惑星分光観測衛星プロジェクトチーム
Profile Information
- Affiliation
- Institute of Space and Astronautical Science, Japan Aerospace Exploration AgencySchool of Physical Sciences, The Graduate University for Advanced Studies
- Degree
- 理学博士(Mar, 1998)
- J-GLOBAL ID
- 200901028844431929
- researchmap Member ID
- 5000050859
- External link
銀河、銀河団などの宇宙の大規模構造の形成と進化の研究。主にX線による観測を手段とします。
愛知県一宮高校卒業、
名古屋大学 理学部卒業、
東京大学理学系研究科 理学博士取得、
宇宙科学研究所、SRON(NL)にてポスドク。
現在、JAXA/宇宙科学研究所勤務。
愛知県一宮高校卒業、
名古屋大学 理学部卒業、
東京大学理学系研究科 理学博士取得、
宇宙科学研究所、SRON(NL)にてポスドク。
現在、JAXA/宇宙科学研究所勤務。
Major Research Interests
10Research Areas
2Research History
7-
Nov, 2020 - Present
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Nov, 2020 - Present
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Sep, 2020 - Present
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Apr, 2007 - Present
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Nov, 2020 - Mar, 2021
Awards
3Major Papers
73-
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, 71(3), Nov, 2018 Peer-reviewedWe present results of a search for unidentified line emission and absorption signals in the 2-12keV energy band of spectra extracted from Perseus Cluster core region observations obtained with the 5eV energy resolution Hitomi Soft X-ray Spectrometer. No significant unidentified line emission or absorption is found. Line flux upper limits (1 sigma per resolution element) vary with photon energy and assumed intrinsic width, decreasing from 100 photons cm$^{-2}$ s$^{-1}$ sr $^{-1}$ at 2keV to $<10$ cm$^{-2}$ s$^{-1}$ sr $^{-1}$ over most of the 5-10 keV energy range for a Gaussian line with Doppler broadening of 640 km/s. Limits for narrower and broader lines have a similar energy dependence and are systematically smaller and larger, respectively. These line flux limits are used to constrain the decay rate of hypothetical dark matter candidates. For the sterile neutrino decay rate, new constraints over the the mass range of 4-24 keV with mass resolution better than any previous X-ray analysis are obtained. Additionally, the accuracy of relevant thermal spectral models and atomic data are evaluated. The Perseus cluster spectra may be described by a composite of multi-temperature thermal and AGN power-law continua. Superposed on these, a few line emission signals possibly originating from unmodeled atomic processes (including Si XIV and Fe XXV) are marginally detected and tabulated. Comparisons with previous X-ray upper limits and future prospects for dark matter searches using high-energy resolution spectroscopy are discussed....
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The Astrophysical Journal, 837(1) L15-L15, Jul 25, 2016High-resolution X-ray spectroscopy with Hitomi was expected to resolve the origin of the faint unidentified E=3.5 keV emission line reported in several low-resolution studies of various massive systems, such as galaxies and clusters, including the Perseus cluster. We have analyzed the Hitomi first-light observation of the Perseus cluster. The emission line expected for Perseus based on the XMM-Newton signal from the large cluster sample under the dark matter decay scenario is too faint to be detectable in the Hitomi data. However, the previously reported 3.5 keV flux from Perseus was anomalously high compared to the sample-based prediction. We find no unidentified line at the reported high flux level. Taking into account the XMM measurement uncertainties for this region, the inconsistency with Hitomi is at a 99% significance for a broad dark-matter line and at 99.7% for a narrow line from the gas. We do not find anomalously high fluxes of the nearby faint K line or the Ar satellite line that were proposed as explanations for the earlier 3.5 keV detections. We do find a hint of a broad excess near the energies of high-n transitions of Sxvi (E=3.44 keV rest-frame) -- a possible signature of charge exchange in the molecular nebula and another proposed explanation for the unidentified line. While its energy is consistent with XMM pn detections, it is unlikely to explain the MOS signal. A confirmation of this interesting feature has to wait for a more sensitive observation with a future calorimeter experiment.
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Nature (London), 535(7610), Jul 15, 2016Clusters of galaxies are the most massive gravitationally-bound objects in the Universe and are still forming. They are thus important probes of cosmological parameters and a host of astrophysical processes. Knowledge of the dynamics of the pervasive hot gas, which dominates in mass over stars in a cluster, is a crucial missing ingredient. It can enable new insights into mechanical energy injection by the central supermassive black hole and the use of hydrostatic equilibrium for the determination of cluster masses. X-rays from the core of the Perseus cluster are emitted by the 50 million K diffuse hot plasma filling its gravitational potential well. The Active Galactic Nucleus of the central galaxy NGC1275 is pumping jetted energy into the surrounding intracluster medium, creating buoyant bubbles filled with relativistic plasma. These likely induce motions in the intracluster medium and heat the inner gas preventing runaway radiative cooling; a process known as Active Galactic Nucleus Feedback. Here we report on Hitomi X-ray observations of the Perseus cluster core, which reveal a remarkably quiescent atmosphere where the gas has a line-of-sight velocity dispersion of 164+/-10 km/s in a region 30-60 kpc from the central nucleus. A gradient in the line-of-sight velocity of 150+/-70 km/s is found across the 60 kpc image of the cluster core. Turbulent pressure support in the gas is 4% or less of the thermodynamic pressure, with large scale shear at most doubling that estimate. We infer that total cluster masses determined from hydrostatic equilibrium in the central regions need little correction for turbulent pressure.
Misc.
87Books and Other Publications
1Presentations
4Teaching Experience
2-
May, 2022 - May, 2022Space and Earth Physics Introduction (Rikkyo University)
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Apr, 2020 - Mar, 2021Basic Physics (Salesian Polytechnic)
Professional Memberships
2-
Apr, 2022 - Present
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Jul, 2021 - Present
Research Projects
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Grants-in-Aid for Scientific Research Grant-in-Aid for Transformative Research Areas (A), Japan Society for the Promotion of Science, Nov, 2020 - Mar, 2025
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Grants-in-Aid for Scientific Research Grant-in-Aid for Scientific Research (C), Japan Society for the Promotion of Science, Apr, 2014 - Mar, 2018
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Grants-in-Aid for Scientific Research Grant-in-Aid for Scientific Research (C), Japan Society for the Promotion of Science, Apr, 2012 - Mar, 2015
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Grants-in-Aid for Scientific Research, Japan Society for the Promotion of Science, 2007 - 2009
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科学研究費補助金(若手研究(B)), 文部科学省, 2004 - 2006
