XRISM Project Team

渡辺 伸

ワタナベ シン  (Shin Watanabe)

基本情報

所属
国立研究開発法人宇宙航空研究開発機構 宇宙科学研究所 宇宙物理学研究系 准教授
学位
博士(理学)(2004年3月 東京大学)

研究者番号
60446599
ORCID ID
 https://orcid.org/0000-0003-0441-7404
J-GLOBAL ID
202001021434500706
researchmap会員ID
R000012970

主要な論文

 215
  • Hitomi Collaboration, 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, Shiu-Hang Lee, Maurice A. Leutenegger, Olivier 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, 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, Stephane 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. Serlemtsos, 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, Shin Watanabe, Norbert Werner, 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, Yuusuke Uchida
    Publications of the Astronomical Society of Japan 70(6) 2018年10月1日  査読有り責任著者
    We present the results from the Hitomi Soft Gamma-ray Detector (SGD) observation of the Crab nebula. The main part of SGD is a Compton camera, which in addition to being a spectrometer, is capable of measuring polarization of gamma-ray photons. The Crab nebula is one of the brightest X-ray / gamma-ray sources on the sky, and, the only source from which polarized X-ray photons have been detected. SGD observed the Crab nebula during the initial test observation phase of Hitomi. We performed the data analysis of the SGD observation, the SGD background estimation and the SGD Monte Carlo simulations, and, successfully detected polarized gamma-ray emission from the Crab nebula with only about 5 ks exposure time. The obtained polarization fraction of the phase-integrated Crab emission (sum of pulsar and nebula emissions) is (22.1 $\pm$ 10.6)% and, the polarization angle is 110.7$^o$ + 13.2 / $-$13.0$^o$ in the energy range of 60--160 keV (The errors correspond to the 1 sigma deviation). The confidence level of the polarization detection was 99.3%. The polarization angle measured by SGD is about one sigma deviation with the projected spin axis of the pulsar, 124.0$^o$ $\pm$0.1$^o$.
  • Shin Watanabe, Hiroyasu Tajima, Yasushi Fukazawa, Yuto Ichinohe, Shin'ichiro Takeda, Teruaki Enoto, Taro Fukuyama, Shunya Furui, Kei Genba, Kouichi Hagino, Astushi 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 and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 765 192-201 2015年9月2日  査読有り筆頭著者責任著者
    The Soft Gamma-ray Detector (SGD) is one of the instrument payloads onboard ASTRO-H, and will cover a wide energy band (60--600 keV) 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 (CdTe) 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 CdTe 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 13312 pixels are processed by 208 ASICs developed for the SGD. Good energy resolution is afforded by semiconductor sensors and low noise ASICs, and the obtained energy resolutions with the prototype Si and CdTe pixel sensors are 1.0--2.0 keV (FWHM) at 60 keV and 1.6--2.5 keV (FWHM) 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 keV (FWHM) at 356 keV and 10.5 keV (FWHM) at 662 keV, respectively, 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.
  • Shin Watanabe, Shin-nosuke Ishikawa, Hiroyuki Aono, Shin'ichiro Takeda, Hirokazu Odaka, Motohide Kokubun, Tadayuki Takahashi, Kazuhiro Nakazawa, Hiroyasu Tajima, Mitsunobu Onishi, Yoshikatsu Kuroda
    IEEE Transactions on Nuclear Science 56(3) 777-782 2008年11月4日  査読有り筆頭著者責任著者
    We developed CdTe double-sided strip detectors (DSDs or cross strip detectors) and evaluated their spectral and imaging performance for hard X-rays and gamma-rays. Though the double-sided strip configuration is suitable for imagers with a fine position resolution and a large detection area, CdTe diode DSDs with indium (In) anodes have yet to be realized due to the difficulty posed by the segmented In anodes. CdTe diode devices with aluminum (Al) anodes were recently established, followed by a CdTe device in which the Al anodes could be segmented into strips. We developed CdTe double-sided strip devices having Pt cathode strips and Al anode strips, and assembled prototype CdTe DSDs. These prototypes have a strip pitch of 400 micrometer. Signals from the strips are processed with analog ASICs (application specific integrated circuits). We have successfully performed gamma-ray imaging spectroscopy with a position resolution of 400 micrometer. Energy resolution of 1.8 keV (FWHM: full width at half maximum) was obtained at 59.54 keV. Moreover, the possibility of improved spectral performance by utilizing the energy information of both side strips was demonstrated. We designed and fabricated a new analog ASIC, VA32TA6, for the readout of semiconductor detectors, which is also suitable for DSDs. A new feature of the ASIC is its internal ADC function. We confirmed this function and good noise performance that reaches an equivalent noise charge of 110 e- under the condition of 3-4 pF input capacitance.
  • Shin Watanabe, Masao Sako, Manabu Ishida, Yoshitaka Ishisaki, Steven M. Kahn, Takayoshi Kohmura, Fumiaki Nagase, Frederik Paerels, Tadayuki Takahashi
    Astrophysical Journal 651(1 I) 421-437 2006年7月3日  査読有り筆頭著者責任著者
    We present results from quantitative modeling and spectral analysis of the high mass X-ray binary Vela X-1 obtained with the Chandra HETGS. The spectra exhibit emission lines from H-like and He-like ions driven by photoionization, as well as fluorescent emission lines from several elements in lower charge states. In order to interpret and make full use of the high-quality data, we have developed a simulator, which calculates the ionization and thermal structure of a stellar wind photoionized by an X-ray source, and performs Monte Carlo simulations of X-ray photons propagating through the wind. The emergent spectra are then computed as a function of the viewing angle accurately accounting for photon transport in three dimensions including dynamics. From comparisons of the observed spectra with the simulation results, we are able to find the ionization structure and the geometrical distribution of material in Vela X-1 that can reproduce the observed spectral line intensities and continuum shapes at different orbital phases remarkably well. It is found that a large fraction of X-ray emission lines from highly ionized ions are formed in the region between the neutron star and the companion star. We also find that the fluorescent X-ray lines must be produced in at least three distinct regions --(1)the extended stellar wind, (2)reflection off the stellar photosphere, and (3)in a distribution of dense material partially covering and possibly trailing the neutron star, which may be associated with an accretion wake. Finally, from detailed analysis of the emission lines, we demonstrate that the stellar wind is affected by X-ray photoionization.
  • Shin Watanabe, Takaaki Tanaka, Kazuhiro Nakazawa, Takefumi Mitani, Kousuke Oonuki, Tadayuki Takahashi, Takeshi Takashima, Hiroyasu Tajima, Yasushi Fukazawa, Masaharu Nomachi, Shin Kubo, Mitsunobu Onishi, Yoshikatsu Kuroda
    IEEE Transactions on Nuclear Science 52(5 III) 2045-2051 2005年10月  査読有り筆頭著者責任著者
    We are developing a Compton camera based on Si and CdTe semiconductor imaging devices with high energy resolution. In this paper, results from the most recent prototype are reported. The Compton camera consists of six layered double-sided Si Strip detectors and CdTe pixel detectors, which are read out with low noise analog ASICs, VA32TAs. We obtained Compton reconstructed images and spectra of line gamma-rays from 122 keV to 662 keV. The energy resolution is 9.1 keV and 14 keV at 356 keV and 511 keV, respectively. © 2005 IEEE.
  • Shin Watanabe, Masao Sako, Manabu Ishida, Yoshitaka Ishisaki, Steve M. Kahn, Takayoshi Kohmura, Umeyo Morita, Fumiaki Nagase, Frederik Paerels, Tadayuki Takahashi
    Astrophysical Journal 597(1 II) 2003年9月12日  査読有り筆頭著者責任著者
    We report the detection of a fully-resolved, Compton-scattered emission line in the X-ray spectrum of the massive binary GX 301-2 obtained with the High Energy Transmission Grating Spectrometer onboard the Chandra X-ray Observatory. The iron K-alpha fluorescence line complex observed in this system consists of an intense narrow component centered at an energy of E = 6.40 keV and a redward shoulder that extends down to ~6.24 keV, which corresponds to an energy shift of a Compton back-scattered iron K-alpha photon. From detailed Monte Carlo simulations and comparisons with the observed spectra, we are able to directly constrain the physical properties of the scattering medium, including the electron temperature and column density, as well as an estimate for the metal abundance.
  • Tadayui Takahashi, Shin Watanabe
    IEEE Transactions on Nuclear Science 48(4 I) 950-959 2001年7月20日  査読有り
    Cadmium telluride (CdTe) and cadmium zinc telluride (CdZnTe) have been regarded as promising semiconductor materials for hard X-ray and Gamma-ray detection. The high atomic number of the materials (Z_{Cd} =48, Z_{Te} =52) gives a high quantum efficiency in comparison with Si. The large band-gap energy (Eg ~ 1.5 eV) allows us to operate the detector at room temperature. However, a considerable amount of charge loss in these detectors produces a reduced energy resolution. This problem arises due to the low mobility and short lifetime of holes. Recently, significant improvements have been achieved to improve the spectral properties based on the advances in the production of crystals and in the design of electrodes. In this overview talk, we summarize (1) advantages and disadvantages of CdTe and CdZnTe semiconductor detectors and (2) technique for improving energy resolution and photopeak efficiencies. Applications of these imaging detectors in future hard X-ray and Gamma-ray astronomy missions are briefly discussed.

MISC

 220
  • Keigo Okuma, Kazuhiro Nakazawa, Shin'ichiro Takeda, Mii Ando, Yuki Omiya, Manari Oguchi, Atsuya Tanaka, Yuna Tsuji, Shin Watanabe, Tadayuki Takahashi, Masahiko Kobayashi, Naoki Ishida, Takahiro Minami, Mitsunobu Onishi, Toshihiko Arai
    Proceedings of 38th International Cosmic Ray Conference — PoS(ICRC2023) 2023年8月18日  
  • 小高裕和, 新井翔大, 市橋正裕, 高嶋聡, 丹波翼, 南木宙斗, 馬場彩, 青山一天, 櫻井真由, 清水虎冴, 田中雅士, 谷口日奈子, 中島理幾, 中曽根太地, 寄田浩平, 一戸悠人, KHANGULYAN Dmitry, 井上芳幸, 内田悠介, 須田祐介, 高橋弘充, 深沢泰司, 辻直美, 廣島渚, 八幡和志, 米田浩基, 渡辺伸, ARAMAKI Tsuguo, KARAGIORGI Georgia, MUKHERJEE Reshmi
    日本天文学会年会講演予稿集 2023 2023年  
  • 米田浩基, 新井翔大, 市橋正裕, 小高裕和, 高嶋聡, 丹波翼, 南木宙斗, 馬場彩, 青山一天, 岩澤広大, 櫻井真由, 清水虎冴, 田中雅士, 谷口日奈子, 中島理機, 中曽根太地, 寄田浩平, 一戸悠人, KHANGULYAN Dmitry, 井上芳幸, 内田悠介, 須田祐介, 高橋弘充, 深沢泰司, 辻直美, 廣島渚, 八幡和志, 渡辺伸, ARAMAKI Tsuguo, KARAGIORGI Georgia, MUKHERJEE Reshmi
    日本物理学会講演概要集(CD-ROM) 78(1) 2023年  
  • 中澤知洋, 石田学, 内田裕之, 小高裕和, 幸村孝由, 佐藤寿紀, 澤田真理, 鈴木寛大, 高橋弘充, 田中孝明, 鶴剛, 中嶋大, 野田博文, 萩野浩一, 松本浩典, 村上弘志, 森浩二, 山口弘悦, 米山友景, 渡辺伸
    日本天文学会年会講演予稿集 2023 2023年  
  • 林克洋, 田代信, 田代信, 寺田幸功, 寺田幸功, 高橋弘充, 信川正順, 水野恒史, 宇野伸一郎, 久保田あや, 中澤知洋, 渡辺伸, 飯塚亮, 佐藤理江, 米山友景, 吉田鉄生, BALUTA Chris, 海老沢研, 江口智士, 深澤泰司, 橋口葵, 勝田哲, 北口貴雄, 小高裕和, 大野雅功, 太田直美, 阪間美南, 阪本菜月, 志達めぐみ, 塩入匠, 丹波翼, 谷本敦, 寺島雄一, 坪井陽子, 内田和海, 内田悠介, 内山秀樹, 山田智史, 山内茂雄
    日本天文学会年会講演予稿集 2023 2023年  

講演・口頭発表等

 93
  • 外山裕一, 東俊行A, 石田勝彦A, 一戸悠人B, 大豆生田創B, 岡田信二, 奥村拓馬C, 桂川美穂D, 河村成肇E, 神田聡太郎, 木野康志F, 小西蓮F, 小湊菜央B, 佐々木喬祐, 佐藤寿紀B, 下村浩一郎, 高橋忠幸D, 竹下聡史E, 武田伸一郎, 竜野秀行C, 反保元伸E, 中島良太F, 名取寛顕E, 野田博文G, 橋本直H, 早川亮大B, 三宅康博E, 山下琢磨F, 山田真也B, 渡辺伸D, D.A. BennettI, W.B. DorieseI, M.S. DurkinI, J.W. FowlerI, J.D. GardI, G.C. HiltonI, K.M. MorganI, G.C. O'NeilI, C.D. ReintsemaI, D.R. SchmidtI, P. StrasserE, D.S. SwetzI, J.N. UllomI
    日本物理学会2024年春季大会 2024年3月18日
  • 小高裕和, 石渡幸太, 井上芳幸, 河村穂登, 白濱健太郎, 高嶋聡, 巽隆太朗, 袴田知宏, 松下友亮, 善本真梨那, 青山一天A, 荒井紳太朗A, 石川皓貴A, 内海和伸A, 清水虎冴A, 田中雅士A, 谷口日奈子A, 中島理幾A, 𡈽方歌乃A, 矢野裕太郎A, 寄田浩平A, 新井翔大B, 市橋正裕B, 岩田季也B, 加藤辰明B, 萩野浩一B, 馬場彩B, 一戸悠人C, 内田悠介D, 大熊佳吾E, 中澤知洋E, Dmitry KhangulyanF, 須田祐介G, 高橋弘充G, 深沢泰司G, 丹波翼H, 渡辺伸H, 白石卓也I, 辻直美I, 廣島渚J, 八幡和志K, 米田浩基L, Tsuguo AramakiM, Georgia KaragiorgiN, Reshmi MukherjeeO, GRAMSコラボレーション
    日本物理学会2024年春季大会 2024年3月18日
  • 寺田幸功A, 志達めぐみB, 塩入匠, 新居田祐基B, 澤田真理C, 小湊隆D, 田代信A, 戸田謙一A, 前島弘則A, 夏苅権A, 高橋弘充E, 信川正順F, 水野恒史E, 宇野伸一郎G, 中澤知洋H, 内山秀樹I, 久保田あやJ, 寺島雄一B, 深沢泰司E, 山内茂雄K, 太田直美K, 北口貴雄L, 勝田哲, 坪井陽子M, 海老沢研A, 内田悠介N, 江口智士O, 林克洋A, 谷本敦P, 米山友景M, 山田智史L, 内田和海A, 吉田鉄生A, 金丸善朗A, 小川翔司A, 星野晶夫A, 渡辺伸A, 飯塚亮A, Holland MattQ, Loewenstein MichaelQ, R, Miller EricS, Yaqoob TahirT, Baluta ChrisQ, Sakamoto NF, Shiraki AK, Nemoto NM, Omiya YH, Suzuki NK, Yoshimoto MT, Okuma KH
    日本物理学会2024年春季大会 2024年3月18日
  • 林克洋A, 田代信A, B, 寺田幸功A, 高橋弘充C, 信川正順D, 水野恒史C, 宇野伸一郎, 中澤知洋F, 内山秀樹G, 久保田あやH, 寺島雄一I, 深澤泰司C, 山内茂雄J, 太田直美J, 北口貴雄K, 勝田哲B, 坪井陽子L, 志達めぐみI, 海老沢研A, 内田悠介M, 江口智士N, 谷本敦O, 米山友景L, 山田智史K, 内田和海A, 吉田鉄生A, 金丸善朗A, 小川翔司A, 星野晶夫A, 渡辺伸A, 飯塚亮A, Matt HollandP, Michael LoewensteinP, Q, Eric MillerR, Tahir YaqoobP, Chris BalutaP, 塩入匠B, 阪本菜月C, 白木天音J, 新居田祐基I, 根本登L, 大宮悠希F, 鈴木那梨J, 善本真梨那S, 大熊佳吾F
    日本物理学会2024年春季大会 2024年3月18日
  • 成影 典之, 三石 郁之, 渡辺 伸, 坂尾 太郎, 高橋 忠幸, 長澤 俊作, Kavli IPMU, 南 喬博, 佐藤 慶暉, 清水 里香, 加島 颯太, 開発機構, 作田 皓基, 安福 千貴, 藤井 隆登, 吉田 有 佑, 馬場 萌花, 須崎 理恵, 草野 完也, 学, ISEE, 金子 岳史, 高棹 真介, Glesener Lindsay, FOXSI-4 チーム
    日本天文学会2024年春季年会 2024年3月13日

共同研究・競争的資金等の研究課題

 15