也, 福山太郎, 太田方之, 渡辺伸, 国分紀秀, 高橋忠幸, 田島宏康, 田中孝明, 榎戸輝揚, 深沢泰司, ほか HXI, SGD チーム

    日本物理学会 2012年秋季大会  2012年9月11日 

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    記述言語:日本語   会議種別:口頭発表(一般)  

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  • SGD Data Analysis: Background Rejection (and Polarimetry) 招待有り 国際会議

    Yuto Ichinohe

    Mini Workshop "Exploring Nonthermal Universe with the Soft Gamma-ray Detector"  2012年5月17日 

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    記述言語:英語   会議種別:口頭発表(招待・特別)  

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  • Simulation study of the 511 keV annihilation line observation with the Soft Gamma-ray Detector onboard ASTRO-H 国際会議

    Yuto Ichinohe, Hirokazu Odaka, Tamotsu Sato, Shin’ichiro Takeda, Shin Watanabe, Motohide Kokubun, Tadayuki Takahashi, Hiroyasu Tajima, Takaaki Tanaka, Yasunobu Uchiyama, Kazuhiro Nakazawa

    International Workshop on Positrons in Astrophysics  2012年3月20日 

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    記述言語:英語   会議種別:ポスター発表  

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  • ASTRO-H 衛星搭載軟ガンマ線検出器(SGD)に向けたコンプトンイメージング法の研究

    一戸悠人, 武田伸一郎, 小高裕和, 渡辺伸, 福山太郎, 斉藤新也, 萩野浩一, 佐藤有, 太田方之, 国分紀秀, 高橋忠幸, 田島宏康, 田中孝明, 榎戸輝揚, 水野恒史, 深沢泰司, ほか HXI, SGD チーム

    日本物理学会 2011年秋季大会  2011年9月16日 

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    記述言語:日本語   会議種別:口頭発表(一般)  

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  • Challenge to polarisation science by using ASTRO-H 国際会議

    Yuto Ichinohe

    2nd ASTRO-H Summer School  2011年8月24日 

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    記述言語:英語   会議種別:ポスター発表  

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▼全件表示

共同研究・競争的資金等の研究

  • 高精度X線分光とガス形態から探る銀河団プラズマの統一描像

    科学研究費助成事業 

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    2016年4月 - 2018年3月

    資金種別:競争的資金

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  • 半導体コンプトン望遠鏡を用いた電子・陽電子対消滅放射による宇宙物理学の開拓

    科学研究費助成事業 

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    2013年4月 - 2016年3月

    資金種別:競争的資金

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