Faculty Profiles - NAKAZAWA Kazuhiro

写真a

NAKAZAWA Kazuhiro

Organization

Kobayashi-Maskawa Institute for the Origin of Particles and the Universe (KMI) Associate professor

Graduate School

Graduate School of Science

External link

Degree 1

博士(理学) （ 2001.3 東京大学）

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Research Interests 8

宇宙物理
ブラックホール
人工衛星
X線
clusters of galaxies
hard X-ray
gamma ray
X-ray astronomy

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Research Areas 2

Natural Science / Theoretical studies related to particle-, nuclear-, cosmic ray and astro-physics
Natural Science / Astronomy

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Current Research Project and SDGs 2

雷雲中での粒子加速とガンマ線放射の研究
宇宙X線MeVガンマ線観測

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Research History 2

The University of Tokyo Lecturer

2007.4 - 2017.12

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Country：Japan
JAXA 宇宙科学研究所助教

2001.7 - 2007.3

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Country：Japan

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Education 1

The University of Tokyo Graduate School, Division of Science

1996.4 - 2001.3

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Country： Japan

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Professional Memberships 3

日本地球惑星科学連合

2019.1
日本天文学会
日本物理学会

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Papers 116

A broadband x-ray imaging spectroscopy in the 2030s: the FORCE mission

Koji Mori, Takeshi G. Tsuru, Kazuhiro Nakazawa, Yoshihiro Ueda, Shin Watanabe, Takaaki Tanaka, Manabu Ishida, Hironori Matsumoto, Hisamitsu Awaki, Hiroshi Murakami, Masayoshi Nobukawa, Ayaki Takeda, Yasushi Fukazawa, Hiroshi Tsunemi, Tadayuki Takahashi, Ann E. Hornschemeier, Takashi Okajima, William W. Zhang, Brian J. Williams, Tonia Venters, Kristin Madsen, Mihoko Yukita, Hiroki Akamatsu, Aya Bamba, Teruaki Enoto, Yutaka Fujita, Akihiro Furuzawa, Kouichi Hagino, Kosei Ishimura, Masayuki Itoh, Tetsu Kitayama, Shogo B. Kobayashi, Takayoshi Kohmura, Aya Kubota, Misaki Mizumoto, Tsunefumi Mizuno, Hiroshi Nakajima, Kumiko K. Nobukawa, Hirofumi Noda, Hirokazu Odaka, Naomi Ota, Toshiki Sato, Megumi Shidatsu, Hiromasa Suzuki, Hiromitsu Takahashi, Atsushi Tanimoto, Yukikatsu Terada, Yuichi Terashima, Hiroyuki Uchida, Yasunobu Uchiyama, Hiroya Yamaguchi, Yoichi Yatsu

Space Telescopes and Instrumentation 2022: Ultraviolet to Gamma Ray 2022.8

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Publishing type：Research paper (international conference proceedings) Publisher：SPIE

DOI： 10.1117/12.2628772
The Compton Spectrometer and Imager Project for MeV Astronomy

Tomsick J.A., Boggs S.E., Zoglauer A., Wulf E., Mitchell L., Phlips B., Sleator C., Brandt T., Shih A., Roberts J., Jean P., von Ballmoos P., Oliveros J.M., Smale A., Kierans C., Hartmann D., Leising M., Ajello M., Burns E., Fryer C., Saint-Hilaire P., Malzac J., Tavecchio F., Fioretti V., Bulgarelli A., Ghirlanda G., Chang H.K., Takahashi T., Nakazawa K., Matsumoto S., Melia T., Siegert T., Lowell A., Lazar H., Beechert J., Gulick H.

Proceedings of Science Vol. 395 2022.3

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Publisher：Proceedings of Science

The Compton Spectrometer and Imager (COSI) is a 0.2-5 MeV Compton telescope capable of imaging, spectroscopy, and polarimetry of astrophysical sources. Such capabilities are made possible by COSI's germanium cross-strip detectors, which provide high efficiency, high resolution spectroscopy and precise 3D positioning of photon interactions. Science goals for COSI include studies of 0.511 MeV emission from antimatter annihilation in the Galaxy, mapping radioactive elements from nucleosynthesis, determining emission mechanisms and source geometries with polarization, and detecting and localizing multimessenger sources. The instantaneous field of view (FOV) for the germanium detectors is >25% of the sky, and they are surrounded on the sides and bottom by active shields, providing background rejection as well as allowing for detection of gamma-ray bursts or other gamma-ray flares over >50% of the sky. We have completed a Phase A concept study to consider COSI as a Small Explorer (SMEX) satellite mission, and here we discuss the advances COSI-SMEX provides for astrophysics in the MeV bandpass.

Scopus
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 Vol. 4 ( 2 ) 2018.4

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Language：Japanese Publishing type：Research paper (scientific journal) Publisher：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

Scopus
Discovery of diffuse radio source in Abell 1060

Kurahara, K; Akahori, T; Oki, A; Omiya, Y; Nakazawa, K

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 2024.2

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DOI： 10.1093/pasj/psae011

Web of Science
Relativistic Runaway Electron Avalanche Development Near the Electric Field Threshold in Inhomogeneous Air Reviewed

G. S. Diniz, Y. Wada, Y. Ohira, K. Nakazawa, M. Tsurumi, T. Enoto

Geophysical Research Letters Vol. 50 ( 20 ) 2023.10

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Publishing type：Research paper (scientific journal) Publisher：American Geophysical Union (AGU)

Abstract

Relativistic Runaway Electrons Avalanches (RREAs) development depends on the applied electric field and the environment's air density. This dependency controls the RREA exponential growth length scale. The RREA development affects the bremsstrahlung excess occurring due to the passage of charged particles through the thundercloud's electric fields, the gamma‐ray glow. We used Monte Carlo simulations to develop an empirical model showing the RREA behavior in a realistic atmospheric density profile. The new formulation shows how the density variation modulates the electron population under electric field strengths near the RREA electric field threshold. The model limits the initial RREA altitude range as a function of the electric field strength. The new model is valid between ∼0.6 and ∼18 km, covering the relevant heights to investigate the generation of ground‐detected gamma‐ray glows.

DOI： 10.1029/2023GL105087

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An engineering balloon-borne test of a liquid argon radiation detector for the GRAMS experiment (1): overview

ODAKA Hirokazu, HAKAMADA Tomoaki, YOSHITOMO Marina, AOYAMA Kazutaka, UTSUMI Yorinobu, TANAKA Masashi, NAKAJIMA Riki, YORITA Kohei, ARAI Shota, KATO Tatsuaki, TAKASHIMA Satoshi, BAMBA Aya, TAMBA Tsubasa, TSUJI Naomi, ARAMAKI Tsuguo, TAKAHASHI Hiromitsu, OKUMA Keigo, NAKAZAWA Kazuhiro

Balloon Symposium: 2023 2023.10

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Language：Japanese

CiNii Research
sub-MeV imaging observation using balloon-borne narrow field-of-view semiconductor Compton camera

NAKAZAWA Tomohiro, TAKEDA Shin'ichiro, OKUMA Keigo, ANDO Miyu, WATANABE Shin, TAKAHASHI Tadayuki, KOBAYASHI Masahiko, ISHIDA Naoki, OGUCHI Manari, TANAKA Atsuya, NISHIMURA Yuta, ONISHI Mitsunobu, ARAI Toshihiko

Balloon Symposium: 2023 2023.10

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Language：Japanese

CiNii Research
An engineering balloon-borne test of a liquid argon radiation detector for the GRAMS experiment (2): Results of the flight

AOYAMA Kazutaka, UTSUMI Yorinobu, TANAKA Masashi, NAKAJIMA Riki, YORITA Kohei, ODAKA Hirokazu, HAKAMADA Tomoaki, YOSHITOMO Marina, ARAI Shota, KATO Tatsuaki, TAKASHIMA Satoshi, BAMBA Aya, TAMBA Tsubasa, TSUJI Naomi, ARAMAKI Tsuguo, TAKAHASHI Hiromitsu, OKUMA Keigo, NAKAZAWA Kazuhiro

Balloon Symposium: 2023 2023.10

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Language：Japanese

CiNii Research
GRBAlpha: The smallest astrophysical space observatory

Pál, A; Ohno, M; Mészáros, L; Werner, N; Rípa, J; Csák, B; Dafciková, M; Frajt, M; Fukazawa, Y; Hanak, P; Hudec, J; Husáriková, N; Kapus, J; Kasal, M; Kolár, M; Koleda, M; Laszlo, R; Lipovsky, P; Mizuno, T; Münz, F; Nakazawa, K; Rezenov, M; Smelko, M; Takahashi, H; Topinka, M; Urbanec, T; Breuer, JP; Bozóki, T; Dálya, G; Enoto, T; Frei, Z; Friss, G; Galgóczi, G; Hroch, F; Ichinohe, Y; Kapás, K; Kiss, LL; Matake, H; Odaka, H; Poon, H; Povalac, A; Takátsy, J; Torigoe, K; Uchida, N; Uchida, Y

ASTRONOMY & ASTROPHYSICS Vol. 677 2023.8

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Publisher：Astronomy and Astrophysics

Aims. Since it launched on 22 March 2021, the 1U-sized CubeSat GRBAlpha operates and collects scientific data on high-energy transients, making it the smallest astrophysical space observatory to date. GRBAlpha is an in-orbit demonstration of a gamma-ray burst (GRB) detector concept suitably small to fit into a standard 1U volume. As was demonstrated in a companion paper, GRBAlpha adds significant value to the scientific community with accurate characterization of bright GRBs, including the recent outstanding event of GRB 221009A. Methods. The GRB detector is a 75 × 75 × 5 mm CsI(Tl) scintillator wrapped in a reflective foil (ESR) read out by an array of SiPM detectors, multi-pixel photon counters by Hamamatsu, driven by two separate redundant units. To further protect the scintillator block from sunlight and protect the SiPM detectors from particle radiation, we applied a multi-layer structure of Tedlar wrapping, anodized aluminium casing, and a lead-alloy shielding on one edge of the assembly. The setup allows observations of gamma radiation within the energy range of 70- 890 keV with an energy resolution of ~30%. Results. Here, we summarize the system design of the GRBAlpha mission, including the electronics and software components of the detector, some aspects of the platform, and the current semi-autonomous operations. In addition, details are given about the raw data products and telemetry in order to encourage the community to expand the receiver network for our initiatives with GRBAlpha and related experiments.

DOI： 10.1051/0004-6361/202346182

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The peak flux of GRB 221009A measured with GRBAlpha

Rípa, J; Takahashi, H; Fukazawa, Y; Werner, N; Münz, F; Pál, A; Ohno, M; Dafcíková, M; Meszáros, L; Csák, B; Husáriková, N; Kolár, M; Galgóczi, G; Breuer, JP; Hroch, F; Hudec, J; Kapus, J; Frajt, M; Rezenov, M; Laszlo, R; Koleda, M; Smelko, M; Hanák, P; Lipovsky, P; Urbanec, T; Kasal, M; Povalac, A; Uchida, Y; Poon, H; Matake, H; Nakazawa, K; Uchida, N; Bozóki, T; Dálya, G; Enoto, T; Frei, Z; Friss, G; Ichinohe, Y; Kapás, K; Kiss, LL; Mizuno, T; Odaka, H; Takátsy, J; Topinka, M; Torigoe, K

ASTRONOMY & ASTROPHYSICS Vol. 677 2023.8

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Publisher：Astronomy and Astrophysics

Context. On 2022 October 9 the brightest gamma-ray burst (GRB) ever observed lit up the high-energy sky. It was detected by a multitude of instruments, attracting the close attention of the GRB community, and saturated many detectors. Aims. GRBAlpha, a nano-satellite with a form factor of a 1U CubeSat, detected this extraordinarily bright long-duration GRB, GRB 221009A, without saturation but affected by pile-up. We present light curves of the prompt emission in 13 energy bands, from 80 keV to 950 keV, and performed a spectral analysis to calculate the peak flux and peak isotropic-equivalent luminosity. Methods. Since the satellite s attitude information is not available for the time of this GRB, more than 200 incident directions were probed in order to find the median luminosity and its systematic uncertainty. Results. We find that the peak flux in the 80-800 keV range (observer frame) was Fph p = 1300+ -1200 200 ph cm-2 s-1, or Ferg p = 5:7+ -3 0::7 7×10-4 erg cm-2 s-1, and the fluence in the same energy range of the first GRB episode, which lasted 300 s and was observable by GRBAlpha, was S = 2:2+1:4 -0:3 × 10-2 erg cm-2, or S bol = 4:9+0:8 -0:5 × 10-2 erg cm-2 for the extrapolated range of 0:9-8690 keV. We infer the isotropic-equivalent released energy of the first GRB episode to be Eiso bol = 2:8+ -0 0::8 5 × 1054 erg in the 1-10 000 keV band (rest frame at z = 0:15). The peak isotropic-equivalent luminosity in the 92-920 keV range (rest frame) was Liso p = 3:7+ -2 0::5 5 × 1052 erg s-1, and the bolometric peak isotropic-equivalent luminosity was Lp;bol iso = 8:4+-21::55 × 1052 erg s-1 (4 s scale) in the 1-10 000 keV range (rest frame). The peak emitted energy is Ep*= Ep(1 + z) = 1120 ± 470 keV. Our measurement of Lp;bol iso is consistent with the Yonetoku relation. It is possible that, due to the spectral evolution of this GRB and the orientation of GRBAlpha at the peak time, the true values of peak flux, fluence, Liso, and Eiso are even higher.

DOI： 10.1051/0004-6361/202346128

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Development of miniSGD, a proof-of-concept balloon experiment for a narrow field of view Si/CdTe semiconductor Compton telescope

Keigo Okuma, Kazuhiro Nakazawa, Shin'ichiro Takeda, Mii Ando, Yuki Omiya, Manari Oguchi, Atsuya Tanaka, Yuna Tsuji, Shin Watanabe, Tadayuki Takahashi, Masahiko Kobayashi, Naoki Ishida, Takahiro Minami, Mitsunobu Onishi, Toshihiko Arai

Proceedings of 38th International Cosmic Ray Conference — PoS(ICRC2023) 2023.8

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Publishing type：Research paper (international conference proceedings) Publisher：Sissa Medialab

DOI： 10.22323/1.444.0899
Termination of Downward‐oriented Gamma‐ray Glow by Normal‐polarity In‐cloud Discharge Activity

Y. Wada, T. Wu, D. Wang, T. Enoto, K. Nakazawa, T. Morimoto, Y. Nakamura, T. Shinoda, H. Tsuchiya

Journal of Geophysical Research: Atmospheres Vol. 128 ( 15 ) 2023.8

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Publishing type：Research paper (scientific journal) Publisher：American Geophysical Union (AGU)

DOI： 10.1029/2023JD038606

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Citizen science "Thundercloud Project" -- multi-point radiation measurements of gamma-ray glows from accelerated electrons in thunderstorms

Teruaki Enoto, Miwa Tsurumi, Yuko Ikkatai, Ting Wu, Daohong Wang, Taro Shinoda, Kazuhiro Nakazawa, Naoki Tsuji, Gabriel Diniz, Jun Kataoka, Masashi Kamogawa, Toru Takagaki, Shoko Miyake, Takeshi Morimoto, Yoshitaka Nakamura, Harufumi Tsuchiya

Proceedings of 38th International Cosmic Ray Conference — PoS(ICRC2023) 2023.8

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Publishing type：Research paper (international conference proceedings) Publisher：Sissa Medialab

DOI： 10.22323/1.444.1607
Citizen Science Observation of a Gamma‐Ray Glow Associated With the Initiation of a Lightning Flash

M. Tsurumi, T. Enoto, Y. Ikkatai, T. Wu, D. Wang, T. Shinoda, K. Nakazawa, N. Tsuji, G. S. Diniz, J. Kataoka, N. Koshikawa, R. Iwashita, M. Kamogawa, T. Takagaki, S. Miyake, D. Tomioka, T. Morimoto, Y. Nakamura, H. Tsuchiya

Geophysical Research Letters Vol. 50 ( 13 ) 2023.7

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Publishing type：Research paper (scientific journal) Publisher：American Geophysical Union (AGU)

DOI： 10.1029/2023GL103612

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Citizen Science Observation of a Gamma‐Ray Glow Associated With the Initiation of a Lightning Flash

Tsurumi M., Enoto T., Ikkatai Y., Wu T., Wang D., Shinoda T., Nakazawa K., Tsuji N., Diniz G. S., Kataoka J., Koshikawa N., Iwashita R., Kamogawa M., Takagaki T., Miyake S., Tomioka D., Morimoto T., Nakamura Y., Tsuchiya H.

Geophysical Research Letters Vol. 50 ( 13 ) 2023.7

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Language：English

Gamma-ray glows are observational evidence of relativistic electron acceleration due to the electric field in thunderclouds. However, it is yet to be understood whether such relativistic electrons contribute to the initiation of lightning discharges. To tackle this question, we started the citizen science “Thundercloud Project, ” where we map radiation measurements of glows from winter thunderclouds along Japan's sea coast area. We developed and deployed 58 compact gamma-ray monitors at the end of 2021. On 30 December 2021, five monitors simultaneously detected a glow with its radiation distribution horizontally extending for 2 km. The glow terminated coinciding with a lightning flash at 04:08:34 JST, which was recorded by the two radio-band lightning mapping systems, FALMA and DALMA. The initial discharges during the preliminary breakdown started above the glow, that is, in vicinity of the electron acceleration site. This result provides one example of possible connections between electron acceleration and lightning initiation.

CiNii Research
Ambient Conditions of Winter Thunderstorms in Japan to Reproduce Observed Gamma‐Ray Glow Energy Spectra

G. S. Diniz, Y. Wada, Y. Ohira, K. Nakazawa, M. Tsurumi, T. Enoto

Journal of Geophysical Research: Atmospheres Vol. 128 ( 10 ) 2023.5

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Publishing type：Research paper (scientific journal) Publisher：American Geophysical Union (AGU)

DOI： 10.1029/2022JD038246

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Diffuse radio source candidate in CIZA J1358.9−4750

Kohei Kurahara, Takuya Akahori, Ruta Kale, Hiroki Akamatsu, Yutaka Fujita, Liyi Gu, Huib Intema, Kazuhiro Nakazawa, Nobuhiro Okabe, Yuki Omiya, Viral Parekh, Timothy Shimwell, Motokazu Takizawa, Reinout J Van Weeren

Publications of the Astronomical Society of Japan Vol. 75 ( Supplement_1 ) page： S138 - S153 2023.2

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Publishing type：Research paper (scientific journal) Publisher：Oxford University Press (OUP)

Abstract

We report on results of our upgraded Giant Metrewave Radio Telescope (uGMRT) observations for an early-stage merging galaxy cluster, CIZA J1358.9−4750 (CIZA1359), in Band-3 (300–500 MHz). We achieved the image dynamic range of ∼38000 using the direction dependent calibration and found a candidate of diffuse radio emission at 4σrms significance. The flux density of the candidate at 400 MHz, 24.04 ± 2.48 mJy, is significantly positive compared to noise, where its radio power, 2.40 × 1024 W Hz−1, is consistent with those of typical diffuse radio sources of galaxy clusters. The candidate is associated with a part of the X-ray shock front at which the Mach number reaches its maximum value of $\mathcal {M}\sim 1.7$. The spectral index (Fν ∝ να) of the candidate, α = −1.22 ± 0.33, is in agreement with an expected value derived from the standard diffusive shock acceleration (DSA) model. However, such a low Mach number with a short acceleration time would require seed cosmic rays supplied from active galactic nucleus (AGN) activities of member galaxies, as suggested in some other clusters. Indeed, we found seven AGN candidates inside the diffuse source candidate. Assuming the energy equipartition between magnetic fields and cosmic rays, the magnetic field strength of the candidate was estimated to be 2.1 μG. We also find head–tail galaxies and radio phoenixes or fossils near CIZA1359.

DOI： 10.1093/pasj/psac098

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XMM-Newton view of the shock heating in an early merging cluster, CIZA J1358.9$-$4750 Reviewed

Y. Omiya, K. Nakazawa, K. Matsushita, S. B. Kobayashi, N. Okabe, K. Sato, T. Tamura, Y. Fujita, L. Gu, T. Kitayama, T. Akahori, K. Kurahara, T. Yamaguchi

Vol. 75 ( 1 ) page： 37 - 51 2023.2

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CIZA J1358.9-4750 is a nearby galaxy cluster in the early phase of a major
merger. The two-dimensional temperature map using XMM-Newton EPIC-PN
observation confirms the existence of a high temperature region, which we call
the "hot region", in the "bridge region" connecting the two clusters. The ~ 500
kpc wide region between the southeast and northwest boundaries also has higher
pseudo pressure compared to the unshocked regions, suggesting the existence of
two shocks. The southern shock front is clearly visible in the X-ray surface
brightness image and has already been reported by Kato et al. (2015). The
northern one, on the other hand, is newly discovered. To evaluate their Mach
number, we constructed a three-dimensional toy merger model with overlapping
shocked and unshocked components in line of sight. The unshocked and preshock
ICM conditions are estimated based on those outside the interacting bridge
region assuming point symmetry. The hot region spectra are modeled with
two-temperature thermal components, assuming that the shocked condition follows
the Rankin-Hugoniot relation with the preshock condition. As a result, the
shocked region is estimated to have a line-of-sight depth of ~ 1 Mpc with a
Mach number of ~ 1.3 in the southeast shock and ~ 1.7 in the northwest shock.
The age of the shock waves is estimated to be ~ 260 Myr. This three dimensional
merger model is consistent with the Sunyaev-Zeldovich signal obtained using the
Planck observation within the CMB fluctuations. The total flow of the kinetic
energy of the ICM through the southeast shock was estimated to be ~ 2.2 x
$10^{42}$ erg/s. Assuming that 10 % of this energy is converted into ICM
turbulence, the line-of-sight velocity dispersion is calculated to be ~ 200
km/s, which is basically resolvable via coming high spectral resolution
observations.

DOI： 10.1093/pasj/psac087

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arXiv

Other Link： http://arxiv.org/pdf/2210.02145v2
Solar Neutron and Gamma-ray Spectroscopy Mission: SONGS

Yamaoka K., Tajima H., Nobashi D., Usami M., Miyata K., Inamori T., Park J.H., Ito K., Matsushita K., Watabe T., Nakazawa K., Masuda S., Takahashi H., Watanabe K.

Proceedings of Science Vol. 395 2022.3

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Publisher：Proceedings of Science

Fast neutrons generated by the interaction between ions and the solar atmosphere are important observation problems to clarify the ion acceleration mechanism in the Sun, but so far neutrons have been detected from only 12 X-class solar flares in the highland on the ground due to the influence of atmospheric absorption. As for observations in space, SEDA-AP at the International Space Station continued to operate until 2018 and succeeded in neutron detection from 52 solar flares, but there are currently no dedicated space missions. In order to overcome this situation, we have been designing and developing 3U CubeSat and novel neutron/gamma-ray sensors since 2018 with the aim of performing satellite observations from outer space. The sensor consists of the multi-layered plastic scintillator bars readout with Si PM, which is a semiconductor photo-sensor, and detects fast neutrons from the tracks of ejected protons by elastic scattering. Furthermore, by placing GAGG scintillator arrays at the bottom, it is designed to be sensitive to gamma-rays based on the principle of the Compton camera. In this presentation, we will report on the scientific motivation and the development status of CubeSat and neutron/gamma-ray sensors.

Scopus
Solar Neutron and Gamma-ray Spectroscopy Mission: SONGS

Kazutaka Yamaoka, Hiroyasu Tajima, Daiki Nobashi, Masaki Usami, Kikuko Miyata, Takaya Inamori, Ji Hyun Park, Kazuya Ito, Koji Matsushita, Toyoki Watabe, Kazuhiro Nakazawa, Satoshi Masuda, Hiromitsu Takahashi, Kyoko Watanabe

Proceedings of Science Vol. 395 2022.3

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Publishing type：Research paper (international conference proceedings)

Fast neutrons generated by the interaction between ions and the solar atmosphere are important observation problems to clarify the ion acceleration mechanism in the Sun, but so far neutrons have been detected from only 12 X-class solar flares in the highland on the ground due to the influence of atmospheric absorption. As for observations in space, SEDA-AP at the International Space Station continued to operate until 2018 and succeeded in neutron detection from 52 solar flares, but there are currently no dedicated space missions. In order to overcome this situation, we have been designing and developing 3U CubeSat and novel neutron/gamma-ray sensors since 2018 with the aim of performing satellite observations from outer space. The sensor consists of the multi-layered plastic scintillator bars readout with Si PM, which is a semiconductor photo-sensor, and detects fast neutrons from the tracks of ejected protons by elastic scattering. Furthermore, by placing GAGG scintillator arrays at the bottom, it is designed to be sensitive to gamma-rays based on the principle of the Compton camera. In this presentation, we will report on the scientific motivation and the development status of CubeSat and neutron/gamma-ray sensors.

Scopus
Characteristics of Low‐Frequency Pulses Associated With Downward Terrestrial Gamma‐Ray Flashes

Y. Wada, T. Morimoto, Y. Nakamura, T. Wu, T. Enoto, K. Nakazawa, T. Ushio, T. Yuasa, H. Tsuchiya

Geophysical Research Letters Vol. 49 ( 5 ) 2022.3

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Language：Japanese Publishing type：Research paper (scientific journal) Publisher：American Geophysical Union (AGU)

DOI： 10.1029/2021GL097348

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Other Link： https://onlinelibrary.wiley.com/doi/full-xml/10.1029/2021GL097348
Atmospheric Electron Spatial Range Extended by Thundercloud Electric Field Below the Relativistic Runaway Electron Avalanche Threshold

G. Diniz, Y. Wada, Y. Ohira, K. Nakazawa, T. Enoto

Journal of Geophysical Research: Atmospheres Vol. 127 ( 3 ) 2022.2

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Language：Japanese Publishing type：Research paper (scientific journal) Publisher：American Geophysical Union (AGU)

DOI： 10.1029/2021JD035958

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Other Link： https://onlinelibrary.wiley.com/doi/full-xml/10.1029/2021JD035958
Balloon-borne narrow field of view semiconductor Compton telescope concept: miniSGD

Kazuhiro Nakazawa, Keigo Okuma, Yuna Tsuji, Shinichiro Takeda, Mii Ando, Yuki Omiya, Manari Oguchi, Atsuya Tanaka, Shin Watanabe, Tadayuki Takahashi, Mitsunobu Onishi, Toshihiko Arai, Masahiko Kobayashi, Naoki Ishida

Space Telescopes and Instrumentation 2022: Ultraviolet to Gamma Ray Vol. 12181 2022

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Publishing type：Research paper (international conference proceedings) Publisher：SPIE

DOI： 10.1117/12.2628199

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Xappl: software framework for the XRISM pre-pipeline

Satoshi Eguchi, Makoto Tashiro, Yukikatsu Terada, Hiromitsu Takahashi, Masayoshi Nobukawa, Tsunefumi Mizuno, Shin'ichiro Uno, Aya Kubota, Kazuhiro Nakazawa, Shin Watanabe, Ryo Iizuka, Rie Sato, Tomokage Yoneyama, Chris Baluta, Ken Ebisawa, Yasushi Fukazawa, Katsuhiro Hayashi, So Kato, Satoru Katsuda, Takao Kitaguchi, Hirokazu Odaka, Masanori Ohno, Naomi Ota, Minami Sakama, Ryohei Sato, Megumi Shidatsu, Yasuharu Sugawara, Tsubasa Tamba, Atsushi Tanimoto, Yuichi Terashima, Yohko Tsuboi, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Shigeo Yamauchi, Masaaki Sakano, Tessei Yoshida, Satoshi Yamada

Space Telescopes and Instrumentation 2022: Ultraviolet to Gamma Ray Vol. 12181 2022

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DOI： 10.1117/12.2629316

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SOlar Neutron and Gamma-ray Spectroscopy Mission (SONGS)

Kazutaka Yamaoka, Hiroyasu Tajima, Kikuko Miyata, Masaki Usami, Toyoki Watabe, Koji Matsushita, Kazuya Ito, Kazuhiro Nakazawa, Satoshi Masuda, Koichi Tani, Masaki Arai, Satoshi Hatori, Kyo Kume, Satoshi Mizushima, Hiromitsu Takahashi, Kyoko Watanabe

Proceedings of SPIE - The International Society for Optical Engineering Vol. 12181 2022

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Publishing type：Research paper (international conference proceedings)

The SOlar Neutron and Gamma-ray Spectroscopy (SONGS) mission is a 3U cubesat dedicated for detecting neutrons and gamma-rays associated with intense solar flares. Solar neutron observations have not been in progress because ground-based observations are affected by attenuation in the Earth atmosphere, and there is no dedicated mission in space at present. Hence, we are now developing in collaboration between science and engineering people at universities, and preparing for launch around 2024 during the next solar maximum. The SONGS carries a novel radiation detector which consists of multi-layered plastic scintillator bars and GAGG(Ce) scintillator array so that it can determine energies for both neutrons and gamma-rays. In total 704 signals from Silicon photo-multipliers (SiPMs) are processed by 45 ASICs with very low power consumption, and realized within limited resources. In this presentation, we will describe scientific motivation, mission and instrument overview, and results from the bread-board model (BBM).

DOI： 10.1117/12.2629131

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Early results from GRBAlpha and VZLUSAT-2

Rípa, J; Pál, A; Ohno, M; Werner, N; Mészáros, L; Csák, B; Dafcikova, M; Dániel, V; Dudás, J; Frajt, M; Hanák, P; Hudec, J; Junas, M; Kapus, J; Kasal, M; Koleda, M; Laszlo, R; Lipovsky, P; Münz, F; Rezenov, M; Smelko, M; Svoboda, P; Takahashi, H; Topinka, M; Urbanec, T; Breuer, JP; Enoto, T; Frei, Z; Fukazawa, Y; Galgóczi, G; Hroch, F; Ichinohe, Y; Kiss, L; Matake, H; Mizuno, T; Nakazawa, K; Odaka, H; Poon, H; Uchida, N; Uchida, Y

SPACE TELESCOPES AND INSTRUMENTATION 2022: ULTRAVIOLET TO GAMMA RAY Vol. 12181 2022

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Publisher：Proceedings of SPIE - The International Society for Optical Engineering

We present the detector performance and early science results from GRBAlpha, a 1U CubeSat mission, which is a technological pathfinder to a future constellation of nanosatellites monitoring gamma-ray bursts (GRBs). GRBAlpha was launched in March 2021 and operates on a 550 km altitude sun-synchronous orbit. The gamma-ray burst detector onboard GRBAlpha consists of a 75×75×5 mm CsI(Tl) scintillator, read out by a dual-channel multi-pixel photon counter (MPPC) setup. It is sensitive in the a1/430-900 keV range. The main goal of GRBAlpha is the in-orbit demonstration of the detector concept, verification of the detector's lifetime, and measurement of the background level on low-Earth orbit, including regions inside the outer Van Allen radiation belt and in the South Atlantic anomaly. GRBAlpha has already detected five, both long and short, GRBs and two bursts were detected within a time-span of only 8 hours, proving that nanosatellites can be used for routine detection of gamma-ray transients. For one GRB, we were able to obtain a high resolution spectrum and compare it with measurements from the Swift satellite. We find that, due to the variable background, the time fraction of about 67% of the low-Earth polar orbit is suitable for gamma-ray burst detection. One year after launch, the detector performance is good and the degradation of the MPPC photon counters remains at an acceptable level. The same detector system, but double in size, was launched in January 2022 on VZLUSAT-2 (3U CubeSat). It performs well and already detected three GRBs and two solar flares. Here, we present early results from this mission as well.

DOI： 10.1117/12.2629332

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Current status of development of lightweight x-ray mirror with carbon fiber reinforced plastic (CFRP)

Hisamitsu Awaki, Norika Kametani, Ryuta Imamura, Manabu Ishida, Masahiro Iwasaki, Kenshin Kodani, Yoshitomo Maeda, Hironori Matsumoto, Koji Mori, Kazuhiro Nakazawa, Tsuyoshi Ozaki, Hirofumi Suzuki, Hiromitsu Takahashi, Takeshi Tsuru, Shin Utsunomiya

Space Telescopes and Instrumentation 2022: Ultraviolet to Gamma Ray Vol. 12181 2022

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Publishing type：Research paper (international conference proceedings) Publisher：SPIE

DOI： 10.1117/12.2629705

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Catalog of gamma-ray glows during four winter seasons in Japan

Y. Wada, T. Matsumoto, T. Enoto, K. Nakazawa, T. Yuasa, Y. Furuta, D. Yonetoku, T. Sawano, G. Okada, H. Nanto, S. Hisadomi, Y. Tsuji, G. S. Diniz, K. Makishima, H. Tsuchiya

Physical Review Research Vol. 3 ( 4 ) 2021.11

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Language：Japanese Publishing type：Research paper (scientific journal) Publisher：American Physical Society (APS)

DOI： 10.1103/PhysRevResearch.3.043117

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Other Link： http://harvest.aps.org/v2/journals/articles/10.1103/PhysRevResearch.3.043117/fulltext
Multiple Gamma‐ray Glows and a Downward TGF Observed from Nearby Thunderclouds

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

Journal of Geophysical Research: Atmospheres Vol. 126 ( 18 ) 2021.9

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Language：Japanese Publishing type：Research paper (scientific journal) Publisher：American Geophysical Union (AGU)

DOI： 10.1029/2021JD034543

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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 Vol. 358 2021.7

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Publisher：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.

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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 Vol. 358 2021.7

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Publisher：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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Detailed design of the science operations for the XRISM mission Reviewed

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

Journal of Astronomical Telescopes, Instruments, and Systems Vol. 7 ( 3 ) 2021.7

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Language：English Publishing type：Research paper (scientific journal) Publisher：SPIE-Intl Soc Optical Eng

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. (C) The Authors. Published by SPIE under a Creative Commons Attribution 4.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI.

DOI： 10.1117/1.JATIS.7.3.037001

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

Kawamura, S; Ando, M; Seto, N; Sato, S; Musha, M; Kawano, I; Yokoyama, J; Tanaka, T; Ioka, K; Akutsu, T; Takashima, T; Agatsuma, K; Araya, A; Aritomi, N; Asada, H; Chiba, T; Eguchi, S; Enoki, M; Fujimoto, MK; Fujita, R; Futamase, T; Harada, T; Hayama, K; Himemoto, Y; Hiramatsu, T; Hong, FL; Hosokawa, M; Ichiki, K; Ikari, S; Ishihara, H; Ishikawa, T; Itoh, Y; Ito, T; Iwaguchi, S; Izumi, K; Kanda, N; Kanemura, S; Kawazoe, F; Kobayashi, S; Kohri, K; Kojima, Y; Kokeyama, K; Kotake, K; Kuroyanagi, S; Maeda, K; Matsushita, S; Michimura, Y; Morimoto, T; Mukohyama, S; Nagano, K; Nagano, S; Naito, T; Nakamura, K; Nakamura, T; Nakano, H; Nakao, K; Nakasuka, S; Nakayama, Y; Nakazawa, K; Nishizawa, A; Ohkawa, M; Oohara, K; Sago, N; Saijo, M; Sakagami, M; Sakai, S; Sato, T; Shibata, M; Shinkai, H; Shoda, A; Somiya, K; Sotani, H; Takahashi, R; Takahashi, H; Akiteru, T; Taniguchi, K; Taruya, A; Tsubono, K; Tsujikawa, S; Ueda, A; Ueda, K; Watanabe, I; Yagi, K; Yamada, R; Yokoyama, S; Yoo, CM; Zhu, ZH

PROGRESS OF THEORETICAL AND EXPERIMENTAL PHYSICS Vol. 2021 ( 5 ) 2021.5

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Language：Japanese Publisher：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

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Meteorological Aspects of Gamma‐Ray Glows in Winter Thunderstorms

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

Geophysical Research Letters Vol. 48 ( 7 ) 2021.4

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Language：Japanese Publishing type：Research paper (scientific journal) Publisher：American Geophysical Union (AGU)

DOI： 10.1029/2020GL091910

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Other Link： https://onlinelibrary.wiley.com/doi/full-xml/10.1029/2020GL091910
Simulations of expected signal and background of gamma-ray sources by large field-of-view detectors aboard CubeSats

G{\'{a } }bor Galg{\'{o } }czi, Jakub {\v{R } }{\'{\i } }pa, Riccardo Campana, Norbert Werner, Andr{\'{a } }s P{\'{a } }l, Masanori Ohno, L{\'{a } }szl{\'{o } } M{\'{e } }sz{\'{a } }ros, Tsunefumi Mizuno, Norbert Tarcai, Kento Torigoe, Nagomi Uchida, Yasushi Fukazawa, Hiromitsu Takahashi, Kazuhiro Nakazawa, Naoyoshi Hirade, Kengo Hirose, Syohei Hisadomi, Teruaki Enoto, Hirokazu Odaka, Yuto Ichinohe, Zsolt Frei, L{\'{a } }szl{\'{o } } Kiss

Journal of Astronomical Telescopes, Instruments, and Systems Vol. 7 ( 2 ) 2021.4

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Language：Japanese Publishing type：Research paper (scientific journal) Publisher：{SPIE}-Intl Soc Optical Eng

DOI： 10.1117/1.JATIS.7.2.028004

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Annealing of proton radiation damages in Si-PM at room temperature Reviewed International coauthorship

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 Vol. 986 page： 164673 - 164673 2021.1

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Language：English Publishing type：Research paper (scientific journal) Publisher：ELSEVIER

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 similar to 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 degrees C, the threshold energies of both MPPCs reduced by several tens of percent after irradiation, but below 0 degrees 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

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Detail plans and preparations for the science operations of the XRISM mission

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

Proceedings of SPIE - The International Society for Optical Engineering Vol. 11444 2021

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Language：Japanese Publishing type：Research paper (international conference proceedings)

© 2020 SPIE 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

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The XRISM science data center: Optimizing the scientific return from a unique X-ray observatory

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

Proceedings of SPIE - The International Society for Optical Engineering Vol. 11444 2021

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Language：Japanese Publishing type：Research paper (international conference proceedings)

© 2020 SPIE 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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Status of x-ray imaging and spectroscopy mission (XRISM)

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

Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray Vol. 11444 2021

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Language：Japanese Publishing type：Research paper (international conference proceedings) Publisher：SPIE

DOI： 10.1117/12.2565812

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

Hisamitsu Awaki, Nozomi Aida, Kazunori Asakura, Maho Hanaoka, Kengo Hattori, Kazunori Ishibashi, Manabu Ishida, Ayami Ishikura, Yoshitomo Maeda, Hironori Matsumoto, Yusuke Matsushita, Taisei Mineta, Ikuyuki Mitsuishi, Takuya Miyazawa, Nozomi Nakaniwa, Kazuhiro Nakazawa, Yuuichi Ode, Chisato Oue, Kenmei Sawagami, Satoshi Sugita, Hitomi Suzuki, Hiromitsu Takahashi, Yuusuke Uchida, Ryuya Yamamoto, Marina Yoshimoto

Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray Vol. 11444 2021

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DOI： 10.1117/12.2561890

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

Pál, A; Ohno, M; Mészáros, L; Werner, N; Ripa, J; Frajt, M; Hirade, N; Hudec, J; Kapus, J; Koleda, M; Laszlo, R; Lipovsky, P; Matake, H; Smelko, M; Uchida, N; Csák, B; Enoto, T; Frei, Z; Fukazawa, Y; Galgóczi, G; Hirose, K; Hisadomi, S; Ichinohe, Y; Kiss, LL; Mizuno, T; Nakazawa, K; Odaka, H; Takahashi, H; Torigoe, K

SPACE TELESCOPES AND INSTRUMENTATION 2020: ULTRAVIOLET TO GAMMA RAY Vol. 11444 2021

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Language：Japanese Publisher：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

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Solar Neutron Spectrometer Onboard a 3U CubeSat

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

TRANSACTIONS OF THE JAPAN SOCIETY FOR AERONAUTICAL AND SPACE SCIENCES, AEROSPACE TECHNOLOGY JAPAN Vol. 19 ( 3 ) page： 354 - 359 2021

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Language：English Publisher：THE JAPAN SOCIETY FOR AERONAUTICAL AND SPACE SCIENCES

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.

DOI： 10.2322/tastj.19.354

CiNii Research
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 2020.12

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DOI： 10.1117/12.2560928
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 2020.12

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DOI： 10.1117/12.2561341
Photonuclear Reactions in Lightning I: Verification and Modeling of Reaction and Propagation Processes

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

Journal of Geophysical Research: Atmospheres Vol. 125 ( 20 ) 2020.10

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DOI： 10.1029/2020JD033193

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Photonuclear Reactions in Lightning II: Comparison between Observation and Simulation Model

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

Journal of Geophysical Research: Atmospheres Vol. 125 ( 20 ) 2020.10

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Language：Japanese Publishing type：Research paper (scientific journal) Publisher：American Geophysical Union (AGU)

DOI： 10.1029/2020JD033194

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

Kouichi Hagino, Hirokazu Odaka, Goro Sato, Tamotsu Sato, Hiromasa Suzuki, Tsunefumi Mizuno, Madoka Kawaharada, Masanori Ohno, Kazuhiro Nakazawa, Shogo B. Kobayashi, Hiroaki Murakami, Katsuma Miyake, Makoto Asai, Tatsumi Koi, Greg Madejski, Shinya Saito, Dennis H. Wright, Teruaki Enoto, Yasushi Fukazawa, Katsuhiro Hayashi, Jun Kataoka, Junichiro Katsuta, Motohide Kokubun, Philippe Laurent, François Lebrun, Olivier Limousin, Daniel Maier, Kazuo Makishima, Kunishiro Mori, Takeshi Nakamori, Toshio Nakano, Hirofumi Noda, Masayuki Ohta, 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 Vol. 6 ( 4 ) 2020.10

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Language：Japanese Publishing type：Research paper (scientific journal) Publisher：SPIE-Intl Soc Optical Eng

DOI： 10.1117/1.JATIS.6.4.046003

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

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

Progress of Theoretical and Experimental Physics Vol. 2020 ( 10 ) 2020.10

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Language：Japanese Publishing type：Research paper (scientific journal) Publisher：Oxford University Press (OUP)

<title>Abstract</title>
We designed, developed, and deployed a distributed sensor network aiming at observing high-energy ionizing radiation, primarily gamma rays, from winter thunderclouds and lightning in coastal areas of Japan. Starting in 2015, we have installed, in total, more than 15 units of ground-based detector system 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 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 objective, methodology, and results of our experiment, with a stress on its instrumentation.

DOI： 10.1093/ptep/ptaa115

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

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

Astronomy & Astrophysics Vol. 638 page： A138 - A138 2020.6

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Language：Japanese Publishing type：Research paper (scientific journal) Publisher：EDP Sciences

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 <italic>z</italic> ∼ 1 to <italic>z</italic> ∼ 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 <italic>Hitomi</italic> 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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Photoneutron detection in lightning by gadolinium orthosilicate scintillators Reviewed

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

Physical Review D Vol. 101 ( 10 ) 2020.5

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Language：English Publishing type：Research paper (scientific journal) Publisher：American Physical Society (APS)

DOI： 10.1103/PhysRevD.101.102007

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Other Link： http://harvest.aps.org/v2/journals/articles/10.1103/PhysRevD.101.102007/fulltext
High Peak-Current Lightning Discharges Associated With Downward Terrestrial Gamma-Ray Flashes

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

Journal of Geophysical Research: Atmospheres Vol. 125 ( 4 ) 2020.2

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Language：Japanese Publishing type：Research paper (scientific journal)

©2020. American Geophysical Union. All Rights Reserved. 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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The simulation framework of the timing-based localization for future all-sky gamma-ray observations with a fleet of Cubesats

Ohno, M; Werner, N; Päl, A; Meszáros, L; Ichinohe, Y; Rípa, 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

X-RAY, OPTICAL, AND INFRARED DETECTORS FOR ASTRONOMY IX Vol. 11454 2020

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Language：Japanese Publisher：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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A wide-band X-ray observatory FORCE: Current status of science study and mission proposal

Nakazawa K., Mori K., Tsuru T. G., Ueda Y., Ishida M., Matsumoto H., Awaki H., Murakami H., Terada Y., Kubota A., Bamba A., Odaka H., Yatsu Y., Kohmura T., Hagino K., Kobayashi S. B., Uchiyama Y., Kitayama T., Takahashi T., Watanabe S., Iizuka R., Yamaguchi H., Ohashi T., Nakajima M., Furuzawa A., Tanaka T., Uchida H., Noda H., Tsunemi H., Ito M., Nobukawa M., Nobukawa K., Ota N., Terashima Y., Fukazawa Y., Mizuno T., Takahashi H., Ohno M., Takeda A., Hornschemeier A. E., Okajima T., Zhang W. W., Williams B. J., the FORCE team

Meeting Abstracts of the Physical Society of Japan Vol. 75.1 page： 523 - 523 2020

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Language：Japanese Publisher：The Physical Society of Japan

DOI： 10.11316/jpsgaiyo.75.1.0_523
A new possible accretion scenario for ultra-luminous X-ray sources Reviewed

S. B. Kobayashi, K. Nakazawa, K. Makishima

MON NOT R ASTRON SOC Vol. 489 ( 1 ) page： 366 - 384 2019.10

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DOI： 10.1093/mnras/stz2139

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Space gravitational-wave antennas DECIGO and B-DECIGO Reviewed

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 Vol. 28 ( 12 ) 2019.9

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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 Pabry-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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Downward Terrestrial Gamma-Ray Flash Observed in a Winter Thunderstorm Reviewed

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

Physical Review Letters Vol. 123 ( 6 ) page： 061103 2019.8

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DOI： 10.1103/PhysRevLett.123.061103

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PubMed

Other Link： http://harvest.aps.org/v2/journals/articles/10.1103/PhysRevLett.123.061103/fulltext
Estimation of the detected background by the future gamma ray transient mission CAMELOT Reviewed International coauthorship

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 Vol. 340 ( 7 ) page： 666 - 673 2019.8

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Language：English Publishing type：Research paper (scientific journal) Publisher：WILEY-V C H VERLAG GMBH

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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Spectral properties of gamma-ray bursts observed by the Suzaku wide-band all-sky monitor Reviewed

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 Vol. 71 ( 4 ) 2019.8

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DOI： 10.1093/pasj/psz054

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Gamma-ray glow preceding downward terrestrial gamma-ray flash Reviewed

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

Communications Physics Vol. 2 ( 67 ) page： 1 - 9 2019.6

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Language：English Publishing type：Research paper (scientific journal)

© 2019, The Author(s). 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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Event-selection technique for the multi-layer Si−CdTe Compton camera onboard Hitomi

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

Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment Vol. 924 page： 327 - 331 2019.4

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Language：Japanese Publishing type：Research paper (scientific journal)

© 2018 Elsevier B.V. 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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Performance study of a large CsI(Tl) scintillator with an MPPC readout for nanosatellites used to localize gamma-ray bursts Reviewed

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

Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment Vol. 924 page： 316 - 320 2019.4

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DOI： 10.1016/j.nima.2018.08.039

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

Makishima, K; Murakami, H; Enoto, T; Nakazawa, K

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN Vol. 71 ( 1 ) 2019.1

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Language：Japanese Publisher：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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Completeness of Cyclic Proofs for Symbolic Heaps with Inductive Definitions

Tatsuta Makoto, Nakazawa Koji, Kimura Daisuke

PROGRAMMING LANGUAGES AND SYSTEMS, APLAS 2019 Vol. 11893 page： 367 - 387 2019

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Publisher：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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Solar neutron and gamma-ray detector for a 3U Cubesat

Kazutaka Yamaoka, Hiroyasu Tajima, Kikuko Miyata, Takaya Inamori, Yoshinori Sasai, Hiroaki Kawahara, Ji Hyun Park, Kazuhiro Nakazawa, Satoshi Masuda, Koji Matsushita, Kazuya Itoh, Daiki Nobashi, Hiromitsu Takahashi, Kyoko Watanabe

Proceedings of Science Vol. 358 2019

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Language：Japanese Publishing type：Research paper (international conference proceedings)

© Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). 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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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 Vol. 358 2019

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Language：Japanese Publisher：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.

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

Aharonian, F; Akamatsu, H; Akimoto, F; Allen, SW; Angelini, L; Audard, M; Awaki, H; Axelsson, M; Bamba, A; Bautz, MW; Blandford, R; Brenneman, LW; Brown, GV; Bulbul, E; Cackett, EM; Chernyakova, M; Chiao, MP; Coppi, PS; Costantini, E; de Plaa, J; de Vries, CP; den Herder, JW; Done, C; Dotani, T; Ebisawa, K; Eckart, ME; Enoto, T; Ezoe, Y; Fabian, AC; Ferrigno, C; Foster, AR; Fujimoto, R; Fukazawa, Y; Furuzawa, A; Galeazzi, M; Gallo, LC; Gandhi, P; Giustini, M; Goldwurm, A; Gu, LY; Guainazzi, M; Haba, Y; Hagino, K; Hamaguchi, K; Harrus, IM; Hatsukade, I; Hayashi, K; Hayashi, T; Hayashida, K; Hiraga, JS; Hornschemeier, A; Hoshino, A; Hughes, JP; Ichinohe, Y; Iizuka, R; Inoue, H; Inoue, Y; Ishida, M; Ishikawa, K; Ishisaki, Y; Iwai, M; Kaastra, J; Kallman, T; Kamae, T; Kataoka, J; Katsuda, S; Kawai, N; Kelley, RL; Kilbourne, CA; Kitaguchi, T; Kitamoto, S; Kitayama, T; Kohmura, T; Kokubun, M; Koyama, K; Koyama, S; Kretschmar, P; Krimm, HA; Kubota, A; Kunieda, H; Laurent, P; Lee, SH; Leutenegger, MA; Limousin, O; Loewenstein, M; Long, KS; Lumb, D; Madejski, G; Maeda, Y; Maier, D; Makishima, K; Markevitch, M; Matsumoto, H; Matsushita, K; McCammon, D; McNamara, BR; Mehdipour, M; Miller, ED; Miller, JM; Mineshige, S; Mitsuda, K; Mitsuishi, I; Miyazawa, T; Mizuno, T; Mori, H; Mori, K; Mukai, K; Murakami, H; Mushotzky, RF; Nakagawa, T; Nakajima, H; Nakamori, T; Nakashima, S; Nakazawa, K; Nobukawa, KK; Nobukawa, M; Noda, H; Odaka, H; Ohashi, T; Ohno, M; Okajima, T; Ota, N; Ozaki, M; Paerels, F; Paltani, S; Petre, R; Pinto, C; Porter, FS; Pottschmidt, K; Reynolds, CS; Safi-Harb, S; Saito, S; Sakai, K; Sasaki, T; Sato, G; Sato, K; Sato, R; Sawada, M; Schartel, N; Serlemtsos, PJ; Seta, H; Shidatsu, M; Simionescu, A; Smith, RK; Soong, Y; Stawarz, L; Sugawara, Y; Sugita, S; Szymkowiak, A; Tajima, H; Takahashi, H; Takahashi, T; Takeda, S; Takei, Y; Tamagawa, T; Tamura, T; Tanaka, T; Tanaka, Y; Tanaka, YT; Tashiro, MS; Tawara, Y; Terada, Y; Terashima, Y; Tombesi, F; Tomida, H; Tsuboi, Y; Tsujimoto, M; Tsunemi, H; Tsuru, TG; Uchida, H; Uchiyama, H; Uchiyama, Y; Ueda, S; Ueda, Y; Uno, S; Urry, CM; Ursino, E; Watanabe, S; Werner, N; Wilkins, DR; Williams, BJ; Yamada, S; Yamaguchi, H; Yamaoka, K; Yamasaki, NY; Yamauchi, M; Yamauchi, S; Yaqoob, T; Yatsu, Y; Yonetoku, D; Zhuravleva, I; Zoghbi, A; Uchida, Y

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN Vol. 70 ( 6 ) 2018.12

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Language：Japanese Publisher：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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Termination of Electron Acceleration in Thundercloud by Intra/Inter-cloud Discharge Reviewed

Yuuki Wada, Gregory S. Bowers, Teruaki Enoto, Masashi Kamogawa, Yoshitaka Nakamura, Takeshi Morimoto, David M. Smith, Yoshihiro Furuta, Kazuhiro Nakazawa, Takayuki Yuasa, Atsushi Matsuki, Mamoru Kubo, Toru Tamagawa, Kazuo Makishima, Harufumi Tsuchiya

Geophysical Research Letters, Vol. 45 ( 11 ) page： 5700 - 5707 2018.6

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Language：English Publishing type：Research paper (scientific journal)

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

DOI： 10.1029/2018GL077784

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arXiv
ATCA 16 cm observation of CIZA J1358.9-4750: Implication of merger stage and constraint on non-thermal properties Reviewed

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 Vol. 70 ( 3 ) 2018.6

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Language：Japanese Publishing type：Research paper (scientific journal)

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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Hitomi X-ray observation of the pulsar wind nebula G21.5-0.9 Reviewed

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, Stéphane 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, Łukasz 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, Toshiki Sato, Nozomu Nakaniwa, Hiroaki Murakami, Benson Guest

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN Vol. 70 ( 3 ) 2018.6

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Language：Japanese Publishing type：Research paper (scientific journal) Publisher：Oxford University Press (OUP)

DOI： 10.1093/pasj/psy027

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

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 Vol. 70 ( 3 ) 2018.6

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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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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 Reviewed

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

NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT Vol. 891 page： 92 - 105 2018.5

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Language：English Publishing type：Research paper (scientific journal) Publisher：ELSEVIER SCIENCE BV

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 degrees, 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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Design and performance of Soft Gamma-ray Detector onboard the Hitomi (ASTRO-H) satellite Reviewed

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

Journal of Astronomical Telescopes, Instruments, and Systems Vol. 4 ( 2 ) 2018.4

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Language：English Publishing type：Research paper (scientific journal) Publisher：SPIE

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

DOI： 10.1117/1.JATIS.4.2.021411

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The Hitomi X-Ray Observatory, Part 2 Reviewed

Kelley Richard L, Nakazawa Kazuhiro

JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS Vol. 4 ( 2 ) 2018.4

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DOI： 10.1117/1.JATIS.4.2.021401

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

Hagino K.

Journal of Astronomical Telescopes, Instruments, and Systems Vol. 4 ( 2 ) 2018.4

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Publisher：Journal of Astronomical Telescopes, Instruments, and Systems

DOI： 10.1117/1.JATIS.4.2.021409

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HITOMI (ASTRO-H) X-ray astronomy satellite Reviewed

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

Journal of Astronomical Telescopes, Instruments, and Systems Vol. 4 ( 2 ) 2018.4

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Language：Japanese

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

DOI： 10.1117/1.JATIS.4.2.021402

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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 Vol. 70 ( 2 ) 2018.3

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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.

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

Aharonian F.

Publications of the Astronomical Society of Japan Vol. 70 ( 2 ) 2018.3

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Atmospheric gas dynamics in the Perseus cluster observed with Hitomi Reviewed

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, Rebecca E A Canning, 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, Tasuku Hayashi, Kiyoshi Hayashida, Junko S Hiraga, Ann Hornschemeier, Akio Hoshino, John P Hughes, Yuto Ichinohe, Ryo Iizuka, Hajime Inoue, Shota 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, Stéphane 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, Łukasz Stawarz, Yasuharu Sugawara, Satoshi Sugita, Andrew Szymkowiak, Hiroyasu Tajima, Hiromitsu Takahashi, Tadayuki Takahashi, Shin’ichiro Takeda, Yoh Takei, Toru Tamagawa, Takayuki Tamura, Keigo Tanaka, 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, Qian H S Wang, 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

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN Vol. 70 ( 2 ) 2018.3

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Language：Japanese Publishing type：Research paper (scientific journal) Publisher：Oxford University Press (OUP)

DOI： 10.1093/pasj/psx138

Web of Science
Temperature structure in the Perseus cluster core observed with Hitomi Reviewed

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, Maki Furukawa, 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, Yuichi Kato, 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, Stéphane 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, Łukasz Stawarz, Yasuharu Sugawara, Satoshi Sugita, Andrew Szymkowiak, Hiroyasu Tajima, Hiromitsu Takahashi, Tadayuki Takahashi, Shiníchiro 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, Shiníchiro 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

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN Vol. 70 ( 2 ) 2018.3

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DOI： 10.1093/pasj/psy004

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Scopus
Search for thermal X-ray features from the Crab nebula with the Hitomi soft X-ray spectrometer Reviewed

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, 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, Stéphane 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, Toshiki Sato, Makoto Sawada, Norbert Schartel, Peter J Serlemtsos, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall K Smith, Yang Soong, Łukasz 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, Nozomu Tominaga, Takashi J Moriya

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN Vol. 70 ( 2 ) 2018.3

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Language：Japanese Publishing type：Research paper (scientific journal) Publisher：Oxford University Press (OUP)

DOI： 10.1093/pasj/psx072

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Measurements of resonant scattering in the Perseus Cluster core with Hitomi SXS Reviewed

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, Maki Furukawa, 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 O Limousin, Michael Loewenstein, Knox S Long, David Lumb, Greg Madejski, Yoshitomo Maeda, Daniel Maier, Kazuo Makishima, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian R McNamara, Missagh Mehdipour, Eric D Miller, Jon M Miller, Shin Mineshige, 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, Anna Ogorzalek, Takaya Ohashi, Masanori Ohno, Takashi Okajima, Naomi Ota, Masanobu Ozaki, Frits Paerels, Stéphane 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, Łukasz Stawarz, Yasuharu Sugawara, Satoshi Sugita, Andrew Szymkowiak, Hiroyasu Tajima, Hiromitsu Takahashi, Tadayuki Takahashi, Shiníchiro 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, Shiníchiro 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

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN Vol. 70 ( 2 ) 2018.3

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Language：Japanese Publishing type：Research paper (scientific journal) Publisher：Oxford University Press (OUP)

DOI： 10.1093/pasj/psx127

Web of Science

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

Felix Aharonian, Hiroki Akamatsu, Fumie Akimoto, Steven W. Allen, Lorella Angelini, Marc Audard, Hisamitsu Awaki, Magnus Axelsson, Aya Bamba, Marshall W. Bautz, Roger Blandford, Laura W. Brenneman, Gregory V. Brown, Esra Bulbul, Edward M. Cackett, Maria Chernyakova, Meng P. Chiao, Paolo S. Coppi, Elisa Costantini, Jelle De Plaa, Cor P. De Vries, Jan Willem Den Herder, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Teruaki Enoto, Yuichiro Ezoe, Andrew C. Fabian, Carlo Ferrigno, Adam R. Foster, Ryuichi Fujimoto, Yasushi Fukazawa, Akihiro Furuzawa, Massimiliano Galeazzi, Luigi C. Gallo, Poshak Gandhi, Margherita Giustini, Andrea Goldwurm, Liyi Gu, Matteo Guainazzi, Yoshito Haba, Kouichi Hagino, Kenji Hamaguchi, Ilana M. Harrus, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Kiyoshi Hayashida, Junko S. Hiraga, Ann Hornschemeier, Akio Hoshino, John P. Hughes, Yuto Ichinohe, Ryo Iizuka, Hajime Inoue, Yoshiyuki Inoue, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Masachika Iwai, Jelle Kaastra, Tim Kallman, Tsuneyoshi Kamae, Jun Kataoka, Satoru Katsuda, Nobuyuki Kawai, Richard L. Kelley, Caroline A. Kilbourne, Takao Kitaguchi, Shunji Kitamoto, Tetsu Kitayama, Takayoshi Kohmura, Motohide Kokubun, Katsuji Koyama, Shu Koyama, Peter Kretschmar, Hans A. Krimm, Aya Kubota, Hideyo Kunieda, Philippe Laurent, L. E.E. Shiu-Hang, Maurice A. Leutenegger, Olivier O. Limousin, Michael Loewenstein, Knox S. Long, David Lumb, Greg Madejski, Yoshitomo Maeda, Daniel Maier, Kazuo Makishima, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian R. McNamara, Missagh Mehdipour, Eric D. Miller, Jon M. Miller, Shin Mineshige

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

DOI： 10.1093/pasj/psx083

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PubMed
Hitomi observations of the LMC SNR N 132 D: Highly redshifted X-ray emission from iron ejecta Reviewed

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, Stéphane 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, Toshiki Sato, Makoto Sawada, Norbert Schartel, Peter J Serlemtsos, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall K Smith, Yang Soong, Łukasz 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

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN Vol. 70 ( 2 ) 2018.3

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Language：Japanese Publishing type：Research paper (scientific journal) Publisher：Oxford University Press (OUP)

DOI： 10.1093/pasj/psx151

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

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 O Limousin, Michael Loewenstein, Knox S Long, David Lumb, Greg Madejski, Yoshitomo Maeda, Daniel Maier, Kazuo Makishima, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian R McNamara, Missagh Mehdipour, Eric D Miller, Jon M Miller, Shin Mineshige, 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, Stéphane Paltani, Robert Petre, Ciro Pinto, Frederick S Porter, Katja Pottschmidt, Christopher S Reynolds, Samar Safi-Harb, Shinya Saito, Kazuhiro Sakai, Toru Sasaki, Goro Sato, Kosuke Sato, Rie Sato, Makoto Sawada, Norbert Schartel, Peter J Serlemitsos, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall K Smith, Yang Soong, Łukasz 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, Taiki Kawamuro

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN Vol. 70 ( 2 ) 2018.3

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Language：Japanese Publishing type：Research paper (scientific journal) Publisher：Oxford University Press (OUP)

DOI： 10.1093/pasj/psx147

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Glimpse of the highly obscured HMXB IGR J16318-4848 with Hitomi Reviewed

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 O Limousin, Michael Loewenstein, Knox S Long, David Lumb, Greg Madejski, Yoshitomo Maeda, Daniel Maier, Kazuo Makishima, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian R McNamara, Missagh Mehdipour, Eric D Miller, Jon M Miller, Shin Mineshige, 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, Stéphane 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, Łukasz Stawarz, Yasuharu Sugawara, Satoshi Sugita, Andrew Szymkowiak, Hiroyasu Tajima, Hiromitsu Takahashi, Tadayuki Takahashi, Shiníchiro 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, Shiníchiro 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, Nozomi Nakaniwa

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN Vol. 70 ( 2 ) 2018.3

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Language：Japanese Publishing type：Research paper (scientific journal) Publisher：Oxford University Press (OUP)

DOI： 10.1093/pasj/psx154

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Atomic data and spectral modeling constraints from high-resolution X-ray observations of the Perseus cluster with Hitomi Reviewed

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, Natalie Hell, 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, Stéphane 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, Łukasz 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, A J J Raassen

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN Vol. 70 ( 2 ) 2018.3

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Language：Japanese Publishing type：Research paper (scientific journal) Publisher：Oxford University Press (OUP)

DOI： 10.1093/pasj/psx156

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An estimation of the white dwarf mass in the Dwarf Nova GK Persei with NuSTAR observations of two states Reviewed

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

Monthly Notices of the Royal Astronomical Society Vol. 474 ( 2 ) page： 1564 - 1571 2018.2

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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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The hitomi X-Ray observatory Reviewed

Richard L. Kelley, Kazuhiro Nakazawa

Journal of Astronomical Telescopes, Instruments, and Systems Vol. 4 ( 1 ) 2018.1

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Language：English Publishing type：Research paper (scientific journal) Publisher：SPIE

DOI： 10.1117/1.JATIS.4.1.011201

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Multiwavelength study of X-ray luminous clusters in the Hyper Suprime-Cam Subaru Strategic Program S16A field Reviewed

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

Publications of the Astronomical Society of Japan Vol. 70 ( Special Issue 1 ) 2018.1

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Language：English Publishing type：Research paper (scientific journal) Publisher：Oxford University Press

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

DOI： 10.1093/pasj/psx132

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The analysis of gamma ray from winter thundercloud in Kanazawa between 2015 and 2017

Matsumoto Takahiro, Bamba Aya, Yonetoku Daisuke, Sawano Tatsuya, Wada Yuuki, Furuta Yoshihiro, Nakazawa Kazuhiro, Enoto Teruaki, Yuasa Takayuki, Makishima Kazuo, Tsuchiya Harufumi, Odaka Hirokazu

Meeting Abstracts of the Physical Society of Japan Vol. 73 ( 0 ) page： 134 - 134 2018

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Language：Japanese Publisher：The Physical Society of Japan

DOI： 10.11316/jpsgaiyo.73.2.0_134

CiNii Research
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

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

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

Proc. SPIE 10699, 2018 Vol. 10699 2018

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Publishing type：Research paper (international conference proceedings)

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

DOI： 10.1117/12.2309344

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arXiv
Monitoring of gamma-ray bursts with a fleet of nanosatellites

Å˜Ãpa J., Werner N., PÃ¡l A., Ohno M., Tarcai N., Torigoe K., Tanaka K., Uchida N., MÃ©szÃ¡ros L., GalgÃ³czi G., Fukazawa Y., Mizuno T., Takahashi H., Nakazawa K., VÃ¡rhegyi Z., Enoto T., Odaka H., Ichinohe Y., Frei Z., Kiss L.

Proceedings of the International Astronautical Congress, IAC Vol. 2018-October 2018

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Language：Japanese Publisher：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
Long-term test of a stacked CdTe mini-HXI setup Reviewed

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 Vol. 912 page： 199 - 204 2018

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Language：English Publishing type：Research paper (scientific journal) Publisher：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

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Concept of X-ray Astronomy Recovery Mission Reviewed

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

SPACE TELESCOPES AND INSTRUMENTATION 2018: ULTRAVIOLET TO GAMMA RAY Vol. 10699 2018

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Language：English Publishing type：Research paper (international conference proceedings) Publisher：SPIE-INT SOC OPTICAL ENGINEERING

The ASTRO-H mission was designed and developed through an international collaboration of JAXA, NASA, ESA, and the CSA. It was successfully launched on February 17, 2016, and then named Hitomi. During the in-orbit verification phase, the on-board observational instruments functioned as expected. The intricate coolant and refrigeration systems for soft X-ray spectrometer (SXS, a quantum micro-calorimeter) and soft X-ray imager (SXI, an X-ray CCD) also functioned as expected. However, on March 26, 2016, operations were prematurely terminated by a series of abnormal events and mishaps triggered by the attitude control system. These errors led to a fatal event: the loss of the solar panels on the Hitomi mission. The X-ray Astronomy Recovery Mission (or, XARM) is proposed to regain the key scientific advances anticipated by the international collaboration behind Hitomi. XARM will recover this science in the shortest time possible by focusing on one of the main science goals of Hitomi, "Resolving astrophysical problems by precise high-resolution X-ray spectroscopy".(1) This decision was reached after evaluating the performance of the instruments aboard Hitomi and the mission's initial scientific results, and considering the landscape of planned international X-ray astrophysics missions in 2020's and 2030's.Hitomi opened the door to high-resolution spectroscopy in the X-ray universe. It revealed a number of discrepancies between new observational results and prior theoretical predictions. Yet, the resolution pioneered by Hitomi is also the key to answering these and other fundamental questions. The high spectral resolution realized by XARM will not offer mere refinements; rather, it will enable qualitative leaps in astrophysics and plasma physics. XARM has therefore been given a broad scientific charge: "Revealing material circulation and energy transfer in cosmic plasmas and elucidating evolution of cosmic structures and objects". To fulfill this charge, four categories of science objectives that were defined for Hitomi will also be pursued by XARM; these include (1) Structure formation of the Universe and evolution of clusters of galaxies; (2) Circulation history of baryonic matters in the Universe; (3) Transport and circulation of energy in the Universe; (4) New science with unprecedented high resolution X-ray spectroscopy. In order to achieve these scientific objectives, XARM will carry a 6 x 6 pixelized X-ray micro-calorimeter on the focal plane of an X-ray mirror assembly, and an aligned X-ray CCD camera covering the same energy band and a wider field of view. This paper introduces the science objectives, mission concept, and observing plan of XARM.

DOI： 10.1117/12.2309455

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

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

Proc. SPIE 10699, Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray Vol. 10699 2018

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DOI： 10.1117/12.2313228

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CAMELOT: Cubesats Applied for MEasuring and LOcalising Transients mission overview

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

Proc. SPIE 10699, Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray Vol. 10699 2018

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DOI： 10.1117/12.2313764

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Mass production of the gamma-ray detector using a large CsI and mapping observation of winter thunderclouds

Matsumoto Takahiro, Wada Yuki, Furuta Yoshihiro, Sino Manami, Nakazawa Kazuhiro, Enoto Teruaki, Yuasa Takayuki, Makisima Kazuo, Nakano Toshio, Tsuchiya Harufumi

Meeting Abstracts of the Physical Society of Japan Vol. 73.1 ( 0 ) page： 414 - 414 2018

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Language：Japanese Publisher：The Physical Society of Japan

DOI： 10.11316/jpsgaiyo.73.1.0_414

CiNii Research
Triggering of photonuclear reactions by a lightning discharge

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

Meeting Abstracts of the Physical Society of Japan Vol. 73.1 ( 0 ) page： 176 - 176 2018

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Language：Japanese Publisher：The Physical Society of Japan

DOI： 10.11316/jpsgaiyo.73.1.0_176

CiNii Research
Development of in-orbit radioactivation background simulation and its application to the Hard X-ray Imager onboard Hitomi

Odaka Hirokazu, Asai Makoto, Hagino Kouichi, Koi Tatsumi, Madejski Greg, Mizuno Tsunefumi, Ohno Masanori, Saito Shinya, Wright Dennis, Nakazawa Kazuhiro

Meeting Abstracts of the Physical Society of Japan Vol. 73.2 ( 0 ) page： 163 - 163 2018

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Language：Japanese Publisher：The Physical Society of Japan

DOI： 10.11316/jpsgaiyo.73.2.0_163

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Discovery of photonuclear reactions triggered by lightning discharge: On-ground detection of neutrons and positrons

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

Meeting Abstracts of the Physical Society of Japan Vol. 73.1 ( 0 ) page： 422 - 422 2018

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Language：Japanese Publisher：The Physical Society of Japan

DOI： 10.11316/jpsgaiyo.73.1.0_422

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Multi-point Measurement Campaigns of Gamma Rays from Thunderclouds and Lightning in Japan International coauthorship

中澤知洋, 土屋晴文

Proceedings of XVI International Conference on Atmospheric Electricity Vol. - page： 1 - 13 2018

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Suzaku and Chandra observations of the galaxy cluster RXC J1053.7+5453 with a radio relic Reviewed

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 Vol. 69 ( 6 ) 2017.12

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Language：English Publishing type：Research paper (scientific journal) Publisher：OXFORD UNIV PRESS

We present the results of Suzaku and Chandra observations of the galaxy cluster RXC J1053.7+5453 (z = 0.0704), which contains a radio relic. The radio relic is located at a distance of similar to 540 kpc from the X-ray peak toward the west. We measured the temperature of this cluster for the first time. The resultant temperature in the center is similar to 1.3 keV, which is lower than the value expected from the X-ray luminosity-temperature and the velocity dispersion-temperature relations. Though we did not find a significant temperature jump at the outer edge of the relic, our results suggest that the temperature decreases outward across the relic. Assuming the existence of the shock at the relic, its Mach number becomes M similar or equal to 1.4. A possible spatial variation of Mach number along the relic is suggested. Additionally, a sharp surface brightness edge is found at a distance of similar to 160 kpc from the X-ray peak toward the west in the Chandra image. We performed X-ray spectral and surface brightness analyses around the edge with the Suzaku and Chandra data, respectively. The obtained surface brightness and temperature profiles suggest that this edge is not a shock but likely a cold front. Alternatively, it cannot be ruled out that thermal pressure is really discontinuous across the edge. In this case, if the pressure across the surface brightness edge is in equilibrium, other forms of pressure sources, such as cosmic-rays, are necessary. We searched for the non-thermal inverse Compton component in the relic region. Assuming a photon index Gamma = 2.0, the resultant upper limit of the flux is 1.9 x 10(-14) erg s(-1) cm(-2) for a 4.50 x 10(-3) deg(2) area in the 0.3-10 keV band, which implies that the lower limit of magnetic field strength becomes 0.7 mu G.

DOI： 10.1093/pasj/psx095

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Photonuclear reactions triggered by lightning discharge Reviewed

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

NATURE Vol. 551 ( 7681 ) page： 481 - + 2017.11

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Language：English Publishing type：Research paper (scientific journal) Publisher：NATURE PUBLISHING GROUP

Lightning and thunderclouds are natural particle accelerators(1). Avalanches of relativistic runaway electrons, which develop in electric fields within thunderclouds(2,3), emit bremsstrahlung gamma-rays. These gamma-rays have been detected by ground-based observatories(4-9), by airborne detectors(10) and as terrestrial gamma-ray flashes from space(10-14). The energy of the gamma-rays is sufficiently high that they can trigger atmospheric photonuclear reactions(10,15-19) that produce neutrons and eventually positrons via beta(+) decay of the unstable radioactive isotopes, most notably N-13, which is generated via N-14 + gamma -> N-13 + n, where gamma denotes a photon and n a neutron. However, this reaction has hitherto not been observed conclusively, despite increasing observational evidence of neutrons(7,20,21) and positrons(10,22) 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 gamma-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 gamma-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 time-scale and spectral cutoff at about 10 megaelectronvolts of the gamma-ray afterglow are well explained by de-excitation gamma-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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Solar abundance ratios of the iron-peak elements in the Perseus cluster Reviewed

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

NATURE Vol. 551 ( 7681 ) page： 478 - + 2017.11

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Language：English Publishing type：Research paper (scientific journal) Publisher：NATURE PUBLISHING GROUP

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

DOI： 10.1038/nature24301

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Suzaku Wide-band All-sky Monitor (WAM) observations of GRBs and SGRs Reviewed

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

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN Vol. 69 ( 3 ) 2017.6

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Language：English Publisher：OXFORD UNIV PRESS

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: Bi4Ge3O12) 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 (similar to 600 cm(2) at 1MeV 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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A hard-to-soft state transition of Aquila X-1 observed with Suzaku Reviewed

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

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN Vol. 69 ( 2 ) 2017.4

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Language：English Publishing type：Research paper (scientific journal) Publisher：OXFORD UNIV PRESS

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 similar to 30 ks. Across the transition, the 0.8-10 keV X-Ray Imaging Spectrometer count rate increased by a factor similar to 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 x 10(37) erg s(-1) to 5.1 x 10(37) 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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Suzaku observations of the merging galaxy cluster Abell 2255: The northeast radio relic Reviewed

H. Akamatsu, M. Mizuno, N. Ota, Y-Y. Zhang, R. J. van Weeren, H. Kawahara, Y. Fukazawa, J. S. Kaastra, M. Kawaharada, K. Nakazawa, T. Ohashi, H. J. A. Rottgering, M. Takizawa, J. Vink, F. Zandanel

ASTRONOMY & ASTROPHYSICS Vol. 600 page： A100 2017.4

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Language：English Publishing type：Research paper (scientific journal) Publisher：EDP SCIENCES S A

We present the results of deep 140 ks Suzaku X-ray observations of the north-east (NE) radio relic of the merging galaxy cluster Abell 2255. The temperature structure of Abell 2255 is measured out to 0.9 times the virial radius (1.9 Mpc) in the NE direction for the first time. The Suzaku temperature map of the central region suggests a complex temperature distribution, which agrees with previous work. Additionally, on a larger-scale, we confirm that the temperature drops from 6 keV around the cluster center to 3 keV at the outskirts, with two discontinuities at r similar to 5' (450 kpc) and similar to 12' (1100 kpc) from the cluster center. Their locations coincide with surface brightness discontinuities marginally detected in the XMM-Newton image, which indicates the presence of shock structures. From the temperature drop, we estimate the Mach numbers to be M-inner similar to 1.2 and, M-outer similar to 1:4. The first structure is most likely related to the large cluster core region (similar to 350-430 kpc), and its Mach number is consistent with the XMM-Newton observation (M similar to 1.24: Sakelliou & Ponman 2006, MNRAS, 367, 1409). Our detection of the second temperature jump, based on the Suzaku key project observation, shows the presence of a shock structure across the NE radio relic. This indicates a connection between the shock structure and the relativistic electrons that generate radio emission. Across the NE radio relic, however, we find a significantly lower temperature ratio (T-1/T-2 similar to 1.44 +/- 0.16 corresponds to M-X (ray) similar to 1.4) than the value expected from radio wavelengths, based on the standard diffusive shock acceleration mechanism (T-1/T-2 > 3.2 or M-Radio > 2.8). This may suggest that under some conditions, in particular the NE relic of A2255 case, the simple diffusive shock acceleration mechanism is unlikely to be valid, and therefore, more a sophisticated mechanism is required.

DOI： 10.1051/0004-6361/201628400

Web of Science
Hitomi Constraints on the 3.5 keV Line in the Perseus Galaxy Cluster Reviewed

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

ASTROPHYSICAL JOURNAL LETTERS Vol. 837 ( 1 ) page： 668 - 672 2017.3

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Language：English Publishing type：Research paper (scientific journal) Publisher：IOP PUBLISHING LTD

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

DOI： 10.3847/2041-8213/aa61fa

Web of Science

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Suzaku and Chandra observations of CIZA J1700.8-3144, a cluster of galaxies in the Zone of Avoidance Reviewed

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

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN Vol. 69 ( 1 ) 2017.2

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Language：English Publishing type：Research paper (scientific journal) Publisher：OXFORD UNIV PRESS

We present the Chandra and Suzaku observations of 1RXS J170047.8-314442, located towards the Galactic bulge, to reveal a wide-band (0.3-10 keV) X-ray morphology and spectrum of this source. With the Chandra observation, no point source was found at the position of 1RXSJ170047.8-314442. 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-ray emission had a nearly circular shape with a spatial extent of similar to 3'.5, the surface brightness profile was not axisymmetric; a bright spot-like emission was found at similar to 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 beta-model; beta 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 similar to 6 keV, 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 keV and a redshift parameter of z = 0.1 +/- 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 1RXSJ170047.8-314442 by Kocevski et al. (2007, ApJ, 662, 224): CIZA J1700.8-3144, a member of the cluster catalogue in the Zone of Avoidance. The estimated bolometric X-ray luminosity of 5.9 x 10(44) erg s(-1) was among the lowest with this temperature, suggesting that this cluster is far from relaxed.

DOI： 10.1093/pasj/psw106

Web of Science

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Suzaku observations of spectral variations of the ultra-luminous X-ray source Holmberg IX X-1 Reviewed

Shogo B. Kobayashi, Kazuhiro Nakazawa, Kazuo Makishima

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN Vol. 69 ( 1 ) 2017.2

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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 >= 2 keV, with little change in the <= 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

Web of Science
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 Vol. 509 page： 509 - 514 2017

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Web of Science
The status of DECIGO Reviewed

Shuichi Sato, Seiji Kawamura, Masaki Ando, Takashi Nakamura, Kimio Tsubono, Akito Araya, Ikkoh Funaki, Kunihito Ioka, Nobuyuki Kanda, Shigenori Moriwaki, Mitsuru Musha, Kazuhiro Nakazawa, Kenji Numata, Shin Ichiro Sakai, Naoki Seto, Takeshi Takashima, Takahiro Tanaka, Kazuhiro Agatsuma, Koh Suke Aoyanagi, Koji Arai, Hideki Asada, Yoichi Aso, Takeshi Chiba, Toshikazu Ebisuzaki, Yumiko Ejiri, Motohiro Enoki, Yoshiharu Eriguchi, Masa Katsu Fujimoto, Ryuichi Fujita, Mitsuhiro Fukushima, Toshifumi Futamase, Katsuhiko Ganzu, Tomohiro Harada, Tatsuaki Hashimoto, Kazuhiro Hayama, Wataru Hikida, Yoshiaki Himemoto, Hisashi Hirabayashi, Takashi Hiramatsu, Feng Lei Hong, Hideyuki Horisawa, Mizuhiko Hosokawa, Kiyotomo Ichiki, Takeshi Ikegami, Kaiki T. Inoue, Koji Ishidoshiro, Hideki Ishihara, Takehiko Ishikawa, Hideharu Ishizaki, Hiroyuki Ito, Yousuke Itoh, Nobuki Kawashima, Fumiko Kawazoe, Naoko Kishimoto, Kenta Kiuchi, Shiho Kobayashi, Kazunori Kohri, Hiroyuki Koizumi, Yasufumi Kojima, Keiko Kokeyama, Wataru Kokuyama, Kei Kotake, Yoshihide Kozai, Hideaki Kudoh, Hiroo Kunimori, Hitoshi Kuninaka, Kazuaki Kuroda, Kei Ichi Maeda, Hideo Matsuhara, Yasushi Mino, Osamu Miyakawa, Shinji Miyoki, Mutsuko Y. Morimoto, Tomoko Morioka, Toshiyuki Morisawa, Shinji Mukohyama, Shigeo Nagano, Isao Naito, Kouji Nakamura, Hiroyuki Nakano, Kenichi Nakao, Shinichi Nakasuka, Yoshinori Nakayama, Erina Nishida, Kazutaka Nishiyama, Atsushi Nishizawa, Yoshito Niwa, Taiga Noumi, Yoshiyuki Obuchi, Masatake Ohashi, Naoko Ohishi, Masashi Ohkawa, Norio Okada, Kouji Onozato, Kenichi Oohara, Norichika Sago, Motoyuki Saijo, Masaaki Sakagami, Shihori Sakata, Misao Sasaki

Journal of Physics: Conference Series Vol. 840 ( 1 ) 2017

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Language：Japanese Publishing type：Research paper (international conference proceedings)

© Published under licence by IOP Publishing Ltd. 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

Web of Science

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

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

20TH EUROPEAN WHITE DWARF WORKSHOP Vol. 509 page： 509 - 514 2017

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Language：English Publishing type：Research paper (international conference proceedings) Publisher：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
Improvement of scintillator's reflector toward the improvement of the performance for Compton scattering type polarimeter

Saito Yo, Gunji Shuichi, Nakamori Takeshi, Okumura Akira, Nakazawa Kazuhiro, Kurosawa Shunsuke, Watanabe Naoki, Karube Atsuhito

Meeting Abstracts of the Physical Society of Japan Vol. 72.2 ( 0 ) page： 414 - 414 2017

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Language：Japanese Publisher：The Physical Society of Japan

DOI： 10.11316/jpsgaiyo.72.2.0_414

CiNii Research
Focusing on relativistic universe and cosmic evolution: The FORCE mission

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

Proceedings of Science 2017

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Publishing type：Research paper (international conference proceedings)

The Focusing On Relativistic universe and Cosmic Evolution (FORCE) mission is proposed as a future Japan-lead X-ray observatory to be launched in the mid 2020s. FORCE is a successor of Hitomi, focusing on the braodband X-ray imaging spectroscopy in 1–80 keV with a significantly higher angular resolution of < 15′′ in half-power diameter. The sensitivity above 10 keV will be 10 times higher than that of any previous hard X-ray missions with simultaneous soft X-ray coverage. The satellite is planned to be launched by the Epsilon vehicle by ISAS/JAXA. In the current design concept, FORCE is equipped with three identical pairs of supermirrors and wideband X-ray detectors. The focal length of the mirrors is 10 m. The silicon mirror with multi-layer coating is our primary choice of optics to achieve a good angular resolution for the wide energy band while maintaining a light weight. The detector is a hybrid of a SOI-CMOS silicon-pixel detector and a CdTe detector responsible for the softer and harder energy bands, respectively. It is basically a descendant of the hard X-ray imager onboard Hitomi with its soft-band detector replaced with the SOI-CMOS. The primary scientific objective of the FORCE mission is to trace the cosmic formation history by searching for “missing black holes” in the entire range of the mass spectrum of BHs: “buried” supermassive black holes (SMBHs) (> 104 M), intermediate-mass black holes (102–104 M), and “orphan” stellar-mass black holes (< 102 M). Also, investigation of the nature of relativistic particles at various astrophysical shocks is in our scope, with high-angular-resolution X-ray observations with the broadband coverage. FORCE will open a new era in these fields.

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Books 3

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（ Role： Joint author）

天文月報 2016.11

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X 線、γ線で探る宇宙の構造と進化

高橋忠幸, 中澤知洋（ Role： Joint author）

応用物理学会誌 2012

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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（ Role： Joint author）

天文月報, 2002.7

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MISC 71

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 Vol. 2021 2021

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A wide-band X-ray observatory FORCE: Mission and Spacecraft design study improvements in 2020

中澤知洋, 森浩二, 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, 石田学, 渡辺伸, 山口弘悦, 大橋隆哉, 中嶋大, 古澤彰浩, 鶴剛, 上田佳宏, 田中孝明, 内田裕之, 松本浩典, 野田博文, 常深博, 信川正順, 太田直美, 信川久実子, 伊藤真之, 粟木久光, 寺島雄一, 深沢泰司, 水野恒史, 高橋弘充, 武田彩希, 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) Vol. 76 ( 1 ) 2021

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multiple long burst that terminated by lightning on January 2020

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) Vol. 75 ( 2 ) 2020

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A wide-band X-ray observatory FORCE: Science study and proposal status update

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) Vol. 75 ( 2 ) 2020

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Development of solar neutron and gamma-ray detector for 3U CubeSat

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) Vol. 75 ( 1 ) 2020

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Gamma-ray Observation of Winter Thunderclouds: the progress of multi - point observation in 2019

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) Vol. 2020 2020

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Gamma-ray Observation of Winter Thundercloud: Progress of multi-point observation in 2019

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) Vol. 75 ( 1 ) 2020

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Gamma-ray Observation of Winter Thunderclouds: Long-distance tracking of gamma-ray glow observed in December 2014 with monitoring posts

辻結菜, 中澤知洋, 久富章平, 榎戸輝揚, 和田有希, 湯浅孝行, 古田禄大, 土屋晴文, 楳本大悟, 篠田太郎, 加藤雅也

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

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Gamma-ray Observation of Winter Thunderclouds: Long-distance tracking of long burst with monitoring posts

辻結菜, 中澤知洋, 久富章平, FABIANI Alexia, 榎戸輝揚, 和田有希, 和田有希, 湯浅考行, 古田禄大, 土屋晴文, 楳本大悟, 篠田太郎, 加藤雅也

日本地球惑星科学連合大会予稿集(Web) Vol. 2020 2020

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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 Vol. 112 page： 471 - 473 2019.7
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) Vol. 74 ( 1 ) page： ROMBUNNO.14aK407‐11 2019.3

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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) Vol. 2019 page： ROMBUNNO.1H07 2019.3

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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) Vol. 2019 page： ROMBUNNO.MIS27‐10 (WEB ONLY) 2019

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J-GLOBAL
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) Vol. 2019 2019

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J-GLOBAL
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 Vol. 2019 2019

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J-GLOBAL
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 Vol. 2019 2019

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J-GLOBAL
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

Meeting Abstracts of the Physical Society of Japan Vol. 73 page： 492 - 492 2018.10

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

DOI： 10.11316/jpsgaiyo.73.1.0_492

arXiv
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 Vol. 2018 page： 227 2018.8

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J-GLOBAL
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 Vol. 2018 page： 156 2018.8

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J-GLOBAL
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 Vol. 2018 page： 220 2018.8

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J-GLOBAL
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

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN Vol. 70 ( 4 ) 2018.5

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Language：English Publishing type：Internal/External technical report, pre-print, etc. Publisher：OXFORD UNIV PRESS

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

DOI： 10.1093/pasj/psy069

Web of Science

arXiv
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) Vol. 73 ( 1 ) page： ROMBUNNO.25pK307‐5 2018.3

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J-GLOBAL
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) Vol. 73 ( 1 ) page： ROMBUNNO.22pK305‐7 - 176 2018.3

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Language：Japanese Publisher：The Physical Society of Japan

DOI： 10.11316/jpsgaiyo.73.1.0_176

CiNii Research

J-GLOBAL
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) Vol. 73 ( 1 ) page： ROMBUNNO.22aK308‐7 - 422 2018.3

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DOI： 10.11316/jpsgaiyo.73.1.0_422

CiNii Research

J-GLOBAL
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) Vol. 73 ( 1 ) page： ROMBUNNO.22aK308‐8 - 423 2018.3

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DOI： 10.11316/jpsgaiyo.73.1.0_423

J-GLOBAL
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) Vol. 73 ( 1 ) page： ROMBUNNO.22aK307‐7 - 414 2018.3

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DOI： 10.11316/jpsgaiyo.73.1.0_414

CiNii Research

J-GLOBAL
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) Vol. 2018 page： ROMBUNNO.3E01 2018.3

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J-GLOBAL
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 Vol. 2018 page： 239 2018.2

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J-GLOBAL
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 Vol. 2018 page： 71 2018.2

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J-GLOBAL
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 Vol. 2018 page： 239 2018.2

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J-GLOBAL
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 Vol. 2018 page： 231 2018.2

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J-GLOBAL
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 Vol. 2018 page： 171 2018.2

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J-GLOBAL
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 Vol. 2018 page： 240 2018.2

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J-GLOBAL
「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 Vol. 2018 page： 227 2018.2

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J-GLOBAL
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 Vol. 2018 page： 228 2018.2

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J-GLOBAL
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 Vol. 2018 page： 148 2018.2

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J-GLOBAL
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) Vol. 72 ( 2 ) page： ROMBUNNO.13pU32‐6 2017.9

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J-GLOBAL
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) Vol. 72 ( 2 ) page： ROMBUNNO.15aU33‐4 - 412 2017.9

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DOI： 10.11316/jpsgaiyo.72.2.0_412

J-GLOBAL
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) Vol. 72 ( 2 ) page： ROMBUNNO.15aU33‐5 - 413 2017.9

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DOI： 10.11316/jpsgaiyo.72.2.0_413

J-GLOBAL
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) Vol. 72 ( 2 ) page： ROMBUNNO.15aU33‐6 2017.9

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J-GLOBAL
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 Vol. 2017 page： 262 2017.8

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J-GLOBAL
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 Vol. 2017 page： 186 2017.8

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J-GLOBAL
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 Vol. 2017 page： 184 2017.8

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J-GLOBAL
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 Vol. 2017 page： 242 2017.8

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J-GLOBAL
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 Vol. 2017 page： 275 2017.8

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J-GLOBAL
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 Vol. 2017 page： 175 2017.8

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J-GLOBAL
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 Vol. 2017 page： 242 2017.8

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J-GLOBAL
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 Vol. 2017 page： 186 2017.8

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J-GLOBAL
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 Vol. 2017 page： 148 2017.8

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J-GLOBAL
「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 Vol. 2017 page： 246 2017.8

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「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 Vol. 2017 page： 147 2017.8

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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) Vol. 72 ( 1 ) page： ROMBUNNO.20aK21‐5 - 508 2017.3

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DOI： 10.11316/jpsgaiyo.72.1.0_508

J-GLOBAL
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) Vol. 72 ( 1 ) page： ROMBUNNO.19pK41‐9 - 501 2017.3

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DOI： 10.11316/jpsgaiyo.72.1.0_501

J-GLOBAL
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) Vol. 72 ( 1 ) page： ROMBUNNO.19pK41‐7 - 499 2017.3

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DOI： 10.11316/jpsgaiyo.72.1.0_499

J-GLOBAL
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) Vol. 72 ( 1 ) page： ROMBUNNO.19pK41‐8 - 500 2017.3

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DOI： 10.11316/jpsgaiyo.72.1.0_500

J-GLOBAL
長周期の連星X線パルサーは1013G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) Vol. 72 ( 1 ) page： ROMBUNNO.17pK41‐8 2017.3

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J-GLOBAL
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 Vol. 2017 page： 141 2017.2

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J-GLOBAL
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 Vol. 2017 page： 179 2017.2

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J-GLOBAL
長周期X線パルサーX Perseiが>1013G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 Vol. 2017 page： 250 2017.2

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J-GLOBAL
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 Vol. 2017 page： 233 2017.2

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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 Vol. 2017 page： 55 2017.2

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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 Vol. 2017 page： 190 2017.2

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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 Vol. 2017 page： 180 2017.2

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J-GLOBAL
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 Vol. 2017 page： 190 2017.2

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「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 Vol. 2017 page： 259 2017.2

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J-GLOBAL
「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 Vol. 2017 page： 186 2017.2

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J-GLOBAL
In-orbit performance of the hard X-ray and soft gamma-ray instruments onboard Hitomi

2017.1

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17th Space Science Symposium (January 5-6, 2017. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS)Sagamihara Campus), Sagamihara, Kanagawa Japan
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) Vol. 2017 page： ROMBUNNO.MIS18‐05 (WEB ONLY) 2017

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Gamma-ray Observation of Accelerated Electrons in the Thunderstorm Electric Fields: Development of Data Acquisition System and Operation of Multipoint Observation in Hokuriku

Wada Y., Makishima K., Kamogawa M., Takita M., Yonetoku D., Sawano T., Watarai K., Yoneguchi K., Kimura K., Kitano K., the GROWTH collaboration collaboration, Enoto T., Yuasa T., Nakazawa K., Tsuchiya H., Nakano T., Okuda K., Furuta Y., Umemoto D.

Meeting Abstracts of the Physical Society of Japan Vol. 72 ( 0 ) page： 503 - 503 2017

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DOI： 10.11316/jpsgaiyo.72.1.0_503

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Gamma-ray Observation of Accelerated Electrons in the Thunderstorm Electric Fields: New Development to A Multipoint Observation Network

Enoto T., Makishima K., Kamogawa M., Takita M., Yonetoku D., Sawano T., Watarai K., Yoneguchi K., Kimura K., Kitano K., the GROWTH collaboration collaboration, Wada Y., Yuasa T., Nakazawa K., Tsuchiya H., Nakano T., Okuda K., Furuta Y., Umemoto D.

Meeting Abstracts of the Physical Society of Japan Vol. 72 ( 0 ) page： 502 - 502 2017

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DOI： 10.11316/jpsgaiyo.72.1.0_502

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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) Vol. 2017 page： ROMBUNNO.MIS05‐02 (WEB ONLY) 2017

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To the head of MISC.▲

Research Project for Joint Research, Competitive Funding, etc. 2

雷放電からのガンマ線放射が人々に与えうる被曝量の最大値を求める測定装置の開発

2021.8 - 2023.3

公益財団法人立松財団研究助成

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Authorship：Principal investigator Grant type：Competitive

Grant amount：\3000000 （ Direct Cost: \3000000 ）
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？

2020.4 - 2021.3

研究助成

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Grant amount：\1000000

To the head of Research Project for Joint Research, Competitive Funding, etc..▲

KAKENHI (Grants-in-Aid for Scientific Research) 9

Study of the expansion and contraction of the upper atmosphere realized by the world's first dedicated atmospheric X-ray observation instrument aboard the ISS

Grant number：23H00151 2023.4 - 2027.3

Japan Society for the Promotion of Science Grants-in-Aid for Scientific Research Grant-in-Aid for Scientific Research (A)

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Study on the lightning initiation problem via observations of high-energy atmospheric phenomena

Grant number：22H00145 2022.4 - 2026.3

Japan Society for the Promotion of Science Grants-in-Aid for Scientific Research Grant-in-Aid for Scientific Research (A)

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High resolution study of MeV gamma-ray flashes from lightning discharges using high-speed semiconductor imagers

Grant number：21H00166 2021.4 - 2023.3

Japan Society for the Promotion of Science Grants-in-Aid for Scientific Research Grant-in-Aid for Scientific Research on Innovative Areas (Research in a proposed research area)

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Authorship：Principal investigator

Grant amount：\6630000 （ Direct Cost: \5100000 、 Indirect Cost：\1530000 ）
Opening of MeV astronomy with semiconductor Compton camera

Grant number：20H00157 2020.4 - 2024.3

Japan Society for the Promotion of Science Grants-in-Aid for Scientific Research Grant-in-Aid for Scientific Research (A)

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Grant amount：\44850000 （ Direct Cost: \34500000 、 Indirect Cost：\10350000 ）
Study of high timing resolution imaging of Terrestrial Gamma-ray Flashes from aircrafts

Grant number：19K21899 2019.6 - 2021.3

Japan Society for the Promotion of Science Grants-in-Aid for Scientific Research Grant-in-Aid for Challenging Research (Exploratory)

Nakazawa Kazuhiro

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Grant amount：\6370000 （ Direct Cost: \4900000 、 Indirect Cost：\1470000 ）

The Terrestrial Gamma-ray Flash (TGF), a sudden MeV gamma ray synchronized with lightning discharges, is so powerful that it can be observed from satellites, and its observational understanding is important because the radiation dose of aircraft flying near the electron acceleration regions in thunderclouds can be large. Because of the extremely high luminosity, we have developed a new detector demonstrator that uses Cherenkov light instead of the conventional scintillator detector. The direction of incidence of gamma rays can also be determined by measuring both ends of the acrylic rod with the MPPC. Although we could not conduct experiments with a 10 MeV gamma-ray source due to COVID19, we verified the direction measurements using cosmic rays. We succeeded in establishing a compact, lightweight, and low-power-consumption prototype of the device.
Investigation on photonuclear reactions associated with electron acceleration in lightning and thunderclouds

Grant number：18H01236 2018.4 - 2021.3

Japan Society for the Promotion of Science Grants-in-Aid for Scientific Research Grant-in-Aid for Scientific Research (B)

TSUCHIYA Harufumi

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Lightning and thunderclouds generate X rays by bremsstrahlung, similar to X-ray generators in the medical field. Recently, it has been found that in addition to the generation of X rays and gamma rays, high-energy bremsstrahlung photons from lightning collide with atomic nuclei, causing a photonuclear reaction in which neutrons are produced. In this study, we investigated the details of the gamma-ray flashes that cause photonuclear reactions. As a result, it was estimated that quintillion high-energy electrons contribute to the gamma-ray flash, and the produced neutrons spread over 1 km from the production point, with a decay time of about 50 milliseconds.
Observations of free precession of magnetars and estimation of their internal magnetic fields

Grant number：15H03653 2015.4 - 2018.3

Japan Society for the Promotion of Science Grants-in-Aid for Scientific Research Grant-in-Aid for Scientific Research (B)

Makishima Kazuo

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Authorship：Coinvestigator(s)

Using the Suzaku observatory, we had discovered long-period phase-modulation effects in the hard X-ray pulses from two mangetars. This was interpreted as a result of free precession in neutron stars that are axially deformed by ultra-strong toroidal fields hidden in them. In the present study, we analyzed X-ray data of these two magnetars obtained with the US NuSTAR satellite, and successfully reconfirmed the pulse-phase modulation effects in both objects. However, the modulation amplitudes in these objects were considerably different from those measured with Suzaku. In another magnetar observed with Suzaku in 2010, a similar phase modulation phenomenon in the hard X-ray pulses was discovered at a period of 48 ksec. Using the X-ray data from the MAXI observatory, we studied relations between the X-ray intensities and pulse-peiriod derivatives of various binary X-ray pulsars. Then, the object named X Perses was found to have magnetic fields which are comparable to those of magnetars.
Observing where the huge kinetic energy from merging clusters of galaxies goes

Grant number：15H03639 2015.4 - 2018.3

Japan Society for the Promotion of Science Grants-in-Aid for Scientific Research Grant-in-Aid for Scientific Research (B)

Nakazawa Kazuhiro, TAKIZAWA MOTOKAZU, KATO YUICHI

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Authorship：Principal investigator

Grant amount：\16380000 （ Direct Cost: \12600000 、 Indirect Cost：\3780000 ）

Kinetic energy released in merging cluster of galaxies initiates, hot gas heating, turbulence, particle acceleration, and magnetic field amplification. To understand how the initial energy is converted into those non-thermal energies, we performed two research works. Firstly, we observed the early-phase merging cluster CIZA J1358.9-4750 with three X-ray observatories and GHz radio, and confirmed it is really in its early phase. Secondly, we aimed at observing such merging clusters with ASTRO-H satellite, capable of fine doppler imaging and high-temperature hottest gas detection. In this work, we performed optimization of detector operation and analysis parameters of the Hard X-ray Imager (HXI). After the launch in 2016/2. we verified the world's best sensitivity of the HXI in orbit. Right before actual observations start, the satellite was lost. Based on these achievements, we obtained a set of technical lessons to be used for future high-sensitivity hard X-ray survey.
Study of nonthermal phenomena of galaxy clusters through next generation multiwave obserbations and theoretical simulations

Grant number：26400218 2014.4 - 2018.3

Japan Society for the Promotion of Science Grants-in-Aid for Scientific Research Grant-in-Aid for Scientific Research (C)

Takizawa Motokazu, NAKAZAWA Kazuhiro, KITAYAMA Tetsu

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Authorship：Collaborating Investigator(s) (not designated on Grant-in-Aid)

We investigated the particle acceleration processes and physical status of the galaxy cluster radio relics through X-ray and radio observations, and constructed a theoretical model for them.In particular,we showed that the particle acceleration processes in the "toothbrush" radio relic cannot be explained by a simple diffusive shock acceleration model.We conducted SZ observations by ALMA with a spatial resolution of 5 arcsec, which is the highest ever, and found that the very high temperature component is located in the significantly different position from the X-ray peak. We contributed the PASJ invited review paper about the cosmic magnetism in low frequency radio astronomy as a coauther.

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To the head of KAKENHI (Grants-in-Aid for Scientific Research).▲