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 招聘研究開発員
- 学位
- 理学博士(中央大学)理学修士(中央大学)
- J-GLOBAL ID
- 201201017168289883
- researchmap会員ID
- 7000000018
学歴
4-
- 2011年
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- 2008年
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- 2006年
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- 2002年
委員歴
1-
2012年
論文
27-
Monthly Notices of the Royal Astronomical Society 484(2) 2229-2233 2019年4月 査読有り
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Astrophysical Journal, Supplement Series 238(2) 2018年10月
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PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 70(3) 2018年6月 査読有り
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Journal of Astronomical Telescopes, Instruments, and Systems 4(2) 2018年4月 査読有り
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Astrophysical Journal, Supplement Series 235(1) 2018年3月
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PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 70(2) 2018年3月 査読有り
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PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 70(2) 2018年3月 査読有り
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PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 70(2) 2018年3月 査読有り
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Publications of the Astronomical Society of Japan 70(2) 2018年3月1日 査読有り
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PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 70(2) 2018年3月 査読有り
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PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 70(2) 2018年3月 査読有り
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PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 70(2) 2018年3月 査読有り
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PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 70(2) 2018年3月 査読有り
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PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 70(2) 2018年3月 査読有り
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2018年2月14日We present results from the Hitomi X-ray observation of a young<br /> composite-type supernova remnant (SNR) G21.5$-$0.9, whose emission is dominated<br /> by the pulsar wind nebula (PWN) contribution. The X-ray spectra in the 0.8-80<br /> keV range obtained with the Soft X-ray Spectrometer (SXS), Soft X-ray Imager<br /> (SXI) and Hard X-ray Imager (HXI) show a significant break in the continuum as<br /> previously found with the NuSTAR observation. After taking into account all<br /> known emissions from the SNR other than the PWN itself, we find that the Hitomi<br /> spectra can be fitted with a broken power law with photon indices of<br /> $\Gamma_1=1.74\pm0.02$ and $\Gamma_2=2.14\pm0.01$ below and above the break at<br /> $7.1\pm0.3$ keV, which is significantly lower than the NuSTAR result ($\sim9.0$<br /> keV). The spectral break cannot be reproduced by time-dependent particle<br /> injection one-zone spectral energy distribution models, which strongly<br /> indicates that a more complex emission model is needed, as suggested by recent<br /> theoretical models. We also search for narrow emission or absorption lines with<br /> the SXS, and perform a timing analysis of PSR J1833$-$1034 with the HXI and<br /> SGD. No significant pulsation is found from the pulsar. However, unexpectedly,<br /> narrow absorption line features are detected in the SXS data at 4.2345 keV and<br /> 9.296 keV with a significance of 3.65 $\sigma$. While the origin of these<br /> features is not understood, their mere detection opens up a new field of<br /> research and was only possible with the high resolution, sensitivity and<br /> ability to measure extended sources provided by an X-ray microcalorimeter.
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SPACE TELESCOPES AND INSTRUMENTATION 2018: ULTRAVIOLET TO GAMMA RAY 10699 2018年 査読有り
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NATURE 551(7681) 478-+ 2017年11月 査読有り
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ASTROPHYSICAL JOURNAL 832(2) 2016年12月 査読有り
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Publications of the Astronomical Society of Japan 68(5) 2016年10月1日 査読有り
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ApJ, 837, L15 (2017) 837 2016年7月26日
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NATURE 535(7610) 117-+ 2016年7月 査読有り
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SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY 9905 2016年 査読有り
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Publications of the Astronomical Society of Japan 67(6) p.121 2015年12月
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Société Royale des Sciences de Liège, Bulletin 80 724-728 2011年1月
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ASTRONOMY & ASTROPHYSICS 490(1) 259-264 2008年10月
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PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 60 S49-S56 2008年2月 査読有り
MISC
16-
Proceedings of Science 2017年1月1日
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2015年11月4日Colliding Wolf-Rayet (WR) winds produce thermal X-ray emission widely<br /> observed by X-ray telescopes. In wide WR+O binaries, such as WR 140, the X-ray<br /> flux is tied to the orbital phase, and is a direct probe of the winds'<br /> properties. In the Galactic center, $\sim$30 WRs orbit the super massive black<br /> hole (SMBH) within $\sim$10", leading to a smorgasbord of wind-wind collisions.<br /> To model the X-ray emission of WR 140 and the Galactic center, we perform 3D<br /> hydrodynamic simulations to trace the complex gaseous flows, and then carry out<br /> 3D radiative transfer calculations to compute the variable X-ray spectra. The<br /> model WR 140 RXTE light curve matches the data well for all phases except the<br /> X-ray minimum associated with periastron, while the model spectra agree with<br /> the RXTE hardness ratio and the shape of the Suzaku observations throughout the<br /> orbit. The Galactic center model of the Chandra flux and spectral shape match<br /> well in the region r$<$3", but the model flux falls off too rapidly beyond this<br /> radius.
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Suzaku-MAXI 2014: Expanding the Frontiers of the X-ray Universe pp.pp220-221 2014年9月
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Suzaku-MAXI 2014: Expanding the Frontiers of the X-ray Universe pp.pp208-209 2014年9月
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Suzaku-MAXI 2014: Expanding the Frontiers of the X-ray Universe pp.pp164-165 2014年9月
講演・口頭発表等
68所属学協会
3Works(作品等)
1共同研究・競争的資金等の研究課題
3-
科学研究費補助金 若手研究(B) 2016年4月 - 2019年3月
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科学研究費補助金 特別研究促進費 2009年4月 - 2011年3月
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2005年