Curriculum Vitaes
Profile Information
- Affiliation
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency
- Degree
- 理学博士(中央大学)理学修士(中央大学)
- J-GLOBAL ID
- 201201017168289883
- researchmap Member ID
- 7000000018
Research Interests
2Research Areas
2Education
4-
- 2011
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- 2008
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- 2002
Committee Memberships
1-
2012
Papers
27-
Monthly Notices of the Royal Astronomical Society, 484(2) 2229-2233, Apr, 2019 Peer-reviewed
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PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, 70(6), Oct 1, 2018
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Astrophysical Journal, Supplement Series, 238(2), Oct, 2018
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PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, 70(3), Jun, 2018 Peer-reviewed
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Journal of Astronomical Telescopes, Instruments, and Systems, 4(2), Apr, 2018 Peer-reviewed
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Astrophysical Journal, Supplement Series, 235(1), Mar, 2018
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PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, 70(2), Mar, 2018 Peer-reviewed
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PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, 70(2), Mar, 2018 Peer-reviewed
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PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, 70(2), Mar, 2018 Peer-reviewed
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Publications of the Astronomical Society of Japan, 70(2), Mar 1, 2018 Peer-reviewed
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PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, 70(2), Mar, 2018 Peer-reviewed
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PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, 70(2), Mar, 2018 Peer-reviewed
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PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, 70(2), Mar, 2018 Peer-reviewed
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PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, 70(2), Mar, 2018 Peer-reviewed
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PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, 70(2), Mar, 2018 Peer-reviewed
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Feb 14, 2018We 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 Peer-reviewed
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NATURE, 551(7681) 478-+, Nov, 2017 Peer-reviewed
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ASTROPHYSICAL JOURNAL, 832(2), Dec, 2016 Peer-reviewed
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Publications of the Astronomical Society of Japan, 68(5), Oct 1, 2016 Peer-reviewed
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ApJ, 837, L15 (2017), 837, Jul 26, 2016
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NATURE, 535(7610) 117-+, Jul, 2016 Peer-reviewed
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SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY, 9905, 2016 Peer-reviewed
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PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, 67(6) p.121, Dec, 2015
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Société Royale des Sciences de Liège, Bulletin, 80 724-728, Jan, 2011
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ASTRONOMY & ASTROPHYSICS, 490(1) 259-264, Oct, 2008
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PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, 60 S49-S56, Feb, 2008 Peer-reviewed
Misc.
16-
Proceedings of Science, Jan 1, 2017
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Nov 4, 2015Colliding 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, Sep, 2014
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Suzaku-MAXI 2014: Expanding the Frontiers of the X-ray Universe, pp.pp208-209, Sep, 2014
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Suzaku-MAXI 2014: Expanding the Frontiers of the X-ray Universe, pp.pp164-165, Sep, 2014
Presentations
68Professional Memberships
3Works
1Research Projects
3-
科学研究費補助金 若手研究(B), Apr, 2016 - Mar, 2019
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科学研究費補助金 特別研究促進費, Apr, 2009 - Mar, 2011
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2005
