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 教授東京大学大学院 理学系研究科 物理学専攻 教授量子場計測システム国際拠点(QUP) (主任研究者)北里大学大学院 理学研究科 客員教授
- 学位
- 博士（理学）(1996年3月 東京大学)
- ORCID ID
https://orcid.org/0000-0003-4885-5537- J-GLOBAL ID
- 200901003330670433
- Researcher ID
- C-2252-2008
- researchmap会員ID
- 5000019022
- 外部リンク
経歴
2-
2002年7月 - 2018年1月
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1993年 - 2002年
学歴
2-
1989年4月 - 1993年3月
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1985年4月 - 1989年3月
委員歴
2-
2017年10月 - 2023年9月
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2014年10月 - 2017年9月
論文
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IEEE Transactions on Applied Superconductivity 35(5) 1-4 2025年8月 査読有り
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The Astrophysical Journal Letters 982(1) L5-L5 2025年3月12日 査読有り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 査読有り
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Publications of the Astronomical Society of Japan 77(1) L1-L8 2024年12月26日 査読有り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 査読有り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.
MISC
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Proceedings of SPIE - The International Society for Optical Engineering 7011 2008年 査読有りMultiplexed readout of TES (Transition Edge Sensor) signals is one of the key technologies needed to realize large format arrays of microcalorimeters in future X-ray missions. In the FDM (Frequency-Domain Multiplexing) approach using MHz biasing frequencies, a wide band-width FLL (Flux Locked Loop) circuit is essential to compensate the phase delay between the TES sensor and the room temperature circuits. An analog feedback circuit using a lock-in amplifier technique and phase shifters with a very low noise pre-amplifier is being developed. This circuit will be tested with an actual TES array and an 8-input SQUID in the EURECA project.
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Proceedings of SPIE - The International Society for Optical Engineering 7011 2008年 査読有りThe Soft X-ray Spectrometer (SXS) onboard the NeXT (New exploration X-ray Telescope) is an X-ray spectrometer utilizing an X-ray microcalorimeter array. Combined with the soft X-ray telescope of 6 m focal length, the instrument will have a ∼ 290cm2 effective at 6.7 keV. With the large effective area and the energy resolution as good as 6 eV (FWHM), the instrument is very suited for the high-resolution spectroscopy of iron K emission line. One of the major scientific objectives of SXS is to determine turbulent and/or macroscopic motions of the hot gas in clusters of galaxies of up to z ∼ 1. The instruments will use 6 × 6 or 8 × 8 format microcalorimeter array which is similar to that of Suzaku XRS. The detector will be cooled to a cryogenic temperature of 50 mK by multi-stage cooling system consisting of adiabatic demagnetization refrigerator, super fluid He, a 3He Joule Thomson cooler, and double-stage Stirling cycle cooler.
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SPACE TELESCOPES AND INSTRUMENTATION 2008: ULTRAVIOLET TO GAMMA RAY, PTS 1 AND 2 7011 2008年 査読有りSpatially resolved X-ray spectroscopy with high spectral resolution allows the study of astrophysical processes in extended sources with unprecedented sensitivity. This includes the measurement of abundances, temperatures, densities, ionisation stages as well as turbulence and velocity structures in these sources. An X-ray calorimeter is planned for the Russian mission Spektr Rontgen-Gamma (SRG), to be launched in 2011. During the first half year (pointed phase) it will study the dynamics and composition of of the hot gas in massive clusters of galaxies and in supernova remnants (SNR). During the survey phase it will produce the first all sky maps of line-rich spectra of the interstellar medium (ISM). Spectral analysis will be feasible for typically every 5 degrees x 5 degrees region on the sky. Considering the very short time-scale for the development of this instrument it consists of a combination of well developed systems. For the optics an extra eROSITA mirror, also part of the Spektr-RG payload, will be used. The detector will be based on spare parts of the detector flown on Suzaku combined with a rebuild of the electronics and the cooler will be based oil the design for the Japanese mission NeXT, In this paper we will present the science and give an overview of the instrument.
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2008 IEEE/LEOS INTERNATIONAL CONFERENCE ON OPTICAL MEMS AND NANOPHOTONICS 104-105 2008年 査読有りX-ray reflectivity of an ultra light-weight X-ray optic using MEMS technologies was measured in two different energies (0.28 keV and 1.49 keV). The obtained reflectivities can be understood by considering the mirror surface structures.
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SPACE TELESCOPES AND INSTRUMENTATION 2008: ULTRAVIOLET TO GAMMA RAY, PTS 1 AND 2 7011 2008年 査読有りThe SXS (Soft X-ray Spectrometer) onboard the coming Japanese X-ray satellite NeXT (New Exploration Xray Telescope) and the SXC (Spectrum-RC X-ray Calorimeter) in Spectrum-RG mission are microcalorimeter array spectrometers which will achieve high spectral resolution of similar to 6 eV in 0.3-10.0 keV energy band. These spectrometers are well-suited to address key problems in high-energy astrophysics. To achieve these high spectral sensitivities, these detectors require to be operated under 50 mK by using very efficient cooling systems including adiabatic demagnetization refrigerator (ADR,). For both missions, we propose a two-stage series ADR as a cooling system below 1 K, in which two units of ADR consists of magnetic cooling material, a superconducting magnet, and a heat switch are operated step by step. Three designs of the ADR are proposed for SXS/SXC. In all three designs, ADR can attain the required hold time of 23 hours at 50 mK and cooling power of 0.4 mu W with a low magnetic fields (1.5/1.5 Tesla or 2.0/3.0 Tesla) in a small configuration (180 mm phi x 319 mm in length). We also fabricated a new portable refrigerator for a, technology investigation of two-stage ADR. Two units of ADR have been installed at the bottom of liquid He tank. By using this dewar, important technologies such as an operation of two-stage cooling cycle, tight temperature control less than 1 mu K (in rms) stability, a, magnetic shielding, saltpills, and gas-gap heat switches are evaluated.
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SPACE TELESCOPES AND INSTRUMENTATION 2008: ULTRAVIOLET TO GAMMA RAY, PTS 1 AND 2 7011 2008年 査読有りThe EURECA (EURopean-JapanEse Calorimeter Array) project aims to demonstrate the science performance and technological readiness of an imaging X-ray spectrometer based on a micro-calorimeter array for application in future X-ray astronomy missions, like Constellation-X and XEUS. The prototype instrument consists of a 5 x 5 pixel array of TES-based micro-calorimeters read out by by two SQUID-amplifier channels using frequency-domain-multiplexing (FDM). The SQUID-amplifiers are linearized by digital base-band feedback. The detector array is cooled in a cryogen-free cryostat consisting of a pulse tube cooler and a two stage ADR. A European-Japanese consortium designs, fabricates, and tests this prototype instrument. This paper describes the instrument concept, and shows the design and status of the various sub-units, like the TES detector array, LC-filters, SQUID-amplifiers, AC-bias sources, digital electronics, etc.
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HIGH ENERGY, OPTICAL, AND INFRARED DETECTORS FOR ASTRONOMY III 7021 2008年 査読有りOur recent development of transition-edge sensor (TES) microcalorimeters for future X-ray astronomical missions such as DIOS is reported. In-house micromaching processes has been established aiming at prompt fabrication of TES devices. With a single-pixel TES microcalorimeter and an Au absorber, the energy resolution of 4.8 eV at 5.9 keV is achieved. 16 x 16 pixel arrays of TES microcalorimeters are successfully fabricated by using deep dry etching technique. The energy resolution is 11 eV and 26 eV with and without all Au absorber; respectively. The worse energy resolution than a single-pixel TES is due to large decrease of TES sensitivity and increase of transition temperature after etching. The reason for these phenomena is under investigation. In parallel, mushroom-type Au absorber structures are being tested. Furthermore, to precisely measure TES sensitivities and heart capacity, an experimental setup for impedance measurements is established.
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SPACE TELESCOPES AND INSTRUMENTATION 2008: ULTRAVIOLET TO GAMMA RAY, PTS 1 AND 2 7011 2008年 査読有りWe present the current status of a small X-ray mission DIOS (Diffuse Intergalactic Oxygen Surveyor), consisting of a 4-stage X-ray telescope and an array of TES microcalorimeters, cooled with mechanical coolers, with a total weight of about 400 kg. The mission will perform survey observations of warm-hot intergalactic medium using OVII and OVIII emission lines. with the energy coverage Lip to 1.5 keV. The wide field of view of about. 50 ' diameter, superior energy resolution close to 2 eV FWHM, and very low background will together enable us a, wide range of science for diffuse X-ray sources. We briefly describe the. current status of the development of the satellite, and the subsystems.
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SPACE TELESCOPES AND INSTRUMENTATION 2008: ULTRAVIOLET TO GAMMA RAY, PTS 1 AND 2 7011 2008年 査読有りThe NeXT (New exploration X-ray Telescope). the new Japanese X-ray Astronomy Satellite following Suzaku, is all international X-ray mission which is currently planed for launch in 2013. NeXT is a combination of wide band X-ray spectroscopy (3-80 keV) provided by multi-layer coating, focusing hard X-ray mirror and hard X-ray imaging detectors, and high energy-resolution soft X-ray spectroscopy (0.3-10 keV) provided by thin-foil X-ray optics and a micro-calorimeter array. The mission will also carry an X-ray CCD camera as a focal plane detector for a soft, X-ray telescope and a non-focusing soft, gamma-ray detector. With these instruments, NeXT Covers very wide energy range from 0.3 keV to 600 keV. The micro-calorimeter system will be developed by international collaboration lead ISAS/JAXA and NASA. The simultaneous broad bandpass, coupled with high spectral resolution of Delta E similar to 7 eV by the micro-calorimeter will enable a wide variety of important, science themes to be pursued.
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AIP Conference Proceedings 1016 367-372 2008年We studied the properties of the intra-cluster medium (ICM) in two clusters of galaxies (AWM 7 and Abell 1060) and two groups (HCG 62 and NGC 507) observed with the 5th Japanese X-ray astronomical satellite, Suzaku. We measured for the first time precise cumulative ICM metal masses and distributions for various elements, such as O, Ne, Mg, Si, S, Fe, within 0.1 and ∼0.3 r180. Because of the good XIS sensitivity to emission lines, especially below 2 keV, we directly measured O and Mg line intensities and obtained abundances. Comparing our results with supernova nucleosynthesis models, the number ratio of Type II (SNe II) to Type Ia (SNe Ia) is estimated to be ∼3.5, assuming the metal mass in the ICM is represented by the sum of products synthesized in SNe Ia and SNe II. Normalized by the K-band luminosities of present galaxies, and including the metals in stars, the integrated number of past SNe II explosions is estimated to be close to or somewhat higher than the star formation rate determined from Hubble Deep Field observations.
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日本物理学会講演概要集 62(2) 110-110 2007年8月21日
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日本物理学会講演概要集 62(2) 110-110 2007年8月21日
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日本物理学会講演概要集 62(1) 102-102 2007年2月28日
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日本物理学会講演概要集 62(1) 102-102 2007年2月28日
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HEATING VERSUS COOLING IN GALAXIES AND CLUSTERS OF GALAXIES 395-+ 2007年 査読有り
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Progress of Theoretical Physics Supplement 169(169) 45-48 2007年Status of the Suzaku survey for non-thermal hard X-ray emission from clusters of galaxies is reported. Utilizing the lowest and stable detector background of both the HXD and the XIS instruments, Suzaku achieved high sensitivity for hard X-ray diffuse emission survey. Deep (> 100 ks) observations of a merging cluster A3376 present an upper limit of ∼ 10 -11 erg cm-2 s_1 in the 15-50 keV band (Kawano et al. and this work). Other analyses using the HXD (Centaurus and A1060, Kitaguchi et al.) and the XIS (HCG 62, Tokoi et al.) are also briefly summarized.
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Proceedings of SPIE - The International Society for Optical Engineering 6688(1) 67-89 2007年 査読有りHow structures of various scales formed and evolved from the early Universe up to present time is a fundamental question of astrophysics. EDGE1will trace the cosmic history of the baryons from the early generations of massive stars by Gamma-Ray Burst (GRB) explosions, through the period of galaxy cluster formation, down to the very low redshift Universe, when between a third and one half of the baryons are expected to reside in cosmic filaments undergoing gravitational collapse by dark matter (the so-called warm hot intragalactic medium). In addition EDGE, with its unprecedented capabilities, will provide key results in many important fields. These scientific goals are feasible with a medium class mission using existing technology combined with innovative instrumental and observational capabilities by: (a) observing with fast reaction Gamma-Ray Bursts with a high spectral resolution (R - 500). This enables the study of their (star-forming) environment and the use of GRBs as back lights of large scale cosmological structures (b) observing and surveying extended sources (galaxy clusters, WHIM) with high sensitivity using two wide field of view X-ray telescopes (one with a high angular resolution and the other with a high spectral resolution). The mission concept includes four main instruments: a Wide-field Spectrometer with excellent energy resolution (3 eV at 0.6 keV), a Wide-Field Imager with high angular resolution (HPD 15") constant over the full 1.4 degree field of view, and a Wide Field Monitor with a FOV of 1/4 of the sky, which will trigger the fast repointing to the GRB. Extension of its energy response up to 1 MeV will be achieved with a GRB detector with no imaging capability. This mission is proposed to ESA as part of the Cosmic Vision call. We will briefly review the science drivers and describe in more detail the payload of this mission.
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ESO Astrophysics Symposia 2007 398-400 2007年 査読有りWe carried out observations of the central and 20′ east offset regions of the cluster of galaxies Abell 1060 with Suzaku. Spatially resolved X-ray spectral=analysis has revealed temperature and abundance profiles of Abell 1060 out to 27′ ≃ 380 h70 -1kpc, which corresponded to ∼0.3 rvir. The temperature decrease of the intra cluster medium from 3.4 keV at the center to 2.2 keV in the outskirt region are clearly observed. Si, S and Fe abundances also decrease by more than 50% from the center to the outer parts, while Mg shows a fairly constant abundance of ∼ 0.7 solar within r < 17′. O shows a lower abundance of ∼0.3 solar in the central region (r < 6′), and indicates a similar feature with Mg, however it is sensitive to the estimated contribution of the Galactic components at the outer annuli (r > 13′). Results on temperature and abundances of Si, S, and Fe are consistent with those derived by XMM-Newton at r < 13′ The formation and metal enrichment of the cluster are discussed based on implications of our results. © 2007 Springer-Verlag Berlin Heidelberg.
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日本物理学会講演概要集 61(1) 87-87 2006年3月4日
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日本物理学会講演概要集 61(1) 94-94 2006年3月4日
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Space Telescopes and Instrumentation II: Ultraviolet to Gamma Ray, Pts 1 and 2 6266 G2660-G2660 2006年 査読有りWe present our proposal for a small X-ray mission DIOS (Diffuse Intergalactic Oxygen Surveyor), consisting of a 4-stage X-ray telescope and an array of TES microcalorimeters, cooled with mechanical coolers, with a total weight of about 400 kg. The mission will perform survey observations of warm-hot intergalactic medium using OVII and OVIII emission lines, with the energy coverage up to 1.5 keV. The wide field of view of about 50' diameter, superior energy resolution close to 2 eV FWHM, and very low background will together enable us a wide range of science for diffuse X-ray sources. We briefly describe the design of the satellite, performance of the subsystems and the expected results.
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Space Telescopes and Instrumentation II: Ultraviolet to Gamma Ray, Pts 1 and 2 6266 Z2661-Z2661 2006年 査読有りEURECA (EURopean-JapanEse Calorimeter Array) comprises a 5 x 5 pixel imaging TES-based micro-calorimeter array read-out by SQUID-based frequency-domain-multiplexed electronics and cooled down by an adiabatic demagnetization refrigerator. A European-Japanese consortium designs, fabricates, and tests this prototype instrument with the aim to show within about 2 years technology readiness of a TES-based X-ray imaging micro-calorimeter array in anticipation of future X-ray astronomy missions, like XEUS (ESA), Constellation-X (NASA), NEXT (JAXA), DIOS (JAXA), ESTREMO (ASI), and NEW (Dutch-multinational). This paper describes the instrument concept, and shows the design of the various sub-units, like the TES detector array, LC-filters, SQUID-amplifiers, flux-locked-loop electronics, AC-bias sources, etc.
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日本物理学会講演概要集 60(1) 208-208 2005年3月4日
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Development of a microcalorimeter array for the Diffuse Intergalactic Oxygen Surveyor (DIOS) missionProceedings of SPIE - The International Society for Optical Engineering 5501 123-134 2004年 査読有りWe are developing a superconducting transition-edge sensor (TES) microcalorimeter array for the Diffuse Intergalactic Oxygen Surveyor (DIOS) mission. DIOS is a relatively small Japanese X-ray mission which will study large-scale distribution of the warm-hot intergalactic medium (WHIM) using OVII and OVIII emission lines. The satellite weighs about 400 kg equipped with a four-reflection X-ray telescope (FXT) and a TES microcalorimeter array (XSA). The design goal of the observing system is an effective area larger than 100 cm2 at the oxygen line energy, a field of view about 50 arcmin square, and an energy resolution about 2 eV in the energy range of 0.3-1 keV. The TES microcalorimeter array provides the large field of view and good energy resolution at the same time. We plan to install an array comprising 16 × 16 pixels with an overall size of 1 cm square, which is cooled with a cryogen-free cooler. Pixels are readout by multiplexing signals using a multi-input SQUID amplifier, with each input connected to a TES microcalorimeter which is AC biased with a different frequency. We report the design and present status of the XSA system development.
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JOURNAL OF THE KOREAN PHYSICAL SOCIETY 45 2004年 査読有り
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低温工学・超電導学会講演概要集 = Meetings of Cryogenics and Superconductivity 68 270-270 2003年5月21日
担当経験のある科目(授業)
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2003年3月 - 現在宇宙物理学特論I (隔年開講，前期） (東京大学大学院)
所属学協会
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2010年 - 現在
共同研究・競争的資金等の研究課題
22-
日本学術振興会 科学研究費助成事業 2020年11月 - 2025年3月
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日本学術振興会 科学研究費助成事業 学術変革領域研究(A) 2020年11月 - 2025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(A) 2019年4月 - 2022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) 2018年4月 - 2022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) 2018年4月 - 2021年3月
教育内容やその他の工夫
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件名宇宙研での大学院教育概要宇宙の構造形成の観測的研究を主に極低温観測技術を用いて行なっている。東京大学，北里大学から大学院学生をうけいれ，大学院では，新しい検出器の開発とその応用および観測的研究の専門教育を行なう。大学院では，「誰もやったことがないこと」を自ら行なう力をつけることを目標にする。
● 指導学生等の数
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年度2018年度(FY2018)博士課程学生数1修士課程学生数1
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年度2019年度(FY2019)博士課程学生数1修士課程学生数3
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年度2020年度(FY2020)博士課程学生数1修士課程学生数3
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年度2018年度(FY2018)博士課程学生数1修士課程学生数1
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年度2019年度(FY2019)博士課程学生数1修士課程学生数3
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年度2020年度(FY2020)博士課程学生数1修士課程学生数3
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年度2022年度(FY2022)博士課程学生数3修士課程学生数2
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年度2023年度(FY2023)博士課程学生数2修士課程学生数1
● 指導学生の顕著な論文
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指導学生名高久諒太所属大学東京大学著者名, ジャーナル名, 巻号ページ（出版年）Takaku et al. , Journal of Applied Physics, 128(22), id.225302, (2020)論文タイトルBroadband, millimeter-wave anti-reflective structures on sapphire ablatedwith femto-second laserDOIhttp://doi.org/10.1063/5.0022765
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指導学生名中島裕貴所属大学Univ. of Tokyo著者名, ジャーナル名, 巻号ページ（出版年）Nakashima et al. Applied Physics Letters, 117 122601 (2020)論文タイトルLow-noise microwave SQUID multiplexed readout of 38 x-ray transition-edge sensor microcalorimetersDOIhttp://doi.org/10.1063/5.0016333
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指導学生名紺野良平所属大学Kitasato Univ.著者名, ジャーナル名, 巻号ページ（出版年）Konno et al. Journal of Low Temperature Physics 199, 654 (2019)論文タイトルDevelopment of TES micsrocalorimters with solar-axion converterDOIhttp://doi.org/10.1007/s10909-019-02257-9
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指導学生名山本亮所属大学Univ. of Tokyo著者名, ジャーナル名, 巻号ページ（出版年）Yamamoto et al. , Journal of Cosmokogy and Astrophysics, 02 (2020) 011論文タイトルA Search for a Contribution from Axion-Like Particles to the X-Ray Diffuse Background Utilizing the Earth's Magnetic FieldDOIhttp://doi.org/10.1088/1475-7516/2020/02/011
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指導学生名関谷典央所属大学University. of Tokyo著者名, ジャーナル名, 巻号ページ（出版年）Sekiya, Yamasaki, and Mitsuda, Publications of Astronomical Society in Japan, 68(SP1), S31 (2016)論文タイトルSearch for a keV Signature of Radiatively Decaying Dark Matter with Suzaku XIS Observations of the X-ray Diffuse BackgroundDOIhttp://doi.org/10.1093/pasj/psv081
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指導学生名三石郁之所属大学Univ. of Tokyo著者名, ジャーナル名, 巻号ページ（出版年）Mitsuishi, Yamasaki, and Takei, Publications of Astronomical Society in Japan, 65, 44 (2013)論文タイトルAn X-Ray Study of the Galactic-Scale Starburst-Driven Outflow in NGC 253DOIhttp://doi.org/10.1093/pasj/65.2.44
● 専任大学名
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専任大学名東京大学（University of Tokyo)
● 所属する所内委員会
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所内委員会名ナノエレクトロニクスクリーンルーム運営委員会
