研究者業績
基本情報
- 所属
- 国立研究開発法人宇宙航空研究開発機構 宇宙科学研究所 宇宙物理学研究系 教授総合研究大学院大学 先端学術院 宇宙科学コース 教授東京科学大学 理学院物理学系物理学コース 特定教授関西学院大学 大学院理工学研究科 客員教授
- 学位
- 理学博士(東京大学)
- J-GLOBAL ID
- 200901025041369206
- researchmap会員ID
- 1000144439
専門はＸ線天文学。特に、中性子星やブラックホールを含むX線連星の観測的研究および衛星搭載X線CCDカメラの開発研究。
受賞
1-
1996年
論文
231-
The Astrophysical Journal Letters 982(1) L5-L5 2025年3月12日Abstract We present XRISM Resolve observations of the core of the hot, relaxed galaxy cluster Abell 2029 (A2029). We find that the line-of-sight bulk velocity of the intracluster medium (ICM) within the central 180 kpc is at rest with respect to the brightest cluster galaxy, with a 3σ upper limit of ∣v bulk∣ < 100 km s−1. We robustly measure the field-integrated ICM velocity dispersion to be σ v = 169 ± 10 km s−1, obtaining similar results for both single-temperature and two-temperature plasma models to account for the cluster cool core. This result, if ascribed to isotropic turbulence, implies a subsonic ICM with Mach number and a nonthermal pressure fraction of 2.6 ± 0.3%. The turbulent velocity is similar to what was measured in the core of the Perseus cluster by Hitomi, but here in a more massive cluster with an ICM temperature of 7 keV, the limit on the nonthermal pressure fraction is even more stringent. Our result is consistent with expectations from simulations of relaxed clusters, but it is on the low end of the predicted distribution, indicating that A2029 is an exceptionally relaxed cluster with no significant impacts from either a recent minor merger or active galactic nucleus activity.
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Nature 638(8050) 365-369 2025年2月12日
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Publications of the Astronomical Society of Japan 2024年12月26日Abstract Sagittarius A East is a supernova remnant with a unique surrounding environment, as it is located in the immediate vicinity of the supermassive black hole at the Galactic center, Sagittarius A$^{*}$. The X-ray emission of the remnant is suspected to show features of overionized plasma, which would require peculiar evolutionary paths. We report on the first observation of Sagittarius A East with the X-Ray Imaging and Spectroscopy Mission (XRISM). Equipped with a combination of a high-resolution microcalorimeter spectrometer and a large field-of-view CCD imager, we for the first time resolved the Fe xxv K-shell lines into fine structure lines and measured the forbidden-to-resonance intensity ratio to be $1.39 \pm 0.12$, which strongly suggests the presence of overionized plasma. We obtained a reliable constraint on the ionization temperature just before the transition into the overionization state, of $\gt\! 4\:$keV. The recombination timescale was constrained to be $\lt\! 8 \times 10^{11} \:$cm$^{-3}\:$s. The small velocity dispersion of $109 \pm 6\:$km$\:$s$^{-1}$ indicates a low Fe ion temperature $\lt\! 8\:$keV and a small expansion velocity $\lt\! 200\:$km$\:$s$^{-1}$. The high initial ionization temperature and small recombination timescale suggest that either rapid cooling of the plasma via adiabatic expansion from dense circumstellar material or intense photoionization by Sagittarius A$^{*}$ in the past may have triggered the overionization.
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The Astrophysical Journal Letters 977(2) L34-L34 2024年12月11日Abstract The X-ray binary system Cygnus X-3 (4U 2030+40, V1521 Cyg) is luminous but enigmatic owing to the high intervening absorption. High-resolution X-ray spectroscopy uniquely probes the dynamics of the photoionized gas in the system. In this Letter, we report on an observation of Cyg X-3 with the XRISM/Resolve spectrometer, which provides unprecedented spectral resolution and sensitivity in the 2–10 keV band. We detect multiple kinematic and ionization components in absorption and emission whose superposition leads to complex line profiles, including strong P Cygni profiles on resonance lines. The prominent Fe xxv Heα and Fe xxvi Lyα emission complexes are clearly resolved into their characteristic fine-structure transitions. Self-consistent photoionization modeling allows us to disentangle the absorption and emission components and measure the Doppler velocity of these components as a function of binary orbital phase. We find a significantly higher velocity amplitude for the emission lines than for the absorption lines. The absorption lines generally appear blueshifted by ∼−500–600 km s−1. We show that the wind decomposes naturally into a relatively smooth and large-scale component, perhaps associated with the background wind itself, plus a turbulent, denser structure located close to the compact object in its orbit.
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Publications of the Astronomical Society of Japan 2024年10月10日Abstract We present an initial analysis of the X-Ray Imaging and Spectroscopy Mission (XRISM) first-light observation of the supernova remnant (SNR) N 132D in the Large Magellanic Cloud. The Resolve microcalorimeter has obtained the first high-resolution spectrum in the 1.6–10 keV band, which contains K-shell emission lines of Si, S, Ar, Ca, and Fe. We find that the Si and S lines are relatively narrow, with a broadening represented by a Gaussian-like velocity dispersion of $\sigma _v \sim 450$ km s$^{-1}$. However, the Fe He$\alpha$ lines are substantially broadened with $\sigma _v \sim 1670$ km s$^{-1}$. This broadening can be explained by a combination of the thermal Doppler effect due to the high ion temperature and the kinematic Doppler effect due to the SNR expansion. Assuming that the Fe He$\alpha$ emission originates predominantly from the supernova ejecta, we estimate the reverse shock velocity at the time when the bulk of the Fe ejecta were shock heated to be $-1000 \lesssim V_{\rm rs}$ (km s$^{-1}$) $\lesssim 3300$ (in the observer frame). We also find that Fe Ly$\alpha$ emission is redshifted with a bulk velocity of $\sim 890$ km s$^{-1}$, substantially larger than the radial velocity of the local interstellar medium surrounding N 132D. These results demonstrate that high-resolution X-ray spectroscopy is capable of providing constraints on the evolutionary stage, geometry, and velocity distribution of SNRs.
MISC
201-
Publications of the Astronomical Society of Japan 70(2) 2018年3月1日
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J. Astron. Telesc. Instrum. Syst. 4(1), 011211 (2018) 4(1) 2018年1月22日
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Proceedings of SPIE - The International Society for Optical Engineering 10699 2018年1月1日
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70(2) 2017年7月1日The Crab nebula originated from a core-collapse supernova (SN) explosion<br /> observed in 1054 A.D. When viewed as a supernova remnant (SNR), it has an<br /> anomalously low observed ejecta mass and kinetic energy for an Fe-core collapse<br /> SN. Intensive searches were made for a massive shell that solves this<br /> discrepancy, but none has been detected. An alternative idea is that the SN1054<br /> is an electron-capture (EC) explosion with a lower explosion energy by an order<br /> of magnitude than Fe-core collapse SNe. In the X-rays, imaging searches were<br /> performed for the plasma emission from the shell in the Crab outskirts to set a<br /> stringent upper limit to the X-ray emitting mass. However, the extreme<br /> brightness of the source hampers access to its vicinity. We thus employed<br /> spectroscopic technique using the X-ray micro-calorimeter onboard the Hitomi<br /> satellite. By exploiting its superb energy resolution, we set an upper limit<br /> for emission or absorption features from yet undetected thermal plasma in the<br /> 2-12 keV range. We also re-evaluated the existing Chandra and XMM-Newton data.<br /> By assembling these results, a new upper limit was obtained for the X-ray<br /> plasma mass of <~ 1Mo for a wide range of assumed shell radius, size, and<br /> plasma temperature both in and out of the collisional equilibrium. To compare<br /> with the observation, we further performed hydrodynamic simulations of the Crab<br /> SNR for two SN models (Fe-core versus EC) under two SN environments (uniform<br /> ISM versus progenitor wind). We found that the observed mass limit can be<br /> compatible with both SN models if the SN environment has a low density of <~<br /> 0.03 cm-3 (Fe core) or <~ 0.1 cm-3 (EC) for the uniform density, or a<br /> progenitor wind density somewhat less than that provided by a mass loss rate of<br /> 10-5 Mo yr-1 at 20 km s-1 for the wind environment.
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ASTROPHYSICAL JOURNAL LETTERS 837(1) 2017年3月
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SPACE TELESCOPES AND INSTRUMENTATION 2016: OPTICAL, INFRARED, AND MILLIMETER WAVE 9904 2016年 査読有り
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日本物理学会講演概要集 69(2) 37-37 2014年8月22日
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日本物理学会講演概要集 69(1) 129-129 2014年3月5日
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日本物理学会講演概要集 68(1) 134-134 2013年3月26日
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PASJ : publications of the Astronomical Society of Japan 64(5) "112-1"-"112-11" 2012年10月25日
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電子情報通信学会技術研究報告. SANE, 宇宙・航行エレクトロニクス 112(229) 17-22 2012年10月3日Japan Aerospace Exploration Agency (JAXA) has been developing an X-ray astronomy satellite named "ASTRO-H", which will be launched in 2014. This paper provides a summary of the design overview and development status of an electrical power subsystem for ASTRO-H. The subsystem consists of rigid solar array paddles that generate approximately 3500W at the end of life of the system, a power control unit that delivers an unregulated 50V bus power supply, shunt dissipators, battery charge control units, two 100-Ah Li-ion batteries, and a non-explosive actuator controller. Currently, manufacturing and verification tests for the satellite system have been implemented for the launch.
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日本物理学会講演概要集 67(2) 119-119 2012年8月24日
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日本物理学会講演概要集 67(2) 119-119 2012年8月24日
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Astrophysical Journal 753(2) 2012年7月10日
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PASJ : publications of the Astronomical Society of Japan 64(3) "53-1"-"53-12" 2012年6月25日
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日本物理学会講演概要集 67(1) 139-139 2012年3月5日
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SUZAKU 2011: Exploring the X-ray Universe: Suzaku and Beyond. AIP Conference Proceedings 1427 247-248 2012年3月
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SUZAKU 2011: EXPLORING THE X-RAY UNIVERSE: SUZAKU AND BEYOND 1427 253-254 2012年 査読有り
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日本物理学会講演概要集 66(2) 112-112 2011年8月24日
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日本物理学会講演概要集 65(2) 83-83 2010年8月18日
所属学協会
4-
2000年1月 - 現在
共同研究・競争的資金等の研究課題
15-
日本学術振興会 科学研究費助成事業 基盤研究(C) 2019年4月 - 2023年3月
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日本学術振興会 科学研究費助成事業 新学術領域研究(研究領域提案型) 2012年6月 - 2017年3月
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日本学術振興会 科学研究費助成事業 2012年4月 - 2015年3月
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日本学術振興会 科学研究費助成事業 基盤研究(B) 2010年4月 - 2013年3月
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日本学術振興会 科学研究費助成事業 特別研究員奨励費 2005年 - 2007年
● 指導学生等の数
1-
年度2021年度(FY2021)修士課程学生数2連携大学院制度による学生数2学術特別研究員数1
● 専任大学名
1-
専任大学名総合研究大学院大学（SOKENDAI)
