2021/11/02 更新

写真a

ナカザワ カズヒロ
中澤 知洋
NAKAZAWA Kazuhiro
所属
素粒子宇宙起源研究所 現象解析研究部門 准教授
大学院担当
大学院理学研究科
職名
准教授
外部リンク

学位 1

  1. 博士(理学) ( 2001年3月   東京大学 ) 

研究キーワード 8

  1. ブラックホール

  2. 人工衛星

  3. X線

  4. 宇宙物理

  5. 銀河団

  6. 硬X線

  7. ガンマ線

  8. X線天文学

研究分野 2

  1. 自然科学一般 / 素粒子、原子核、宇宙線、宇宙物理にする理論

  2. 自然科学一般 / 天文学

現在の研究課題とSDGs 2

  1. 雷雲中での粒子加速とガンマ線放射の研究

  2. 宇宙X線MeVガンマ線観測

経歴 2

  1. 東京大学   大学院理学系研究科物理学専攻   講師

    2007年4月 - 2017年12月

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    国名:日本国

  2. JAXA   宇宙科学研究所   助教

    2001年7月 - 2007年3月

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    国名:日本国

学歴 1

  1. 東京大学   理学系研究科   物理学専攻

    1996年4月 - 2001年3月

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    国名: 日本国

所属学協会 3

  1. 日本地球惑星科学連合

    2019年1月 - 現在

  2. 日本天文学会

  3. 日本物理学会

 

論文 87

  1. Multiple Gamma-Ray Glows and a Downward TGF Observed From Nearby Thunderclouds

    Hisadomi S., Nakazawa K., Wada Y., Tsuji Y., Enoto T., Shinoda T., Morimoto T., Nakamura Y., Yuasa T., Tsuchiya H.

    JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES   126 巻 ( 18 )   2021年9月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Journal of Geophysical Research: Atmospheres  

    Around 17:00 on January 12, 2020 (UTC), radiation detectors installed at two locations with a 1.35 km separation in Kanazawa City, Japan, captured a total of four gamma-ray enhancements. The first pair was simultaneously observed at the two locations at 17:03 and were abruptly terminated by a lightning discharge. The remaining two enhancements were also nearly simultaneously observed (Formula presented.) 3 min later, and one of them was also terminated by another lightning discharge. At the last termination, a downward terrestrial gamma-ray flash and a negative energetic in-cloud pulse were observed. Both pairs were associated with thundercloud cells. In the first pair, simultaneous detection in two locations 1.35 km apart suggests either a gamma-ray glow emerged in-between and time variability of its intensity were directly observed or there were two (or more) gamma-ray glows in the cell which reached the two detectors coincidentally. In the latter pair, the peak time in the downwind detector was (Formula presented.) 40 s later than that of the upwind detector. If the irradiation region moved with the cell, it would have taken ∼110 s. The discrepancy suggests either the glow moved 2.5 times faster than the cell or there were two (or more) glows in the cell. Also, the fact that the thunderstorm cell hosting the latter glows experienced the lightning discharge (Formula presented.) 3 min before suggests that the strong electric field in the cell can develop within a few minutes.

    DOI: 10.1029/2021JD034543

    Web of Science

    Scopus

  2. Detailed design of the science operations for the XRISM mission

    Terada Yukikatsu, Holland Matt, Loewenstein Michael, Tashiro Makoto, Takahashi Hiromitsu, Nobukawa Masayoshi, Mizuno Tsunefumi, Tamura Takayuki, Uno Shin'ichiro, Watanabe Shin, Baluta Chris, Burns Laura, Ebisawa Ken, Eguchi Satoshi, Fukazawa Yasushi, Hayashi Katsuhiro, Iizuka Ryo, Katsuda Satoru, Kitaguchi Takao, Kubota Aya, Miller Eric, Mukai Koji, Nakashima Shinya, Nakazawa Kazuhiro, Odaka Hirokazu, Ohno Masanori, Ota Naomi, Sato Rie, Sawada Makoto, Sugawara Yasuharu, Shidatsu Megumi, Tamba Tsubasa, Tanimoto Atsushi, Terashima Yuichi, Tsuboi Yohko, Uchida Yuusuke, Uchiyama Hideki, Yamauchi Shigeo, Yaqoob Tahir

    JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS   7 巻 ( 3 )   2021年7月

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    記述言語:日本語   出版者・発行元:Journal of Astronomical Telescopes, Instruments, and Systems  

    X-Ray Imaging and Spectroscopy Mission (XRISM) is an x-ray astronomical mission led by the Japan Aerospace Exploration Agency (JAXA) and National Aeronautics and Space Administration (NASA), with collaboration from the European Space Agency (ESA) and other international participants, that is planned for launch in 2022 (Japanese fiscal year), to quickly restore high-resolution x-ray spectroscopy of astrophysical objects using the microcalorimeter array after the loss of Hitomi satellite. In order to enhance the scientific outputs of the mission, the Science Operations Team (SOT) is structured independently from the Instrument Teams (ITs) and the Mission Operations Team. The responsibilities of the SOT are divided into four categories: (1) guest observer program and data distributions, (2) distribution of analysis software and the calibration database, (3) guest observer support activities, and (4) performance verification and optimization activities. Before constructing the operations concept of the XRISM mission, lessons on the science operations learned from past Japanese x-ray missions (ASCA, Suzaku, and Hitomi) are reviewed, and 15 kinds of lessons are identified by categories, such as lessons on the importance of avoiding non-public ("animal") tools, coding quality of public tools in terms of the engineering viewpoint and calibration accuracy, tight communications with ITs and operations teams, and well-defined task division between scientists and engineers. Among these lessons, (a) the importance of early preparation of the operations from the ground stage, (b) construction of an independent team for science operations separate from the instrument development, and (c) operations with well-defined duties by appointed members are recognized as key lessons for XRISM. Based on this, (i) the task division between the mission and science operations and (ii) the subgroup structure within the XRISM Team are defined in detail as the XRISM operations concept. Based on this operations concept, the detailed plan of the science operations is designed as follows. The science operations tasks are shared among Japan, the USA, and Europe and are performed by three centers: the Science Operations Center (SOC) at JAXA, the Science Data Center (SDC) at NASA, and European Space Astronomy Centre (ESAC) at the ESA. The SOT is defined as a combination of the SOC and SDC. The SOC is designed to perform tasks close to the spacecraft operations, such as spacecraft planning of science targets, quick-look health checks, and prepipeline data processing. The SDC covers tasks regarding data calibration processing (pipeline processing) and maintenance of analysis tools. The data-archive and user-support activities are planned to be covered both by the SOC and SDC. Finally, the details of the science operations tasks and the tools for science operations are defined and prepared before launch. This information is expected to be helpful for the construction of science operations of future x-ray missions.

    DOI: 10.1117/1.JATIS.7.3.037001

    Web of Science

    Scopus

  3. Current status of space gravitational wave antenna DECIGO and B-DECIGO

    Kawamura Seiji, Ando Masaki, Seto Naoki, Sato Shuichi, Musha Mitsuru, Kawano Isao, Yokoyama Jun'ichi, Tanaka Takahiro, Ioka Kunihito, Akutsu Tomotada, Takashima Takeshi, Agatsuma Kazuhiro, Araya Akito, Aritomi Naoki, Asada Hideki, Chiba Takeshi, Eguchi Satoshi, Enoki Motohiro, Fujimoto Masa-Katsu, Fujita Ryuichi, Futamase Toshifumi, Harada Tomohiro, Hayama Kazuhiro, Himemoto Yoshiaki, Hiramatsu Takashi, Hong Feng-Lei, Hosokawa Mizuhiko, Ichiki Kiyotomo, Ikari Satoshi, Ishihara Hideki, Ishikawa Tomohiro, Itoh Yousuke, Ito Takahiro, Iwaguchi Shoki, Izumi Kiwamu, Kanda Nobuyuki, Kanemura Shinya, Kawazoe Fumiko, Kobayashi Shiho, Kohri Kazunori, Kojima Yasufumi, Kokeyama Keiko, Kotake Kei, Kuroyanagi Sachiko, Maeda Kei-ichi, Matsushita Shuhei, Michimura Yuta, Morimoto Taigen, Mukohyama Shinji, Nagano Koji, Nagano Shigeo, Naito Takeo, Nakamura Kouji, Nakamura Takashi, Nakano Hiroyuki, Nakao Kenichi, Nakasuka Shinichi, Nakayama Yoshinori, Nakazawa Kazuhiro, Nishizawa Atsushi, Ohkawa Masashi, Oohara Kenichi, Sago Norichika, Saijo Motoyuki, Sakagami Masaaki, Sakai Shin-ichiro, Sato Takashi, Shibata Masaru, Shinkai Hisaaki, Shoda Ayaka, Somiya Kentaro, Sotani Hajime, Takahashi Ryutaro, Takahashi Hirotaka, Akiteru Takamori, Taniguchi Keisuke, Taruya Atsushi, Tsubono Kimio, Tsujikawa Shinji, Ueda Akitoshi, Ueda Ken-ichi, Watanabe Izumi, Yagi Kent, Yamada Rika, Yokoyama Shuichiro, Yoo Chul-Moon, Zhu Zong-Hong

    PROGRESS OF THEORETICAL AND EXPERIMENTAL PHYSICS   2021 巻 ( 5 )   2021年5月

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    記述言語:日本語   出版者・発行元:Progress of Theoretical and Experimental Physics  

    The Deci-hertz Interferometer Gravitational Wave Observatory (DECIGO) is a future Japanese space mission with a frequency band of 0.1 Hz to 10 Hz. DECIGO aims at the detection of primordial gravitational waves, which could have been produced during the inflationary period right after the birth of the Universe. There are many other scientific objectives of DECIGO, including the direct measurement of the acceleration of the expansion of the Universe, and reliable and accurate predictions of the timing and locations of neutron star/black hole binary coalescences. DECIGO consists of four clusters of observatories placed in heliocentric orbit. Each cluster consists of three spacecraft, which form three Fabry-Pérot Michelson interferometers with an arm length of 1000 km. Three DECIGO clusters will be placed far from each other, and the fourth will be placed in the same position as one of the other three to obtain correlation signals for the detection of primordial gravitational waves. We plan to launch B-DECIGO, which is a scientific pathfinder for DECIGO, before DECIGO in the 2030s to demonstrate the technologies required for DECIGO, as well as to obtain fruitful scientific results to further expand multi-messenger astronomy.

    DOI: 10.1093/ptep/ptab019

    Web of Science

    Scopus

  4. Meteorological Aspects of Gamma-Ray Glows in Winter Thunderstorms

    Wada Y., Enoto T., Kubo M., Nakazawa K., Shinoda T., Yonetoku D., Sawano T., Yuasa T., Ushio T., Sato Y., Diniz G. S., Tsuchiya H.

    GEOPHYSICAL RESEARCH LETTERS   48 巻 ( 7 )   2021年4月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Geophysical Research Letters  

    During three winter seasons from November 2016 to March 2019, 11 gamma-ray glows were detected at a single observation site of our ground-based gamma-ray monitoring network in Kanazawa, Japan. These events are analyzed with observations of an X-band radar network, a ceilometer, a disdrometer, and a weather monitor. All the detected glows were connected to convective high-reflectivity regions of more than 35 dBZ, developed up to an altitude of >2 km. They were also accompanied by heavy precipitation of graupels. Therefore, graupels in the lower layer of thunderclouds that correspond to high-reflectivity regions can form strong electric fields producing gamma-ray glows. Also, these events are compared with a limited sample of nondetection cases, but no significant differences in meteorological conditions were found between detection and nondetection cases in the present study.

    DOI: 10.1029/2020GL091910

    Web of Science

    Scopus

    その他リンク: https://onlinelibrary.wiley.com/doi/full-xml/10.1029/2020GL091910

  5. Simulations of expected signal and background of gamma-ray sources by large field-of-view detectors aboard CubeSats

    Galgoczi Gabor, Ripa Jakub, Campana Riccardo, Werner Norbert, Pal Andras, Ohno Masanori, Meszaros Laszlo, Mizuno Tsunefumi, Tarcai Norbert, Torigoe Kento, Uchida Nagomi, Fukazawa Yasushi, Takahashi Hiromitsu, Nakazawa Kazuhiro, Hirade Naoyoshi, Hirose Kengo, Hisadomi Syohei, Enoto Teruaki, Odaka Hirokazu, Ichinohe Yuto, Frei Zsolt, Kiss Laszlo

    JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS   7 巻 ( 2 )   2021年4月

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    記述言語:日本語   出版者・発行元:Journal of Astronomical Telescopes, Instruments, and Systems  

    In recent years, the number of CubeSats (U-class spacecrafts) launched into space has increased exponentially marking the dawn of the nanosatellite technology. In general, these satellites have a much smaller mass budget compared to conventional scientific satellites, which limits shielding of scientific instruments against direct and indirect radiation in space. We present a simulation framework to quantify the signal in large field-of-view gamma-ray scintillation detectors of satellites induced by x-ray/gamma-ray transients, by taking into account the response of the detector. Furthermore, we quantify the signal induced by x-ray and particle background sources at a Low-Earth Orbit outside South Atlantic Anomaly and polar regions. Finally, we calculate the signal-to-noise ratio (SNR) taking into account different energy threshold levels. Our simulation can be used to optimize material composition and predict detectability of various astrophysical sources by CubeSats. We apply the developed simulation to a satellite belonging to a planned CAMELOT CubeSat constellation. This project mainly aims to detect short and long gamma-ray bursts (GRBs) and as a secondary science objective, to detect soft gamma-ray repeaters (SGRs) and terrestrial gamma-ray flashes (TGFs). The simulation includes a detailed computer-aided design model of the satellite to take into account the interaction of particles with the material of the satellite as accurately as possible. Results of our simulations predict that CubeSats can complement the large space observatories in high-energy astrophysics for observations of GRBs, SGRs, and TGFs. For the detectors planned to be on board the CAMELOT CubeSats, the simulations show that detections with SNR of at least 9 for median GRB and SGR fluxes are achievable.

    DOI: 10.1117/1.JATIS.7.2.028004

    Web of Science

    Scopus

  6. Annealing of proton radiation damages in Si-PM at room temperature

    Hirade Naoyoshi, Takahashi Hiromitsu, Uchida Nagomi, Ohno Masanori, Torigoe Kento, Fukazawa Yasushi, Mizuno Tsunefumi, Matake Hiroto, Hirose Kengo, Hisadomi Syouhei, Nakazawa Kazuhiro, Yamaoka Kazutaka, Werner Norbert, Ripa Jakub, Hatori Satoshi, Kume Kyo, Mizushima Satoshi

    NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT   986 巻   2021年1月

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    記述言語:日本語   出版者・発行元:Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment  

    We report the radiation damage results of two new types of Multi-Pixel Photon Counter (MPPC) under the 200 MeV proton beam, for cosmic gamma-ray observations with CubeSats. The new MPPCs, S13360-6050CS and S14160-6050HS, have recently become commercially available by Hamamatsu Photonics K.K. (HPK). After 100 rad irradiation, the dark current increased by a factor of ∼100 and the threshold energy of gamma-ray detection by CsI scintillator increased, but S14160-6050HS was less degraded. We then confirmed the annealing effects of the dark current and threshold energy for both. The decrease rate of the dark current in both MPPCs were similar to those in the previous works. At 20 °C, the threshold energies of both MPPCs reduced by several tens of percent after irradiation, but below 0 °C, the threshold energy of S14160-6050HS was not significantly lowered. We also confirmed that annealing began before one month post-irradiation.

    DOI: 10.1016/j.nima.2020.164673

    Web of Science

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  7. Attenuation characteristics of a Ce:Gd3Al2Ga3O12 scintillator

    Nagomi Uchida, Hiromitsu Takahashi, Masanori Ohno, Tsunefumi Mizuno, Yasushi Fukazawa, Masao Yoshino, Kei Kamada, Yuui Yokota, Akira Yoshikawa

    NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT   986 巻   2021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  

    Attenuation characteristics of scintillation photons from Ce-doped Gd3Al2Ga3O12 (Ce:GAGG) scintillators were investigated by measuring samples of various sizes. Scintillation light is attenuated by two factors. The first is self-absorption of the Ce:GAGG scintillator itself, and the second is geometrical effects such as reflection properties caused by reflector wrapping. The attenuation coefficient of the Ce:GAGGs was determined as 0.00155 +/- 0.00006 mm(-1) indicating that the scintillation light decays to 1/e as it passes approximately 645 +/- 26 mm through the Ce:GAGG. This attenuation does not affect the entire wavelength range; however, it significantly occurs only in the wavelength range from 460 nm to 510 nm where emission and absorption overlap. In the narrow Ce:GAGG scintillator used in this experiment, the geometrical attenuation effect was in the overall wavelength, and the attenuation coefficient was 0.010 +/- 0.001 mm(-1). In this setup, the self-absorption effect only occupied 10% of the whole attenuation, while geometrical attenuation significantly affected the number of detected photons.

    DOI: 10.1016/j.nima.2020.164725

    Web of Science

  8. GRBAlpha: A 1U CubeSat mission for validating timing-based gamma-ray burst localization

    Pal Andras, Ohno Masanori, Meszaros Laszlo, Werner Norbert, Ripa Jakub, Frajt Marcel, Hirade Naoyoshi, Hudec Jan, Kapus Jakub, Koleda Martin, Laszlo Robert, Lipovsky Pavol, Matake Hiroto, Smelko Miroslav, Uchida Nagomi, Csak Balazs, Enoto Teruaki, Frei Zsolt, Fukazawa Yasushi, Galgoczi Gabor, Hirose Kengo, Hisadomi Syohei, Ichinohe Yuto, Kiss Laszlo L., Mizuno Tsunefumi, Nakazawa Kazuhiro, Odaka Hirokazu, Takahashi Hiromitsu, Torigoe Kento

    SPACE TELESCOPES AND INSTRUMENTATION 2020: ULTRAVIOLET TO GAMMA RAY   11444 巻   2021年

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    記述言語:日本語   出版者・発行元:Proceedings of SPIE - The International Society for Optical Engineering  

    GRBAlpha is a 1U CubeSat mission with an expected launch date in the first half of 2021. It carries a 75 × 75 × 5 mm CsI(Tl) scintillator, read out by a dual-channel multi-pixel photon counter (MPPC) setup, to detect gamma-ray bursts (GRBs). The GRB detector is an in-orbit demonstration for the detector system on the Cubesats Applied for MEasuring and LOcalising Transients (CAMELOT) mission. While GRBAlpha provides 1/8th of the expected effective area of CAMELOT, the comparison of the observed light curves with other existing GRB monitoring satellites will allow us to validate the core idea of CAMELOT, i.e. the feasibility of timing-based localization.

    DOI: 10.1117/12.2561351

    Web of Science

    Scopus

  9. Detail Plans and Preparations for the Science Operations of the XRISM mission

    Terada Yukikatsu, Holland Matthew, Loewenstein Michael, Tashiro Makoto, Takahashi Hiromitsu, Nobukawa Masayoshi, Mizuno Tsunefumi, Tamura Takayuki, Uno Shin'ichiro, Watanabe Shin, Baluta Chris, Burns Laura, Ebisawa Ken, Eguchi Satoshi, Fukazawa Yasushi, Hayashi Katsuhiro, Iizuka Ryo, Katsuda Satoru, Kitaguchi Takao, Kubota Aya, Miller Eric, Mukai Koji, Nakashima Shinya, Nakazawa Kazuhiro, Odaka Hirokazu, Ohno Masanori, Ota Naomi, Sato Rie, Sugawara Yasuharu, Shidatsu Megumi, Tamba Tsubasa, Tanimoto Atsushi, Terashima Yuichi, Tsuboi Yohko, Uchida Yuusuke, Uchiyama Hideki, Yamauchi Shigeo, Yaqoob Tahir

    SPACE TELESCOPES AND INSTRUMENTATION 2020: ULTRAVIOLET TO GAMMA RAY   11444 巻   2021年

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    記述言語:日本語   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:Proceedings of SPIE - The International Society for Optical Engineering  

    The XRISM is the X-ray astronomical mission led by JAXA/NASA/ESA with international participation, plan to be launched in 2022 (Japanese fiscal year), to quickly recover the high-resolution X-ray spectroscopy of astrophysical objects using the micro-calorimeter array after the failure of Hitomi. To enhance the scientific outputs of the mission, the Science Operations Team (SOT) is structured independently from the instrument teams and the mission operation team (MOT). The responsibilities of the SOT are summarized into four categories: 1) Guest observer program and data distributions, 2) Distribution of the analyses software and calibration database, 3) Guest observer supporting activities, and 4) the performance verification and optimization (PVO) activities. Before constructing the Operations Concept of the XRISM mission, the lessons on the Science Operations learned from the past Japanese X-ray missions (ASCA, Suzaku, and Hitomi) are reviewed, and 16 kinds of lessons are identified by the above categories: lessons on the importance of avoiding nonpublic (“animal”) tools, coding quality of public tools both on the engineering viewpoint and the calibration accuracy, tight communications with instrument teams and operations team, well-defined task division between scientists and engineers etc. Among these lessons, a) importance of the early preparations of the operations from the ground stage, b) construction of the independent team for the Science Operations from the instrument developments, and c) operations with well-defined duties by appointed members are recognized as the key lessons for XRISM. Then, i) the task division between the Mission and Science Operations and ii) the subgroup structure within the XRISM team are defined in detail as the XRISM Operations Concept. Then, following the Operations Concept, the detail plan of the Science Operations is designed as follows. The Science Operations tasks are shared among Japan, US, and Europe operated by three centers, the Science Operations Center (SOC) at JAXA, the Science Data Center (SDC) at NASA, and European Space Astronomy Centre (ESAC) at ESA. The SOT is defined as a combination of the SOC and SDC; the SOC is designed to perform tasks close to the spacecraft operations, such as spacecraft planning of science targets, quick-look health checks, pre-pipeline data processing, etc., and the SDC covers the tasks on the data calibration processing (pipeline processing), maintenance of the analysis tools etc. The data-archive and users-support activities are planned to be covered both by the SOC and SDC. Finally, the details of the Science Operations tasks and the tools for the Science Operations are also described in this paper. This information would be helpful for a construction of Science Operations of future X-ray missions.

    DOI: 10.1117/12.2560861

    Web of Science

    Scopus

  10. New method to make a smooth surface on Carbon Fiber Reinforced Plastic (CFRP) substrate

    Awaki H., Aida N., Asakura K., Hanaoka M., Hattori K., Ishibashi K., Ishida M., Ishikura A., Maeda Y., Matsumoto H., Matsushita Y., Mineta T., Mitsuishi I, Miyazawa T., Nakaniwa N., Nakazawa K., Ode Y., Oue C., Sawagami K., Sugita S., Suzuki H., Takahashi H., Uchida Y., Yamamoto R., Yoshimoto M.

    SPACE TELESCOPES AND INSTRUMENTATION 2020: ULTRAVIOLET TO GAMMA RAY   11444 巻   2021年

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    記述言語:日本語   出版者・発行元:Proceedings of SPIE - The International Society for Optical Engineering  

    CFRP is a composite material composed of carbon fiber and resin. CFRP is commonly applied to the aerospace industry which requires lightweight and intensity. Thanks to superior formability of CFRP, we can form shape of Wolter-1 optics, which consists of paraboloid and hyperboloid, to a monolithic substrate. Since the surface roughness of a CFRP substrate is a few µm, we have to make the smooth surface for reflecting X-rays on the CFRP substrate. We have developed a new method of shaping the reflective surface instead of the replica method used in lightweight X-ray mirrors such as Astro-H. In the new method, the reflective surface is formed by pasting thin sheet-glasses with 100 µm thick onto the CFRP substrate. The thin sheet-glass has a surface roughness about 0.4 nm as measured by Zygo. We fabricated a CFRP mirror pasting thin sheet-glasses, and then coated tungsten on the mirror in June 2020. The figure error (s) of the CFRP mirror was achieved to be about 1-2 µm by stacking the CFRP mirror on the housing module. X-ray imaging quality of the CFRP mirror was measured at Spring-8 in July 2020. The half-power diameter of the CFRP mirror was estimated to be about 150 arcsec, which was nearly equal to the prediction from a distribution of the slope error deduced from the surface profile. We describe a future plan to improve the image quality of the CFRP mirror.

    DOI: 10.1117/12.2561890

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  11. The XRISM Science Data Center: Optimizing the scientific return from a unique X-ray observatory

    Loewenstein Michael, Hill Robert S., Holland Matthew P., Miller Eric D., Yaqoob Tahir, Doyle Trisha F., Hall Patricia L., Braun Efrem, Baluta Chris, Mukai Koji, Terada Yukikatsu, Tashiro Makoto, Takahashi Hiromitsu, Nobukawa Masayoshi, Mizuno Tsunefumi, Tamura Takayuki, Uno Shin'ichiro, Watanabe Shin, Ebisawa Ken, Eguchi Satoshi, Fukazawa Yasushi, Hayashi Katsuhiro, Iizuka Ryo, Katsuda Satoru, Kitaguchi Takao, Kubota Aya, Nakashima Shinya, Nakazawa Kazuhiro, Odaka Hirokazu, Ohno Masanori, Ota Naomi, Sato Rie, Sugawara Yasuharu, Shidatsu Megumi, Tamba Tsubasa, Tanimoto Atsushi, Terashima Yuichi, Tsuboi Yohko, Uchida Yuusuke, Uchiyama Hideki, Yamauchi Shigeo

    SPACE TELESCOPES AND INSTRUMENTATION 2020: ULTRAVIOLET TO GAMMA RAY   11444 巻   2021年

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    記述言語:日本語   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:Proceedings of SPIE - The International Society for Optical Engineering  

    The X-Ray Imaging and Spectroscopy Mission, XRISM, is currently scheduled to launch in 2022 with the objective of building on the brief, but significant, successes of the ASTRO-H (Hitomi) mission in solving outstanding astrophysical questions using high resolution X-ray spectroscopy. The XRISM Science Operations Team (SOT) consists of the JAXA-led Science Operations Center (SOC) and NASA-led Science Data Center (SDC), which work together to optimize the scientific output from the Resolve high-resolution spectrometer and the Xtend wide-field imager through planning and scheduling of observations, processing and distribution of data, development and distribution of software tools and the calibration database (CaldB), support of ground and in-flight calibration, and support of XRISM users in their scientific investigations of the energetic universe. Here, we summarize the roles and responsibilities of the SDC and its current status and future plans. The Resolve instrument poses particular challenges due to its unprecedented combination of high spectral resolution and throughput, broad spectral coverage, and relatively small field-of-view and large pixel-size. We highlight those challenges and how they are being met.

    DOI: 10.1117/12.2560840

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  12. Status of X-Ray Imaging and Spectroscopy Mission (XRISM)

    Tashiro Makoto, Maejima Hironori, Toda Kenichi, Kelley Richard, Reichenthal Lillian, Hartz Leslie, Petre Robert, Williams Brian, Guainazzi Matteo, Costantini Elisa, Fujimoto Ryuichi, Hayashida Kiyoshi, Henegar-Leon Joy, Holland Matt, Ishisaki Yoshitaka, Kilbourne Caroline, Loewenstein Mike, Matsushita Kyoko, Mori Koji, Okajima Takashi, Porter F. Scott, Sneiderman Gary, Takei Yoh, Terada Yukikatsu, Tomida Hiroshi, Yamaguchi Hiroya, Watanabe Shin, Akamatsu Hiroki, Arai Yoshitaka, Audard Marc, Awaki Hisamitsu, Babyk Iurii, Bamba Aya, Bando Nobutaka, Behar Ehud, Bialas Thomas, Boissay-Malaquin Rozenn, Brenneman Laura, Brown Greg, Canavan Edgar, Chiao Meng, Comber Brian, Corrales Lia, Cumbee Renata, de Vries Cor, den Herder Jan-Willem, Dercksen Johannes, Diaz-Trigo Maria, DiPirro Michael, Done Chris, Dotani Tadayasu, Ebisawa Ken, Eckart Megan, Eckert Dominique, Eguchi Satoshi, Enoto Teruaki, Ezoe Yuichiro, Ferrigno Carlo, Fujita Yutaka, Fukazawa Yasushi, Furuzawa Akihiro, Gallo Luigi, Gorter Nathalie, Grim Martin, Gu Liyi, Hagino Kouichi, Hamaguchi Kenji, Hatsukade Isamu, Hawthorn David, Hayashi Katsuhiro, Hell Natalie, Hiraga Junko, Hodges-Kluck Edmund, Horiuchi Takafumi, Hornschemeier Ann, Hoshino Akio, Ichinohe Yuto, Iga Sayuri, Iizuka Ryo, Ishida Manabu, Ishihama Naoki, Ishikawa Kumi, Ishimura Kosei, Jaffe Tess, Kaastra Jelle, Kallman Timothy, Kara Erin, Katsuda Satoru, Kenyon Steven, Kimball Mark, Kitaguchi Takao, Kitamoto Shunji, Kobayashi Shogo, Kobayashi Akihide, Kohmura Takayoshi, Kubota Aya, Leutenegger Maurice, Li Muzi, Lockard Tom, Maeda Yoshitomo, Markevitch Maxim, Martz Connor, Matsumoto Hironori, Matsuzaki Keiichi, McCammon Dan, McLaughlin Brian, McNamara Brian, Miko Joseph, Miller Eric, Miller Jon, Minesugi Kenji, Mitani Shinji, Mitsuishi Ikuyuki, Mizumoto Misaki, Mizuno Tsunefumi, Mukai Koji, Murakami Hiroshi, Mushotzky Richard, Nakajima Hiroshi, Nakamura Hideto, Nakazawa Kazuhiro, Natsukari Chikara, Nigo Kenichiro, Nishioka Yusuke, Nobukawa Kumiko, Nobukawa Masayoshi, Noda Hirofumi, Odaka Hirokazu, Ogawa Mina, Ohashi Takaya, Ohno Masahiro, Ohta Masayuki, Okamoto Atsushi, Ota Naomi, Ozaki Masanobu, Paltani Stephane, Plucinsky Paul, Pottschmidt Katja, Sampson Michael, Sasaki Takahiro, Sato Kosuke, Sato Rie, Sato Toshiki, Sawada Makoto, Seta Hiromi, Shibano Yasuko, Shida Maki, Shidatsu Megumi, Shigeto Shuhei, Shinozaki Keisuke, Shirron Peter, Simionescu Aurora, Smith Randall, Someya Kazunori, Soong Yang, Sugawara Keisuke, Sugawara Yasuharu, Szymkowiak Andy, Takahashi Hiromitsu, Takeshima Toshiaki, Tamagawa Toru, Tamura Keisuke, Tanaka Takaaki, Tanimoto Atsushi, Terashima Yuichi, Tsuboi Yohko, Tsujimoto Masahiro, Tsunemi Hiroshi, Tsuru Takeshi, Uchida Hiroyuki, Uchida Yuusuke, Uchiyama Hideki, Ueda Yoshihiro, Uno Shinichiro, Vink Jacco, Watanabe Tomomi, Witthoeft Michael, Wolfs Rob, Yamada Shinya, Yamaoka Kazutaka, Yamasaki Noriko, Yamauchi Makoto, Yamauchi Shigeo, Yanagase Keiichi, Yaqoob Tahir, Yasuda Susumu, Yoshida Tessei, Yoshioka Nasa, Zhuravleva Irina

    SPACE TELESCOPES AND INSTRUMENTATION 2020: ULTRAVIOLET TO GAMMA RAY   11444 巻   2021年

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    記述言語:日本語   出版者・発行元:Proceedings of SPIE - The International Society for Optical Engineering  

    The X-Ray Imaging and Spectroscopy Mission (XRISM) is the successor to the 2016 Hitomi mission that ended prematurely. Like Hitomi, the primary science goals are to examine astrophysical problems with precise high-resolution X-ray spectroscopy. XRISM promises to discover new horizons in X-ray astronomy. XRISM carries a 6 x 6 pixelized X-ray micro-calorimeter on the focal plane of an X-ray mirror assembly and a co-aligned X-ray CCD camera that covers the same energy band over a large field of view. XRISM utilizes Hitomi heritage, but all designs were reviewed. The attitude and orbit control system were improved in hardware and software. The number of star sensors were increased from two to three to improve coverage and robustness in onboard attitude determination and to obtain a wider field of view sun sensor. The fault detection, isolation, and reconfiguration (FDIR) system was carefully examined and reconfigured. Together with a planned increase of ground support stations, the survivability of the spacecraft is significantly improved.

    DOI: 10.1117/12.2565812

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  13. Solar Neutron Spectrometer Onboard a 3U CubeSat

    YAMAOKA Kazutaka, MATSUSHITA Koji, ITO Kazuya, NOBASHI Daiki, TAKAHASHI Hiromitsu, WATANABE Kyoko, TAJIMA Hiroyasu, MIYATA Kikuko, INAMORI Takaya, SASAI Yoshinori, KAWAHARA Hiroaki, PARK Ji Hyun, NAKAZAWA Kazuhiro, MASUDA Satoshi

    TRANSACTIONS OF THE JAPAN SOCIETY FOR AERONAUTICAL AND SPACE SCIENCES, AEROSPACE TECHNOLOGY JAPAN   19 巻 ( 3 ) 頁: 354 - 359   2021年

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    記述言語:英語   出版者・発行元:一般社団法人 日本航空宇宙学会  

    <p>Solar neutron observations are very important for understanding of nucleon acceleration mechanism in solar flares, but there are only a few tens of detection since the discovery in 1980. This is because solar neutron observations have been mainly carried out from not space but the ground with insufficient sensitivity. For microsatellite applications, we have designed very compact and high sensitive solar neutron and gamma-ray spectrometer utilizing a novel photo-sensor Silicon photo-multiplier. This paper describes concept, design and performance of our detector for micro/nanosatellite applications.</p>

    DOI: 10.2322/tastj.19.354

    CiNii Article

  14. Current status of the x-ray mirror for the XL-Calibur experiment

    Kengo Hattori, Hironori Matsumoto, Quincy Abarr, Hisamitsu Awaki, Richard Bose, Dana Braun, Gianluigi De Geronimo, Paul Dowkontt, Teruaki Enoto, Manel Errando, Yasushi Fukazawa, Thomas A. Gadson, Victor Guarino, Shuichi Gunji, Kiyoshi Hayashida, Scott E. Heatwole, Shuntaro Ide, Manabu Ishida, Nirmal Iyer, Henric Krawczynski, Yoshitomo Maeda, Takuya Miyazawa, Hirofumi Noda, Takashi Okajima, Hiromitsu Takahashi, Keisuke Tamura, Hiroshi Tsunemi, Fabian Kislat, Mózsi Kiss, Takao Kitaguchi, Rakhee Kushwah, James Lanzi, Shaorui Li, Lindsey Lisalda, Tsunefumi Mizuno, Nozomi Nakaniwa, Mark Pearce, Zachary Peterson, Brian Rauch, David Stuchlik, Mai Takeo, Toru Tamagawa, Kazumi Uchida, Andrew T. West

    Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray     2020年12月

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    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  

    DOI: 10.1117/12.2560928

  15. Satellite mission: PhoENiX (Physics of Energetic and Non-thermal plasmas in the X (= magnetic reconnection) region)

    Noriyuki Narukage, Mitsuo Oka, Yasushi Fukazawa, Keiichi Matsuzaki, Shin Watanabe, Taro Sakao, Kouichi Hagino, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Iku Shinohara, Masumi Shimojo, Shinsuke Takasao, Hiroshi Tanabe, Munetaka Ueno, Tadayuki Takahashi, Takeshi Takashima, Masayuki Ohta

    Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray     2020年12月

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    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  

    DOI: 10.1117/12.2561341

  16. Photonuclear Reactions in Lightning: 1. Verification and Modeling of Reaction and Propagation Processes

    Wada Y., Enoto T., Nakazawa K., Odaka H., Furuta Y., Tsuchiya H.

    JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES   125 巻 ( 20 )   2020年10月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Journal of Geophysical Research: Atmospheres  

    We report simulation results of photonuclear reactions in the atmosphere triggered by a downward terrestrial gamma ray flash in lightning. Possible channels of reactions in the atmosphere and their cross-sections are verified with the ENDF/B-VII.1 library. Monte Carlo simulations with two stages are then performed with the Geant4 framework. In the first stage, electrons following the relativistic runaway electron avalanche spectrum are produced in a mass model of the atmosphere, and production of photoneutrons and β+-decay nuclei is calculated based on the nuclear data library. In total 1 × 1013 neutrons and 4 × 1012 β+-decay nuclei are produced by 1018 energetic electrons above 1 MeV. In the second stage, propagation of the photoneutrons and positrons from the β+-decay nuclei in the previous stage is calculated. As a result, we model on-ground distributions of fluxes and energy spectra for neutrons, neutron-related gamma rays, and annihilation ones. The simulation model is to be compared with photonuclear events detected in low-charge-center winter thunderstorms.

    DOI: 10.1029/2020JD033193

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  17. Photonuclear Reactions in Lightning: 2. Comparison Between Observation and Simulation Model

    Wada Y., Enoto T., Nakazawa K., Yuasa T., Furuta Y., Odaka H., Makishima K., Tsuchiya H.

    JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES   125 巻 ( 20 )   2020年10月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Journal of Geophysical Research: Atmospheres  

    During a winter thunderstorm on 6 February 2017 in Japan, photonuclear reactions such as 14N(γ, n)13N were triggered by a downward terrestrial gamma-ray flash (TGF), as reported by Enoto et al. (2017, https://doi.org/10.1038/nature24630). In the present paper, we compare the observation with a simulation model of downward TGFs and subsequent photonuclear reactions constructed by the first paper of the series and Wada, Enoto, Nakazawa, et al. (2019, https://doi.org/10.1103/physrevlett.123.061103). The observation and model consist of three components: annihilation gamma rays from positrons produced by β+-decay nuclei, deexcitation gamma rays originating from neutron captures, and radiation doses by TGF photons. Each component of the observation is reproduced by the simulation model, and we constrain a relation between the number of avalanche electrons and their production altitude of the downward TGF. The constraints by three components match within an order of magnitude. The downward TGF is estimated to comprise (0.5–2.5) × 1019 avalanche electrons above 1 MeV produced at an altitude of 1.4–2.7 km. Despite differences in altitude, direction, and season, downward TGFs in winter thunderstorms are thought to have the same mechanism of electron acceleration and multiplication in lightning as TGFs observed by in-orbit satellites.

    DOI: 10.1029/2020JD033194

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  18. Origin of the in-orbit instrumental background of the Hard X-ray Imager onboard Hitomi

    Hagino Kouichi, Odaka Hirokazu, Sato Goro, Sato Tamotsu, Suzuki Hiromasa, Mizuno Tsunefumi, Kawaharada Madoka, Ohno Masanori, Nakazawa Kazuhiro, Kobayashi Shogo B., Murakami Hiroaki, Miyake Katsuma, Asai Makoto, Koi Tatsumi, Madejski Greg, Saito Shinya, Wright Dennis H., Enoto Teruaki, Fukazawa Yasushi, Hayashi Katsuhiro, Kataoka Jun, Katsuta Junichiro, Kokubun Motohide, Laurent Philippe, Lebrun Francois, Limousin Olivier, Maier Daniel, Makishima Kazuo, Mori Kunishiro, Nakamori Takeshi, Nakano Toshio, Noda Hirofumi, Ohta Masayuki, Sato Rie, Tajima Hiroyasu, Takahashi Hiromitsu, Takahashi Tadayuki, Takeda Shin'ichiro, Tanaka Takaaki, Terada Yukikatsu, Uchiyama Hideki, Uchiyama Yasunobu, Watanabe Shin, Yamaoka Kazutaka, Yatsu Yoichi, Yuasa Takayuki

    JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS   6 巻 ( 4 )   2020年10月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Journal of Astronomical Telescopes, Instruments, and Systems  

    Understanding and reducing in-orbit instrumental backgrounds are essential to achieving high sensitivity in hard x-ray astronomical observations. The observational data of the Hard X-ray Imager (HXI) onboard the Hitomi satellite provide useful information on the background components due to its multilayer configuration with different atomic numbers: The HXI consists of a stack of four layers of Si (Z = 14) detectors and one layer of cadmium telluride (CdTe) (Z = 48, 52) detector surrounded by well-Type Bi4Ge3O12 active shields. Based on the observational data, the backgrounds of the top Si layer, the three underlying Si layers, and the CdTe layer are inferred to be dominated by different components, namely, low-energy electrons, albedo neutrons, and proton-induced radioactivation, respectively. Monte Carlo simulations of the in-orbit background of the HXI reproduce the observed background spectrum of each layer well, thereby quantitatively verifying the above hypothesis. In addition, we suggest the inclusion of an electron shield to reduce the background.

    DOI: 10.1117/1.JATIS.6.4.046003

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  19. Thundercloud Project: Exploring high-energy phenomena in thundercloud and lightning

    Yuasa Takayuki, Wada Yuuki, Enoto Teruaki, Furuta Yoshihiro, Tsuchiya Harufumi, Hisadomi Shohei, Tsuji Yuna, Okuda Kazufumi, Matsumoto Takahiro, Nakazawa Kazuhiro, Makishima Kazuo, Miyake Shoko, Ikkatai Yuko

    PROGRESS OF THEORETICAL AND EXPERIMENTAL PHYSICS   2020 巻 ( 10 )   2020年10月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Progress of Theoretical and Experimental Physics  

    We have designed, developed, and deployed a distributed sensor network to observe high-energy ionizing radiation, primarily gamma rays, from winter thunderclouds and lightning in coastal areas of Japan. Starting in 2015, we have installed a total of more than 15 ground-based detector systems in Ishikawa Prefecture and Niigata Prefecture, and accumulated 551 days of observation time in four winter seasons from late 2015 to early 2019. In this period, our system recorded 51 gamma-ray radiation events from thundercloud and lightning. Highlights of the science results obtained from this unprecedented amount of data include the discovery of photonuclear reaction in lightning which produces neutrons and positrons along with gamma rays, and deeper insights into the life cycle of a particle-acceleration and gamma-ray-emitting region in a thundercloud. The present paper reviews the objective, methodology, and results of our experiment, with an emphasis on its instrumentation.

    DOI: 10.1093/ptep/ptaa115

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  20. Implications of the mild gas motion found with Hitomi in the core of the Perseus cluster

    Gu Liyi, Makishima Kazuo, Matsumoto Ryoji, Nakazawa Kazuhiro, Shimasaku Kazuhiro, Inada Naohisa, Kodama Tadayuki, Xu Haiguang, Kawaharada Madoka

    ASTRONOMY & ASTROPHYSICS   638 巻   頁: A138 - A138   2020年6月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Astronomy and Astrophysics  

    Based mainly on X-ray observations, we study the interactions between the intracluster medium (ICM) in clusters of galaxies and their member galaxies. Through (magneto)hydrodynamic and gravitational channels, moving galaxies are expected to drag the ICM around them, and then transfer some fraction of their dynamical energies on cosmological timescales to the ICM. This hypothesis is in line with several observations, including the possible cosmological infall of galaxies toward the cluster center, found over redshifts of z? ∼? 1 to z? ∼? 0. Further assuming that the energy lost by these galaxies is first converted into ICM turbulence and then dissipated, this picture can explain the subsonic and uniform ICM turbulence, measured with Hitomi in the core region of the Perseus cluster. The scenario may also explain several other unanswered problems regarding clusters of galaxies, such as what prevents the ICM from underoing the expected radiative cooling, how the various mass components in nearby clusters have attained different radial distributions, and how a thermal stability is realized between hot and cool ICM components that co-exist around cD galaxies. This view is also considered to pertain to the general scenario of galaxy evolution, including their environmental effects.

    DOI: 10.1051/0004-6361/201936437

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  21. Photoneutron detection in lightning by gadolinium orthosilicate scintillators

    Wada Y., Nakazawa K., Enoto T., Furuta Y., Yuasa T., Makishima K., Tsuchiya H.

    PHYSICAL REVIEW D   101 巻 ( 10 )   2020年5月

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    記述言語:日本語   出版者・発行元:Physical Review D  

    During a winter thunderstorm on 24 November 2017, a downward terrestrial gamma-ray flash took place and triggered photonuclear reactions with atmospheric nitrogen and oxygen nuclei, coincident with a lightning discharge at the Kashiwazaki-Kariwa nuclear power station in Japan. We directly detected neutrons produced by the photonuclear reactions with gadolinium orthosilicate scintillation crystals installed at sea level. Two gadolinium isotopes included in the scintillation crystals, Gd155 and Gd157, have large cross sections of neutron captures to thermal neutrons such as Gd155(n,γ)Gd156 and Gd157(n,γ)Gd158. Deexcitation gamma rays from Gd156 and Gd158 are self-absorbed in the scintillation crystals, and make spectral-line features which can be distinguished from other non-neutron signals. The neutron burst lasted for ∼100 ms, and neutron fluences are estimated to be >52 and >31 neutrons cm-2 at two observation points inside the power station. Gadolinium orthosilicate scintillators work as valid detectors for thermal neutrons in lightning.

    DOI: 10.1103/PhysRevD.101.102007

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  22. High Peak-Current Lightning Discharges Associated With Downward Terrestrial Gamma-Ray Flashes

    Wada Y., Enoto T., Nakamura Y., Morimoto T., Sato M., Ushio T., Nakazawa K., Yuasa T., Yonetoku D., Sawano T., Kamogawa M., Sakai H., Furuta Y., Makishima K., Tsuchiya H.

    JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES   125 巻 ( 4 )   2020年2月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Journal of Geophysical Research: Atmospheres  

    During 2017–2018 winter operation of the Gamma-Ray Observation of Winter Thunderclouds experiment in Japan, two downward terrestrial gamma-ray flashes (TGFs) that triggered atmospheric photonuclear reactions were detected. They took place during winter thunderstorms on 5 December 2017 and 9 January 2018 at Kanazawa, Ishikawa Prefecture, Japan. Each event coincided with an intracloud/intercloud discharge, which had a negative-polarity peak current higher than 150 kA. Their radio waveforms in the low-frequency band are categorized as a distinct lightning type called “energetic in-cloud pulse” (EIP). Negative-polarity EIPs have been previously suggested to be highly associated with downward TGFs, and the present observations provide evidence of the correlation between them for the first time. Furthermore, both of the downward TGFs followed “gamma-ray glows,” minute-lasting high-energy emissions from thunderclouds. It is suggested that the negative EIPs took place with downward propagating negative leaders or upward positive ones developed in highly electrified regions responsible for the gamma-ray glows.

    DOI: 10.1029/2019JD031730

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  23. The simulation framework of the timing-based localization for future all-sky gamma-ray observations with a fleet of CubeSats

    Ohno M., Werner N., Pál A., Mészáros L., Ichinohe Y., Řípa J., Topinka M., Munz F., Galgóczi G., Fukazawa Y., Mizuno T., Takahashi H., Uchida N., Torigoe K., Hirade N., Hirose K., Matake H., Nakazawa K., Hisadomi S., Odaka H., Enoto T., Hudec J., Kapus J., Koleda M., Laszlo R.

    Proceedings of SPIE - The International Society for Optical Engineering   11454 巻   2020年

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    記述言語:日本語   出版者・発行元:Proceedings of SPIE - The International Society for Optical Engineering  

    The timing-based localization, which utilize the triangulation principle with the different arrival time of gammaray photons, with a fleet of Cubesats is a unique and powerful solution for the future all-sky gamma-ray observation, which is a key for identification of the electromagnetic counterpart of the gravitational wave sources. The Cubesats Applied for MEasuring and Localising Transients (CAMELOT) mission is now being promoted by the Hungarian and Japanese collaboration with a basic concept of the nine Cubesats constellations in low earth orbit. The simulation framework for estimation of the localization capability has been developed including orbital parameters, an algorithm to estimate the expected observed profile of gamma-ray photons, finding the peak of the cross-correlation function, and a statistical method to find a best-fit position and its uncertainty. It is revealed that a degree-scale localization uncertainty can be achieved by the CAMELOT mission concept for bright short gamma-ray bursts, which could be covered by future large field of view ground-based telescopes. The new approach utilizing machine-learning approach is also investigated to make the procedure automated for the future large scale constellations. The trained neural network with 106 simulated light curves generated by the artificial short burst templates successfully predicts the time-delay of the real light curve and achieves a comparable performance to the cross-correlation algorithm with full automated procedures.

    DOI: 10.1117/12.2562253

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  24. A new possible accretion scenario for ultra-luminous X-ray sources

    Kobayashi Shogo B., Nakazawa K., Makishima K.

    MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY   489 巻 ( 1 ) 頁: 366 - 384   2019年10月

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    記述言語:日本語   出版者・発行元:Monthly Notices of the Royal Astronomical Society  

    Using archival data from Suzaku, XMM-Newton, and NuSTAR, nine representative ultra-luminous X-ray sources (ULXs) in nearby galaxies were studied. Their X-ray spectra were all reproduced with a multicolour disc emission model plus its Comptonization. However, the spectral shapes of individual sources changed systematically depending on the luminosity, and defined three typical spectral states. These states differ either in the ratio between the Comptonizing electron temperature and the innermost disc temperature, or in the product of Compton y-parameter and fraction of the Comptonized disc photons. The luminosity range at which a particular state emerges was found to scatter by a factor of up to 16 among the eight ULXs. By further assuming that the spectral state is uniquely determined by the Eddington ratio, the sample ULXs are inferred to exhibit a similar scatter in their masses. This gives a model-independent support to the interpretation of ULXs in terms of relatively massive black holes. None of the spectra showed noticeable local structures. Especially, no Fe K-shell absorption/emission lines were detected, with upper limits of 30-40 eV in equivalent width from the brightest three among the sample: NGC 1313 X-1, Holmberg IX X-1, and IC 342 X-1. These properties disfavour ordinary mass accretion from a massive companion star, and suggest direct Bondi-Hoyle accretion from dense parts of the interstellar medium.

    DOI: 10.1093/mnras/stz2139

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  25. Space gravitational-wave antennas DECIGO and B-DECIGO 査読有り

    Kawamura Seiji, Nakamura Takashi, Ando Masaki, Seto Naoki, Akutsu Tomotada, Funaki Ikkoh, Ioka Kunihito, Kanda Nobuyuki, Kawano Isao, Musha Mitsuru, Nakazawa Kazuhiro, Sato Shuichi, Takashima Takeshi, Tanaka Takahiro, Tsubono Kimio, Yokoyama Jun'ichi, Agatsuma Kazuhiro, Aoyanagi Koh-suke, Arai Koji, Araya Akito, Aritomi Naoki, Asada Hideki, Aso Yoichi, Chen Dan, Chiba Takeshi, Ebisuzaki Toshikazu, Eguchi Satoshi, Ejiri Yumiko, Enoki Motohiro, Eriguchi Yoshiharu, Fujimoto Masa-Katsu, Fujita Ryuichi, Fukushima Mitsuhiro, Futamase Toshifumi, Gondo Rina, Harada Tomohiro, Hashimoto Tatsuaki, Hayama Kazuhiro, Hikida Wataru, Himemoto Yoshiaki, Hirabayashi Hisashi, Hiramatsu Takashi, Hong Feng-Lei, Horisawa Hideyuki, Hosokawa Mizuhiko, Ichiki Kiyotomo, Ikegami Takeshi, Inoue Kaiki T., Ishihara Hideki, Ishikawa Takehiko, Ishizaki Hideharu, Ito Hiroyuki, Itoh Yousuke, Izumi Kiwamu, Kanemura Shinya, Kawashima Nobuki, Kawazoe Fumiko, Kishimoto Naoko, Kiuchi Kenta, Kobayashi Shiho, Kohri Kazunori, Koizumi Hiroyuki, Kojima Yasufumi, Kokeyama Keiko, Kokuyama Wataru, Kotake Kei, Kozai Yoshihide, Kunimori Hiroo, Kuninaka Hitoshi, Kuroda Kazuaki, Kuroyanagi Sachiko, Maeda Kei-ichi, Matsuhara Hideo, Matsumoto Nobuyuki, Michimura Yuta, Miyakawa Osamu, Miyamoto Umpei, Miyoki Shinji, Morimoto Mutsuko Y., Morisawa Toshiyuki, Moriwaki Shigenori, Mukohyama Shinji, Nagano Shigeo, Nakamura Kouji, Nakano Hiroyuki, Nakao Kenichi, Nakasuka Shinichi, Nakayama Yoshinori, Nishida Erina, Nishizawa Atsushi, Niwa Yoshito, Noumi Taiga, Obuchi Yoshiyuki, Ohishi Naoko, Ohkawa Masashi, Okada Kenshi, Okada Norio, Okutomi Koki, Oohara Kenichi, Sago Norichika, Saijo Motoyuki, Saito Ryo, Sakagami Masaaki, Sakai Shin-ichiro, Sakata Shihori, Sasaki Misao, Sato Takashi, Shibata Masaru, Shibata Kazunori, Shimo-oku Ayumi, Shinkai Hisaaki, Shoda Ayaka, Somiya Kentaro, Sotani Hajime, Suemasa Aru, Sugiyama Naoshi, Suwa Yudai, Suzuki Rieko, Tagoshi Hideyuki, Takahashi Fuminobu, Takahashi Kakeru, Takahashi Keitaro, Takahashi Ryutaro, Takahashi Ryuichi, Takahashi Hirotaka, Akiteru Takamori, Takano Tadashi, Tanaka Nobuyuki, Taniguchi Keisuke, Taruya Atsushi, Tashiro Hiroyuki, Torii Yasuo, Toyoshima Morio, Tsujikawa Shinji, Ueda Akitoshi, Ueda Ken-ichi, Ushiba Takafumi, Utashima Masayoshi, Wakabayashi Yaka, Yagi Kent, Yamamoto Kazuhiro, Yamazaki Toshitaka, Yoo Chul-Moon, Yoshida Shijun, Yoshino Taizoh

    INTERNATIONAL JOURNAL OF MODERN PHYSICS D   28 巻 ( 12 )   2019年9月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:International Journal of Modern Physics D  

    DECi-hertz Interferometer Gravitational-wave Observatory (DECIGO) is a future Japanese space gravitational-wave antenna. The most important objective of DECIGO, among various sciences to be aimed at, is to detect gravitational waves coming from the inflation of the universe. DECIGO consists of four clusters of spacecraft, and each cluster consists of three spacecraft with three Fabry-Perot Michelson interferometers. As a pathfinder mission of DECIGO, B-DECIGO will be launched, hopefully in the 2020s, to demonstrate technologies necessary for DECIGO as well as to lead to fruitful multimessenger astronomy. B-DECIGO is a small-scale or simpler version of DECIGO with the sensitivity slightly worse than that of DECIGO, yet good enough to provide frequent detection of gravitational waves.

    DOI: 10.1142/S0218271818450013

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  26. Downward Terrestrial Gamma-Ray Flash Observed in a Winter Thunderstorm 査読有り

    Wada Y., Enoto T., Nakazawa K., Furuta Y., Yuasa T., Nakamura Y., Morimoto T., Matsumoto T., Makishima K., Tsuchiya H.

    PHYSICAL REVIEW LETTERS   123 巻 ( 6 ) 頁: 061103   2019年8月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Physical Review Letters  

    During a winter thunderstorm on 24 November 2017, a strong burst of gamma rays with energies up to ∼10 MeV was detected coincident with a lightning discharge, by scintillation detectors installed at the Kashiwazaki-Kariwa Nuclear Power Station at sea level in Japan. The burst had a subsecond duration, which is suggestive of photoneutron production. The leading part of the burst was resolved into four intense gamma-ray bunches, each coincident with a low-frequency radio pulse. These bunches were separated by 0.7-1.5 ms, with a duration of 1 ms each. Thus, the present burst may be considered as a "downward" terrestrial gamma-ray flash (TGF), which is analogous to upgoing TGFs observed from space. Although the scintillation detectors were heavily saturated by these bunches, the total dose associated with them was successfully measured by ionization chambers, employed by nine monitoring posts surrounding the power plant. From this information and Monte Carlo simulations, the present downward TGF is suggested to have taken place at an altitude of 2500±500 m, involving 8-4+8×1018 avalanche electrons with energies above 1 MeV. This number is comparable to those in upgoing TGFs.

    DOI: 10.1103/PhysRevLett.123.061103

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    その他リンク: http://harvest.aps.org/v2/journals/articles/10.1103/PhysRevLett.123.061103/fulltext

  27. Estimation of the detected background by the future gamma ray transient mission CAMELOT

    Ripa Jakub, Galgoczi Gabor, Werner Norbert, Pal Andras, Ohno Masanori, Meszaros Laszlo, Mizuno Tsunefumi, Tarcai Norbert, Torigoe Kento, Uchida Nagomi, Fukazawa Yasushi, Takahashi Hiromitsu, Nakazawa Kazuhiro, Hirade Naoyoshi, Hirose Kengo, Hisadomi Syohei, Enoto Teruaki, Odaka Hirokazu, Ichinohe Yuto, Frei Zsolt, Kiss Laszlo

    ASTRONOMISCHE NACHRICHTEN   340 巻 ( 7 ) 頁: 666 - 673   2019年8月

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    記述言語:日本語   出版者・発行元:Astronomische Nachrichten  

    This study presents a background estimation for the CubeSats Applied for MEasuring and LOcalising Transients (CAMELOT), which is a proposed fleet of nanosatellites for the all-sky monitoring and timing-based localization of gamma ray transients with precise localization capability at low Earth orbits. CAMELOT will allow us to observe and precisely localize short gamma ray bursts (GRBs) associated with kilonovae, long GRBs associated with core-collapse massive stars, magnetar outbursts, terrestrial gamma ray flashes, and gamma ray counterparts to gravitational wave sources. A fleet of at least nine 3U CubeSats is proposed to be equipped with large and thin CsI(Tl) scintillators read out by multipixel photon counters (MPPC). A careful study of the radiation environment in space is necessary to optimize the detector casing, estimate the duty cycle due to the crossing of the South Atlantic Anomaly and polar regions, and minimize the effect of the radiation damage of MPPCs.

    DOI: 10.1002/asna.201913673

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  28. Spectral properties of gamma-ray bursts observed by the Suzaku wide-band all-sky monitor 査読有り

    Ohmori Norisuke, Yamaoka Kazutaka, Yamauchi Makoto, Urata Yuji, Ohno Masanori, Sugita Satoshi, Hurley Kevin, Tashiro Makoto S., Fukazawa Yasushi, Iwakiri Wataru, Katsukura Daisuke, Kokubun Motohide, Makishima Kazuo, Murakami Souta, Nakagawa Yujin E., Nakazawa Kazuhiro, Odaka Katsuya, Takahashi Kaito, Takahashi Tadayuki, Terada Yukikatsu

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   71 巻 ( 4 )   2019年8月

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    記述言語:日本語   出版者・発行元:Publications of the Astronomical Society of Japan  

    We have systematically studied the spectral properties of 302 localized gamma-ray bursts (GRBs) observed by the Suzaku wide-band all-sky monitor (WAM) from 2005 August to 2010 December. The energy spectra in the 100-5000 keV range integrated over the entire emission and the 1 s peak were fitted by three models: a single power law, a power law with an exponential cutoff (CPL), and the GRB Band function (GRB). Most of the burst spectra were well fitted by a single power law. The average photon index α was -2.11 and -1.73 for long and short bursts, respectively. For the CPL and GRB models, the low-energy and high-energy photon indices (α and β) for the entire emission spectra were consistent with previous measurements. The averages of the α and β were -0.90 and -2.65 for long-duration GRBs, while the average α was -0.55 and the β was not well constrained for short-duration GRBs. However, the average peak energy Epeak was 645 and 1286 keV for long- and short-duration GRBs respectively, which are higher than previous Fermi/GBM measurements (285 keV and 736 keV). The α and Epeak of the 1 s peak spectra were larger, i.e., the spectra were harder, than the total fluence spectra. Spectral simulations based on Fermi-GBM results suggest that the higher Epeaks measured by the Suzaku WAM could be due to detector selection bias, mainly caused by the limited energy range above 100 keV.

    DOI: 10.1093/pasj/psz054

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  29. Gamma-ray glow preceding downward terrestrial gamma-ray flash 査読有り

    Wada Yuuki, Enoto Teruaki, Nakamura Yoshitaka, Furuta Yoshihiro, Yuasa Takayuki, Nakazawa Kazuhiro, Morimoto Takeshi, Sato Mitsuteru, Matsumoto Takahiro, Yonetoku Daisuke, Sawano Tatsuya, Sakai Hideo, Kamogawa Masashi, Ushio Tomoo, Makishima Kazuo, Tsuchiya Harufumi

    COMMUNICATIONS PHYSICS   2 巻 ( 67 ) 頁: 1 - 9   2019年6月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Communications Physics  

    Two types of high-energy events have been detected from thunderstorms. One is “terrestrial gamma-ray flashes” (TGFs), sub-millisecond emissions coinciding with lightning discharges. The other is minute-lasting “gamma-ray glows”. Although both phenomena are thought to originate from relativistic runaway electron avalanches in strong electric fields, the connection between them is not well understood. Here we report unequivocal simultaneous detection of a gamma-ray glow termination and a downward TGF, observed from the ground. During a winter thunderstorm in Japan on 9 January 2018, our detectors caught a gamma-ray glow, which moved for ~100 s with ambient wind, and then abruptly ceased with a lightning discharge. Simultaneously, the detectors observed photonuclear reactions triggered by a downward TGF, whose radio pulse was located within ~1 km from where the glow ceased. It is suggested that the highly-electrified region producing the glow was related to the initiation of the downward TGF.

    DOI: 10.1038/s42005-019-0168-y

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  30. Event-selection technique for the multi-layer Si-CdTe Compton camera onboard Hitomi

    Ohno Masanori, Fukazawa Yasushi, Mizuno Tsunefumi, Takahashi Hiromitsu, Tanaka Yasuyuki, Katsuta Jun'ichiro, Kawano Takafumi, Habata Sho, Okada Chiho, Ohashi Norie, Teramae Takuto, Tanaka Koji, Takahashi Tadayuki, Kokubun Motohide, Watanabe Shin, Sato Goro, Sato Rie, Ohta Masayuki, Uchida Yusuke, Tamaru Ryota, Yoneda Hiroki, Nakazawa Kazuhiro, Murakami Hiroaki, Tajima Hiroyasu, Yamaoka Kazutaka, Kinoshita Masaomi, Hayashi Katsuhiro, Kitaguchi Takao, Odaka Hirokazu

    NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT   924 巻   頁: 327 - 331   2019年4月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment  

    The soft gamma-ray detector (SGD) onboard Hitomi, which has a unique design concept, based on the combination of a ”narrow-field multi-layer semi-conductor Compton camera” and an active shielding, realizes astronomical observations in the 60−600 keV energy band with a high sensitivity. Development of optimum event selection criteria is essential for deriving the best observational performance of the SGD, but it is challenging because many parameters such as the detected photon energy, the Compton-scattering angle, and distance of each hit, among others, are non-linearly correlated. In this study, we propose a new method for distinguishing the signal from the background in the multi-parameter space utilizing a machine-learning approach. Our preliminary result, which uses both on-ground experimental data with good photon statistics and flight data with real in-orbit background and signal information, suggests that this approach might a good guide for an optimal event selection by the Compton camera.

    DOI: 10.1016/j.nima.2018.09.114

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

    Torigoe Kento, Fukazawa Yasushi, Galgoczi Gabor, Mizuno Tsunefumi, Nakazawa Kazuhiro, Ohno Masanori, Pal Andras, Takahashi Hiromitsu, Tanaka Koji, Tarcai Norbert, Uchida Nagomi, Werner Norbert, Enoto Teruaki, Frei Zsolt, Ichinohe Yuto, Kiss Laszlo, Odaka Hirokazu, Ripa Jakub, Varhegyi Zsolt

    NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT   924 巻   頁: 316 - 320   2019年4月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment  

    We are designing a fleet of nanosatellites to perform accurate position determinations of short-duration gamma-ray bursts by measuring arrival time differences. To achieve sufficient photon statistics to measure the arrival times precisely under the severe limitations of size, mass and power consumption, we propose the use of large-area CsI(Tl) scintillators which provide a high light output and the use of a small-sized multipixel photon counters (MPPC), a kind of SiPM, that have low power consumption. We plan to use one of the latest-model MPPCs provided by Hamamatsu Photonics, namely, S13360-6050CS, which has an active area of 6×6 mm2. We have compared the performance of two scintillators of different sizes (150×75×5 mm3 and 100×75×5 mm3); the bigger one is the maximum size that can be mounted on a three-unit satellite, according to CubeSat standards. We have found that the light yield of the bigger scintillator is lower than that of the smaller one, but the difference is only approximately 13%, and each has an energy threshold of ∼10 keV at 25∘C. We have tested one- and two-MPPC readout and confirmed the same energy thresholds. The light yield for the two-MPPC readout is 1.4 times as high as that for the one-MPPC readout. We have also examined the position dependence of the light yield by using radiation from a 241Am (59.5 keV) source, and confirmed that uniformity was improved, and energy resolution got better by ∼7% for two-MPPC readout.

    DOI: 10.1016/j.nima.2018.08.039

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  32. A NuSTAR study of the 55 ks hard X-ray pulse-phase modulation in the magnetar 4U 0142+61

    Makishima Kazuo, Murakami Hiroaki, Enoto Teruaki, Nakazawa Kazuhiro

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   71 巻 ( 1 )   2019年1月

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    記述言語:日本語   出版者・発行元:Publications of the Astronomical Society of Japan  

    Archival NuSTAR data of the magnetar 4U 0142+61, acquired in 2014 March for a total time span of 258 ks, were analyzed. This is to reconfirm the 55 ks modulation in the hard X-ray pulse phases of this source, found with a Suzaku observation in 2009 (Makishima et al.,2014, Phys. Rev. Lett., 112, 171102). Indeed, the 10-70 keV X-ray pulsation, detected with NuSTAR at 8.68917 s, was found to be also phase-modulated (at >98% confidence) at the same ∼55 ks period, or half that value. Furthermore, a brief analysis of another Suzaku data set of 4U 0142+61, acquired in 2013, reconfirmed the same 55 ks phase modulation in the 15-40 keV pulses. Thus, the hard X-ray pulse-phase modulation was detected with Suzaku (in 2009 and 2013) and NuSTAR (in 2014) at a consistent period. However, the modulation amplitude varied significantly; A ∼ 0.7 s with Suzaku (in 2009), A ∼ 1.2 s with Suzaku (in 2013), and A ∼ 0.17 s with NuSTAR. In addition, the phase modulation properties detected with NuSTAR differed considerably between the first 1/3 and the latter 2/3 of the observation. In energies below 10 keV, the pulse-phase modulation was not detected with either Suzaku or NuSTAR. These results reinforce the view of Makishima et al. (2014, Phys. Rev. Lett., 112, 171102); the neutron star in 4U 0142+61 keeps free precession, under a slight axial deformation due probably to ultra-high toroidal magnetic fields of ∼10 16 G. The wobbling angle of precession should remain constant, but the pulse-phase modulation amplitude varies on time scales of months to years, presumably as asymmetry of the hard X-ray emission pattern around the star's axis changes.

    DOI: 10.1093/pasj/psy129

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  33. Gamma-ray observations at the coastal area of Japan Sea in winter seasons

    Tsuchiya H., Enoto T., Wada Y., Furuta Y., Nakazawa K., Yuasa T., Umemoto D., Makishima K.

    Proceedings of Science   358 巻   2019年

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    記述言語:日本語   出版者・発行元:Proceedings of Science  

    Since 2006, The Gamma Ray Observation of Winter Thunderclouds (GROWTH) collaboration has operated radiation measurement networks at the coastal area of Japan sea. The area is famous for its frequent occurrence of winter thunderstorms. We aims at elucidating how particles in lightning and thunderclouds are accelerated to relativistic energies. More than 10-years observations reveal that there are two types of radiation bursts associated with winter thunderstorms. One is a "long burst" or a "gamma-ray glow" lasting for a few tens of seconds to a few minutes. The other is a "short burst" in association with lightning. In order to expand the observational network, we have developed a small type of a radiation detector. In this paper, we focus on recent several findings obtained by the new detectors. One is a combination of a short burst and a long one, showing simultaneous detection of prompt gamma rays extending to ~10 MeV and the 511-keV annihilation ones. These gamma-ray signals demonstrate the occurrence of photonuclear reactions in lightning. Another is an event that a gamma-ray glow suddenly ceased just prior to lightning, suggesting a relation between lightning and the two types of radiation bursts. On the basis of these results, we discuss the production mechanism of gamma rays related to thunderstorms and the lightning initiation problem.

    Scopus

  34. Completeness of Cyclic Proofs for Symbolic Heaps with Inductive Definitions

    Tatsuta Makoto, Nakazawa Koji, Kimura Daisuke

    PROGRAMMING LANGUAGES AND SYSTEMS, APLAS 2019   11893 巻   頁: 367 - 387   2019年

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    出版者・発行元:Lecture Notes in Computer Science (including subseries Lecture Notes in Artificial Intelligence and Lecture Notes in Bioinformatics)  

    DOI: 10.1007/978-3-030-34175-6_19

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  35. Solar neutron and gamma-ray detector for a 3U Cubesat

    Yamaoka K., Tajima H., Miyata K., Inamori T., Sasai Y., Kawahara H., Park J.H., Nakazawa K., Masuda S., Matsushita K., Itoh K., Nobashi D., Takahashi H., Watanabe K.

    Proceedings of Science   358 巻   2019年

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    記述言語:日本語   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:Proceedings of Science  

    Solar neutron observations are very important on understanding of particle acceleration mechanism in the Sun. However, previous ground-based observations with large area telescope (~10 m2)at high latitude are not sensitive to solar neutrons due to attenuation in the earth atmosphere and roughly 10 detection since its discovery in 1980. From space, the SEDA-AP instrument with much smaller area (100 cm2) onboard the International Space Station (ISS) monitored solar neutrons including charged particles, and successfully detected more than 30 detection since its launch in 2009. Unfortunately the SEDA-AP operation was stopped on March 2018. To overcome situation for no mission dedicated for solar neutrons, we have designed and developed a solar neutron and gamma-ray detector for a 3U cubesat with a size of 30×10×10 cm. Actually we launched the 50-kg class ChubuSat-2 satellite for solar neutron observations on February 2016, and have now been adjusting it to a 3U cubesat application. The solar neutron and gamma-ray detector consists of multi-layered plastic scintillator bars, and GAGG(Ce) scintillator array, and both of them are read out with silicon photo-multipliers (Si PMs). More than 600 signals from Si PMs are processed by ASICs. In this paper, we will describe details of the detector and performance of its breadboard model (BBM).

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  36. Detection of polarized gamma-ray emission from the Crab nebula with the Hitomi Soft Gamma-ray Detector

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

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   70 巻 ( 6 )   2018年12月

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    記述言語:日本語   出版者・発行元:Publications of the Astronomical Society of Japan  

    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 data analysis of the SGD observation, SGD background estimation, and 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%±10.6%), and the polarization angle is 110°.7 + 13°.2/-13°.0 in the energy range of 60.160 keV (the errors correspond to the 1 σ 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 ± 0°.0.1.

    DOI: 10.1093/pasj/psy118

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  37. Termination of Electron Acceleration in Thundercloud by Intracloud/Intercloud Discharge 査読有り

    Wada Y., Bowers G. S., Enoto T., Kamogawa M., Nakamura Y., Morimoto T., Smith D. M., Furuta Y., Nakazawa K., Yuasa T., Matsuki A., Kubo M., Tamagawa T., Makishima K., Tsuchiya H.

    GEOPHYSICAL RESEARCH LETTERS   45 巻 ( 11 ) 頁: 5700 - 5707   2018年6月

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    掲載種別:研究論文(学術雑誌)   出版者・発行元:Geophysical Research Letters  

    An on-ground observation program for high energy atmospheric phenomena in<br />
    winter thunderstorms along Japan Sea has been performed via measurements of<br />
    gamma-ray radiation, atmospheric electric field and low-frequency radio band.<br />
    On February 11, 2017, the radiation detectors recorded gamma-ray emission<br />
    lasting for 75 sec. The gamma-ray spectrum extended up to 20 MeV and was<br />
    reproduced by a cutoff power-law model with a photon index of<br />
    $1.36^{+0.03}_{-0.04}$, being consistent with a Bremsstrahlung radiation from a<br />
    thundercloud (as known as a gamma-ray glow and a thunderstorm ground<br />
    enhancement). Then the gamma-ray glow was abruptly terminated with a nearby<br />
    lightning discharge. The low-frequency radio monitors, installed $\sim$50 km<br />
    away from the gamma-ray observation site recorded leader development of an<br />
    intra/inter-cloud discharge spreading over $\sim$60 km area with a $\sim$300 ms<br />
    duration. The timing of the gamma-ray termination coincided with the moment<br />
    when the leader development of the intra/inter-cloud discharge passed 0.7 km<br />
    horizontally away from the radiation monitors. The intra/inter-cloud discharge<br />
    started $\sim$15 km away from the gamma-ray observation site. Therefore, the<br />
    glow was terminated by the leader development, while it did not trigger the<br />
    lightning discharge in the present case.

    DOI: 10.1029/2018GL077784

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    arXiv

  38. ATCA 16 cm observation of CIZA J1358.9-4750: Implication of merger stage and constraint on non-thermal properties 査読有り

    Akahori Takuya, Kato Yuichi, Nakazawa Kazuhiro, Ozawa Takeaki, Gu Liyi, Takizawa Motokazu, Fujita Yutaka, Nakanishi Hiroyuki, Okabe Nobuhiro, Makishima Kazuo

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   70 巻 ( 3 )   2018年6月

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    記述言語:日本語   出版者・発行元:Publications of the Astronomical Society of Japan  

    We report the Australia Telescope Compact Array 16 cm observation of CIZA J1358.9-4750. Recent X-ray studies imply that this galaxy cluster is composed of merging, binary clusters. Using the EW367 configuration, we found no significant diffuse radio emission in and around the cluster. An upper limit of the total radio power at 1.4 GHz is ∼1.1 × 1022 W Hz-1 in 30 square arcminutes, which is a typical size for radio relics. It is known that an empirical relation holds between the total radio power and X-ray luminosity of the host cluster. The upper limit is about one order of magnitude lower than the power expected from the relation. Very young (∼70 Myr) shocks with low Mach numbers (∼1.3), which are often seen at an early stage of merger simulations, are suggested by the previous X-ray observation. The shocks may generate cosmic-ray electrons with a steep energy spectrum, which is consistent with non-detection of bright (>1023 W Hz-1) relic in this 16 cm band observation. Based on the assumption of energy equipartition, the upper limit gives a magnetic field strength of below 0.68f(Dlos/1 Mpc)-1(γmin/200)-1 μG, where f is the cosmic-ray total energy density over the cosmic-ray electron energy density, Dlos is the depth of the shock wave along the sightline, and min is the lower cutoff Lorentz factor of the cosmic-ray electron energy spectrum.

    DOI: 10.1093/pasj/psy042

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

    Aharonian Felix, Akamatsu Hiroki, Akimoto Fumie, Allen Steven W., Angelini Lorella, Audard Marc, Awaki Hisamitsu, Axelsson Magnus, Bamba Aya, Bautz Marshall W., Blandford Roger, Brenneman Laura W., Brown Gregory V, Bulbul Esra, Cackett Edward M., Chernyakova Maria, Chiao Meng P., Coppi Paolo S., Costantini Elisa, de Plaa Jelle, de Vries Cor P., den Herder Jan-Willem, Done Chris, Dotani Tadayasu, Ebisawa Ken, Eckart Megan E., Enoto Teruaki, Ezoe Yuichiro, Fabian Andrew C., Ferrigno Carlo, Foster Adam R., Fujimoto Ryuichi, Fukazawa Yasushi, Furuzawa Akihiro, Galeazzi Massimiliano, Gallo Luigi C., Gandhi Poshak, Giustini Margherita, Goldwurm Andrea, Gu Liyi, Guainazzi Matteo, Haba Yoshito, Hagino Kouichi, Hamaguchi Kenji, Harrus Ilana M., Hatsukade Isamu, Hayashi Katsuhiro, Hayashi Takayuki, Hayashida Kiyoshi, Hiraga Junko S., Hornschemeier Ann, Hoshino Akio, Hughes John P., Ichinohe Yuto, Iizuka Ryo, Inoue Hajime, Inoue Yoshiyuki, Ishida Manabu, Ishikawa Kumi, Ishisaki Yoshitaka, Iwai Masachika, Kaastra Jelle, Kallman Tim, Kamae Tsuneyoshi, Kataoka Jun, Katsuda Satoru, Kawai Nobuyuki, Kelley Richard L., Kilbourne Caroline A., Kitaguchi Takao, Kitamoto Shunji, Kitayama Tetsu, Kohmura Takayoshi, Kokubun Motohide, Koyama Katsuji, Koyama Shu, Kretschmar Peter, Krimm Hans A., Kubota Aya, Kunieda Hideyo, Laurent Philippe, Lee Shiu-Hang, Leutenegger Maurice A., Limousin Olivier, Loewenstein Michael, Long Knox S., Lumb David, Madejski Greg, Maeda Yoshitomo, Maier Daniel, Makishima Kazuo, Markevitch Maxim, Matsumoto Hironori, Matsushita Kyoko, McCammon Dan, McNamara Brian R., Mehdipour Missagh, Miller Eric D., Miller Jon M., Mineshige Shin, Mitsuda Kazuhisa, Mitsuishi Ikuyuki, Miyazawa Takuya, Mizuno Tsunefumi, Mori Hideyuki, Mori Koji, Mukai Koji, Murakami Hiroshi, Mushotzky Richard F., Nakagawa Takao, Nakajima Hiroshi, Nakamori Takeshi, Nakashima Shinya, Nakazawa Kazuhiro, Nobukawa Kumiko K., Nobukawa Masayoshi, Noda Hirofumi, Odaka Hirokazu, Ohashi Takaya, Ohno Masanori, Okajima Takashi, Ota Naomi, Ozaki Masanobu, Paerels Frits, Paltani Stephane, Petre Robert, Pinto Ciro, Porter Frederick S., Pottschmidt Katja, Reynolds Christopher S., Safi-Harb Samar, Saito Shinya, Sakai Kazuhiro, Sasaki Toru, Sato Goro, Sato Kosuke, Sato Rie, Sawada Makoto, Schartel Norbert, Serlemtsos Peter J., Seta Hiromi, Shidatsu Megumi, Simionescu Aurora, Smith Randall K., Soong Yang, Stawarz Lukasz, Sugawara Yasuharu, Sugita Satoshi, Szymkowiak Andrew, Tajima Hiroyasu, Takahashi Hiromitsu, Takahashi Tadayuki, Takeda Shinichiro, Takei Yoh, Tamagawa Toru, Tamura Takayuki, Tanaka Takaaki, Tanaka Yasuo, Tanaka Yasuyuki T., Tashiro Makoto S., Tawara Yuzuru, Terada Yukikatsu, Terashima Yuichi, Tombesi Francesco, Tomida Hiroshi, Tsuboi Yohko, Tsujimoto Masahiro, Tsunemi Hiroshi, Tsuru Takeshi Go, Uchida Hiroyuki, Uchiyama Hideki, Uchiyama Yasunobu, Ueda Shutaro, Uno Shinichiro, Ueda Yoshihiro, Urry C. Megan, Ursino Eugenio, Watanabe Shin, Werner Norbert, Wilkins Dan R., Williams Brian J., Yamada Shinya, Yamaguchi Hiroya, Yamaoka Kazutaka, Yamasaki Noriko Y., Yamauchi Makoto, Yamauchi Shigeo, Yaqoob Tahir, Yatsu Yoichi, Yonetoku Daisuke, Zhuravleva Irina, Zoghbi Abderahmen, Sato Toshiki, Nakaniwa Nozomu, Murakami Hiroaki, Guest Benson

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   70 巻 ( 3 )   2018年6月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Publications of the Astronomical Society of Japan  

    We present results from the Hitomi X-ray observation of a young composite-type supernova remnant (SNR) G21.5-0.9, whose emission is dominated by the pulsar wind nebula (PWN) contribution. The X-ray spectra in the 0.8-80 keV range obtained with the Soft X-ray Spectrometer (SXS), Soft X-ray Imager, and Hard X-ray Imager (HXI) show a significant break in the continuum as previously found with the NuSTAR observation. After taking into account all known emissions from the SNR other than the PWN itself, we find that the Hitomi spectra can be fitted with a broken power law with photon indices of 1 = 1.74 ± 0.02 and 2 = 2.14 ± 0.01 below and above the break at 7.1 ± 0.3 keV, which is significantly lower than the NuSTAR result (∼9.0 keV). The spectral break cannot be reproduced by time-dependent particle injection one-zone spectral energy distribution models, which strongly indicates that a more complex emission model is needed, as suggested by recent theoretical models. We also search for narrow emission or absorption lines with the SXS, and perform a timing analysis of PSR J1833-1034 with the HXI and the Soft Gamma-ray Detector. No significant pulsation is found from the pulsar. However, unexpectedly, narrow absorption line features are detected in the SXS data at 4.2345 keV and 9.296 keV with a significance of 3.65 s. While the origin of these features is not understood, their mere detection opens up a new field of research and was only possible with the high resolution, sensitivity, and ability to measure extended sources provided by an X-ray microcalorimeter.

    DOI: 10.1093/pasj/psy027

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  40. Multiwavelength study of X-ray luminous clusters in the Hyper Suprime-Cam Subaru Strategic Program S16A field (vol 70, S22, 2018) 査読有り

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

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   70 巻 ( 3 )   2018年6月

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    記述言語:日本語   出版者・発行元:Publications of the Astronomical Society of Japan  

    In the published version of this article, (Publications of the Astronomical Society of Japan, Volume 70, Issue SP1, 2018, S22, first published online 21 December 2017, doi: 10.1093/pasj/psx132), the following error appears: The caption for figure 3 appears under figure 4 and the caption for figure 4 appears under figure 3. The publisher apologises for the error.(Figure Persenetd).

    DOI: 10.1093/pasj/psy024

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  41. Modeling of proton-induced radioactivation background in hard X-ray telescopes: Geant4-based simulation and its demonstration by Hitomi's measurement in a low Earth orbit 査読有り

    Odaka Hirokazu, Asai Makoto, Hagino Kouichi, Koi Tatsumi, Madejski Greg, Mizuno Tsunefumi, Ohno Masanori, Saito Shinya, Sato Tamotsu, Wright Dennis H., Enoto Teruaki, Fukazawa Yasushi, Hayashi Katsuhiro, Kataoka Jun, Katsuta Junichiro, Kawaharada Madoka, Kobayashi Shogo B., Kokubun Motohide, Laurent Philippe, Lebrun Francois, Limousin Olivier, Maier Daniel, Makishima Kazuo, Mimura Taketo, Miyake Katsuma, Mori Kunishiro, Murakami Hiroaki, Nakamori Takeshi, Nakano Toshio, Nakazawa Kazuhiro, Noda Hirofumi, Ohta Masayuki, Ozaki Masanobu, Sato Goro, Sato Rie, Tajima Hiroyasu, Takahashi Hiromitsu, Takahashi Tadayuki, Takeda Shin'ichiro, Tanaka Takaaki, Tanaka Yasuyuki, Terada Yukikatsu, Uchiyama Hideki, Uchiyama Yasunobu, Watanabe Shin, Yamaoka Kazutaka, Yasuda Tetsuya, Yatsu Yoichi, Yuasa Takayuki, Zoglauer Andreas

    NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT   891 巻   頁: 92 - 105   2018年5月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment  

    Hard X-ray astronomical observatories in orbit suffer from a significant amount of background due to radioactivation induced by cosmic-ray protons and/or geomagnetically trapped protons. Within the framework of a full Monte Carlo simulation, we present modeling of in-orbit instrumental background which is dominated by radioactivation. To reduce the computation time required by straightforward simulations of delayed emissions from activated isotopes, we insert a semi-analytical calculation that converts production probabilities of radioactive isotopes by interaction of the primary protons into decay rates at measurement time of all secondary isotopes. Therefore, our simulation method is separated into three steps: (1) simulation of isotope production, (2) semi-analytical conversion to decay rates, and (3) simulation of decays of the isotopes at measurement time. This method is verified by a simple setup that has a CdTe semiconductor detector, and shows a 100-fold improvement in efficiency over the straightforward simulation. To demonstrate its experimental performance, the simulation framework was tested against data measured with a CdTe sensor in the Hard X-ray Imager onboard the Hitomi X-ray Astronomy Satellite, which was put into a low Earth orbit with an altitude of 570 km and an inclination of 31°, and thus experienced a large amount of irradiation from geomagnetically trapped protons during its passages through the South Atlantic Anomaly. The simulation is able to treat full histories of the proton irradiation and multiple measurement windows. The simulation results agree very well with the measured data, showing that the measured background is well described by the combination of proton-induced radioactivation of the CdTe detector itself and thick Bi4Ge3O12 scintillator shields, leakage of cosmic X-ray background and albedo gamma-ray radiation, and emissions from naturally contaminated isotopes in the detector system.

    DOI: 10.1016/j.nima.2018.02.071

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  42. In-orbit performance and calibration of the Hard X-ray Imager onboard Hitomi (ASTRO-H) 査読有り

    Kouichi Hagino, Kazuhiro Nakazawa, Goro Sato, Motohide Kokubun, Teruaki Enoto, Yasushi Fukazawa, Katsuhiro Hayashi, Jun Kataoka, Junichiro Katsuta, Shogo B. Kobayashi, Philippe Laurent, Francois Lebrun, Olivier Limousin, Daniel Maier, Kazuo Makishima, Taketo Mimura, Katsuma Miyake, Tsunefumi Mizuno, Kunishiro Mori, Hiroaki Murakami, Takeshi Nakamori, Toshio Nakano, Hirofumi Noda, Hirokazu Odaka, Masanori Ohno, Masayuki Ohta, Shinya Saito, Rie Sato, Hiroyasu Tajima, Hiromitsu Takahashi, Tadayuki Takahashi, Shin'ichiro Takeda, Takaaki Tanaka, Yukikatsu Terada, Hideki Uchiyama, Yasunobu Uchiyama, Shin Watanabe, Kazutaka Yamaoka, Yoichi Yatsu, Takayuki Yuasa

    Journal of Astronomical Telescopes, Instruments, and Systems   4 巻 ( 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)   出版者・発行元:SPIE  

    The Hard X-ray Imager (HXI) onboard Hitomi (ASTRO-H) is an imaging spectrometer covering hard x-ray energies of 5 to 80 keV. Combined with the Hard X-ray Telescope, it enables imaging spectroscopy with an angular resolution of 10.7 half-power diameter, in a field of view of 9' × 9'. The main imager is composed of four layers of Si detectors and one layer of CdTe detector, stacked to cover a wide energy band up to 80 keV, surrounded by an active shield made of Bi4Ge3O12 scintillator to reduce the background. The HXI started observations 12 days before the Hitomi loss and successfully obtained data from G21.5-0.9, Crab, and blank sky. Utilizing these data, we calibrate the detector response and study properties of in-orbit background. The observed Crab spectra agree well with a powerlaw model convolved with the detector response, within 5% accuracy. We find that albedo electrons in specified orbit strongly affect the background of the Si top layer and establish a screening method to reduce it. The background level over the full field of view after all the processing and screening is as low as the preflight requirement of 1 - 3 × 10-4 counts s-1 cm-2 keV-1.

    DOI: 10.1117/1.JATIS.4.2.021409

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  43. In-orbit performance and calibration of the Hard X-ray Imager onboard Hitomi (ASTRO-H) 査読有り

    Kouichi Hagino, Kazuhiro Nakazawa, Goro Sato, Motohide Kokubun, Teruaki Enoto, Yasushi Fukazawa, Katsuhiro Hayashi, Jun Kataoka, Junichiro Katsuta, Shogo B. Kobayashi, Philippe Laurent, Francois Lebrun, Olivier Limousin, Daniel Maier, Kazuo Makishima, Taketo Mimura, Katsuma Miyake, Tsunefumi Mizuno, Kunishiro Mori, Hiroaki Murakami, Takeshi Nakamori, Toshio Nakano, Hirofumi Noda, Hirokazu Odaka, Masanori Ohno, Masayuki Ohta, Shinya Saito, Rie Sato, Hiroyasu Tajima, Hiromitsu Takahashi, Tadayuki Takahashi, Shin'ichiro Takeda, Takaaki Tanaka, Yukikatsu Terada, Hideki Uchiyama, Yasunobu Uchiyama, Shin Watanabe, Kazutaka Yamaoka, Yoichi Yatsu, Takayuki Yuasa

    Journal of Astronomical Telescopes, Instruments, and Systems   4 巻 ( 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)   出版者・発行元:SPIE  

    The Hard X-ray Imager (HXI) onboard Hitomi (ASTRO-H) is an imaging spectrometer covering hard x-ray energies of 5 to 80 keV. Combined with the Hard X-ray Telescope, it enables imaging spectroscopy with an angular resolution of 10.7 half-power diameter, in a field of view of 9' × 9'. The main imager is composed of four layers of Si detectors and one layer of CdTe detector, stacked to cover a wide energy band up to 80 keV, surrounded by an active shield made of Bi4Ge3O12 scintillator to reduce the background. The HXI started observations 12 days before the Hitomi loss and successfully obtained data from G21.5-0.9, Crab, and blank sky. Utilizing these data, we calibrate the detector response and study properties of in-orbit background. The observed Crab spectra agree well with a powerlaw model convolved with the detector response, within 5% accuracy. We find that albedo electrons in specified orbit strongly affect the background of the Si top layer and establish a screening method to reduce it. The background level over the full field of view after all the processing and screening is as low as the preflight requirement of 1 - 3 × 10-4 counts s-1 cm-2 keV-1.

    DOI: 10.1117/1.JATIS.4.2.021409

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

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

    JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS   4 巻 ( 2 )   2018年4月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Journal of Astronomical Telescopes, Instruments, and Systems  

    Hitomi (ASTRO-H) was the sixth Japanese X-ray satellite that carried instruments with exquisite energy resolution of <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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  45. In-orbit performance and calibration of the Hard X-ray Imager onboard Hitomi (ASTRO-H)

    Hagino K.

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

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    出版者・発行元:Journal of Astronomical Telescopes, Instruments, and Systems  

    DOI: 10.1117/1.JATIS.4.2.021409

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  46. In-orbit performance and calibration of the Hard X-ray Imager onboard Hitomi (ASTRO-H)

    Hagino Kouichi, Nakazawa Kazuhiro, Sato Goro, Kokubun Motohide, Enoto Teruaki, Fukazawa Yasushi, Hayashi Katsuhiro, Kataoka Jun, Katsuta Junichiro, Kobayashi Shogo B., Laurent Philippe, Lebrun Francois, Limousin Olivier, Maier Daniel, Makishima Kazuo, Mimura Taketo, Miyake Katsuma, Mizuno Tsunefumi, Mori Kunishiro, Murakami Hiroaki, Nakamori Takeshi, Nakano Toshio, Noda Hirofumi, Odaka Hirokazu, Ohno Masanori, Ohta Masayuki, Saito Shinya, Sato Rie, Tajima Hiroyasu, Takahashi Hiromitsu, Takahashi Tadayuki, Takeda Shin'ichiro, Tanaka Takaaki, Terada Yukikatsu, Uchiyama Hideki, Uchiyama Yasunobu, Watanabe Shin, Yamaoka Kazutaka, Yatsu Yoichi, Yuasa Takayuki

    JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS   4 巻 ( 2 )   2018年4月

  47. Hitomi (ASTRO-H) X-ray Astronomy Satellite 査読有り

    Takahashi Tadayuki, Kokubun Motohide, Mitsuda Kazuhisa, Kelley Richard L., Ohashi Takaya, Aharonian Felix, Akamatsu Hiroki, Akimoto Fumie, Allen Steven W., Anabuki Naohisa, Angelini Lorella, Arnaud Keith, Asai Makoto, Audard Marc, Awaki Hisamitsu, Axelsson Magnus, Azzarello Philipp, Baluta Chris, Bamba Aya, Bando Nobutaka, Bautz Marshall W., Bialas Thomas, Blandford Roger, Boyce Kevin, Brenneman Laura W., Brown Gregory V., Bulbul Esra, Cackett Edward M., Canavan Edgar, Chernyakova Maria, Chiao Meng P., Coppi Paolo S., Costantini Elisa, Dell Steve O', DiPirro Michael, Done Chris, Dotani Tadayasu, Doty John, Ebisawa Ken, Eckart Megan E., Enoto Teruaki, Ezoe Yuichiro, Fabian Andrew C., Ferrigno Carlo, Foster Adam R., Fujimoto Ryuichi, Fukazawa Yasushi, Funk Stefan, Furuzawa Akihiro, Galeazzi Massimiliano, Gallo Luigi C., Gandhi Poshak, Gilmore Kirk, Giustini Margherita, Goldwurm Andrea, Gu Liyi, Guainazzi Matteo, Haas Daniel, Haba Yoshito, Hagino Kouichi, Hamaguchi Kenji, Harrus Ilana M., Hatsukade Isamu, Hayashi Takayuki, Hayashi Katsuhiro, Hayashida Kiyoshi, den Herder Jan-Willem, Hiraga Junko S., Hirose Kazuyuki, Hornschemeier Ann, Hoshino Akio, Hughes John P., Ichinohe Yuto, Iizuka Ryo, Inoue Hajime, Inoue Yoshiyuki, Ishibashi Kazunori, Ishida Manabu, Ishikawa Kumi, Ishimura Kosei, Ishisaki Yoshitaka, Itoh Masayuki, Iwai Masachika, Iwata Naoko, Iyomoto Naoko, Jewell Chris, Kaastra Jelle, Kallman Tim, Kamae Tsuneyoshi, Kara Erin, Kataoka Jun, Katsuda Satoru, Katsuta Junichiro, Kawaharada Madoka, Kawai Nobuyuki, Kawano Taro, Kawasaki Shigeo, Khangulyan Dmitry, Kilbourne Caroline A., Kimball Mark, King Ashley, Kitaguchi Takao, Kitamoto Shunji, Kitayama Tetsu, Kohmura Takayoshi, Konami Saori, Kosaka Tatsuro, Koujelev Alex, Koyama Katsuji, Koyama Shu, Kretschmar Peter, Krimm Hans A., Kubota Aya, Kunieda Hideyo, Laurent Philippe, Lee Shiu-Hang, Leutenegger Maurice A., Limousin Olivier, Loewenstein Michael, Long Knox S., Lumb David, Madejski Greg, Maeda Yoshitomo, Maier Daniel, Makishima Kazuo, Markevitch Maxim, Masters Candace, Matsumoto Hironori, Matsushita Kyoko, McCammon Dan, Mcguinness Daniel, McNamar Brian R., Mehdipour Missagh, Miko Joseph, Miller Eric D., Miller Jon M., Mineshige Shin, Minesugi Kenji, Mitsuishi Ikuyuki, Miyazawa Takuya, Mizuno Tsunefumi, Mori Hideyuki, Mori Koji, Moroso Franco, Moseley Harvey, Muench Theodore, Mukai Koji, Murakami Hiroshi, Murakami Toshio, Mushotzky Richard F., Nagano Housei, Nagino Ryo, Nakagawa Takao, Nakajima Hiroshi, Nakamori Takeshi, Nakano Toshio, Nakashima Shinya, Nakazawa Kazuhiro, Namba Yoshiharu, Natsukari Chikara, Nishioka Yusuke, Nobukawa Kumiko K., Nobukawa Masayoshi, Noda Hirofumi, Nomachi Masaharu, Odaka Hirokazu, Ogawa Hiroyuki, Ogawa Mina, Ogi Keiji, Ohno Masanori, Ohta Masayuki, Okajima Takashi, Okamoto Atsushi, Okazaki Tsuyoshi, Ota Naomi, Ozaki Masanobu, Paerels Frits, Paltani Stephane, Parmar Arvind, Petre Robert, Pinto Ciro, de Plaa Jelle, Pohl Martin, Pontius James, Porter Frederick S., Pottschmidt Katja, Ramsey Brian, Reynolds Christopher, Russell Helen, Safi-Harb Samar, Saito Shinya, Sakai Kazuhiro, Sakai Shin-ichiro, Sameshima Hiroaki, Sasaki Toru, Sato Goro, Sato Kosuke, Sato Rie, Sato Yoichi, Sawada Makoto, Schartel Norbert, Serlemitsos Peter J., Seta Hiromi, Shibano Yasuko, Shida Maki, Shidatsu Megumi, Shimada Takanobu, Shinozaki Keisuke, Shirron Peter, Simionescu Aurora, Simmons Cynthia, Smith Randall K., Sneiderman Gary, Soong Yang, Stawarz Lukasz, Sugawara Yasuharu, Sugita Satoshi, Sugita Hiroyuki, Szymkowiak Andrew, Tajima Hiroyasu, Takahashi Hiromitsu, Takeda Shin'ichiro, Takei Yoh, Tamagawa Toru, Tamura Takayuki, Tamura Keisuke, Tanaka Takaaki, Tanaka Yasuo, Tanaka Yasuyuki T., Tashiro Makoto S., Tawara Yuzuru, Terada Yukikatsu, Terashima Yuichi, Tombesi Francesco, Tomida Hiroshi, Tsuboi Yohko, Tsujimoto Masahiro, Tsunemi Hiroshi, Tsuru Takeshi Go, Uchida Hiroyuki, Uchiyama Hideki, Uchiyama Yasunobu, Ueda Shutaro, Ueda Yoshihiro, Ueno Shiro, Uno Shin'ichiro, Urry C. Megan, Ursino Eugenio, de Vries Cor P., Wada Atsushi, Watanabe Shin, Watanabe Tomomi, Werner Norbert, Wik Daniel R., Wilkins Dan R., Williams Brian J., Yamada Shinya, Yamada Takahiro, Yamaguchi Hiroya, Yamaoka Kazutaka, Yamasaki Noriko Y., Yamauchi Makoto, Yamauchi Shigeo, Yaqoob Tahir, Yatsu Yoichi, Yonetoku Daisuke, Yoshida Atsumasa, Yuasa Takayuki, Zhuravleva Irina, Zoghbi Abderahmen

    JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS   4 巻 ( 2 )   2018年4月

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    記述言語:日本語   出版者・発行元:Journal of Astronomical Telescopes, Instruments, and Systems  

    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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  48. Hard x-ray imager onboard Hitomi (ASTRO-H)

    Nakazawa Kazuhiro, Sato Goro, Kokubun Motohide, Enoto Teruaki, Fukazawa Yasushi, Hagino Kouichi, Hayashi Katsuhiro, Kataoka Jun, Katsuta Junichiro, Kobayashi Shogo B., Laurent Philippe, Lebrun Francois, Limousin Olivier, Maier Daniel, Makishima Kazuo, Mizuno Tsunefumi, Mori Kunishiro, Nakamori Takeshi, Nakano Toshio, Noda Hirofumi, Odaka Hirokazu, Ohno Masanori, Ohta Masayuki, Saito Shinya, Sato Rie, Tajima Hiroyasu, Takahashi Hiromitsu, Takahashi Tadayuki, Takeda Shin'ichiro, Tanaka Takaaki, Terada Yukikatsu, Uchiyama Hideki, Uchiyama Yasunobu, Watanabe Shin, Yamaoka Kazutaka, Yatsu Yoichi, Yuasa Takayuki

    JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS   4 巻 ( 2 )   2018年4月

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    記述言語:日本語   出版者・発行元:Journal of Astronomical Telescopes, Instruments, and Systems  

    The hard x-ray imaging spectroscopy system of "Hitomi" x-ray observatory is composed of two sets of hard x-ray imagers (HXI) coupled with hard x-ray telescopes (HXT). With a 12-m focal length, the system provides fine (10:7 half-power diameter) imaging spectroscopy covering about 5 to 80 keV. The HXI sensor consists of a camera, which is composed of four layers of Si and one layer of CdTe semiconductor imagers, and an active shield composed of nine Bi4Ge3O12 scintillators to provide low background. The two HXIs started observation on March 8 and 14, 2016 and were operational until 26 March. Using a Crab observation, 5 to 80 keV energy coverage and good detection efficiency were confirmed. The detector background level of 1 to 3 × 10-4 counts s?1 keV?1 cm?2 (in detector geometrical area) at 5 to 80 keV was achieved, by cutting the high-background time-intervals, adopting sophisticated energy-dependent imager layer selection, and baffling of the cosmic x-ray background and active-shielding. This level is among the lowest of detectors working in this energy band. By comparing the effective area and the background, it was shown that the HXI had a sensitivity that is same to that of NuSTAR for point sources and 3 to 4 times better for largely extended diffuse sources.

    DOI: 10.1117/1.JATIS.4.2.021410

    Web of Science

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  49. The Hitomi X-Ray Observatory, Part 2 査読有り

    Kelley Richard L, Nakazawa Kazuhiro

    JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS   4 巻 ( 2 )   2018年4月

  50. Atmospheric gas dynamics in the Perseus cluster observed with Hitomi

    Aharonia F., Aharonian F., Akamatsu H., Akimoto F., Allen S.W., Angelini L., Audard M., Awaki H., Axelsson M., Bamba A., Bautz M.W., Blandford R., Brenneman L.W., Brown G.V., Bulbul E., Cackett E.M., Canning R.E.A., Chernyakova M., Chiao M.P., Coppi P.S., Costantini E., De Plaa J., De Vries C.P., Den Herder J.W., Done C., Dotani T., Ebisawa K., Eckart M.E., Enoto T., Ezoe Y., Fabian A.C., Ferrigno C., Foster A.R., Fujimoto R., Fukazawa Y., Furuzawa A., Galeazzi M., Gallo L.C., Gandhi P., Giustini M., Goldwurm A., Gu L., Guainazzi M., Haba Y., Hagino K., Hamaguchi K., Harrus I.M., Hatsukade I., Hayashi K., Hayashi T., Hayashi T., Hayashida K., Hiraga J.S., Hornschemeier A., Hoshino A., Hughes J.P., Ichinohe Y., Iizuka R., Inoue H., Inoue S., Inoue Y., Ishida M., Ishikawa K., Ishisaki Y., Iwai M., Kaastra J., Kallman T., Kamae T., Kataoka J., Katsuda S., Kawai N., Kelley R.L., Kilbourne C.A., Kitaguchi T., Kitamoto S., Kitayama T., Kohmura T., Kokubun M., Koyama K., Koyama S., Kretschmar P., Krimm H.A., Kubota A., Kunieda H., Laurent P., Lee S.H., Leutenegger M.A., Limousin O., Loewenstein M., Long K.S., Lumb D., Madejski G., Maeda Y., Maier D., Makishima K., Markevitch M., Matsumoto H., Matsushita K., Mccammon D., Mcnamara B.R.

    Publications of the Astronomical Society of Japan   70 巻 ( 2 )   2018年3月

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    記述言語:日本語   出版者・発行元:Publications of the Astronomical Society of Japan  

    Extending the earlier measurements reported in Hitomi collaboration (2016, Nature, 535, 117), we examine the atmospheric gas motions within the central 100kpc of the Perseus cluster using observations obtained with the Hitomi satellite. After correcting for the point spread function of the telescope and using optically thin emission lines, we find that the line-of-sight velocity dispersion of the hot gas is remarkably low and mostly uniform. The velocity dispersion reaches a maxima of approximately 200 km s-1 toward the central active galactic nucleus (AGN) and toward the AGN inflated northwestern "ghost" bubble. Elsewhere within the observed region, the velocity dispersion appears constant around 100 km s-1. We also detect a velocity gradient with a 100 km s-1 amplitude across the cluster core, consistent with large-scale sloshing of the core gas. If the observed gas motions are isotropic, the kinetic pressure support is less than 10% of the thermal pressure support in the cluster core. The well-resolved, optically thin emission lines have Gaussian shapes, indicating that the turbulent driving scale is likely below 100 kpc, which is consistent with the size of the AGN jet inflated bubbles. We also report the first measurement of the ion temperature in the intracluster medium, which we find to be consistent with the electron temperature. In addition, we present a new measurement of the redshift of the brightest cluster galaxy NGC 1275.

    Scopus

  51. Hitomi X-ray studies of giant radio pulses from the Crab pulsar

    Aharonian F.

    Publications of the Astronomical Society of Japan   70 巻 ( 2 )   2018年3月

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    出版者・発行元:Publications of the Astronomical Society of Japan  

    Scopus

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

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

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   70 巻 ( 2 )   2018年3月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)  

    DOI: 10.1093/pasj/psx138

    Web of Science

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

    Aharonian Felix, Akamatsu Hiroki, Akimoto Fumie, Allen Steven W., Angelini Lorella, Audard Marc, Awaki Hisamitsu, Axelsson Magnus, Bamba Aya, Bautz Marshall W., Blandford Roger, Brenneman Laura W., Brown Gregory V, Bulbul Esra, Cackett Edward M., Chernyakova Maria, Chiao Meng P., Coppi Paolo S., Costantini Elisa, de Plaa Jelle, de Vries Cor P., den Herder Jan-Willem, Done Chris, Dotani Tadayasu, Ebisawa Ken, Eckart Megan E., Enoto Teruaki, Ezoe Yuichiro, Fabian Andrew C., Ferrigno Carlo, Foster Adam R., Fujimoto Ryuichi, Fukazawa Yasushi, Furukawa Maki, Furuzawa Akihiro, Galeazzi Massimiliano, Gallo Luigi C., Gandhi Poshak, Giustini Margherita, Goldwurm Andrea, Gu Liyi, Guainazzi Matteo, Haba Yoshito, Hagino Kouichi, Hamaguchi Kenji, Harrus Ilana M., Hatsukade Isamu, Hayashi Katsuhiro, Hayashi Takayuki, Hayashida Kiyoshi, Hiraga Junko S., Hornschemeier Ann, Hoshino Akio, Hughes John P., Ichinohe Yuto, Iizuka Ryo, Inoue Hajime, Inoue Yoshiyuki, Ishida Manabu, Ishikawa Kumi, Ishisaki Yoshitaka, Iwai Masachika, Kaastra Jelle, Kallman Tim, Kamae Tsuneyoshi, Kataoka Jun, Katsuda Satoru, Kawai Nobuyuki, Kelley Richard L., Kilbourne Caroline A., Kitaguchi Takao, Kitamoto Shunji, Kitayama Tetsu, Kohmura Takayoshi, Kokubun Motohide, Koyama Katsuji, Koyama Shu, Kretschmar Peter, Krimm Hans A., Kubota Aya, Kunieda Hideyo, Laurent Philippe, Lee Shiu-Hang, Leutenegger Maurice A., Limousin Olivier O., Loewenstein Michael, Long Knox S., Lumb David, Madejski Greg, Maeda Yoshitomo, Maier Daniel, Makishima Kazuo, Markevitch Maxim, Matsumoto Hironori, Matsushita Kyoko, McCammon Dan, McNamara Brian R., Mehdipour Missagh, Miller Eric D., Miller Jon M., Mineshige Shin, Mitsuda Kazuhisa, Mitsuishi Ikuyuki, Miyazawa Takuya, Mizuno Tsunefumi, Mori Hideyuki, Mori Koji, Mukai Koji, Murakami Hiroshi, Mushotzky Richard F., Nakagawa Takao, Nakajima Hiroshi, Nakamori Takeshi, Nakashima Shinya, Nakazawa Kazuhiro, Norukawa Kumiko K., Nobukawa Masayoshi, Noda Hirofumi, Odaka Hirokazu, Ogorzalek Anna, Ohashi Takaya, Ohno Masanori, Okajima Takashi, Ota Naomi, Ozaki Masanobu, Paerels Frits, Paltani Stephane, Petre Robert, Pinto Ciro, Porter Frederick S., Pottschmidt Katja, Reynolds Christopher S., Safi-Harb Samar, Saito Shinya, Sakai Kazuhiro, Sasaki Toru, Sato Goro, Sato Kosuke, Sato Rie, Sawada Makoto, Schartel Norbert, Serlemitsos Peter J., Seta Hiromi, Shidatsu Megumi, Simionescu Aurora, Smith Randall K., Soong Yang, Stawarz Lukasz, Sugawara Yasuharu, Sugita Satoshi, Szymkowiak Andrew, Tajima Hiroyasu, Takahashi Hiromitsu, Takahashi Tadayuki, Takeda Shinichiro, Takei Yoh, Tamagawa Toru, Tamura Takayuki, Tanaka Takaaki, Tanaka Yasuo, Tanaka Yasuyuki T., Tashiro Makoto S., Tawara Yuzuru, Terada Yukikatsu, Terashima Yuichi, Tombesi Francesco, Tomida Hiroshi, Tsuboi Yohko, Tsujimoto Masahiro, Tsunemi Hiroshi, Tsuru Takeshi Go, Uchida Hiroyuki, Uchiyama Hideki, Uchiyama Yasunobu, Ueda Shutaro, Ueda Yoshihiro, Uno Shinichiro, Urry C. Megan, Ursino Eugenio, Watanabe Shin, Werner Norbert, Wilkins Dan R., Williams Brian J., Yamada Shinya, Yamaguchi Hiroya, Yamaoka Kazutaka, Yamasaki Noriko Y., Yamauchi Makoto, Yamauchi Shigeo, Yaqoob Tahir, Yatsu Yoichi, Yonetoku Daisuke, Zhuravleva Irina, Zoghbi Abderahmen

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   70 巻 ( 2 )   2018年3月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Publications of the Astronomical Society of Japan  

    Thanks to its high spectral resolution (∼5 eV at 6 keV), the Soft X-ray Spectrometer (SXS) on board Hitomi enables us to measure the detailed structure of spatially resolved emission lines from highly ionized ions in galaxy clusters for the first time. In this series of papers, using the SXS we have measured the velocities of gas motions, metallicities and the multi-temperature structure of the gas in the core of the Perseus Cluster. Here, we show that when inferring physical properties from line emissivities in systems like Perseus, the resonant scattering effect should be taken into account. In the Hitomi waveband, resonant scattering mostly affects the Fe XXV Heα line (w)-the strongest line in the spectrum. The flux measured by Hitomi in this line is suppressed by a factor of ∼1.3 in the inner ∼30 kpc, compared to predictions for an optically thin plasma; the suppression decreases with the distance from the center. The w line also appears slightly broader than other lines from the same ion. The observed distortions of the w line flux, shape, and distance dependence are all consistent with the expected effect of the resonant scattering in the Perseus core. By measuring the ratio of fluxes in optically thick (w) and thin (Fe XXV forbidden, Heβ, Lyα) lines, and comparing these ratios with predictions from Monte Carlo radiative transfer simulations, the velocities of gas motions have been obtained. The results are consistent with the direct measurements of gas velocities from line broadening described elsewhere in this series, although the systematic and statistical uncertainties remain significant. Further improvements in the predictions of line emissivities in plasma models, and deeper observations with future X-ray missions offering similar or better capabilities to the Hitomi SXS, will enable resonant scattering measurements to provide powerful constraints on the amplitude and anisotropy of cluster gas motions.

    DOI: 10.1093/pasj/psx127

    Web of Science

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

    Aharonian Felix, Akamatsu Hiroki, Akimoto Fumie, Allen Steven W., Angelini Lorella, Audard Marc, Awaki Hisamitsu, Axelsson Magnus, Bamba Aya, Bautz Marshall W., Blandford Roger, Brenneman Laura W., Brown Gregory V, Bulbul Esra, Cackett Edward M., Chernyakova Maria, Chiao Meng P., Coppi Paolo S., Costantini Elisa, De Plaa Jelle, De Vries Cor P., Den Herder Jan-Willem, Done Chris, Dotani Tadayasu, Ebisawa Ken, Eckart Megan E., Enoto Teruaki, Ezoe Yuichiro, Fabian Andrew C., Ferrigno Carlo, Foster Adam R., Fujimoto Ryuichi, Fukazawa Yasushi, Furuzawa Akihiro, Galeazzi Massimiliano, Gallo Luigi C., Gandhi Poshak, Giustini Margherita, Goldwurm Andrea, Gu Liyi, Guainazzi Matteo, Haba Yoshito, Hagino Kouichi, Hamaguchi Kenji, Harrus Ilana M., Hatsukade Isamu, Hayashi Katsuhiro, Hayashi Takayuki, Hayashida Kiyoshi, Hiraga Junko S., Hornschemeier Ann, Hoshino Akio, Hughes John P., Ichinohe Yuto, Iizuka Ryo, Inoue Hajime, Inoue Yoshiyuki, Ishida Manabu, Ishikawa Kumi, Ishisaki Yoshitaka, Iwai Masachika, Kaastra Jelle, Kallman Tim, Kamae Tsuneyoshi, Kataoka Jun, Katsuda Satoru, Kawai Nobuyuki, Kelley Richard L., Kilbourne Caroline A., Kitaguchi Takao, Kitamoto Shunji, Kitayama Tetsu, Kohmura Takayoshi, Kokubun Motohide, Koyama Katsuji, Koyama Shu, Kretschmar Peter, Krimm Hans A., Kubota Aya, Kunieda Hideyo, Laurent Philippe, Lee Shiu-Hang, Leutenegger Maurice A., Limousin Olivier O., Loewenstein Michael, Long Knox S., Lumb David, Madejski Greg, Maeda Yoshitomo, Maier Daniel, Makishima Kazuo, Markevitch Maxim, Matsumoto Hironori, Matsushita Kyoko, McCammon Dan, McNamara Brian R., Mehdipour Missagh, Miller Eric D., Miller Jon M., Mineshige Shin, Mitsuda Kazuhisa, Mitsuishi Ikuyuki, Miyazawa Takuya, Mizuno Tsunefumi, Mori Hideyuki, Mori Koji, Mukai Koji, Murakami Hiroshi, Mushotzky Richard F., Nakagawa Takao, Nakajima Hiroshi, Nakamori Takeshi, Nakashima Shinya, Nakazawa Kazuhiro, Nobukawa Kumiko K., Nobukawa Masayoshi, Noda Hirofumi, Odaka Hirokazu, Ohashi Takaya, Ohno Masanori, Okajima Takashi, Oshimizu Kenya, Ota Naomi, Ozaki Masanobu, Paerels Frits, Paltani Stephane, Petre Robert, Pinto Ciro, Porter Frederick S., Pottschmidt Katja, Reynolds Christopher S., Safi-Harb Samar, Saito Shinya, Sakai Kazuhiro, Sasaki Toru, Sato Goro, Sato Kosuke, Sato Rie, Sawada Makoto, Schartel Norbert, Serlemtsos Peter J., Seta Hiromi, Shidatsu Megumi, Simionescu Aurora, Smith Randall K., Soong Yang, Stawarz Lukasz, Sugawara Yasuharu, Sugita Satoshi, Szymkowiak Andrew, Tajima Hiroyasu, Takahashi Hiromitsu, Takahashi Tadayuki, Takeda Shinichiro, Takei Yoh, Tamagawa Toru, Tamura Takayuki, Tanaka Takaaki, Tanaka Yasuo, Tanaka Yasuyuki T., Tashiro Makoto S., Tawara Yuzuru, Terada Yukikatsu, Terashima Yuichi, Tombesi Francesco, Tomida Hiroshi, Tsuboi Yohko, Tsujimoto Masahiro, Tsunemi Hiroshi, Tsuru Takeshi Go, Uchida Hiroyuki, Uchiyama Hideki, Uchiyama Yasunobu, Ueda Shutaro, Ueda Yoshihiro, Uno Shinichiro, Urry C. Megan, Ursino Eugenio, Watanabe Shin, Werner Norbert, Wilkins Dan R., Williams Brian J., Yamada Shinya, Yamaguchi Hiroya, Yamaoka Kazutaka, Yamasaki Noriko Y., Yamauchi Makoto, Yamauchi Shigeo, Yaqoob Tahir, Yatsu Yoichi, Yonetoku Daisuke, Zhuravleva Irina, Zoghbi Abderahmen, Terasawa Toshio, Sekido Mamoru, Takefuji Kazuhiro, Kawai Eiji, Misawa Hiroaki, Tsuchiya Fuminori, Yamazaki Ryo, Kobayashi Eiji, Kisaka Shota, Aoki Takahiro

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   70 巻 ( 2 )   2018年3月

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    掲載種別:研究論文(学術雑誌)  

    DOI: 10.1093/pasj/psx083

    Web of Science

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    PubMed

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

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

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   70 巻 ( 2 )   2018年3月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Publications of the Astronomical Society of Japan  

    We present Hitomi observations of N 132 D, a young, X-ray bright, O-rich core-collapse supernova remnant in the Large Magellanic Cloud (LMC). Despite a very short observation of only 3.7 ks, the Soft X-ray Spectrometer (SXS) easily detects the line complexes of highly ionized S K and Fe K with 16-17 counts in each. The Fe feature is measured for the first time at high spectral resolution. Based on the plausible assumption that the Fe K emission is dominated by He-like ions, we find that the material responsible for this Fe emission is highly redshifted at ∼ 800 km s−1 compared to the local LMC interstellar medium (ISM), with a 90% credible interval of 50-1500 km s−1 if a weakly informative prior is placed on possible line broadening. This indicates (1) that the Fe emission arises from the supernova ejecta, and (2) that these ejecta are highly asymmetric, since no blueshifted component is found. The S K velocity is consistent with the local LMC ISM, and is likely from swept-up ISM material. These results are consistent with spatial mapping that shows the He-like Fe concentrated in the interior of the remnant and the S tracing the outer shell. The results also show that even with a very small number of counts, direct velocity measurements from Doppler-shifted lines detected in extended objects like supernova remnants are now possible. Thanks to the very low SXS background of ∼ 1 event per spectral resolution element per 100 ks, such results are obtainable during short pointed or slew observations with similar instruments. This highlights the power of high-spectral-resolution imaging observations, and demonstrates the new window that has been opened with Hitomi and will be greatly widened with future missions such as the X-ray Astronomy Recovery Mission (XARM) and Athena.

    DOI: 10.1093/pasj/psx151

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

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

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   70 巻 ( 2 )   2018年3月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Publications of the Astronomical Society of Japan  

    The origin of the narrow Fe-Kα fluorescence line at 6.4 keV from active galactic nuclei has long been under debate; some of the possible sites are the outer accretion disk, the broad line region, a molecular torus, or interstellar/intracluster media. In 2016 February-March, we performed the first X-ray microcalorimeter spectroscopy with the Soft X-ray Spectrometer (SXS) on board the Hitomi satellite of the Fanaroff-Riley type I radio galaxy NGC 1275 at the center of the Perseus cluster of galaxies. With the high-energy resolution of ∼5 eV at 6 keV achieved by Hitomi/SXS, we detected the Fe-Kα line with ∼5.4 σ significance. The velocity width is constrained to be 500-1600 km s−1 (FWHM for Gaussian models) at 90% confidence. The SXS also constrains the continuum level from the NGC 1275 nucleus up to ∼20 keV, giving an equivalent width of ∼20 eV for the 6.4 keV line. Because the velocity width is narrower than that of the broad Hα line of ∼2750 km s−1, we can exclude a large contribution to the line flux from the accretion disk and the broad line region. Furthermore, we performed pixel map analyses on the Hitomi/SXS data and image analyses on the Chandra archival data, and revealed that the Fe-Kα line comes from a region within ∼1.6 kpc of the NGC 1275 core, where an active galactic nucleus emission dominates, rather than that from intracluster media. Therefore, we suggest that the source of the Fe-Kα line from NGC 1275 is likely a low-covering-fraction molecular torus or a rotating molecular disk which probably extends from a parsec to hundreds of parsecs scale in the active galactic nucleus system.

    DOI: 10.1093/pasj/psx147

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  57. Glimpse of the highly obscured HMXB IGR J16318-4848 with Hitomi 査読有り

    Aharonian Felix, Akamatsu Hiroki, Akimoto Fumie, Allen Steven W., Angelini Lorella, Audard Marc, Awaki Hisamitsu, Axelsson Magnus, Bamba Aya, Bautz Marshall W., Blandford Roger, Brenneman Laura W., Brown Gregory V, Bulbul Esra, Cackett Edward M., Chernyakova Maria, Chiao Meng P., Coppi Paolo S., Costantini Elisa, de Plaa Jelle, de Vries Cor P., den Herder Jan-Willem, Done Chris, Dotani Tadayasu, Ebisawa Ken, Eckart Megan E., Enoto Teruaki, Ezoe Yuichiro, Fabian Andrew C., Ferrigno Carlo, Foster Adam R., Fujimoto Ryuichi, Fukazawa Yasushi, Furuzawa Akihiro, Galeazzi Massimiliano, Gallo Luigi C., Gandhi Poshak, Giustini Margherita, Goldwurm Andrea, Gu Liyi, Guainazzi Matteo, Haba Yoshito, Hagino Kouichi, Hamaguchi Kenji, Harrus Ilana M., Hatsukade Isamu, Hayashi Katsuhiro, Hayashi Takayuki, Hayashida Kiyoshi, Hiraga Junko S., Hornschemeier Ann, Hoshino Akio, Hughes John P., Ichinohe Yuto, Iizuka Ryo, Inoue Hajime, Inoue Yoshiyuki, Ishida Manabu, Ishikawa Kumi, Ishisaki Yoshitaka, Iwai Masachika, Kaastra Jelle, Kallman Tim, Kamae Tsuneyoshi, Kataoka Jun, Katsuda Satoru, Kawai Nobuyuki, Kelley Richard L., Kilbourne Caroline A., Kitaguchi Takao, Kitamoto Shunji, Kitayama Tetsu, Kohmura Takayoshi, Kokubun Motohide, Koyama Katsuji, Koyama Shu, Kretschmar Peter, Krimm Hans A., Kubota Aya, Kunieda Hideyo, Laurent Philippe, Lee Shiu-Hang, Leutenegger Maurice A., Limousin Olivier O., Loewenstein Michael, Long Knox S., Lumb David, Madejski Greg, Maeda Yoshitomo, Maier Daniel, Makishima Kazuo, Markevitch Maxim, Matsumoto Hironori, Matsushita Kyoko, McCammon Dan, McNamara Brian R., Mehdipour Missagh, Miller Eric D., Miller Jon M., Mineshige Shin, Mitsuda Kazuhisa, Mitsuishi Ikuyuki, Miyazawa Takuya, Mizuno Tsunefumi, Mori Hideyuki, Mori Koji, Mukai Koji, Murakami Hiroshi, Mushotzky Richard F., Nakagawa Takao, Nakajima Hiroshi, Nakamori Takeshi, Nakashima Shinya, Nakazawa Kazuhiro, Norukawa Kumiko K., Nobukawa Masayoshi, Noda Hirofumi, Odaka Hirokazu, Ohashi Takaya, Ohno Masanori, Okajima Takashi, Ota Naomi, Ozaki Masanobu, Paerels Frits, Paltani Stephane, Petre Robert, Pinto Ciro, Porter Frederick S., Pottschmidt Katja, Reynolds Christopher S., Safi-Harb Samar, Saito Shinya, Sakai Kazuhiro, Sasaki Toru, Sato Goro, Sato Kosuke, Sato Rie, Sawada Makoto, Schartel Norbert, Serlemitsos Peter J., Seta Hiromi, Shidatsu Megumi, Simionescu Aurora, Smith Randall K., Soong Yang, Stawarz Lukasz, Sugawara Yasuharu, Sugita Satoshi, Szymkowiak Andrew, Tajima Hiroyasu, Takahashi Hiromitsu, Takahashi Tadayuki, Takeda Shinichiro, Takei Yoh, Tamagawa Toru, Tamura Takayuki, Tanaka Takaaki, Tanaka Yasuo, Tanaka Yasuyuki T., Tashiro Makoto S., Tawara Yuzuru, Terada Yukikatsu, Terashima Yuichi, Tombesi Francesco, Tomida Hiroshi, Tsuboi Yohko, Tsujimoto Masahiro, Tsunemi Hiroshi, Tsuru Takeshi Go, Uchida Hiroyuki, Uchiyama Hideki, Uchiyama Yasunobu, Ueda Shutaro, Ueda Yoshihiro, Uno Shinichiro, Urry C. Megan, Ursino Eugenio, Watanabe Shin, Werner Norbert, Wilkins Dan R., Williams Brian J., Yamada Shinya, Yamaguchi Hiroya, Yamaoka Kazutaka, Yamasaki Noriko Y., Yamauchi Makoto, Yamauchi Shigeo, Yaqoob Tahir, Yatsu Yoichi, Yonetoku Daisuke, Zhuravleva Irina, Zoghbi Abderahmen, Nakaniwa Nozomi

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   70 巻 ( 2 )   2018年3月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Publications of the Astronomical Society of Japan  

    We report on a Hitomi observation of IGRJ16318-4848, a high-mass X-ray binary system with an extremely strong absorption of NH ∼ 1024cm 2. Previous X-ray studies revealed that its spectrum is dominated by strong fluorescence lines of Fe as well as continuum emission lines. For physical and geometrical insight into the nature of the reprocessing material, we utilized the high spectroscopic resolving power of the X-ray microcalorimeter (the soft X-ray spectrometer: SXS) and the wide-band sensitivity by the soft and hard X-ray imagers (SXI and HXI) aboard Hitomi. Even though the photon counts are limited due to unintended off-axis pointing, the SXS spectrum resolves Fe Kα1 and Kα2 lines and puts strong constraints on the line centroid and line width. The line width corresponds to a velocity of 160+-37000 km s-1. This represents the most accurate, and smallest, width measurement of this line made so far from the any X-ray binary, much less than the Doppler broadening and Doppler shift expected from speeds that are characteristic of similar systems. Combined with the K-shell edge energy measured by the SXI and HXI spectra, the ionization state of Fe is estimated to be in the range of Fe I-IV. Considering the estimated ionization parameter and the distance between the X-ray source and the absorber, the density and thickness of the materials are estimated. The extraordinarily strong absorption and the absence of a Compton shoulder component have been confirmed. These characteristics suggest reprocessing materials that are distributed in a narrow solid angle or scattering, primarily by warm free electrons or neutral hydrogen. This measurement was achieved using the SXS detection of 19 photons. It provides strong motivation for follow-up observations of this and other X-ray binaries using the X-ray Astrophysics Recovery Mission and other comparable future instruments.

    DOI: 10.1093/pasj/psx154

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

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

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   70 巻 ( 2 )   2018年3月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Publications of the Astronomical Society of Japan  

    The Hitomi Soft X-ray Spectrometer spectrum of the Perseus cluster, with ∼5 eV resolution in the 2-9 keV band, offers an unprecedented benchmark of the atomic modeling and database for hot collisional plasmas. It reveals both successes and challenges of the current atomic data and models. The latest versions of AtomDB/APEC (3.0.8), SPEX (3.03.00), and CHIANTI (8.0) all provide reasonable fits to the broad-band spectrum, and are in close agreement on best-fit temperature, emission measure, and abundances of a few elements such as Ni. For the Fe abundance, the APEC and SPEX measurements differ by 16%, which is 17 times higher than the statistical uncertainty. This is mostly attributed to the differences in adopted collisional excitation and dielectronic recombination rates of the strongest emission lines. We further investigate and compare the sensitivity of the derived physical parameters to the astrophysical source modeling and instrumental effects. The Hitomi results show that accurate atomic data and models are as important as the astrophysical modeling and instrumental calibration aspects. Substantial updates of atomic databases and targeted laboratory measurements are needed to get the current data and models ready for the data from the next Hitomi-level mission.

    DOI: 10.1093/pasj/psx156

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

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

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   70 巻 ( 2 )   2018年3月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Publications of the Astronomical Society of Japan  

    The Crab nebula originated from a core-collapse supernova (SN) explosion observed in 1054AD. When viewed as a supernova remnant (SNR), it has an anomalously low observed ejecta mass and kinetic energy for an Fe-core-collapse SN. Intensive searches have been made for a massive shell that solves this discrepancy, but none has been detected. An alternative idea is that SN 1054 is an electron-capture (EC) explosion with a lower explosion energy by an order of magnitude than Fe-core-collapse SNe. X-ray imaging searches were performed for the plasma emission from the shell in the Crab outskirts to set a stringent upper limit on the X-ray emitting mass. However, the extreme brightness of the source hampers access to its vicinity. We thus employed spectroscopic technique using the X-ray micro-calorimeter on board the Hitomi satellite. By exploiting its superb energy resolution, we set an upper limit for emission or absorption features from as yet undetected thermal plasma in the 2-12keV range. We also re-evaluated the existing Chandra and XMM-Newton data. By assembling these results, a new upper limit was obtained for the X-ray plasma mass of < 1 M⊙ for a wide range of assumed shell radius, size, and plasma temperature values both in and out of collisional equilibrium. To compare with the observation, we further performed hydrodynamic simulations of the Crab SNR for two SN models (Fe-core versus EC) under two SN environments (uniform interstellar medium versus progenitor wind). We found that the observed mass limit can be compatible with both SN models if the SN environment has a low density of < 0.03 cm-3 (Fe core) or < 0.1 cm-3 (EC) for the uniform density, or a progenitor wind density somewhat less than that provided by a mass loss rate of 10-5M⊙ yr-1 at 20 km s-1for the wind environment.

    DOI: 10.1093/pasj/psx072

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

    Aharonian Felix, Akamatsu Hiroki, Akimoto Fumie, Allen Steven W., Angelini Lorella, Audard Marc, Awaki Hisamitsu, Axelsson Magnus, Bamba Aya, Bautz Marshall W., Blandford Roger, Brenneman Laura W., Brown Gregory V, Bulbul Esra, Cackett Edward M., Chernyakova Maria, Chiao Meng P., Coppi Paolo S., Costantini Elisa, de Plaa Jelle, de Vries Cor P., den Herder Jan-Willem, Done Chris, Dotani Tadayasu, Ebisawa Ken, Eckart Megan E., Enoto Teruaki, Ezoe Yuichiro, Fabian Andrew C., Ferrigno Carlo, Foster Adam R., Fujimoto Ryuichi, Fukazawa Yasushi, Furukawa Maki, Furuzawa Akihiro, Galeazzi Massimiliano, Gallo Luigi C., Gandhi Poshak, Giustini Margherita, Goldwurm Andrea, Gu Liyi, Guainazzi Matteo, Haba Yoshito, Hagino Kouichi, Hamaguchi Kenji, Harrus Ilana M., Hatsukade Isamu, Hayashi Katsuhiro, Hayashi Takayuki, Hayashida Kiyoshi, Hiraga Junko S., Hornschemeier Ann, Hoshino Akio, Hughes John P., Ichinohe Yuto, Iizuka Ryo, Inoue Hajime, Inoue Yoshiyuki, Ishida Manabu, Ishikawa Kumi, Ishisaki Yoshitaka, Iwai Masachika, Kaastra Jelle, Kallman Tim, Kamae Tsuneyoshi, Kataoka Jun, Kato Yuichi, Katsuda Satoru, Kawai Nobuyuki, Kelley Richard L., Kilbourne Caroline A., Kitaguchi Takao, Kitamoto Shunji, Kitayama Tetsu, Kohmura Takayoshi, Kokubun Motohide, Koyama Katsuji, Koyama Shu, Kretschmar Peter, Krimm Hans A., Kubota Aya, Kunieda Hideyo, Laurent Philippe, Lee Shiu-Hang, Leutenegger Maurice A., Limousin Olivier, Loewenstein Michael, Long Knox S., Lumb David, Madejski Greg, Maeda Yoshitomo, Maier Daniel, Makishima Kazuo, Markevitch Maxim, Matsumoto Hironori, Matsushita Kyoko, McCammon Dan, McNamara Brian R., Mehdipour Missagh, Miller Eric D., Miller Jon M., Mineshige Shin, Mitsuda Kazuhisa, Mitsuishi Ikuyuki, Miyazawa Takuya, Mizuno Tsunefumi, Mori Hideyuki, Mori Koji, Mukai Koji, Murakami Hiroshi, Mushotzky Richard F., Nakagawa Takao, Nakajima Hiroshi, Nakamori Takeshi, Nakashima Shinya, Nakazawa Kazuhiro, Norukawa Kumiko K., Nobukawa Masayoshi, Noda Hirofumi, Odaka Hirokazu, Ohashi Takaya, Ohno Masanori, Okajima Takashi, Ota Naomi, Ozaki Masanobu, Paerels Frits, Paltani Stephane, Petre Robert, Pinto Ciro, Porter Frederick S., Pottschmidt Katja, Reynolds Christopher S., Safi-Harb Samar, Saito Shinya, Sakai Kazuhiro, Sasaki Toru, Sato Goro, Sato Kosuke, Sato Rie, Sawada Makoto, Schartel Norbert, Serlemitsos Peter J., Seta Hiromi, Shidatsu Megumi, Simionescu Aurora, Smith Randall K., Soong Yang, Stawarz Lukasz, Sugawara Yasuharu, Sugita Satoshi, Szymkowiak Andrew, Tajima Hiroyasu, Takahashi Hiromitsu, Takahashi Tadayuki, Takeda Shinichiro, Takei Yoh, Tamagawa Toru, Tamura Takayuki, Tanaka Takaaki, Tanaka Yasuo, Tanaka Yasuyuki T., Tashiro Makoto S., Tawara Yuzuru, Terada Yukikatsu, Terashima Yuichi, Tombesi Francesco, Tomida Hiroshi, Tsuboi Yohko, Tsujimoto Masahiro, Tsunemi Hiroshi, Tsuru Takeshi Go, Uchida Hiroyuki, Uchiyama Hideki, Uchiyama Yasunobu, Ueda Shutaro, Ueda Yoshihiro, Uno Shinichiro, Urry C. Megan, Ursino Eugenio, Watanabe Shin, Werner Norbert, Wilkins Dan R., Williams Brian J., Yamada Shinya, Yamaguchi Hiroya, Yamaoka Kazutaka, Yamasaki Noriko Y., Yamauchi Makoto, Yamauchi Shigeo, Yaqoob Tahir, Yatsu Yoichi, Yonetoku Daisuke, Zhuravleva Irina, Zoghbi Abderahmen

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   70 巻 ( 2 )   2018年3月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Publications of the Astronomical Society of Japan  

    The present paper explains the temperature structure of X-ray emitting plasma in the core of the Perseus cluster based on 1.8-20.0 keV data obtained with the Soft X-ray Spectrometer (SXS) on board the Hitomi Observatory. A series of four observations was carried out, with a total effective exposure time of 338 ks that covered a central region of ∼7 in diameter. SXS was operated with an energy resolution of ∼5 eV (full width at half maximum) at 5.9 keV. Not only fine structures of K-shell lines in He-like ions, but also transitions from higher principal quantum numbers were clearly resolved from Si through Fe. That enabled us to perform temperature diagnostics using the line ratios of Si, S, Ar, Ca, and Fe, and to provide the first direct measurement of the excitation temperature and ionization temperature in the Perseus cluster. The observed spectrum is roughly reproduced by a single-temperature thermal plasma model in collisional ionization equilibrium, but detailed line-ratio diagnostics reveal slight deviations from this approximation. In particular, the data exhibit an apparent trend of increasing ionization temperature with the atomic mass, as well as small differences between the ionization and excitation temperatures for Fe, the only element for which both temperatures could be measured. The best-fit two-temperature models suggest a combination of 3 and 5 keV gas, which is consistent with the idea that the observed small deviations from a single-temperature approximation are due to the effects of projecting the known radial temperature gradient in the cluster core along the line of sight. A comparison with the Chandra/ACIS and the XMM-Newton/RGS results, on the other hand, suggests that additional lower-temperature components are present in the intracluster medium (ICM), but not detectable with Hitomi/SXS giving its 1.8-20 keV energy band.

    DOI: 10.1093/pasj/psy004

    Web of Science

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  61. An estimation of the white dwarf mass in the Dwarf Nova GK Persei with NuSTAR observations of two states 査読有り

    Wada Yuuki, Yuasa Takayuki, Nakazawa Kazuhiro, Makishima Kazuo, Hayashi Takayuki, Ishida Manabu

    MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY   474 巻 ( 2 ) 頁: 1564 - 1571   2018年2月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Monthly Notices of the Royal Astronomical Society  

    We report on X-ray observations of the Dwarf Nova GK Persei performed by NuSTAR in 2015. GK Persei, behaving also as an Intermediate Polar, exhibited a Dwarf Nova outburst in 2015 March-April. The object was observed with NuSTAR during the outburst state, and again in a quiescent state wherein the 15-50 keV flux was 33 times lower. Using a multitemperature plasma emission and reflection model, the highest plasma temperature in the accretion column was measured as 19.7-1.0+1.3 keV in outburst and 36.2-3.2+3.5 keV in quiescence. The significant change of the maximum temperature is considered to reflect an accretion-induced decrease of the inner-disc radius Rin, where accreting gas is captured by the magnetosphere. Assuming this radius scales as Rin ∝ M˙ -2/7, where M˙ is themass accretion rate, we obtain Rin = 1.9-0.2+0.4 RWD and Rin = 7.4-1.2+2.1 RWD in outburst and quiescence, respectively, where RWD is the white-dwarf (WD) radius of this system. Utilizing the measured temperatures and fluxes, as well as the standard mass-radius relation ofWDs, we estimate the WD mass as MWD = 0.87 ± 0.08M⊙ including typical systematic uncertainties by 7 per cent. The surface magnetic field is also measured as B ~ 5 × 105 G. These results exemplify a new X-ray method of estimating MWD and B of WDs by using large changes in M.

    DOI: 10.1093/mnras/stx2880

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  62. The hitomi X-Ray observatory 査読有り

    Richard L. Kelley, Kazuhiro Nakazawa

    Journal of Astronomical Telescopes, Instruments, and Systems   4 巻 ( 1 )   2018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:SPIE  

    DOI: 10.1117/1.JATIS.4.1.011201

    Web of Science

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

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

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   70 巻 ( Special Issue 1 )   2018年1月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Publications of the Astronomical Society of Japan  

    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

    Web of Science

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  64. 2015年-2017年冬季の金沢地域における雷雲ガンマ線データの解析

    松元 崇弘, 馬場 彩, 米徳 大輔, 澤野 達哉, 和田 有希, 古田 禄大, 中澤 知洋, 榎戸 輝揚, 湯浅 孝行, 牧島 一夫, 土屋 晴文, 小高 裕和

    日本物理学会講演概要集   73 巻 ( 0 ) 頁: 134 - 134   2018年

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    出版者・発行元:一般社団法人 日本物理学会  

    DOI: 10.11316/jpsgaiyo.73.2.0_134

    CiNii Article

  65. Long-term test of a stacked CdTe mini-HXI setup 査読有り

    Daniel Maier, Benoit Horeau, Philippe Laurent, Olivier Limousin, Diana Renaud, Madoka Kawaharada, Motohide Kokubun, Goro Sato, Tadayuki Takahashi, Shin Watanabe, Kazuhiro Nakazawa, Cesar Boatella Polo

    Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment   912 巻   頁: 199 - 204   2018年

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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 B.V.  

    This work presents a long-term operation of two stacked CdTe double sided strip detectors that are comparable with the CdTe detectors onboard Hitomi's HXI. The goal of this test is to study the evolution of the spectroscopic performance of the detectors during a one year operation cycle which resembles the in-orbit operation cycle of Hitomi HXI. Crystal defects inside CdTe cause a degradation of the spectroscopic performance (polarization effect) of the crystal which is becoming worse during detector operation. In order to prevent crystal polarization, the detectors are reset (switch-off of the depletion voltage) once a day. Our main investigation was to study if a long-term degradation can occur as a result of incomplete depolarization during the reset. We present the hardware setup and the analytical steps that were used to investigate the detector stability during each day and over the whole testing period. For the anode signals our results show at 60 keV: a daily line drift of (−2.8±0.7) eV/ks while the long-term drift is (−1.5±1.2) eV/day. The degradation of the energy resolution is measured to be (+2.4±0.3) eV/ks FWHM and the loss of efficiency is (−0.29±0.02) %/ks.

    DOI: 10.1016/j.nima.2017.11.035

    Scopus

  66. Concept of X-ray Astronomy Recovery Mission

    Tashiro Makoto, Maejima Hironori, Toda Kenichi, Kelley Richard, Reichenthal Lillian, Lobell James, Petre Robert, Guainazzi Matteo, Costantini Elisa, Edison Mark, Fujimoto Ryuichi, Grim Martin, Hayashida Kiyoshi, den Herder Jan-Willem, Ishisaki Yoshitaka, Paltani Stephane, Matsushita Kyoko, Mori Koji, Sneiderman Gary, Takei Yoh, Terada Yukikatsu, Tomida Hiroshi, Akamatsu Hiroki, Angelini Lorella, Arai Yoshitaka, Awaki Hisamitsu, Babyk Iurii, Bamba Aya, Barfknecht Peter, Barnstable Kim, Bialas Thomas, Blagojevic Branimir, Bonafede Joseph, Brambora Clifford, Brenneman Laura, Brown Greg, Brown Kimberly, Burns Laura, Canavan Edgar, Carnahan Tim, Chiao Meng, Comber Brian, Corrales Lia, de Vries Cor, Dercksen Johannes, Diaz-Trigo Maria, Dillard Tyrone, DiPirro Michael, Done Chris, Dotani Tadayasu, Ebisawa Ken, Eckart Megan, Enoto Teruaki, Ezoe Yuichiro, Ferrigno Carlo, Fujita Yutaka, Fukazawa Yasushi, Furuzawa Akihiro, Gallo Luigi, Graham Steve, Gu Liyi, Hagino Kohichi, Hamaguchi Kenji, Hatsukade Isamu, Hawes Dean, Hayashi Takayuki, Hegarty Cailey, Hell Natalie, Hiraga Junko, Hodges-Kluck Edmund, Holland Matt, Hornschemeier Ann, Hoshino Akio, Ichinohe Yuto, Iizuka Ryo, Ishibashi Kazunori, Ishida Manabu, Ishikawa Kumi, Ishimura Kosei, James Bryan, Kallman Timothy, Kara Erin, Katsuda Satoru, Kenyon Steven, Kilbourne Caroline, Kimball Mark, Kitaguchi Takao, Kitamoto Shunji, Kobayashi Shogo, Kohmura Takayoshi, Koyama Shu, Kubota Aya, Leutenegger Maurice, Lockard Tom, Loewenstein Mike, Maeda Yoshitomo, Marbley Lynette, Markevitch Maxim, Martz Connor, Matsumoto Hironori, Matsuzaki Keiichi, McCammon Dan, McNamara Brian, Miko Joseph, Miller Eric, Miller Jon, Minesugi Kenji, Mitsuishi Ikuyuki, Mizuno Tsunefumi, Mori Hideyuki, Mukai Koji, Murakami Hiroshi, Mushotzky Richard, Nakajima Hiroshi, Nakamura Hideto, Nakashima Shinya, Nakazawa Kazuhiro, Natsukari Chikara, Nigo Kenichiro, Nishioka Yusuke, Nobukawa Kumiko, Nobukawa Masayoshi, Noda Hirofumi, Odaka Hirokazu, Ogawa Mina, Ohashi Takaya, Ohno Masahiro, Ohta Masayuki, Okajima Takashi, Okamoto Atsushi, Onizuka Michitaka, Ota Naomi, Ozaki Masanobu, Plucinsky Paul, Porter F. Scott, Pottschmidt Katja, Sato Kosuke, Sato Rie, Sawada Makoto, Seta Hiromi, Shelton Ken, Shibano Yasuko, Shida Maki, Shidatsu Megumi, Shirron Peter, Simionescu Aurora, Smith Randall, Someya Kazunori, Soong Yang, Sugawara Yasuharu, Szymkowiak Andy, Takahashi Hiromitsu, Tamagawa Toru, Tamura Takayuki, Tanaka Takaaki, Terashima Yuichi, Tsuboi Yohko, Tsujimoto Masahiro, Tsunemi Hiroshi, Tsuru Takeshi, Uchida Hiroyuki, Uchiyama Hideki, Ueda Yoshihiro, Uno Shinichiro, Walsh Thomas, Watanabe Shin, Williams Brian, Wolfs Rob, Wright Michael, Yamada Shinya, Yamaguchi Hiroya, Yamaoka Kazutaka, Yamasaki Noriko, Yamauchi Shigeo, Yamauchi Makoto, Yanagase Keiichi, Yaqoob Tahir, Yasuda Susumu, Yoshioka Nasa, Zabala Jaime, Zhuravleva Irina

    SPACE TELESCOPES AND INSTRUMENTATION 2018: ULTRAVIOLET TO GAMMA RAY   10699 巻   2018年

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    記述言語:日本語   出版者・発行元:Proceedings of SPIE - The International Society for 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 × 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

    Web of Science

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

    Ohno Masanori, Werner Norbert, Pal Andras, Ripa Jakub, Galgoczi Gabor, Tarcai Norbert, Varhegyi Zsolt, Fukazawa Yasushi, Mizuno Tsunefumi, Takahashi Hiromitsu, Tanaka Koji, Uchida Nagomi, Torigoe Kento, Nakazawa Kazuhiro, Enoto Teruaki, Odaka Hirokazu, Ichinohe Yuto, Frei Zsolt, Kiss Laszo

    SPACE TELESCOPES AND INSTRUMENTATION 2018: ULTRAVIOLET TO GAMMA RAY   10699 巻   2018年

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    記述言語:日本語   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:Proceedings of SPIE - The International Society for Optical Engineering  

    A fleet of nanosatellites using precise timing synchronization provided by the Global Positioning System is a new concept for monitoring the gamma-ray sky that can achieve both all-sky coverage and good localization accuracy. We are proposing this new concept for the mission CubeSats Applied for MEasuring and LOcalising Transients (CAMELOT). The differences in photon arrival times at each satellite are to be used for source localization. Detectors with good photon statistics and the development of a localization algorithm capable of handling a large number of satellites are both essential for this mission. Large, thin CsI scintillator plates are the current candidates for the detectors because of their high light yields. It is challenging to maximize the light-collection efficiency and to understand the position dependence of such thin plates. We have found a multi-channel readout that uses the coincidence technique to be very effective in increasing the light output while keeping a similar noise level to that of a single channel readout. Based on such a detector design, we have developed a localization algorithm for this mission and have found that we can achieve a localization accuracy better than 20 arc minutes and a rate of about 10 short gamma-ray bursts per year.

    DOI: 10.1117/12.2313228

    Web of Science

    Scopus

  68. CAMELOT: Cubesats Applied for MEasuring and LOcalising Transients - Mission Overview

    Werner Norbert, Ripa Jakub, Pal Andras, Ohno Masanori, Tarcai Norbert, Torigoe Kento, Tanaka Koji, Uchida Nagomi, Meszaros Laszlo, Galgoczi Gabor, Fukazawa Yasushi, Mizuno Tsunefumi, Takahashi Hiromitsu, Nakazawa Kazuhiro, Varhegyi Zsolt, Enoto Teruaki, Odaka Hirokazu, Ichinohe Yuto, Frei Zsolt, Kiss Laszlo

    SPACE TELESCOPES AND INSTRUMENTATION 2018: ULTRAVIOLET TO GAMMA RAY   10699 巻   2018年

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    記述言語:日本語   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:Proceedings of SPIE - The International Society for Optical Engineering  

    We propose a fleet of nanosatellites to perform an all-sky monitoring and timing based localisation of gamma-ray transients. The fleet of at least nine 3U cubesats shall be equipped with large and thin CsI(Tl) scintillator based soft gamma-ray detectors read out by multi-pixel photon counters. For bright short gamma-ray bursts (GRBs), by cross-correlating their light curves, the fleet shall be able to determine the time difference of the arriving GRB signal between the satellites and thus determine the source position with an accuracy of ∼ 100. This requirement demands precise time synchronization and accurate time stamping of the detected gamma-ray photons, which will be achieved by using on-board GPS receivers. Rapid follow up observations at other wavelengths require the capability for fast, nearly simultaneous downlink of data using a global inter-satellite communication network. In terms of all-sky coverage, the proposed fleet will outperform all GRB monitoring missions.

    DOI: 10.1117/12.2313764

    Web of Science

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  69. 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  

  70. Monitoring of gamma-ray bursts with a fleet of nanosatellites

    Řípa J., Werner N., Pál A., Ohno M., Tarcai N., Torigoe K., Tanaka K., Uchida N., Mészáros L., Galgóczi G., Fukazawa Y., Mizuno T., Takahashi H., Nakazawa K., Várhegyi Z., Enoto T., Odaka H., Ichinohe Y., Frei Z., Kiss L.

    Proceedings of the International Astronautical Congress, IAC   2018-October 巻   2018年

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    記述言語:日本語   出版者・発行元:Proceedings of the International Astronautical Congress, IAC  

    We present the results of our feasibility study for a fleet of nano-satellites to perform an all sky monitoring and timing-based localisation of gamma-ray transients. The fleet of nine satellites of the CubeSat standard equipped with scintillator based soft gamma-ray detectors will measure the time difference between the arrival of the signal at the different satellites (the time will be synchronised using GPS) and determine the location of bright gamma-ray bursts in the sky by triangulation. The satellites will downlink the data about the detected transient within minutes, enabling rapid follow-up observations at other wavelengths.

    Scopus

  71. 雷雲ガンマ線の観測プロジェクトと雷での光核反応の検出

    榎戸 輝揚, 中野 俊男, 楳本 大悟, 土屋 晴文, 和田 有希, 古田 禄大, 中澤 知洋, 湯浅 孝行, 奥田 和史, 牧島 一夫, 佐藤 光輝, 佐藤 陽祐

    日本物理学会講演概要集   73 巻 ( 0 ) 頁: 176 - 176   2018年

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    出版者・発行元:一般社団法人 日本物理学会  

    DOI: 10.11316/jpsgaiyo.73.1.0_176

    CiNii Article

  72. 衛星軌道上放射化バックグラウンドシミュレータの開発と「ひとみ」衛星搭載硬X線撮像検出器のデータの再現性

    小高 裕和, 中澤 知洋, Asai Makoto, 萩野 浩一, Koi Tatsumi, Madejski Greg, 水野 恒史, 大野 雅功, 斉藤 新也, Wright Dennis

    日本物理学会講演概要集   73 巻 ( 0 ) 頁: 163 - 163   2018年

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    出版者・発行元:一般社団法人 日本物理学会  

    DOI: 10.11316/jpsgaiyo.73.2.0_163

    CiNii Article

  73. 落雷による光核反応の発見:地上観測による中性子と陽電子の検出

    和田 有希, 中野 俊男, 鈴木 寛大, 楳本 大悟, 土屋 晴文, 古田 禄大, 榎戸 輝揚, 中澤 知洋, 湯浅 孝行, 奥田 和史, 牧島 一夫, 佐藤 光輝, 佐藤 陽祐

    日本物理学会講演概要集   73 巻 ( 0 ) 頁: 422 - 422   2018年

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    出版者・発行元:一般社団法人 日本物理学会  

    DOI: 10.11316/jpsgaiyo.73.1.0_422

    CiNii Article

  74. 大型 CsI 結晶を用いた冬季雷雲由来ガンマ線検出器の量産とそれを用いたマッピング観測

    松元 崇弘, 土屋 晴文, 和田 有希, 古田 禄大, 清野 愛海, 中澤 知洋, 榎戸 輝揚, 湯浅 孝行, 牧島 一夫, 中野 俊男

    日本物理学会講演概要集   73 巻 ( 0 ) 頁: 414 - 414   2018年

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    出版者・発行元:一般社団法人 日本物理学会  

    DOI: 10.11316/jpsgaiyo.73.1.0_414

    CiNii Article

  75. The FORCE mission : Science aim and instrument parameter for broadband X-ray imaging spectroscopy with good angular resolution

    Nakazawa Kazuhiro, Mori Koji, Tsuru Takeshi G., Ueda Yoshihiro, Awaki Hisamitsu, Fukazawa Yasushi, Ishida Manabu, Matsumoto Hironori, Murakami Hiroshi, Okajima Takashi, Takahashi Tadayuki, Tsunemi Hiroshi, Zhang William W.

    SPACE TELESCOPES AND INSTRUMENTATION 2018: ULTRAVIOLET TO GAMMA RAY   10699 巻   2018年

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    出版者・発行元:Proceedings of SPIE - The International Society for Optical Engineering  

    FORCE is a 1.2 tonnes small mission dedicated for wide-band fine-imaging<br />
    x-ray observation. It covers from 1 to 80 keV with a good angular resolution of<br />
    $15&quot;$ half-power-diameter. It is proposed to be launched around mid-2020s and<br />
    designed to reach a limiting sensitivity as good as $F_X (10-40~{\rm keV}) = 3<br />
    \times 10^{-15}$~erg cm$^{-2}$ s$^{-1}$ keV$^{-1}$ within 1~Ms. This number is<br />
    one order of magnitude better than current best one. With its high-sensitivity<br />
    wide-band coverage, FORCE will probe the new science field of &quot;missing BHs&quot;,<br />
    searching for families of black holes of which populations and evolutions are<br />
    not well known. Other point-source and diffuse-source sciences are also<br />
    considered. FORCE will also provide the &quot;hard x-ray coverage&quot; to forthcoming<br />
    large soft x-ray observatories.

    DOI: 10.1117/12.2309344

    Web of Science

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    arXiv

  76. Suzaku and Chandra observations of the galaxy cluster RXC J1053.7+5453 with a radio relic 査読有り

    Itahana Madoka, Takizawa Motokazu, Akamatsu Hiroki, van Weeren Reinout J, Kawahara Hajime, Fukazawa Yasushi, Kaastra Jelle S, Nakazawa Kazuhiro, Ohashi Takaya, Ota Naomi, Rottgering Huub J. A, Vink Jacco, Zandanel Fabio

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   69 巻 ( 6 )   2017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)  

    DOI: 10.1093/pasj/psx095

    Web of Science

  77. Photonuclear reactions triggered by lightning discharge 査読有り

    Enoto Teruaki, Wada Yuuki, Furuta Yoshihiro, Nakazawa Kazuhiro, Yuasa Takayuki, Okuda Kazufumi, Makishima Kazuo, Sato Mitsuteru, Sato Yousuke, Nakano Toshio, Umemoto Daigo, Tsuchiya Harufumi

    NATURE   551 巻 ( 7681 ) 頁: 481 - +   2017年11月

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

    Lightning and thunderclouds are natural particle accelerators. Avalanches of relativistic runaway electrons, which develop in electric fields within thunderclouds, emit bremsstrahlung Î 3-rays. These Î 3-rays have been detected by ground-based observatories, by airborne detectors and as terrestrial Î 3-ray flashes from space. The energy of the Î 3-rays is sufficiently high that they can trigger atmospheric photonuclear reactions that produce neutrons and eventually positrons via β + decay of the unstable radioactive isotopes, most notably 13 N, which is generated via 14 N + Î 3 â †' 13 N + n, where Î 3 denotes a photon and n a neutron. However, this reaction has hitherto not been observed conclusively, despite increasing observational evidence of neutrons and positrons that are presumably derived from such reactions. Here we report ground-based observations of neutron and positron signals after lightning. During a thunderstorm on 6 February 2017 in Japan, a Î 3-ray flash with a duration of less than one millisecond was detected at our monitoring sites 0.5-1.7 kilometres away from the lightning. The subsequent Î 3-ray afterglow subsided quickly, with an exponential decay constant of 40-60 milliseconds, and was followed by prolonged line emission at about 0.511 megaelectronvolts, which lasted for a minute. The observed decay timescale and spectral cutoff at about 10 megaelectronvolts of the Î 3-ray afterglow are well explained by de-excitation Î 3-rays from nuclei excited by neutron capture. The centre energy of the prolonged line emission corresponds to electron-positron annihilation, providing conclusive evidence of positrons being produced after the lightning.

    DOI: 10.1038/nature24630

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  78. Solar abundance ratios of the iron-peak elements in the Perseus cluster 査読有り

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

    NATURE   551 巻 ( 7681 ) 頁: 478 - +   2017年11月

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

    The metal abundance of the hot plasma that permeates galaxy clusters represents the accumulation of heavy elements produced by billions of supernovae. 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. Recent X-ray studies of the intracluster medium found that the abundance ratios of these elements differ substantially from those seen in the Sun, 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, high-resolution 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 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- A nd sub-Chandrasekhar-mass type Ia supernova systems, adding to the mounting evidence that both progenitor types make a substantial contribution to cosmic chemical enrichment.

    DOI: 10.1038/nature24301

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  79. Suzaku Wide-band All-sky Monitor (WAM) observations of GRBs and SGRs 査読有り

    Yamaoka Kazutaka, Ohno Masanori, Tashiro Makoto S., Hurley Kevin, Krimm Hans A., Lien Amy Y., Ohmori Norisuke, Sugita Satoshi, Urata Yuji, Yasuda Tetsuya, Enomoto Junichi, Fujinuma Takeshi, Fukazawa Yasushi, Hanabata Yoshitaka, Iwakiri Wataru, Kawano Takafumi, Kinoshita Ryuuji, Kokubun Motohide, Makishima Kazuo, Matsuoka Shunsuke, Nagayoshi Tsutomu, Nakagawa Yujin, Nakaya Souhei, Nakazawa Kazuhiro, Nishioka Yusuke, Sakamoto Takanori, Takahashi Tadayuki, Takeda Sawako, Terada Yukikatsu, Yabe Seiya, Yamauchi Makoto, Yoshida Hiraku

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   69 巻 ( 3 )   2017年6月

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    記述言語:日本語   出版者・発行元:Publications of the Astronomical Society of Japan  

    We will review results for gamma-ray bursts (GRBs) and soft gamma repeaters (SGRs), obtained from the Suzaku Wide-band All-sky Monitor (WAM) which operated for about 10 years from 2005 to 2015. The WAM is a BGO (bismuth germanate: Bi 4 Ge 3 O 12) lateral shield for the Hard X-ray Detector (HXD), used mainly for rejecting its detector background, but it also works as an all-sky monitor for soft gamma-ray transients in the 50-5000 keV range thanks to its large effective area (∼600 cm 2 at 1 MeV for one detector) and wide field of view (about half of the entire sky). The WAM actually detected more than 1400 GRBs and 300 bursts from SGRs, and this detection number is comparable to that of other GRB-specific instruments. Based on the 10 years of operation, we describe timing and spectral performance for short GRBs, weak GRBs with high redshifts, and time-resolved pulses with good statistics.

    DOI: 10.1093/pasj/psx026

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  80. A hard-to-soft state transition of Aquila X-1 observed with Suzaku 査読有り

    Ono Ko, Makishima Kazuo, Sakurai Soki, Zhang Zhongli, Yamaoka Kazutaka, Nakazawa Kazuhiro

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   69 巻 ( 2 )   2017年4月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Publications of the Astronomical Society of Japan  

    The recurrent soft X-ray transient Aquila X-1 was observed with Suzaku for a gross duration of 79.9 ks, on 2011 October 21 when the object was in a rising phase of an outburst. During the observation, the source exhibited a clear spectral transition from the hard state to the soft state, on a time scale of ∼30 ks. Across the transition, the 0.8-10 keV X-Ray Imaging Spectrometer count rate increased by a factor ∼3, that of Hard X-ray Detector PIN (HXD-PIN) in 15-60 keV decreased by a similar factor, and the unabsorbed 0.1-100 keV luminosity increased from 3.5 × 1037 erg s-1 to 5.1 × 1037 erg s-1. The broadband spectral shape changed continuously, from a power-law-like one with a high-energy cut-off to a more convex one. Throughout the transition, the 0.8-60 keV spectra were successfully described with a model consisting of a multi-color blackbody and a Comptonized blackbody, which are considered to arise from a standard accretion disk and a closer vicinity of the neutron star, respectively. All the model parameters were confirmed to change continuously, from those typical in the hard state to those typical of the soft state. More specifically, the inner disk radius decreased from 31 km to 18 km, the effects of Comptonization on the blackbody photons weakened, and the electron temperature of Comptonization decreased from 10 keV to 3 keV. The derived parameters imply that the Comptonizing corona shrinks towards the final soft state, and/or the radial infall velocity of the corona decreases. These results reinforce the view that the soft and hard states of Aql X-1 (and of similar objects) are described by the same "disk plus Comptonized blackbody" model, but with considerably different parameters.

    DOI: 10.1093/pasj/psw126

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

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

    ASTROPHYSICAL JOURNAL LETTERS   837 巻 ( 1 ) 頁: 668 - 672   2017年3月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Astrophysical Journal Letters  

    High-resolution X-ray spectroscopy with Hitomi was expected to resolve the origin of the faint unidentified E ≈ 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 ≃ 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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  82. Suzaku and Chandra observations of CIZA J1700.8-3144, a cluster of galaxies in the Zone of Avoidance 査読有り

    Mori Hideyuki, Maeda Yoshitomo, Ueda Yoshihiro, Nakazawa Kazuhiro, Tawara Yuzuru

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   69 巻 ( 1 )   2017年2月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Publications of the Astronomical Society of Japan  

    We present the Chandra and Suzaku observations of 1RXS J170047.8-314442, located towards the Galactic bulge, to reveal a wide-band (0.3-10keV) X-ray morphology and spectrum of this source. With the Chandra observation, no point source was found at the position of 1RXS J170047.8-314442. Instead, we revealed the presence of diffuse X-ray emission, via the wide-band X-ray image obtained from the Suzaku XIS. Although the X-rayemission had a nearly circularshape with a spatial extent of ∼3.5, the surface brightness profile was not axisymmetric; a bright spot-like emission was found at ∼ 1' away in the northwestern direction from the center. The radial profile of the surface brightness, except for this spot-like emission, was reproduced with a single β-model; β and the core radius were found to be 1.02 and 1.51, respectively. The X-ray spectrum of the diffuse emission showed an emission line at ∼6keV, indicating an origin of a thermal plasma. The spectrum was well explained with an absorbed, optically-thin thermal plasma model with a temperature of 6.2 keVand a redshift parameter of z= 0.14 ±0.01. Hence, the X-ray emission was considered to arise from the hot gas associated with a cluster of galaxies. Our spectroscopic result confirmed the optical identification of 1RXS J170047.8-314442 by Kocevski et al. (2007, ApJ, 662, 224): CIZAJ1700.8-3144, a member of the cluster catalogue in the Zone of Avoidance. The estimated bolometric X-ray luminosity of 5.9 × 1044 erg s-1 was among the lowest with this temperature, suggesting that this cluster is far from relaxed.

    DOI: 10.1093/pasj/psw106

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  83. Suzaku observations of spectral variations of the ultra-luminous X-ray source Holmberg IX X-1 査読有り

    Shogo B. Kobayashi, Kazuhiro Nakazawa, Kazuo Makishima

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   69 巻 ( 1 )   2017年2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  

    Observations of the ultra-luminous X-ray source (ULX) Holmberg IX X-1 were carried out with Suzaku twice, once on 2012 April 13 and then on 2012 October 24, with exposures of 180 ks and 217 ks, respectively. The source showed a hard power-law shaped spectrum with a mild cutoff at similar to 8 keV, which is typical of ULXs when they are relatively dim. On both occasions, the 0.6-11 keV spectrum was explained successfully in terms of a cool (similar to 0.2 keV) multi-color disk blackbody emission model and thermal Comptonization emission produced by an electron cloud with a relatively low temperature and high optical depth, assuming that a large fraction of the disk-blackbody photons are Comptonized whereas the rest are observed directly. The 0.5-10 keV luminosity was 1.2 x 10(40) erg s(-1) in April, and similar to 14% higher in October. This brightening was accompanied by spectral softening in &gt;= 2 keV, with little change in the &lt;= 2 keV spectral shape. This behavior can be understood if the accretion disk remains unchanged while the electron cloud covers a variable fraction of the disk. The absorbing column density was consistent with the galactic line-of sight value, and did not vary by more than 1.6 x 10(21) cm(-2). Together with the featureless spectra, these properties may not be reconciled easily with the supercritical accretion scenario of this source.

    DOI: 10.1093/pasj/psw108

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  84. NuSTAR Observations of the Dwarf Nova GK Persei in 2015: Comparison between Outburst and Quiescent Phases

    Wada Yuuki, Yuasa Takayuki, Nakazawa Kazuhiro, Makishima Kazuo, Hayashi Takayuki, Ishida Manabu

    20TH EUROPEAN WHITE DWARF WORKSHOP   509 巻   頁: 509 - 514   2017年

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  85. 散乱型偏光度検出器の性能向上を目指したシンチレーターの反射材の改良

    齋藤 耀, 郡司 修一, 中森 健之, 奥村 曉, 中澤 知洋, 黒澤 俊介, 渡邊 直輝, 軽部 敦人

    日本物理学会講演概要集   72 巻 ( 0 ) 頁: 414 - 414   2017年

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    出版者・発行元:一般社団法人 日本物理学会  

    DOI: 10.11316/jpsgaiyo.72.2.0_414

    CiNii Article

  86. The status of DECIGO 査読有り

    Sato Shuichi, Kawamura Seiji, Ando Masaki, Nakamura Takashi, Tsubono Kimio, Araya Akito, Funaki Ikkoh, Ioka Kunihito, Kanda Nobuyuki, Moriwaki Shigenori, Musha Mitsuru, Nakazawa Kazuhiro, Numata Kenji, Sakai Shin-ichiro, Seto Naoki, Takashima Takeshi, Tanaka Takahiro, Agatsuma Kazuhiro, Aoyanagi Koh-suke, Arai Koji, Asada Hideki, Aso Yoichi, Chiba Takeshi, Ebisuzaki Toshikazu, Ejiri Yumiko, Enoki Motohiro, Eriguchi Yoshiharu, Fujimoto Masa-Katsu, Fujita Ryuichi, Fukushima Mitsuhiro, Futamase Toshifumi, Ganzu Katsuhiko, Harada Tomohiro, Hashimoto Tatsuaki, Hayama Kazuhiro, Hikida Wataru, Himemoto Yoshiaki, Hirabayashi Hisashi, Hiramatsu Takashi, Hong Feng-Lei, Horisawa Hideyuki, Hosokawa Mizuhiko, Ichiki Kiyotomo, Ikegami Takeshi, Inoue Kaiki T., Ishidoshiro Koji, Ishihara Hideki, Ishikawa Takehiko, Ishizaki Hideharu, Ito Hiroyuki, Itoh Yousuke, Kawashima Nobuki, Kawazoe Fumiko, Kishimoto Naoko, Kiuchi Kenta, Kobayashi Shiho, Kohri Kazunori, Koizumi Hiroyuki, Kojima Yasufumi, Kokeyama Keiko, Kokuyama Wataru, Kotake Kei, Kozai Yoshihide, Kudoh Hideaki, Kunimori Hiroo, Kuninaka Hitoshi, Kuroda Kazuaki, Maeda Kei-ichi, Matsuhara Hideo, Mino Yasushi, Miyakawa Osamu, Miyoki Shinji, Morimoto Mutsuko Y., Morioka Tomoko, Morisawa Toshiyuki, Mukohyama Shinji, Nagano Shigeo, Naito Isao, Nakamura Kouji, Nakano Hiroyuki, Nakao Kenichi, Nakasuka Shinichi, Nakayama Yoshinori, Nishida Erina, Nishiyama Kazutaka, Nishizawa Atsushi, Niwa Yoshito, Noumi Taiga, Obuchi Yoshiyuki, Ohashi Masatake, Ohishi Naoko, Ohkawa Masashi, Okada Norio, Onozato Kouji, Oohara Kenichi, Sago Norichika, Saijo Motoyuki, Sakagami Masaaki, Sakata Shihori, Sasaki Misao, Sato Takashi, Shibata Masaru, Shinkai Hisaaki, Somiya Kentaro, Sotani Hajime, Sugiyama Naoshi, Suwa Yudai, Suzuki Rieko, Tagoshi Hideyuki, Takahashi Fuminobu, Takahashi Kakeru, Takahashi Keitaro, Takahashi Ryutaro, Takahashi Ryuichi, Takahashi Tadayuki, Takahashi Hirotaka, Akiteru Takamori, Takano Tadashi, Taniguchi Keisuke, Taruya Atsushi, Tashiro Hiroyuki, Torii Yasuo, Toyoshima Morio, Tsujikawa Shinji, Tsunesada Yoshiki, Ueda Akitoshi, Ueda Ken-ichi, Utashima Masayoshi, Wakabayashi Yaka, Yamakawa Hiroshi, Yamamoto Kazuhiro, Yamazaki Toshitaka, Yokoyama Jun'ichi, Yoo Chul-Moon, Yoshida Shijun, Yoshino Taizoh

    11TH INTERNATIONAL LISA SYMPOSIUM   840 巻 ( 1 )   2017年

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    記述言語:日本語   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:Journal of Physics: Conference Series  

    DECIGO (DECi-hertz Interferometer Gravitational wave Observatory) is the planned Japanese space gravitational wave antenna, aiming to detect gravitational waves from astrophysically and cosmologically significant sources mainly between 0.1 Hz and 10 Hz and thus to open a new window for gravitational wave astronomy and for the universe. DECIGO will consists of three drag-free spacecraft arranged in an equilateral triangle with 1000 km arm lengths whose relative displacements are measured by a differential Fabry-Perot interferometer, and four units of triangular Fabry-Perot interferometers are arranged on heliocentric orbit around the sun. DECIGO is vary ambitious mission, we plan to launch DECIGO in era of 2030s after precursor satellite mission, B-DECIGO. B-DECIGO is essentially smaller version of DECIGO: B-DECIGO consists of three spacecraft arranged in an triangle with 100 km arm lengths orbiting 2000 km above the surface of the earth. It is hoped that the launch date will be late 2020s for the present..

    DOI: 10.1088/1742-6596/840/1/012010

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  87. NuSTAR Observations of the Dwarf Nova GK Persei in 2015: Comparison between Outburst and Quiescent Phases 査読有り

    Yuuki Wada, Takayuki Yuasa, Kazuhiro Nakazawa, Kazuo Makishima, Takayuki Hayashi, Manabu Ishida

    20TH EUROPEAN WHITE DWARF WORKSHOP   509 巻   頁: 509 - 514   2017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:ASTRONOMICAL SOC PACIFIC  

    We report on NuSTAR observations of the intermediate polar GK Persei which also behaves as a dwarf nova. It exhibited a dwarf nova outburst in 2015 March April. The object was observed in 3-79 keV X-rays with NuSTAR, once at the outburst peak, and again in 2015 September during quiescence. The 5-50 keV flux during the outburst was 26 times higher than that during the quiescence. With a multi-temperature emission model and a reflection model, we derived the post-shock temperature as 19.2 +/- 0.7 keV in the outburst, and 38.5(-3.6)(+4.1) keV in the quiescence. This temperature difference is considered to reflect changes in the radius at which the accreting matter, forming an accretion disk, is captured by the magnetosphere of the white dwarf (WD). Assuming that this radius scales as the power of -2/7 of the mass accretion rate, and utilizing the two temperature measurements, as well as the standard mass-radius relation of WDs, we determined the WD mass in GK Persei as 0.90 +/- 0.06 solar masses. The magnetic field is estimated as 4 x 10(5) G.

    Web of Science

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書籍等出版物 3

  1. 銀河団同士の衝突による巨大衝撃波の誕生を捉えた

    加藤祐一, 中澤知洋( 担当: 共著)

    天文月報  2016年11月 

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    記述言語:日本語

  2. X 線、γ線で探る宇宙の構造と進化

    高橋忠幸, 中澤知洋( 担当: 共著)

    応用物理学会誌  2012年 

     詳細を見る

    記述言語:日本語

  3. 宇宙科学のすばらしさを伝える

    中澤知洋,前田良知,内山泰伸,大島泰,川崎正寛,穴吹直久, 他,宇宙科学研究所X線天文グループ( 担当: 共著)

    天文月報,  2002年7月 

     詳細を見る

    記述言語:日本語

MISC 68

  1. 超小型衛星による,宇宙空間からの太陽中性子の観測(III)

    山岡和貴, 田島宏康, 宮田喜久子, 稲守孝哉, 野橋大輝, 宇佐見雅己, 中澤知洋, 増田智, 伊藤和也, 松下幸司, 高橋弘充, 渡邉恭子  

    日本天文学会年会講演予稿集2021 巻   2021年

     詳細を見る

  2. 雷活動に関するガンマ線の観測プロジェクト:2020年1月に近接して発生した複数のロングバーストの同時途絶の観測

    久富章平, 中澤知洋, 辻結菜, 榎戸輝揚, 和田有希, 湯浅孝行, 土屋晴文, 篠田太郎, 一方井祐子, 三宅晶子  

    日本物理学会講演概要集(CD-ROM)75 巻 ( 2 )   2020年

     詳細を見る

  3. 広帯域X線の高感度観測衛星FORCE:ミッション提案とサイエンス目的の深化

    中澤知洋, 森浩二, 鶴剛, 上田佳宏, 石田学, 松本浩典, 粟木久光, 村上弘志, 寺田幸功, 久保田あや, 榎戸輝揚, 馬場彩, 小高裕和, 谷津陽一, 小林翔悟, 幸村孝由, 萩野浩一, 内山泰伸, 北山哲, 高橋忠幸, 渡辺伸, 飯塚亮, 山口弘悦, 大橋隆哉, 中嶋大, 古澤彰浩, 田中孝明, 内田裕之, 野田博文, 常深博, 伊藤真之, 信川正順, 信川久実子, 太田直美, 寺島雄一, 深沢泰司, 水野恒史, 高橋弘充, 大野雅功, 赤松弘規, HORNSCHEMEIER A.E, 岡島崇, ZHANG W.W.  

    日本物理学会講演概要集(CD-ROM)75 巻 ( 2 )   2020年

     詳細を見る

  4. 超小型衛星搭載用太陽中性子・ガンマ線検出器の開発

    野橋大輝, 山岡和貴, 田島宏康, 宮田喜久子, 稲守孝哉, PARK Ji Hyun, 中澤知洋, 増田智, 伊藤和也, 松下幸司, 高橋弘充, 渡邉恭子  

    日本物理学会講演概要集(CD-ROM)75 巻 ( 1 )   2020年

     詳細を見る

  5. 雷活動に由来するガンマ線の観測プロジェクト:2019年度の多地点観測の進展

    久富章平, 中澤知洋, 辻結菜, FABIANI Alexia, 榎戸輝揚, 和田有希, 和田有希, 湯浅孝行, 古田禄大, 土屋晴文, 一方井祐子, 三宅晶子  

    日本地球惑星科学連合大会予稿集(Web)2020 巻   2020年

     詳細を見る

  6. 雷活動に由来するガンマ線の観測プロジェクト:2019年度の多地点観測の進展

    久富章平, 中澤知洋, 辻結菜, FABIANI Alexia, 榎戸輝揚, 和田有希, 和田有希, 湯浅孝行, 古田禄大, 土屋晴文, 一方井祐子, 三宅晶子  

    日本物理学会講演概要集(CD-ROM)75 巻 ( 1 )   2020年

     詳細を見る

  7. 世界最高感度を実証した「ひとみ」搭載の硬X線撮像検出器HXI

    中澤知洋, 萩野浩一  

    日本天文学会誌 天文月報112 巻   頁: 471 - 473   2019年7月

  8. 雷活動に由来するガンマ線の観測プロジェクト:多地点観測の進展と大気電場・電波との協同観測

    和田有希, 和田有希, 榎戸輝揚, 松元崇弘, 中澤知洋, 古田禄大, 湯浅孝行, 鴨川仁, BOWERS G. S, 中村佳敬, 森本健志, 玉川徹, 牧島一夫, 牧島一夫, 土屋晴文, 久保守, 松木篤, 米徳大輔, 澤野達哉, SMITH D. M  

    日本物理学会講演概要集(CD-ROM)74 巻 ( 1 ) 頁: ROMBUNNO.14aK407‐11   2019年3月

     詳細を見る

    記述言語:日本語  

    J-GLOBAL

  9. 冬季の雷放電と同期したガンマ線フラッシュの定量評価

    和田有希, 和田有希, 榎戸輝揚, 中澤知洋, 古田禄大, 湯浅孝行, 中村佳敬, 森本健志, 松元崇弘, 牧島一夫, 牧島一夫, 土屋晴文  

    日本原子力学会春の年会予稿集(CD-ROM)2019 巻   頁: ROMBUNNO.1H07   2019年3月

     詳細を見る

    記述言語:日本語  

    J-GLOBAL

  10. 冬季雷における高エネルギー現象の観測プロジェクトの進展

    和田有希, 和田有希, 榎戸輝揚, 松元崇弘, 中澤知洋, 古田禄大, 湯浅孝行, 土屋晴文, 米徳大輔, 澤野達哉, 牧島一夫, 牧島一夫, 鴨川仁, 中村佳敬, 森本健志, 佐藤光輝, 酒井英男, 南戸秀仁, 牛尾知雄  

    日本地球惑星科学連合大会予稿集(Web)2019 巻   頁: ROMBUNNO.MIS27‐10 (WEB ONLY)   2019年

     詳細を見る

    記述言語:日本語  

    J-GLOBAL

  11. 3Uキューブサットによる太陽中性子・ガンマ線観測

    山岡和貴, 田島宏康, 宮田喜久子, 稲守孝哉, 佐々井義矩, 中澤知洋, 増田智, 松下幸司, 伊藤和也, 高橋弘充, 渡邉恭子  

    日本地球惑星科学連合大会予稿集(Web)2019 巻   2019年

     詳細を見る

  12. 超小型衛星による,宇宙空間からの太陽中性子の観測(II)

    山岡和貴, 田島宏康, 佐々井義矩, 宮田喜久子, 稲守孝哉, 中澤知洋, 増田智, 伊藤和也, 松下幸司, 高橋弘充, 渡邉恭子  

    日本天文学会年会講演予稿集2019 巻   2019年

     詳細を見る

  13. 超小型衛星による,宇宙空間からの太陽中性子の観測(III)

    山岡和貴, 田島宏康, 宮田喜久子, 稲守孝哉, PARK Ji Hyun, 野橋大輝, 中澤知洋, 増田智, 伊藤和也, 松下幸司, 高橋弘充, 渡邉恭子  

    日本天文学会年会講演予稿集2019 巻   2019年

     詳細を見る

  14. Detection of polarized gamma-ray emission from the Crab nebula with Hitomi Soft Gamma-ray Detector

    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  

        2018年10月

     詳細を見る

    掲載種別:機関テクニカルレポート,技術報告書,プレプリント等  

    We present the results from the Hitomi Soft Gamma-ray Detector (SGD)<br />
    observation of the Crab nebula. The main part of SGD is a Compton camera, which<br />
    in addition to being a spectrometer, is capable of measuring polarization of<br />
    gamma-ray photons. The Crab nebula is one of the brightest X-ray / gamma-ray<br />
    sources on the sky, and, the only source from which polarized X-ray photons<br />
    have been detected. SGD observed the Crab nebula during the initial test<br />
    observation phase of Hitomi. We performed the data analysis of the SGD<br />
    observation, the SGD background estimation and the SGD Monte Carlo simulations,<br />
    and, successfully detected polarized gamma-ray emission from the Crab nebula<br />
    with only about 5 ks exposure time. The obtained polarization fraction of the<br />
    phase-integrated Crab emission (sum of pulsar and nebula emissions) is (22.1<br />
    $\pm$ 10.6)% and, the polarization angle is 110.7$^o$ + 13.2 / $-$13.0$^o$ in<br />
    the energy range of 60--160 keV (The errors correspond to the 1 sigma<br />
    deviation). The confidence level of the polarization detection was 99.3%. The<br />
    polarization angle measured by SGD is about one sigma deviation with the<br />
    projected spin axis of the pulsar, 124.0$^o$ $\pm$0.1$^o$.

    arXiv

  15. 炭素繊維強化プラスチック(CFRP)へのX線反射面形成法の開発

    粟木久光, 大上千智, 吉田鉄生, 岩切駿, 相田望, 松本浩典, 三石郁之, 大塚康司, 清水貞行, 田村啓輔, 中澤知洋, 石田学, 石田直樹  

    日本天文学会年会講演予稿集2018 巻   頁: 227   2018年8月

     詳細を見る

    記述言語:日本語  

    J-GLOBAL

  16. 銀河面からの軟X線背景放射(5)

    石原雅士, 三石郁之, 中澤知洋  

    日本天文学会年会講演予稿集2018 巻   頁: 156   2018年8月

     詳細を見る

    記述言語:日本語  

    J-GLOBAL

  17. 軟X線から硬X線の広帯域を高感度で撮像分光する小型衛星計画FORCEの現状(7)

    中澤知洋, 森浩二, 鶴剛, 上田佳宏, 松本浩典, 粟木久光, 石田学, 寺島雄一, 常深博, 中嶋大, 田中孝明, 内田裕之, 伊藤真之, 寺田幸功, 久保田あや, 馬場彩, 小高裕和, 高橋忠幸, 谷津陽一, 幸村孝由, 萩野浩一, 小林翔悟, 北山哲, 村上弘志, 信川正順, 太田直美, 深沢泰司, 水野恒史, 高橋弘充, 大野雅功, 古澤彰浩, 武田彩希, 中島真也, 内山泰伸, 渡辺伸, 飯塚亮, 岡島崇, 山口弘悦, 森英之  

    日本天文学会年会講演予稿集2018 巻   頁: 220   2018年8月

     詳細を見る

    記述言語:日本語  

    J-GLOBAL

  18. Discovery of recombining plasma from the faintest GeV SNR HB 21 and a possible scenario of the cosmic ray escaping from SNR shocks

    Hiromasa Suzuki, Aya Bamba, Kazuhiro Nakazawa, Yoshihiro Furuta, Makoto Sawada, Ryo Yamazaki, Katsuji Koyama  

        2018年5月

     詳細を見る

    掲載種別:機関テクニカルレポート,技術報告書,プレプリント等  

    We present an X-ray study of the GeV gamma-ray supernova remnant (SNR) HB 21<br />
    with Suzaku. HB 21 is interacting with molecular clouds and the faintest in the<br />
    GeV band among known GeV SNRs. We discovered strong radiative recombination<br />
    continua of Si and S from the center of the remnant, which provide the direct<br />
    evidence of a recombining plasma (RP). The total emission can be explained with<br />
    the RP and ionizing plasma components. The electron temperature and<br />
    recombination timescale of the RP component were estimated as 0.17 (0.15-0.18)<br />
    keV and 3.2 (2.0-4.8) $\times$ 10$^{11}$ s cm$^{-3}$, respectively. The<br />
    estimated age of the RP (RP age; $\sim$ 170 kyr) is the longest among known<br />
    recombining GeV SNRs, because of very low density of electrons ($\sim$ 0.05<br />
    cm$^{-3}$). We have examined dependencies of GeV spectral indices on each of RP<br />
    ages and SNR diameters for nine recombining GeV SNRs. Both showed possible<br />
    positive correlations, indicating that both the parameters can be good<br />
    indicators of properties of accelerated protons, for instance, degree of escape<br />
    from the SNR shocks. A possible scenario for a process of proton escape is<br />
    introduced; interaction with molecular clouds makes weaker magnetic turbulence<br />
    and cosmic-ray protons escape, simultaneously cooling down the thermal<br />
    electrons and generate an RP.

    DOI: 10.1093/pasj/psy069

    arXiv

  19. X線衛星「ひとみ」搭載軟ガンマ線検出器(SGD)によるかに星雲のガンマ線偏光観測

    渡辺伸, 渡辺伸, 内田悠介, 内田悠介, 田島宏康, 深沢泰司, 一戸悠人, 内山秀樹, 内山泰伸, 榎戸輝揚, 太田方之, 大野雅功, 小高裕和, 片岡淳, 勝田隼一郎, 北口貴雄, 国分紀秀, GOLDWURM A, 斉藤新也, 佐藤悟朗, 佐藤理江, 高橋忠幸, 高橋忠幸, 高橋弘充, 武田伸一郎, 田中孝明, 田中康之, 寺田幸功, 中澤知洋, 中澤知洋, 中野俊男, 中森健之, 野田博文, 萩野浩一, 林克洋, 林克洋, BLANDFORD R, 牧島一夫, MADEJSKI G, 水野恒史, 森國城, 谷津陽一, 山岡和貴, 湯浅孝行, 米徳大輔, LAURENT P, LIMOUSIN O, LEBRUN F  

    日本物理学会講演概要集(CD-ROM)73 巻 ( 1 ) 頁: ROMBUNNO.25pK307‐5   2018年3月

     詳細を見る

    記述言語:日本語  

    J-GLOBAL

  20. 落雷による光核反応の発見:地上観測による中性子と陽電子の検出

    和田有希, 和田有希, 古田禄大, 榎戸輝揚, 中澤知洋, 中澤知洋, 湯浅孝行, 奥田和史, 牧島一夫, 佐藤光輝, 佐藤陽祐, 中野俊男, 楳本大悟, 土屋晴文  

    日本物理学会講演概要集(CD-ROM)73 巻 ( 1 ) 頁: ROMBUNNO.22aK308‐7   2018年3月

     詳細を見る

    記述言語:日本語  

    J-GLOBAL

  21. 落雷による光核反応の発見:シミュレーションによるデータ解釈

    古田禄大, 和田有希, 和田有希, 榎戸輝揚, 中澤知洋, 湯浅孝行, 奥田和史, 牧島一夫, 佐藤光輝, 佐藤陽祐, 中野俊男, 楳本大悟, 土屋晴文  

    日本物理学会講演概要集(CD-ROM)73 巻 ( 1 ) 頁: ROMBUNNO.22aK308‐8   2018年3月

     詳細を見る

    記述言語:日本語  

    J-GLOBAL

  22. 大型CsI結晶を用いた冬季雷雲由来ガンマ線検出器の量産とそれを用いたマッピング観測

    松元崇弘, 和田有希, 和田有希, 古田禄大, 清野愛海, 中澤知洋, 中澤知洋, 榎戸輝揚, 湯浅孝行, 牧島一夫, 中野俊男, 土屋晴文  

    日本物理学会講演概要集(CD-ROM)73 巻 ( 1 ) 頁: ROMBUNNO.22aK307‐7   2018年3月

     詳細を見る

    記述言語:日本語  

    J-GLOBAL

  23. 雷雲ガンマ線の観測プロジェクトと雷での光核反応の検出

    榎戸輝揚, 和田有希, 和田有希, 古田禄大, 中澤知洋, 湯浅孝行, 奥田和史, 牧島一夫, 佐藤光輝, 佐藤陽祐, 中野俊男, 楳本大悟, 土屋晴文, 土屋晴文  

    日本物理学会講演概要集(CD-ROM)73 巻 ( 1 ) 頁: ROMBUNNO.22pK305‐7   2018年3月

     詳細を見る

    記述言語:日本語  

    J-GLOBAL

  24. 日本海沿岸における冬の雷や雷雲に伴う放射線観測

    土屋晴文, 榎戸輝揚, 和田有希, 和田有希, 古田禄大, 中澤知洋, 湯浅孝行, 奥田和史, 牧島一夫, 中野俊男, 楳本大悟  

    日本原子力学会春の年会予稿集(CD-ROM)2018 巻   頁: ROMBUNNO.3E01   2018年3月

     詳細を見る

    記述言語:日本語  

    J-GLOBAL

  25. GRB位置決定のための小型衛星搭載用大型CsIシンチレータのMPPC読み出し性能評価

    鳥越健斗, 深沢泰司, 水野恒史, 高橋弘充, 大野雅功, 田中晃司, 内田和海, WERNER Norbert, WERNER Norbert, WERNER Norbert, PAL Andras, FREI Zsolt, KISS Laszlo, NORBERT Tarcai, 中澤知洋, 榎戸輝揚, 小高裕和, 一戸悠人  

    日本天文学会年会講演予稿集2018 巻   頁: 239   2018年2月

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  26. 重力波対応天体の追観測を目指した超小型GRB観測衛星における位置決定精度の評価

    田中晃司, 深沢泰司, 水野恒史, 高橋弘充, 大野雅功, 内田和海, 鳥越健斗, WERNER Norbert, WERNER Norbert, WERNER Norbert, PAL Andras, FREI Zsolt, KISS Laszlo, NORBERT Tarcai, 中澤知洋, 榎戸輝揚, 小高裕和, 一戸悠人  

    日本天文学会年会講演予稿集2018 巻   頁: 239   2018年2月

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  27. 軟X線から硬X線の広帯域を高感度で撮像分光する小型衛星計画FORCEの現状(6)

    森浩二, 武田彩希, 村上弘志, 寺田幸功, 久保田あや, 中澤知洋, 馬場彩, 谷津陽一, 幸村孝由, 萩野浩一, 小高裕和, 中島真也, 内山泰伸, 斉藤新也, 北山哲, 高橋忠幸, 石田学, 渡辺伸, 飯塚亮, 古澤彰浩, 鶴剛, 上田佳宏, 田中孝明, 内田裕之, 小林翔悟, 松本浩典, 中嶋大, 常深博, 信川正順, 太田直美, 伊藤真之, 粟木久光, 寺島雄一, 深沢泰司, 水野恒史, 高橋弘充, 大野雅功, 岡島崇, 山口弘悦, 森英之  

    日本天文学会年会講演予稿集2018 巻   頁: 231   2018年2月

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  28. 狭輝線I型セイファート銀河Swift J2127.4+5654におけるディレイとハード一次成分

    三宅克馬, 野田博文, 山田真也, 清野愛海, 中澤知洋, 牧島一夫  

    日本天文学会年会講演予稿集2018 巻   頁: 171   2018年2月

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  29. 地上と宇宙から探る雷放電に同期する突発ガンマ線観測への取り組み

    中澤知洋, 榎戸輝揚, 和田有希, 和田有希, 古田禄大, 松元崇弘, 春日知明, 奥田和史, 湯浅孝行, 中野俊男, 楳本大悟, 加藤博, 牧島一夫, 佐藤光輝, 佐藤陽祐, 土屋晴文  

    日本天文学会年会講演予稿集2018 巻   頁: 240   2018年2月

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  30. 「ひとみ」HXIを用いた軌道上中性子バックグラウンドの評価

    鈴木寛大, 中澤知洋, 萩野浩一, 国分紀秀, 佐藤悟朗, 高橋忠幸, 渡辺伸, 太田方之, 佐藤理江, 森國城, 村上浩章, 三宅克馬, 古田禄大, 馬場彩, 鶴剛, 田中孝明, 榎戸輝揚, 小林翔悟, 寺田幸功, 内山秀樹, 谷津洋一, 野田博文, 田島宏康, 山岡和貴, 林克洋, 林克洋, 深沢泰司, 水野恒史, 大野雅功, 高橋弘充, 勝田隼一郎, 中森健之, 内山泰伸, 斉藤新也, 牧島一夫, 小高裕和, 湯浅孝行, 中野俊男, 片岡淳, 三村健人, LEBRUN Francois, LIMOUSIN Olivier, LAURENT Philippe, MAIER Daniel, 武田伸一郎, 森浩二  

    日本天文学会年会講演予稿集2018 巻   頁: 227   2018年2月

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  31. X線衛星代替機XARMにおける科学運用計画

    寺田幸功, 田代信, 田代信, 海老沢研, 深沢泰司, 飯塚亮, 勝田哲, 北口貴雄, 久保田あや, 水野恒史, 中島真也, 中澤知洋, 信川正順, 大野雅功, 太田直美, 志達めぐみ, 菅原泰晴, 高橋弘充, 田村隆幸, 田中康之, 寺島雄一, 坪井陽子, 内山秀樹, 宇野伸一郎, 渡辺伸, 山内茂雄  

    日本天文学会年会講演予稿集2018 巻   頁: 228   2018年2月

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  32. X線天文衛星「ひとみ」搭載SGDによるかに星雲からの偏光ガンマ線の観測

    内田悠介, 渡辺伸, 田島宏康, 深沢泰司, 国分紀秀, 太田方之, 佐藤悟朗, 佐藤理江, 森國城, 高橋忠幸, 高橋忠幸, 水野恒史, 高橋弘充, 大野雅功, 田中康之, 勝田隼一郎, 中澤知洋, 牧島一夫, 小高裕和, 北口貴雄, 中野俊男, 湯浅孝行, 片岡淳, 一戸悠人, 内山秀樹, 内山泰伸, 斉藤新也, 榎戸輝揚, 田中孝明, GOLDWURM A, LAURENT P, LIMOUSIN O, LEBRUN F, 武田伸一郎, 寺田幸功, 中森健之, 野田博文, 萩野浩一, 山岡和貴, 林克洋, 林克洋, BLANDFORD R, MADEJSKI G, 谷津陽一, 米徳大輔  

    日本天文学会年会講演予稿集2018 巻   頁: 148   2018年2月

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  33. X線を用いたKepler超新星残骸中のFeの非等方な膨張構造解析

    春日知明, 佐藤寿紀, 佐藤寿紀, 森浩二, 山口弘悦, 山口弘悦, 馬場彩, 中澤知洋  

    日本天文学会年会講演予稿集2018 巻   頁: 71   2018年2月

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  34. GROWTH実験2014年度データを用いた雷雲ガンマ線イベントの探索法の改善

    楳本大悟, 土屋晴文, 中澤知洋, 湯浅孝行, 榎戸輝揚, 牧島一夫, 古田禄大, 玉川徹, 伊藤伸泰  

    日本物理学会講演概要集(CD-ROM)72 巻 ( 2 ) 頁: ROMBUNNO.13pU32‐6   2017年9月

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  35. 雷雲ガンマ線の地上観測の現状と2017年のGROWTH実験計画

    中澤知洋, 榎戸輝揚, 和田有希, 古田禄大, 楳本大悟, 清野愛海, 樋口裕真, 湯浅孝行, 土屋晴文, 牧島一夫, 中野俊男  

    日本物理学会講演概要集(CD-ROM)72 巻 ( 2 ) 頁: ROMBUNNO.15aU33‐5   2017年9月

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  36. 散乱型偏光度検出器の性能向上を目指したシンチレーターの反射材の改良

    齋藤耀, 郡司修一, 中森健之, 奥村曉, 中澤知洋, 黒澤俊介, 黒澤俊介, 渡邊直輝, 軽部敦人  

    日本物理学会講演概要集(CD-ROM)72 巻 ( 2 ) 頁: ROMBUNNO.15aU33‐6   2017年9月

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  37. モンテカルロシミュレーションによる雷雲ガンマ線放射モデルの構築

    古田禄大, 中澤知洋, 和田有希, 楳本大悟, 榎戸輝揚, 湯浅孝行, 土屋晴文, 牧島一夫  

    日本物理学会講演概要集(CD-ROM)72 巻 ( 2 ) 頁: ROMBUNNO.15aU33‐4   2017年9月

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  38. X線衛星「すざく」を用いたガンマ線連星LS5039のX線パルス探索

    松元崇弘, 榎戸輝揚, 村上浩章, 牧島一夫, 中澤知洋, 馬場彩  

    日本天文学会年会講演予稿集2017 巻   頁: 262   2017年8月

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  39. 銀河団衝突で発生した若い衝撃波の観測研究

    加藤佑一, 中澤知洋, GU Lyli, 赤堀卓也, 滝沢元和, 藤田裕, SIMIONESCU Aurora, 牧島一夫  

    日本天文学会年会講演予稿集2017 巻   頁: 186   2017年8月

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  40. 銀河団中心部でのプラズマの二温度構造:「ひとみ」の測定結果の意義

    牧島一夫, 中島真也, GU Lily, 川原田円, 中澤知洋  

    日本天文学会年会講演予稿集2017 巻   頁: 184   2017年8月

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  41. 軟X線から硬X線の広帯域を高感度で撮像分光する小型衛星計画FORCEの現状(5)

    森浩二, 武田彩希, 村上弘志, 寺田幸功, 久保田あや, 中澤知洋, 馬場彩, 谷津陽一, 幸村孝由, 萩野浩一, 小高裕和, 中島真也, 内山泰伸, 斉藤新也, 北山哲, 高橋忠幸, 石田学, 渡辺伸, 飯塚亮, 古澤彰浩, 鶴剛, 上田佳宏, 田中孝明, 内田裕之, 小林翔悟, 松本浩典, 中嶋大, 常深博, 信川正順, 太田直美, 粟木久光, 寺島雄一, 深沢泰司, 水野恒史, 高橋弘充, 大野雅功, 岡島崇, 山口弘悦, 森英之  

    日本天文学会年会講演予稿集2017 巻   頁: 242   2017年8月

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  42. 矮新星GK PerseiのX線スペクトル解析による白色矮星質量の推定

    和田有希, 和田有希, 湯浅孝行, 中澤知洋, 牧島一夫, 林多佳由, 林多佳由, 石田学  

    日本天文学会年会講演予稿集2017 巻   頁: 275   2017年8月

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  43. 狭輝線I型セイファート銀河NGC4051における一次放射成分の時間変動

    三宅克馬, 野田博文, 山田真也, 清野愛海, 中澤知洋, 牧島一夫  

    日本天文学会年会講演予稿集2017 巻   頁: 175   2017年8月

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  44. 将来の硬X線・ガンマ線衛星に向けたシンチレータ反射材の改良

    清野愛海, 奥田和史, 中澤知洋, 奥村曉, 郡司修一, 牧島一夫  

    日本天文学会年会講演予稿集2017 巻   頁: 242   2017年8月

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  45. 多波長観測から迫る銀河団RXC J1053.7+5453の衝突過程と粒子加速

    板花まどか, 滝沢元和, 赤松弘規, VAN WEEREN R. J, 河原創, 深沢泰司, KAASTRA J. S, 中澤知洋, 大橋隆哉, 太田直美, ROETTGERING H. J. A, VINK J, ZANDANEL F  

    日本天文学会年会講演予稿集2017 巻   頁: 186   2017年8月

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  46. 分子雲衝突に起因する超新星残骸からの宇宙線逃亡シナリオの観測的検証

    鈴木寛大, 馬場彩, 中澤知洋, 山崎了  

    日本天文学会年会講演予稿集2017 巻   頁: 148   2017年8月

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  47. 「ひとみ(ASTRO‐H)」搭載軟ガンマ線検出器における軌道上バックグラウンドの理解

    大野雅功, 深沢泰司, 水野恒史, 高橋弘充, 北口貴雄, 田中康之, 勝田隼一郎, 河野貴文, 幅田翔, 岡田千穂, 大橋礼恵, 寺前拓人, 田中晃司, 高橋忠幸, 国分紀秀, 渡辺伸, 佐藤悟朗, 太田方之, 内田悠介, 都丸亮太, 米田浩基, 小高裕和, 小高裕和, 中澤知洋, 村上浩章, 田島宏康, 木下将臣, 山岡和貴, 林克洋  

    日本天文学会年会講演予稿集2017 巻   頁: 246   2017年8月

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  48. 「すざく」によるKepler超新星残骸の膨張速度測定

    春日知明, 馬場彩, 中澤知洋, 佐藤寿紀  

    日本天文学会年会講演予稿集2017 巻   頁: 147   2017年8月

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  49. 1‐80keVの広帯域X線を高感度で撮像分光する次世代の小型科学衛星計画FORCE:2017年のステータス

    中澤知洋, 森浩二, 村上弘志, 久保田あや, 寺田幸功, 谷津陽一, 馬場彩, 幸村孝由, 内山泰伸, 斉藤新也, 北山哲, 高橋忠幸, 渡辺伸, 中島真也, 萩野浩一, 松本浩典, 古澤彰浩, 鶴剛, 上田佳宏, 田中孝明, 内田裕之, 武田彩希, 常深博, 中嶋大, 信川正順, 太田直美, 粟木久光, 寺島雄一, 深沢泰司, 高橋弘充, 大野雅功, 岡島崇, 山口弘悦, 森英之, 小高裕和  

    日本物理学会講演概要集(CD-ROM)72 巻 ( 1 ) 頁: ROMBUNNO.20aK21‐5   2017年3月

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  50. 長周期の連星X線パルサーは10<sup>13</sup>Gの超強磁場をもつか?

    牧島一夫, 高木利紘, 高木利紘, 笹野理, 三原建弘, 杉崎睦, 谷田部史尭, 谷田部史尭, 中島基樹, 中澤知洋  

    日本物理学会講演概要集(CD-ROM)72 巻 ( 1 ) 頁: ROMBUNNO.17pK41‐8   2017年3月

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  51. GROWTH実験:モンテカルロシミュレーションを用いた,雷雲ガンマ線放射の広がりの解釈

    古田禄大, 楳本大悟, 中澤知洋, 奥田和史, 和田有希, 榎戸輝揚, 湯浅孝行, 土屋晴文, 牧島一夫  

    日本物理学会講演概要集(CD-ROM)72 巻 ( 1 ) 頁: ROMBUNNO.19pK41‐8   2017年3月

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  52. GROWTH実験:コリメーターを用いた雷雲由来ガンマ線の角度分布の測定

    奥田和史, 中澤知洋, 古田禄大, 和田有希, 湯浅孝行, 榎戸輝揚, 鈴木寛大, 楳本大悟, 土屋晴文, 牧島一夫  

    日本物理学会講演概要集(CD-ROM)72 巻 ( 1 ) 頁: ROMBUNNO.19pK41‐9   2017年3月

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  53. GROWTH実験:10年間の継続観測に基づく冬季雷雲由来ガンマ線の研究

    楳本大悟, 土屋晴文, 土屋晴文, 榎戸輝揚, 湯浅孝行, 古田禄大, 奥田和史, 和田有希, 玉川徹, 岡野眞治, 川原田円, 北口貴雄, 岩田憲一, 加藤博, 国分紀秀, 牧島一夫, 牧島一夫, 中澤知洋  

    日本物理学会講演概要集(CD-ROM)72 巻 ( 1 ) 頁: ROMBUNNO.19pK41‐7   2017年3月

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  54. GeVガンマ線超新星残骸HB21のX線観測による過電離プラズマの発見

    鈴木寛大, 馬場彩, 中澤知洋, 澤田真理, 小山勝二  

    日本天文学会年会講演予稿集2017 巻   頁: 141   2017年2月

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  55. 長周期X線パルサーX Perseiが>10<sup>13</sup>Gの超強磁場をもつ可能性

    牧島一夫, 高木利紘, 三原建弘, 杉崎睦, 谷田部史尭, 笹野理, 中澤知洋, 中島基樹  

    日本天文学会年会講演予稿集2017 巻   頁: 250   2017年2月

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  56. 軟X線から硬X線の広帯域を高感度で撮像分光する小型衛星計画FORCEの現状(4)

    森浩二, 村上弘志, 寺田幸功, 久保田あや, 中澤知洋, 馬場彩, 谷津陽一, 幸村孝由, 内山泰伸, 斉藤新也, 北山哲, 高橋忠幸, 渡辺伸, 中島真也, 萩野浩一, 松本浩典, 古澤彰浩, 鶴剛, 上田佳宏, 田中孝明, 内田裕之, 武田彩希, 常深博, 中嶋大, 信川正順, 太田直美, 粟木久光, 寺島雄一, 深沢泰司, 高橋弘充, 大野雅功, 岡島崇, 山口弘悦, 森英之, 小高裕和  

    日本天文学会年会講演予稿集2017 巻   頁: 233   2017年2月

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  57. 超新星残骸SN1006における衝撃波直下での電子加熱と電離速度

    加藤佑一, 勝田哲, 馬場彩, 中澤知洋  

    日本天文学会年会講演予稿集2017 巻   頁: 55   2017年2月

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    記述言語:日本語  

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  58. 衝突銀河団CIZA J1358.9‐4750領域の広がった電波放射の探査

    赤堀卓也, 加藤佑一, 中澤知洋, 小澤武揚, GU Lyli, 滝沢元和, 藤田裕, 中西裕之, 岡部信弘, 牧島一夫  

    日本天文学会年会講演予稿集2017 巻   頁: 190   2017年2月

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  59. 狭輝線1型セイファート銀河NGC 4051のX線時間変動解析 II

    清野愛海, 野田博文, 三宅克馬, 中澤知洋, 牧島一夫  

    日本天文学会年会講演予稿集2017 巻   頁: 180   2017年2月

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  60. すざく衛星によるTriangulum Australis銀河団の超高温領域と非熱的X線放射の探査

    鷹箸颯太, 滝沢元和, 板花まどか, 中澤知洋  

    日本天文学会年会講演予稿集2017 巻   頁: 190   2017年2月

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    記述言語:日本語  

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  61. 「すざく」を用いたLMXBのスペクトル状態遷移の研究 II

    小野光, 牧島一夫, ZHANG Zhongli, 中澤知洋  

    日本天文学会年会講演予稿集2017 巻   頁: 259   2017年2月

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  62. 「すざく」で観測した近傍銀河団・銀河群のエントロピー分布

    佐々木亨, 松下恭子, 佐藤浩介, 横田佳奈, 栗山翼, 菅野祐, 赤松弘規, 藤田裕, 中澤知洋, 岡部信広, 大橋隆哉, 太田直美, 田村隆幸, 滝沢元和  

    日本天文学会年会講演予稿集2017 巻   頁: 186   2017年2月

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    記述言語:日本語  

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  63. SWIFT J2127.4+5654における時間変動を用いたモデル依存しない成分分解

    三宅克馬, 野田博文, 山田真也, 清野愛海, 中澤知洋, 牧島一夫  

    日本天文学会年会講演予稿集2017 巻   頁: 179   2017年2月

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  64. 「ひとみ」搭載硬X線・軟ガンマ線帯観測装置の軌道上性能

    粟木 久光, 松本 浩典, 石田 学, 中澤 知洋, 国分 紀秀, 田島 宏康, 深沢 泰司, 渡辺 伸, 幅 良統, 飯塚 亮, 太田 方之, 佐藤 理江, 高橋 忠幸, 萩野 浩一, 原山 淳, 前田 良知, 吉田 鉄生, 武田 伸一郎, 宮澤 拓也, 榎戸 輝揚, 田中 孝明, 寺田 幸功, 内山 秀樹, 一戸 悠人, 石橋 和紀, 國枝 秀世, 田村 啓輔, 田原 譲, 三石 郁之, 林 克洋, 林 多佳由, 山岡 和貴, 大野 雅功, 北口 貴雄, 高橋 弘充, 田中 康之, 水野 恒史, 杉田 聡司, 谷津 陽一, 野田 博文, 古澤 彰浩, 山内 茂雄, 中森 健之, 中野 俊男, 牧島 一夫, 内山 泰伸, 斉藤 新也, 片岡 淳, Philippe Laurent, Francois Lebrun, Olivier Limousin, 岡島 崇, 森 英之, 小高 裕和, Madejski G., Blanford R., 他「ひとみ」チーム  

    第17回宇宙科学シンポジウム 講演集 = Proceedings of the 17th Space Science Symposium   2017年1月

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    記述言語:日本語   出版者・発行元:宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)  

    第17回宇宙科学シンポジウム (2017年1月5日-6日. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)相模原キャンパス), 相模原市, 神奈川県著者人数: 56名ほか (JAXA staff: Ishida, Manabu ; Kokubun, Motohide ; Watanabe, Shin ; Iizuka, Ryo ; Ohta, Masayuki ; Sato, Rie ; Takahashi, Tadayuki ; Hagino, Koichi ; Harayama, Atsushi ; Maeda, Yoshitomo)資料番号: SA6000060046レポート番号: P-004

    CiNii Article

  65. 雷雲ガンマ線の多地点観測プロジェクト:可搬型検出器の開発と2016年度冬季の観測成果

    和田有希, 榎戸輝揚, 古田禄大, 湯浅孝行, 中澤知洋, 中野俊男, 土屋晴文, 鴨川仁, 米徳大輔, 澤野達哉  

    日本地球惑星科学連合大会予稿集(Web)2017 巻   頁: ROMBUNNO.MIS18‐05 (WEB ONLY)   2017年

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    記述言語:日本語  

    J-GLOBAL

  66. 雷雲ガンマ線の多地点観測プロジェクトが拓く新展開

    榎戸輝揚, 和田有希, 古田禄大, 湯浅孝行, 中澤知洋, 中野俊男, 土屋晴文, 鴨川仁, 米徳大輔, 澤野達哉  

    日本地球惑星科学連合大会予稿集(Web)2017 巻   頁: ROMBUNNO.MIS05‐02 (WEB ONLY)   2017年

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    J-GLOBAL

  67. 雷雲電場による電子加速のガンマ線観測プロジェクト:多地点体制への新展開

    榎戸 輝揚, 牧島 一夫, 鴨川 仁, 瀧田 正人, 米徳 大輔, 澤野 達哉, 渡會 兼也, 米口 一彦, 木村 光一郎, 北野 皓嗣, the GROWTH collaboration, 和田 有希, 湯浅 孝行, 中澤 知洋, 土屋 晴文, 中野 俊男, 奥田 和史, 古田 禄大, 楳本 大悟  

    日本物理学会講演概要集72 巻 ( 0 ) 頁: 502 - 502   2017年

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    記述言語:日本語   出版者・発行元:一般社団法人 日本物理学会  

    <p>雷雲内の強電場で加速された電子からの制動放射ガンマ線を観測するプロジェクトは、2006年に柏崎で観測を開始して以来10年になり、観測事例も蓄積され、基本的な描像は確立しつつある。しかし、電子の加速領域の大きさや継続時間はこれまでの定点観測では把握が難しかったため、石川県内の複数の学校の屋上に、小型で低消費電力の放射線検出器を設置し、マッピング観測を新たに開始した。多地点観測への新展開プロジェクトの狙いと現状を報告する。</p>

    DOI: 10.11316/jpsgaiyo.72.1.0_502

    CiNii Article

    J-GLOBAL

  68. 雷雲電場による電子加速のガンマ線観測プロジェクト:小型読み出し系の開発と北陸地方における多地点運用

    和田 有希, 牧島 一夫, 鴨川 仁, 瀧田 正人, 米徳 大輔, 澤野 達哉, 渡會 兼也, 米口 一彦, 木村 光一郎, 北野 皓嗣, the GROWTH collaboration, 榎戸 輝揚, 湯浅 孝行, 中澤 知洋, 土屋 晴文, 中野 俊男, 奥田 和史, 古田 禄大, 楳本 大悟  

    日本物理学会講演概要集72 巻 ( 0 ) 頁: 503 - 503   2017年

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    記述言語:日本語   出版者・発行元:一般社団法人 日本物理学会  

    <p>雷雲ガンマ線の観測プロジェクトは2015年度より多地点によるマッピング観測を目指し、石川県でも展開を進めている。初年度の運用実績や成果を元にしてADC/FPGAによる読み出し系の改良を中心に開発を行い、小型ガンマ線検出器の台数を増やしつつある。これらの検出器は金沢市内、小松市内、及び柏崎刈羽原発内に設置し、マッピング観測を本格的に開始している。本講演では小型検出器の開発状況、および今年度の運用状況・成果について報告する。</p>

    DOI: 10.11316/jpsgaiyo.72.1.0_503

    CiNii Article

    J-GLOBAL

▼全件表示

共同研究・競争的資金等の研究課題 1

  1. 相対論的電子を生む自然界唯一の静電場加速器は雷雲のどこにあるのか?

    2020年4月 - 2021年3月

    研究助成 

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    配分額:1000000円

科研費 7

  1. 高速半導体イメージャによる雷からのMeVガンマ線フラッシュの精密探査

    研究課題/研究課題番号:21H00166  2021年4月 - 2023年3月

    科学研究費助成事業  新学術領域研究(研究領域提案型)

    中澤 知洋

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    担当区分:研究代表者 

    配分額:6630000円 ( 直接経費:5100000円 、 間接経費:1530000円 )

    雷放電に伴って観測される突発MeVガンマ線は高い光度を持ち、電子が大規模に静電場加速を受けている直接証拠であるが、加速メカニズムはまだ理解されていない。今大事なことは、加速現場の位置を知り、観測の環境を同定することである。しかし極限の高輝度環境の中で~10 MeVガンマ線の入射方向を検知できる装置は既存では存在しない。TimePix3 高速半導体イメージャは、~50 umの精度での3次元トラック能力を有しており、10~MeVガンマ線による電子陽電子対生成をトラックして入射方向を検出できる。その検出方法を確立し、現在北陸に展開中の雷ガンマ線観測装置の小屋にこれを追加して、実観測に臨む。

  2. 半導体コンプトンカメラによるMeV宇宙観測の開拓

    研究課題/研究課題番号:20H00157  2020年4月 - 2024年3月

    科学研究費助成事業  基盤研究(A)

    中澤 知洋, 武田 伸一郎

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    担当区分:研究代表者 

    配分額:44850000円 ( 直接経費:34500000円 、 間接経費:10350000円 )

    最初の2年間は、地上においてSi/CdTe-SCTとシールドを組み合わせた試作検出器を開発し、地上試験を中心にその性能評価を進める。気球搭載のためには、コンパクトかつ低消費電力であることが重要である。研究計画の後半の2年間では、この検出器を改良して大気球用のゴンドラに搭載し、海外の長時間気球への搭載を調整するのと並行して、国内での調整も進め、短時間で良いので高度35-50 km の大気球高度にあげて、その高度でのバックグラウンドなどの観測性能を実証する。このため、2年目ごろから気球実験の視察や、海外コラボレータとの連携による超長時間気球へのチャレンジも進める。

  3. 雷ガンマ線フラッシュを航空機から捉える高時間分解能でのガンマ線撮像への挑戦

    研究課題/研究課題番号:19K21899  2019年6月 - 2021年3月

    挑戦的研究(萌芽)

    中澤 知洋

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    担当区分:研究代表者 

    配分額:6370000円 ( 直接経費:4900000円 、 間接経費:1470000円 )

    雷雲や雷放電から到来する20 MeVに達するガンマ線は、雷雲中に天然の静電場粒子加速器という、自然界で他には見られない現象がある証拠である。宇宙から観測される地球由来の突発ガンマ線が、もし雷雲中の数百mのコンパクトな加速域から放射されていると、そこでの放射線量は非常に大きくなる。科学的な興味だけでなく、航空機への被曝なども無視し得ない可能性もある。しかしあまりに大強度なため、観測装置が飽和しない独特の工夫が必要である。本研究では、地上での雷ガンマ線観測の実績に基づき、あらたにチェレンコフ光検出技術も融合し、ガンマ線を一つ一つ捉え、その到来方向も知る軽量小型の装置を開発する。
    雷雲や雷放電から到来する20 MeVに達するガンマ線は、雷雲中に天然の静電場粒子加速器という、自然界で他には見られない現象がある証拠である。地球由来の突発ガンマ線(Terrestrial Gamma-ray Flash, TGF)は、高度 600-800 km の衛星軌道から観測される場合、100 us 程度の間に10-100個ほどの光子が検出される。Downward TGFと呼ばれる、地上で観測されるケースでは、雷雲から検出器までの距離が 1 km 程度まで近づくため、その強度は数十万倍となり、100 usの間に1マイクログレイに達することが分かっている(e.g. Wada et al. 2019)。さらに、ここからスケールすると、もし雷雲中の~百mのコンパクトな加速域からガンマ線が放射されており、これが数百mの近距離を飛ぶ航空機に照射されると、その放射線量は非常に大きくなる。この短時間にこの強度のガンマ線が照射されると、通常のガンマ線検出器では回路が飽和してしまうため、正確な測定は容易ではない一方で、大量の信号があることは、正しく計測さえできれば、粒子加速の物理を研究する上で非常に有望なターゲットであることも意味する。そこで、大強度なガンマ線が来てもなお、観測装置が飽和しない独特の工夫が重要である。本研究では、あらたにチェレンコフ光を用いたガンマ線検出技術を導入し、ガンマ線を一つ一つ捉え、その到来方向も知る軽量小型装置の開発を目指すものである。2019年度はその立ち上げとして、チェレンコフ光を発生させるPbF4結晶やアクリル、光検出のための半導体光センサー、これを固定する読み出し基板、その後段のアナログおよびADC回路を購入し、実験の準備を進めた。
    2020年5月に予定する兵庫県立大のシンクロトン光設備ニュースバルでの実験を計画しており、この実験へ向けて、装置を組み立て試作機を動作させる予定であった。物品の手配や基板実装など、2020年1月ごろまではほぼ予定通り進めてきたが、2020年3月に実施する予定であった、これらを組み立てた上での総合試験が実施できていない。これは、今回のCOVID19問題への対策(リモート研究および教育への対応準備)を優先させたこと、大学への入校が一時期制限されたことの影響であり、止むを得ないことと考えている。現時点でも、装置一式は組み上げと初期動作試験を待つだけの状態で、実験室に保管されている状態である。これに対応し、3月分の研究を2020年度に繰り越すこととした。
    2020年度は、大学の入校解除がなされ次第、この試作機を組み上げて実験室レベルで、ミューオンや、中性子線源由来の数MeVガンマ線を用いて、できる実験を進めることとする。重要なマイルストーンである、兵庫県立大のシンクロトン光設備ニュースバルでの実験については、今後の施設の運用状況次第である。また2020年冬期には、ニュースバル実験と干渉しない限りにおいて、この試作機を実際に冬季の日本海岸での雷観測に投入することも検討する。

  4. 雷や雷雲中の電子加速に由来する光核反応の検証

    研究課題/研究課題番号:18H01236  2018年4月 - 2021年3月

    土屋 晴文

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    担当区分:研究分担者 

    雷や雷雲から10 MeV に達するような高エネルギー制動放射線が観測されている。こうした制動放射線は電子が雷や雷雲の中で高エネルギーに加速されたことで作られるため、制動放射線の詳細観測により、雷や雷雲中での電子の加速メカニズムの理解を推し進めることができる。驚くべきことに、近年の観測により、雷の中で高エネルギーの制動放射線をきっかけとして大気中の窒素や酸素から中性子が剥ぎ取られる光核反応が起こっていることが明らかになった。しかしながら、光核反応の発生メカニズムや発生条件は、まだよく理解されていない。
    雷や雷雲中での光核反応の詳細をより理解するために、2019年度に日本海沿岸の柏崎刈羽原子力発電所や大学、高校などに、ガンマ線及び中性子検出器などを30台以上設置し、光核反応を引き起こしたと考えられる現象を確認した。また、装置開発を進める一方で過去に得られたデータを解析した結果、雷から地上に向けて発せられる制動放射線(ガンマ線フラッシュ)が光核反応の発生に大きく寄与していることが分かってきた[たとえば、Wada et al. (PRL 2019)]。さらに原子力発電所のモニタリングポストのデータも活用し、ガンマ線フラッシュの発生高度(2500 ± 500 m)や制動放射線を放つ電子の総数(およそ8x10^18個)を見積もり、はじめて地上に向けて発せられるガンマ線フラッシュに関する定量評価を行った。
    ガンマ線フラッシュでは莫大な制動放射線が発生するため、通常、我々が使用する検出器を飽和させてしまう。2019年度、この困難を克服するための時間分解能に優れた検出器の開発を行い、実際に観測を行った。また、光核反応の発生にともなうガンマ線の輝線(即発ガンマ線)を捉える装置も展開した。得られたデータから装置の改良点などを洗い出すことができ、今後の装置性能の向上に繋がるデータを取得できた。
    2019年度には、光核反応に由来する即発ガンマ線や中性子の検出に狙いを定めたCeBrシンチレータやGSOシンチレータ、EJ270シンチレータを搭載した検出器を含め装置を開発し、日本海沿岸地域の複数箇所に装置を展開した。また、光核反応を引き起こすガンマ線フラッシュに特化した検出器の開発及びそれを用いた観測とともに、雷や雷雲の発生点の情報を探るための鉛コリメータを有した検出器の開発及び観測も行った。
    2019年度の気候は暖冬傾向であったため、放射線の増大現象の観測例は少なかった。その中で、光核反応の兆候を示す現象を確認し、2020年春の日本物理学会にて発表を予定していたが、コロナ感染症の拡大防止の一環で日本物理学会は中止となった。この現象に関しては論文投稿に向けて解析を進めている。
    日本海沿岸の冬の雷のみならず、夏の雷からの放射線観測のため、スカイツリーにも放射線観測装置を設置することができ、観測を実施した。2020年度の観測体制の拡張に向けたデータを取得できた。
    2018年度までに得られたデータの解析を実施し論文としてまとめ、3本の査読付き論文を発表した。これらの論文では、光核反応のきっかけとなるガンマ線フラッシュの発生高度や寄与した電子数の推定に加えて、電波観測との同時観測により雷の進展との比較を行い、光核反応の発生メカニズムや条件の理解が進んだ。
    光核反応で生成される中性子及び即発ガンマ線の検出のため、中性子及びガンマ線を効率的に弁別できる、あるいはエネルギー分解能を向上させるなど検出器の高度化を行い、そうした検出器を日本海側地域へ展開していく。2019年度には、20台以上の装置を共同研究者らと設置し、2020年度においては装置台数をさらに増加させる予定である。また、光核反応を引き起こすガンマ線フラッシュの実態の解明に向けて、時間応答に優れた測定システムを構築していく。こうした取り組みを通して、光核反応の発生メカニズムや条件の理解を進めることが可能な観測体制を整えていく。
    装置開発に加えて、近年のデジタル技術の進展を取り入れたソフト的な解析手法の開発も行っていく。具体的には、波形弁別や機械学習を用いた中性子及びガンマ線の効率的な分離を目指す。
    冬の雷のみならず、夏の雷もターゲットとした装置展開を推進していく。冬の雷と比べて夏の雷の発生高度は、通常1 km 以上となる。そのため、装置を高所に設置していく必要があるが、すでに展開済のスカイツリーや、過去に展開経験のある高山の観測所などを含めて拡張を考えていく。

  5. 銀河団衝突の初期に解放される莫大な重力エネルギーの行方の観測

    研究課題/研究課題番号:15H03639  2015年4月 - 2018年3月

    中澤 知洋

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    担当区分:研究代表者 

    配分額:16380000円 ( 直接経費:12600000円 、 間接経費:3780000円 )

    宇宙最大の天体、銀河団が衝突・合体する時に解放される莫大なエネルギーが、高温ガスの加熱、乱流の励起、さらに粒子加速や磁場増幅にどのように使われるかを知るために2つの研究を行なった。衝突銀河団CIZA J1358,9-4750を複数のX線天文衛星と電波天文台で観測し、衝突の初期段階にあること、それにも関わらず複雑な構造を持つことを確認した。並行して超精密分光によるドップラー観測と、高感度硬X線観測による加熱の観測精度向上を目指し、ASRTO-H衛星での観測を目指した。観測はできなかったものの、軌道上でASTRO-Hの硬X線観が世界最高感度にあることを実証し、将来検出器への指針を得た。
    宇宙最大の天体が合体する「銀河団衝突」の中では、莫大なエネルギーが解放され、加熱、乱流、粒子加速などが起きる。しかし、そのエネルギーがどこへ行くかは解明されていない。既存のX線衛星、電波観測で研究を続けつつ、最新のX線衛星ASTRO-Hで、運動エネルギーや加熱をかつてない精度で観測することを目指した。2016年2月に打ち上げられ、担当していた硬X線検出器も世界最高の感度を達成したが、衛星喪失による本格観測には至らなかった。しかし、これまで難しいとされてきた硬X線での高感度観測のレシピを確立し実証できたことで、将来計画をより高性能にできる。

  6. マグネターの 自由歳差運動の観測と内部磁場の推定

    研究課題/研究課題番号:15H03653  2015年4月 - 2018年3月

    牧島 一夫

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    担当区分:研究分担者 

    我々は2つのマグネターで硬X線パルスが、パルス周期の1万倍程度の長周期で位相変調を受けていることを発見した。これは内部の強いトロイダル磁場により、これら中性子星が僅か変形して自由歳差運動が起き、それと自転周期とのうなりが現れたと解釈された。本研究では米国NuSTAR衛星のデータを用い、これら2天体で現象が再確認されたが、変調振幅は「すざく」の値と大幅に変化していた。「すざく」で観測された別のマグネターからは、周期 48 ksで硬X線パルスの位相変調が検出された。MAXIを用いX線パルサーの光度とパルス周期変化率の相関を調べた結果、X Perseiはマグネター並の超強磁場を持つことが判明した。

  7. 次世代多波長観測と理論シミュレーションの連携で解明する銀河団の非熱的現象

    研究課題/研究課題番号:26400218  2014年4月 - 2018年3月

    滝沢 元和

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    担当区分:連携研究者 

    X線と電波観測により銀河団電波レリックでの粒子加速過程とその物理状態を解明し、理論モデルの構築を行った。特にtoothbrush電波レリックでの粒子加速過程が単純な衝撃波統計加速では説明のつかないことを明らかにした。ALMAを用いて5秒角というこれまでにない空間分解能のSZ効果観測をおこない、RX J1347.5-1145銀河団の超高温成分がX線ピークと異なる場所にあることを明確に示した。低周波電波での宇宙磁場研究についてPASJ誌の招待レビュー論文に対して、銀河団のパートなどに分担執筆者として貢献をした。

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