研究者業績
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  2. 山崎 典子

山崎 典子

ヤマサキ ノリコ  (Noriko YAMASAKI)

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

研究キーワード

 8

研究分野

 2

経歴

 2

学歴

 2

委員歴

 2

論文

 240
  • Kohji Yoshikawa, Noriko Y. Yamasaki, Yasushi Suto, Takaya Ohashi, Kazuhisa Mitsuda, Yuzuru Tawara, Akihiro Furuzawa
    Publications of the Astronomical Society of Japan 55(5) 879-890 2003年  査読有り
    Most of the cosmic baryons predicted by the big-bang nucleosynthesis have evaded direct detection. Recent numerical simulations indicate that approximately 30 to 50 percent of the total baryons in the present universe are supposed to take the form of warm/hot intergalactic medium (WHIM) whose X-ray continuum emission is very weak. To identify those missing baryons, we consider in detail the detectability of WHIM directly through the emission lines of O VII (561, 568, 574, 665 eV) and O VIII (653 eV). For this purpose, we create mock spectra of the emission lines of WHIM using a light-cone output of cosmological hydrodynamic simulations. While the predicted fluxes are generally below the current detection limit, an unambiguous detection will be feasible with a dedicated X-ray satellite mission, which we also discuss in detail. Our proposed mission is especially sensitive to a WHIM with gas temperature of T = 106-7 K and overdensity of δ = 10-100 up to a redshift of 0.3 without being significantly contaminated by the cosmic X-ray background and the Galactic emissions. Thus, such a mission provides a unique and important tool to identify a large fraction of otherwise elusive baryons in the universe.
  • A. Kushino, Y. Murakami, N. Y. Yamasaki, T. Ohashi, M. Kurakado
    Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 487(3) 488-493 2002年7月21日  査読有り
    The position determination capability of the series-connected superconducting tunnel junctions (STJs) with Nb/Al/AlOx/Al/Nb junctions as a radiation detector is reported. Four groups of series-connected STJs are fabricated on a single crystal of sapphire substrate surrounding 3.5 × 3.5 mm2 detection area. The signals detected by two STJs with 1.5 mm separation give a time delay caused by the propagation of phonons, and this enables us to measure the irradiated position. Using α-particles of 5.5 MeV, we clearly distinguished the incident positions with a potential resolution of 0.16±0.07 mm (FWHM). Directional dependence in the phonon propagation in the sapphire substrate is not detected. © 2002 Elsevier Science B.V. All rights reserved.
  • T Miyazaki, M Yamazaki, K Futamoto, K Mitsuda, R Fujimoto, N Iyomoto, T Oshima, D Audley, Y Ishisaki, T Kagei, T Ohashi, N Yamasaki, S Shoji, H Kudo, Y Yokoyama
    LOW TEMPERATURE DETECTORS 605 313-316 2002年  査読有り
    In order to realize a large format (e.g. similar to 32 x 32) calorimeter array, it is essential to multiplex calorimeter signals at cryogenic temperatures without losing signal to noise ratio. For this purpose we propose a brand-new readout method, the CABBAGE ((ca) under bar lorimeter (B) under bar ridge (B) under bar iased by an (A) under barC Generator) where an AC biased calorimeters are placed in resistance bridges. In this paper we first describe the principles of CABBAGE and investigate its response and noise. We propose the large format calorimeter array readout using CABBAGEs, and discuss the new TES microcalorimeter readout method without using SQUIDs.
  • Shin Sasaki, Noriko Y. Yamasaki
    Publications of the Astronomical Society of Japan 54(1) L1-L5 2002年  査読有り
    Recent XMM-Newton observations of clusters of galaxies have indicated the soft X-ray spectra to be inconsistent with the simple isobaric cooling flow model. There is almost no feature of the cold gas expected from the model. This shows that we have not yet understood the physics of the hot gas in clusters of galaxies well. A quantitative evaluation of the behavior of gas cooling is important not only for understanding the clusters, themselves, but also for studying cosmology and galaxy formation. To clarify the problem of this reported discrepancy, we have studied scaling relations for clusters of galaxies based on the self-similarity assumption. We also propose an observational strategy to solve this problem.
  • YAMASAKI, NY, OHASHI, T, FURUSHO, T
    Astrophysical Journal 578(2) 2002年  査読有り
  • Akihiro Kushino, Yoshitaka Ishisaki, Umeyo Morita, Noriko Y. Yamasaki, Manabu Ishida, Takaya Ohashi, Yoshihiro Ueda
    Publications of the Astronomical Society of Japan 54(3) 327-352 2002年  査読有り
    We studied the energy spectrum and the large-scale fluctuation of the X-ray background with the ASCA GIS instrument based on the ASCA Medium Sensitivity Survey and Large Sky Survey observations. A total of 91 fields with Galactic latitude |b| &gt 10° were selected with a sky coverage of 50 deg22 and 4.2 Ms of exposure. For each field, non-X-ray events were carefully subtracted and sources brighter than ∼ 2 × 10-13 erg cm-2 s-1 (2-10 keV) were eliminated. Spectral fits with a single power-law model for the individual 0.7-10 keV spectra showed a significant excess below ∼ 2keV, which could be expressed by an additional thermal model with kT ≃ 0.4 keV or a steep power-law model with a photon index of Γsoft ≃ 6. The 0.5-2 keV intensities of the soft thermal component varied significantly from field to field by 1 σ = 52-5 +4% and showed a maximum toward the Galactic Center. This component is considered to be entirely Galactic. As for the hard power-law component, an average photon index of 91 fields was obtained to be Γhard = 1.412 ± 0.007 ± 0.025 and the average 2-10 keV intensity was calculated as FX hard= (6.38 ± 0.04 ± 0.64) × 10-8 erg cm-2 s-1 sr-1(1 σ statistical and systematic errors). The Galactic component is marginally detected in the hard band. The 2-10 keV intensities show a 1 σ deviation of 6.49-0.61 +0.56%, while deviation due to the reproducibility of the particle background is 3.2%. The observed deviation can be explained by the Poisson noise of the source count in the f.o.v. (∼ 0.5 deg2), even assuming a single log N-log S relation on the whole sky. Based on the observed fluctuation and the absolute intensity, an acceptable region of the log N-log S relation was derived, showing a consistent feature with the recent Chandra and XMM-Newton results. The fluctuation of the spectral index was also examined it implied a large amount of hard sources and a substantial variation in the intrinsic source spectra (Γs ≃ 1.1 ± 1.0).
  • Akihiro Kushino, Yuji Aoki, Noriko Y. Yamasaki, Takahiro Namiki, Yoshitaka Ishisaki, Tatsuma D. Matsuda, Takaya Ohashi, Kazuhisa Mitsuda, Takashi Yazawa
    Journal of Applied Physics 90(11) 5812-5818 2001年12月  査読有り
    Garnets doped with rare-earth elements can be used in adiabatic demagnetization refrigerators. We have measured the specific heat and magnetization of a single crystal yttrium aluminum garnet (YAG) doped with 30% Er3+ ion at temperatures between 93 mK and 8 K under magnetic fields up to 8.0T along the 〈111〉 crystal axis. From the specific heat and magnetization, we derived consistent temperature and magnetic-field dependence of the magnetic entropy. Under zero magnetic field, the magnetic entropy begins to decrease below 2 K and becomes half of R ln 2 at ∼ 160 mK. This decrease is considered to be due to an antiferromagnetic short-range ordering among Er3+ ions. This behavior of the specific heat in the measured temperature range can be explained by a model in which both the crystalline-electric-field ground state and the first excited state are included. The operating temperature of the Er3--doped YAG as a magnetic coolant is estimated to extend down to ∼100 mK, which is lower than those with nonsubstituted garnets such as gallium-gadolinium-garnet used in the range ∼4.2-15 K. With a doping level of 30%, we estimate that ∼6 kg of Er3+-doped YAG exhibits the same cooling performance at 60 mK as the 916 g of ferric-ammonium-alum salt used for the x-ray spectrometer (microcalorimeter detectors) on the Astro-E satellite. © 2001 American Institute of Physics.
  • Tae Furusho, Noriko Y. Yamasaki, Takaya Ohashi, Ryo Shibata, Tomohiro Kagei, Yoshitaka Ishisaki, Ken'ichi Kikuchi, Hajime Ezawa, Yasushi Ikebe
    Publications of the Astronomical Society of Japan 53(3) 421-432 2001年6月25日  査読有り
    We present two-dimensional temperature maps of three bright clusters of galaxies (Abell 1060, AWM 7, and the Centaurus cluster), based on multi-pointing observations with the ASCA GIS. The temperatures were derived from hardness ratios by taking into account the XRT response. For the Centaurus cluster, we subtracted the central cool component using the previous ASCA and ROSAT results, and the metallicity gradients observed in AWM 7 and the Centaurus cluster were included in deriving the temperatures. The intracluster medium in Abell 1060 and AWM 7 is almost isothermal from the center to the outer regions with temperatures of 3.3 and 3.9 keV, respectively. The Centaurus cluster exhibits remarkable hot regions within about 30′ from the cluster center, showing a temperature increase of + 0.8 keV from the surrounding level of 3.5 keV, and the outer cool regions with lower temperatures by - 1.3 keV. These results imply that a strong merger has occurred in the Centaurus in the recent 2-3 Gyr, and that the central cool component has survived it. In contrast, the gas in Abell 1060 was well-mixed in an early period, which probably has prevented the development of a central cool component. In AWM 7, mixing of the gas should have occurred in a period earlier than the epoch of metal enrichment.
  • R. Shibata, K. Matsushita, N. Y. Yamasaki, T. Ohashi, M. Ishida, K. Kikuchi, H. Böhringer, H. Matsumoto
    Astrophysical Journal 549(1) 228-243 2001年3月1日  査読有り
    The temperature distribution of the intracluster medium (ICM) in the Virgo Cluster of galaxies has been derived from extensive mapping observations with ASCA covering an area of 19 deg2. In the spectral analysis, the inner region within a radius of ∼60′ from M87 is characterized by an ICM temperature of kT ∼ 2.5 keV with little variation. On the other hand, the outer regions indicate significant variation of the temperature with an amplitude of about 1 keV. The temperature map was produced from the hardness ratio (HR) values with a resolution of about 5′. Besides the previously reported hot region with kT &gt 4 keV between M87 and M49, several hot regions with kT = 3-4 keV are detected in the cluster outskirts. The autocorrelation function for the HR variation shows that the temperature variation is correlated within a size of about 300 kpc, suggesting that gas blobs falling in the Virgo Cluster have a typical size of groups of galaxies. A correlation with the velocity dispersion of member galaxies shows that only the northwest region indicates an unusually large βspec value of 2-4. The upper limit for extended nonthermal emission in the Virgo Cluster is obtained to be LX ∼ 9 × 1041 ergs s-1 in the 2-10 keV band. We discuss that these features consistently indicate that the Virgo Cluster is in a relatively early stage of the cluster evolution.
  • FURUSHO, T, YAMASAKI, NY, OHASHI, T, et al.
    ASTROPHYSICAL JOURNAL 561(2) 2001年  査読有り
  • Hajime Ezawa, Noriko Y. Yamasaki, Takaya Ohashi, Yasushi Fukazawa, Masaharu Hirayama, Hirohiko Honda, Tuneyoshi Kamae, Ken'ichi Kikuchi, Ryo Shibata
    Publications of the Astronomical Society of Japan 53(4) 595-604 2001年  査読有り
    Large-scale distributions of hot-gas temperature and Fe abundance in the Perseus cluster have been studied with multi-pointing observations by the GIS instrument onboard ASCA. Within a radius of 20′ from the cluster center, the energy spectra requires two temperature components, in which the cool component indicates kT ∼ 2 keV and the hot-component temperature shows a significant decline from about 8 keV to 6 keV toward the center. In the outer region of the cluster, the temperature shows a fluctuation with an amplitude of about 2 keV, which suggest that a western region at ∼ 16′ from the cluster center is relatively hotter. As for the Fe abundance, a significant decline with radius is detected from 0.44 solar at the center to ∼0.1 solar at a 50′ offset region. If the observed Fe-K line intensity within 4′ from the center is suppressed by a factor of 2 due to the resonance scattering effect, the corrected Fe mass density follows the galaxy distribution. Finally, our results do not support the large-scale velocity gradients previously reported from the same GIS data.
  • KIKUCHI, K, ITOH, C, KUSHINO, A, et al.
    ASTROPHYSICAL JOURNAL 531(2) 2000年  査読有り
  • 久志野 彰寛, 石川 輝, 山崎 典子, 大橋 隆哉, 菊池 健一, 倉門 雅彦
    放射線 26(1) 41-50 2000年1月1日  
  • Tae Furusho, Noriko Y. Yamasaki, Takaya Ohashi, Yoshitaka Saito, Wolfgang Voges
    Publications of the Astronomical Society of Japan 52(4) 677-684 2000年  査読有り
    An ASCA observation of a region containing a Class 0 protostar IRAS 20386 + 6751 in the Lynds 1157 dark cloud, has been carried out. The protostar was not detected, and the 95% upper limit to the luminosity depends on the assumed NH: LX(0.5-10 keV) &lt 1.1 × 1031 erg s-1 for NH = 1 × 1023 cm-2. A Class I protostar in Lynds 1152, IRAS 20353 + 6742, in the same field was also undetected with an upper limit about three-times as much as the Lynds 1157 level. Besides these non detections, nine new X-ray sources were detected and a spectral analysis was performed for 4 sources. One object (AX J2038 + 6801) shows a hard spectrum with a temperature of kT ∼ 8 keV or a power-law photon index of ∼ 2.0 and absorbed with NH ∼ 2 × 1022 cm-2. Another fainter one (AX J2036 + 6800) has a soft spectrum with most of the emission falling below 2 keV. We examine the possible nature of these new X-ray sources based on their spectral properties.
  • Noriko Y. Yamasaki, Teru Ishikawa, Takaya Ohashi
    Publications of the Astronomical Society of Japan 52(5) 763-767 2000年  査読有り
    An X-ray observation of a famous Lyman-limit quasar PKS 2145+067 at zem = 0.990 was carried out with ASCA. The source showed a 2-10 keV flux of 1.3 × 10-11 erg cm-2 s-1 (LX = 2.5 × 1046 erg s-1 for H0 = 50 km s-1 Mpc-1) described by a power-law spectrum with a photon index of the Γ = 1.63 ± 0.04. In the ASCA energy band, no excess absorption was detected, implying that absorption column density at zab = 0.791 was less than 1.6 × 1021 cm-2 if the absorbing medium had a metal abundance of 0.5 solar. A comparison with previous Einstein Observatory and ROSAT observations shows that PKS 2145+067 has increased in luminosity by a factor of 2-3 between 1991 and 1998.
  • YAMASAKI, NY, KUSHINO, A, ROKUTANDA, E, et al.
    NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT 436(1-2) 1999年  査読有り
  • GALLAGHER, SC, BRANDT, WN, SAMBRUNA, RM, et al.
    ASTROPHYSICAL JOURNAL 519(2) 1999年  査読有り
  • Ken'ichi Kikuchi, Tae Furusho, Hajime Ezawa, Noriko Y. Yamasaki, Takaya Ohashi, Yasushi Fukazawa, Yasushi Ikebe
    Publications of the Astronomical Society of Japan 51(3) 301-315 1999年  査読有り
    We present ASCA results on the distributions of the metallicity and temperature in 3 bright near-by clusters: A4059, MKW 3s, and 2A 0335+096. A significant gradient in the metal abundance is detected in A4059, while other clusters suggest similar gradients with low significance. These features together with recent results on AWM 7 and Perseus clusters suggest that metals injected in the ICM are not effectively mixed in the cluster space. An analysis of the GIS data, without explicitly including the cooling flow model, shows no substantial temperature drop at large radii (at half the virial radii) for the 3 systems. This is contrary to the recent results for 30 clusters by Markevitch et al. (1998, ApJ 503, 77), who assume rather strong cooling flows. The gas mass fraction of these clusters is 10-15% within 1 Mpc, which suggests that a baryonic fraction of about 20%, including the stellar mass, is a common level in galaxy groups and clusters.
  • Noriko Y. Yamasaki, Hiroyuki Miyazaki, Takaya Ohashi, Belinda J. Wilkes
    Publications of the Astronomical Society of Japan 50(1) 19-24 1998年  査読有り
    The X-ray spectrum of the distant QSO PKS 0237-233 (z = 2.223) has been studied with ASCA and ROSAT. The spectrum in the energy range 0.1 keV to 8 keV in the observer's frame is well fitted by a power-law model with a photon index of 1.54 ±0.06 absorbed by the galactic interstellar matter. The lack of excess absorption confirms that such absorption is not a universal property of the high-redshift GHz-peaked spectrum (GPS) sources. From a comparison of the Lyman α and the metal absorption lines in the optical and UV bands, small amount of X-ray absorption constrains the ionization state of the metal line system at z = 1.65 as [HI/H] &gt 2.5 × 10-4 and [CIV/C] &gt 0.11 if the metal line systems have a metal abundance of 0.1 Z(Fisheye).
  • MATSUSHITA, K, MAKISHIMA, K, IKEBE, Y, et al.
    ASTROPHYSICAL JOURNAL 499(1) 1998年  査読有り
  • YAMASAKI, NY, OHASHI, T, KIKUCHI, K, et al.
    (188) 1998年  査読有り
  • H. Kubo, K. Makishima, T. Takahashi, M. Ishida, H. Inoue, M. Matsuoka, N. Yamasaki, K. Suzuki
    Monthly Notices of the Royal Astronomical Society 287(2) 328-332 1997年  査読有り
    Q1745 + 624 is located at redshift z = 3.89, and is one of the most distant quasars observed in the X-ray band. Q1745 + 624 was clearly detected with ASCA in the 0.5-7 keV X-ray band, or in 2.4-34 keV in the quasar rest frame. If the energy spectrum is fitted by a single power law with photoelectric absorption, the photon index becomes 1.68-0.24' +0.25 and the column density NH becomes 2.1-1.4 +1.5 x 1021 cm-2, assuming the absorber to be located at z = 0. This index is steeper than that of the cosmic X-ray background. The spectrum suggests the presence of excess absorption above the Galactic column. If the absorber is at the same redshift as the quasar, then the intrinsic column density NH, is inferred to be 6.1-5.9 +10.8 x 1022cm-2, which is comparable to that seen in nearby Seyfert 2 galaxies. The spectrum shows neither flattening above ∼ 10 keV in the rest frame nor a significant Fe K line. This is in contrast to the X-ray properties of nearby Seyfert galaxies. When compared to lower redshift radio-loud quasars, Q1745 + 624 is inferred to have ∼ 10 times higher luminosity, but a very similar X-ray spectral index as well as a similar spectral energy distribution from the radio to the X-ray bands. © 1997 RAS.
  • N. Y. Yamasaki, T. Ohashi, F. Takahara, S. Yamauchi, K. Koyama, T. Kamae, H. Kaneda, K. Makishima, Y. Sekimoto, M. Hirayama, T. Takahashi, T. Yamagami, S. Gunji, T. Tamura, S. Miyazaki, M. Nomachi
    Astrophysical Journal 481(2) 821-831 1997年  査読有り
    Hard X-ray and γ-ray emissions from the Galactic ridge were studied with the large area proportional counter (LAC) on the Ginga satellite and a balloon-borne detector Welcome-1. In the scanning observations with the LAC, diffuse hard X-rays were detected along the Galactic plane between l = -20° and l = 40°. The measured spectrum shows that a hard component exists in the Galactic ridge emission above 10 keV, in addition to the hot plasma component. The estimated luminosity of the Galactic ridge emission is around 2 × 1038 ergs s-1 in the 3-16 keV band. Welcome-1 observed the γ-ray ridge emission at around l ∼ 345° between 50 and 600 keV. These two results and a recent COMPTEL study suggest that the spectrum of the diffuse Galactic ridge emission extends over the keV-MeV range. From the observed spectral slope, bremsstrahlung by electrons is shown to be the dominant emission mechanism. This implies that low-energy electrons must be supplied continuously to sustain emission in the hard X-ray band. We propose a scenario in which the thermal electrons in the hot plasma responsible for the strong Fe K X-ray emission are shock-accelerated continuously in supernova remnants (SNRs), producing the observed hard X-ray and γ-ray emissions from the Galactic ridge. © 1997. The American Astronomical Society. All rights reserved.
  • EZAWA, H, FUKAZAWA, Y, MAKISHIMA, K, et al.
    ASTROPHYSICAL JOURNAL 490(1) 1997年  査読有り
  • H. Kaneda, K. Makishima, S. Yamauchi, K. Koyama, K. Matsuzaki, N. Y. Yamasaki
    Astrophysical Journal 491(2) 638-652 1997年  査読有り
    X-ray spectra of the Galactic ridge emission in the Scutum arm region have been obtained with ASCA GIS and SIS in the energy range 0.7-10 keV. The observed spectra are basically of thermal emission from thin hot plasmas, and individual K emission lines from helium-like Mg, Si, S, and Fe ions are confirmed in both the GIS and SIS spectra. This means that the Galactic ridge X-ray emission cannot be explained by a single-temperature ionization-equilibrium plasma model. It cannot, however, be reproduced even if a nonequilibrium ionization model is introduced thus multiple plasma components are required. The GIS spectra are fairly well fitted by a double-temperature nonequilibrium ionization plasma model with temperatures of kT ∼ 0.8 keV and kT ∼7 keV. The softer component is found to be in an extremely low ionization state, with net ∼ 109 cm-3 s, while the harder component is in a relatively high ionization state, though not yet in a full equilibrium. The GRXE properties obtained with the GIS are carefully reexamined by the highly resolved spectral-line features with the SIS. The soft and hard components are absorbed by equivalent hydrogen columns of 0.7 × 1022 cm-2 and 4.6 × 1022 cm-2, respectively. The surface brightness of the soft and hard components at b ∼ 0° are estimated to be 1.9 × 10-6 and 5.3 × 10-7 ergs cm-2 s-1 sr-1 respectively, both in the 0.5-10 keV band. The surface brightness of the softer component extends toward significantly higher (∼2°) Galactic latitudes than the harder component, although their actual scale heights may be similar at ∼100 pc if the differences in their observable depths are taken into account. Spectral properties of the two components are seen to depend on the latitude the most noticeable effect is a rapid decrease in the Fe K line equivalent width seen in the hard component. Attempts are made to interpret the two components in terms of diffuse hot plasmas filling the interstellar space. © 1997. The American Astronomical Society. All rights reserved.
  • MATSUSHITA, K, MAKISHIMA, K, ROKUTANDA, E, et al.
    ASTROPHYSICAL JOURNAL 488(2) L125-L128 1997年  査読有り
  • Satoshi Miyazaki, Tadayuki Takahashi, Shuichi Gunji, Masaharu Hirayama, Tuneyoshi Kamae, Yutaro Sekimoto, Tadahisa Tamura, Mitsuaki Tanaka, Noriko Y. Yamasaki, Hajime Inoue, Takako Kano, Takamasa Yamagami, Masaharu Nomachi, Hiroyuki Murakami, John Braga, J. Angelo Neri
    Publications of the Astronomical Society of Japan 48(6) 801-811 1996年  査読有り
    We have studied Cen A (NGC 5128) in the X-ray band (3-20 keV) and soft γ-ray band (40-600 keV) with the Large Area Counter (LAC) of the Ginga sattellite (1989 March and 1990 February) and with a balloon-borne low background detector (Welcome-1, 1991 November), respectively. The observed continuous spectra show a power-law shape (Γ ∼ 1.8) with relatively heavy absorption (NH ∼ 1.5 × 1023H cm-2) at the low-energy end and a possible break at ∼ 180 keV. We analyzed the total spectra as the sum of the direct power-law flux from the central engine, the Compton-scattered flux from a cold cloud near to the engine, and the iron fluorescence-line flux. By assuming that the geometry around the central engine remained unchanged during the two-year period, we studied two possible cold cloud geometries by comparing Monte-Carlo simulations with our observations: the first is the Compton-reflection model in which the cloud forms a slab covering 2π sr behind the central engine, the second is a case where the central source is totally surrounded by a cold cloud. We found that the latter geometry reproduces our data well the observed power-law spectrum is then identified as direct flux from the central engine which undergoes a break at ∼ 180 keV.
  • Shigeo Yamauchi, Hidehiro Kaneda, Katsuji Koyama, Kazuo Makishima, Keiichi Matsuzaki, Takashi Sonobe, Yasuo Tanaka, Noriko Yamasaki
    Publications of the Astronomical Society of Japan 48(2) L15-L20 1996年  査読有り
    We report on the ASCA results of hard X-ray imaging and spectroscopic observations of the galactic ridge (the Scutum arm region). The bulk of X-rays in the field of view could not be explained by an integrated emission of resolved sources, indicating that most of the galactic-ridge X-rays are due to a diffuse thin hot plasma. The X-ray luminosity of discrete sources contributing to the galactic-ridge emission was estimated to be less than -2x1033 erg s-1 in the 2-10 keV energy band. Emission lines from helium-like Si, S, and Fe ions were confirmed in the spectra, which means that the galactic ridge X-ray emission can not be explained by a single temperature ionization equilibrium plasma model. We give some constraints on the origin of the galactic-ridge emission.
  • YAMASAKI, NY, OHASHI, T, TAKAHARA, F, et al.
    ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES 120(4) 1996年  査読有り
  • TAKAHASHI, T, TASHIRO, M, MADEJSKI, G, et al.
    ASTROPHYSICAL JOURNAL 470(2) 1996年  査読有り
    We observed the BL Lac object Mrk 421 with the X-ray satellite ASCA in 1994 as part of a multifrequency observation. The 24 hr observation was conducted 1 day after the onset of a TeV flare detected by the Whipple Observatory and detected an X-ray flare, with no apparent variability in the optical, UV, and EGRET GeV flux. The ASCA 2-10 keV flux peaked at 3.7 × 10-10 ergs cm-2 s-1 and then decreased to 1.8 × 10-10 ergs cm-2 s-1 with a doubling timescale of ∼12 hr. The shape of the X-ray spectrum varied during the observation, such that the hard X-rays always led the soft X-rays, both in brightening and dimming of the source, with a lag of the 0.5-1 keV photons versus those in the 2-7.5 keV band of ∼1 hr. The rapid TeV variability indicates a compact TeV-producing region, suggesting relativistic beaming with a Doppler factor δ ≥ 5. The correlation of the flux in the X-ray and the TeV bands indicates that a high-energy tail of a single electron population is responsible for both X-rays and TeV γ-rays, with radio, IR, UV and X-rays produced via the synchrotron process and GeV and TeV γ-rays produced via Comptonization. Under the assumption that the "soft lag" observed in the X-ray band is due to the synchrotron-lifetime effects, with δ = 5, we calculate the magnetic field for the X-ray-producing region to be ∼0.2 G. The Lorentz factors γcl of the electrons responsible for the emission in the keV and TeV bands are ∼106, consistent with the values implied by the Klein-Nishina limit. © 1996. The American Astronomical Society. All rights reserved.
  • Kazuo Makishima, Makoto Tashiro, Ken Ebisawa, Hajime Ezawa, Yasushi Fukazawa, Shuichi Gunji, Masaharu Hirayama, Eriko Idesawa, Yasushi Ikebe, Manabu Ishida, Yoshitaka Ishisaki, Naoko Iyomoto, Tsuneyoshi Kamae, Hidehiro Kaneda, Ken'ichi Kikuchi, Yoshiki Kohmura, Hidetoshi Kubo, Kyoko Matsushita, Keiichi Matsuzaki, Tatehiro Mihara, Ken'ichiro Nakagawa, Takaya Ohashi, Yoshitaka Saito, Yutaro Sekimoto, Tadayuki Takahashi, Takayuki Tamura, Takeshi Tsuru, Yoshihiro Ueda, Noriko Y. Yamasaki
    Publications of the Astronomical Society of Japan 48(2) 171-189 1996年  査読有り
    The in-orbit performance and calibration of the Gas Imaging Spectrometer (GIS), located on the focal plane of the X-ray astronomy satellite ASCA, are described. An extensive in-orbit calibration has confirmed its basic performance, including a position resolution of 0.6 mm (FWHM) and an energy resolution of 7.8% (FWHM), both at 6 keV. When combined with the X-ray telescope, the GIS sensitivity range becomes 0.7-10 keV. The in-orbit non X-ray background of the GIS has been confirmed to be as low as (5-9) × 10-4 c s-1 cm-2 keV-1 over the 1-10 keV range. The long-term detector gain has been stable within a few % for nearly 3 years. Extensive observations of the Crab Nebula and other sources have provided accurate calibrations of the position response, photometric capability, dead time, and timing accuracy of the GIS. Furthermore, the overall energy response, including the temporal and positional gain variations and the absolute gain scale, has been calibrated to ∼ 1%. Thus, the GIS is working as an all-round cosmic X-ray detector, capable of X-ray imagery, fine X-ray spectroscopy, X-ray photometry with a flux dynamic range covering more than 5 orders of magnitude, and fast X-ray photometry with a time resolution up to 60 μs.
  • Yasushi Fukazawa, Kazuo Makishima, Kyoko Matsushita, Noriko Yamasaki, Takaya Ohashi, Richard F. Mushotzky, Yasuhiro Sakima, Yoshiyuki Tsusaka, Koujun Yamashita
    Publications of the Astronomical Society of Japan 48(3) 395-407 1996年  査読有り
    We observed two groups of galaxies, the NGC 5044 group (WP 23) and Hickson's compact group HCG 51, with ASCA. We detected an extended bright soft X-ray emission, which indicates the existence of large amounts of a hot X-ray emitting gas in both targets. The temperature of the hot gas is ∼ 1 keV for both objects, which is equivalent to their galaxy velocity dispersion. The metal abundance of the gas is 0.3-0.5 solar value for both objects, which is similar to that of rich clusters of galaxies. The Si to Fe abundance ratio is smaller than that of rich clusters of galaxies, although the iron abundances determined by the Fe-L lines are somewhat uncertain. The X-ray luminosities in the 0.5-10 keV band are 1×1043 erg s-1 and 5×1042erg s-1 for the NGC 5044 group and HCG 51, respectively, which are higher by an order of magnitude than those of X-ray bright elliptical galaxies. This makes HCG 51 one of the most X-ray luminous compact groups. Both objects have a total gravitating mass of Mtotal ∼ 2.0 × 1013 M(Fish eye sign), and a gas mass and a galaxy mass of Mgas ∼ Mgalaxy ∼ 1.5 × 1012 M(Fish eye sign). The ratios among these mass components are Mgas/Mgalaxy ∼ 1 and (Mgas + Mgalaxy)/Mtotal ∼ 0.2 within ∼350 kpc for both objects. The latter is similar to previous ROSAT results for many groups of galaxies, while the former is larger than the average value of the ROSAT-observed groups. Moreover, the metal abundances of the present two groups are significantly higher than those of the NGC 2300 group and HCG 62, and are comparable to those of clusters. These suggest that the hot-gas mass and metal abundances can scatter widely among groups, compared to the small variance found among rich clusters.
  • Hidehiro Kaneda, Hajime Ezawa, Masaharu Hirayama, Tuneyoshi Kamae, Hidetoshi Kubo, Keiichi Matsuzaki, Kazuo Makishima, Takanori Ohtsuka, Yoshitaka Saito, Yutaro Sekimoto, Tadayuki Takahashi, Takayuki Tamura, Makoto Tashiro, Naohiko Tsuchida, Toshio Murakami, Mutsumi Sugizaki, Hirokazu Ikeda, Kiwamu Tsukada, Masaharu Nomachi, Shuichi Gunji, Satoshi Miyazaki, Tadahisa Tamura, Noriko Y. Yamasaki, Atsumasa Yoshida
    EUV, X-Ray, and Gamma-Ray Instrumentation for Astronomy VI 2518 85-95 1995年9月1日  
    The ASTRO-E satellite is scheduled for launch in 2000 by the Institute of Space and Astronautical Science (ISAS). In this paper the design and performance of the hard x ray detector (HXD) developed for ASTRO-E are described. The HXD is a combination of YAP/BGO phoswich scintillators and silicon PIN diodes covering a wide energy band of 10 - 700 keV. The detector background is reduced down to several times 10 -6c/s/cm 2/keV, and the sensitivity of the HXD is more than one order of magnitude higher than any other past missions in the range of a few 10 keV to several 100 keV. Thus ASTRO-E HXD is expected to achieve an extreme high performance for detecting cosmic hard x rays and low-energy gamma rays. Astrophysics to be explored with the HXT are expected to be extremely widespread and rich.
  • 斎藤 芳隆, 江澤 元, 釜江 常好, 窪 秀利, 鈴木 清詞, 関本 裕太郎, 高橋 忠幸, 田中 光明, 平山 昌治, 松崎 恵一, 矢島 信之, 山上 隆正, 秋山 弘光, 郡司 修一, 田村 忠久, 能町 正治, 宮崎 聡, 村上 浩之, 森 国城, 山崎 典子, EDBERG Tim
    宇宙科学研究所報告. 特集 32 71-88 1995年3月  
    硬X線/γ線検出器Welcome-1 (mk2)の気球実験における方位角制御のために, リアクションホイールとよじれ戻しモーターを用いた制御方法による方位角制御システムを構築した。制御に用いた部品のパラメーターの評価, 地上, および上空でのパフォーマンスについて報告する。
  • GUNJI, S, HIRAYAMA, M, KAMAE, T, et al.
    ASTROPHYSICAL JOURNAL 428(1) 284-291 1994年  査読有り
    We observed a young rotation-powered pulsar, PSR 1509-58, in the hard X-ray/y-ray or the soft γ-ray band with a balloon-borne detector in Brazil on 1991 November 19 (UT). With a timing analysis we detected pulsations in the energy band 94-240 keV at the 150.687 ms period determined from radio observations. The pulsating flux is (7.1 ± 1.7) × 10-4 cm-2 s-1 in this band, and the energy spectrum follows a power law with photon index α = 1.64 ± 0.4. The averaged pulse profile shows a broad single peak with a sharp rise and has a duty cycle around 50% or higher: these features are similar to what have been observed in the X-ray band by the Ginga satellite. Based on the data available now, the fraction of energy transformed from rotational energy loss to pulsed/ nonpulsed soft γ-ray radiation is estimated. If the solid angle swept by the pulsed beam is about the same as for the Crab pulsar (PSR 0531+21) and the Vela pulsar (PSR 0833-45), PSR 1509-58 turn out to be an extremely efficient pulsar, converting a large fraction of its rotational energy loss to radiation, as the outer gap model predicts. The observed pulsed spectrum, however, is strong in the soft γ-ray band, in a sharp contrast to what has been observed in the Vela pulsar, a pulsar expected to be similar PSR 1509-58 in the outer gap model. The fact that the pulse profile remains broad and single-peaked in the soft γ-ray band is also new for Crab-like pulsars. In these regards, PSR 1509-58 may require some alteration to the standard outer gap model or even a new model for gamma-ray emission in pulsars.
  • T. Kamae, S. Gunji, M. Hirayama, S. Miyazaki, T. Nagato, A. Nakao, Y. Sekimoto, K. Suzuki, T. Takahashi, T. Tamura, M. Tanaka, N. Yamaoka
    IEEE Transactions on Nuclear Science 40(2) 204-207 1993年  査読有り
    We have developed a new kind of phoswich counters that are capable of detecting low flux hard X-ray / γ-ray from localized sources. The counter consists of a small inorganic scintillator with a fast decay time (the detection part) glued to the interior bottom surface of a well-shaped block of another inorganic scintillator with a slow decay time (the shielding part). The well-shaped shielding part acts as an active collimator as well as an active shield. The whole assembly is viewed by a phototube from the exterior bottom surface of the shielding part. By using an appropriate pulse-shape discriminator (PSD), hard X-rays/gamma-rays that have deposited energy only in the detection part can be selected. The first model counter was built by using a new scintillator (GSO) in the detection part and Csl(Tl) in the shielding part. A detector system consisting of 64 such phoswich counters (total area ~ 740 cm&lt sup&gt 2&lt /sup&gt ) was flown on board a baloon, setting a limit to the &lt sup&gt 57&lt /sup&gt Co line flux from SN1987A at around 10&lt sup&gt -4&lt /sup&gt cm&lt sup&gt -2&lt /sup&gt s. The sensitivity for continuum flux was around a few X l0&lt sup&gt -6&lt /sup&gt cm&lt sup&gt -2&lt /sup&gt s&lt sup&gt -1&lt /sup&gt keV&lt sup&gt -1&lt /sup&gt between 100 and 200 keV. Efforts to lower the sensitivity further are under-way. In the second model, Csl(Tl) was replaced by BGO and radioactive contaminations in GSO were reduced. More improvements are to be made the in near future to reach a sensitivity (3σ) around 5 X 10&lt sup&gt -7&lt /sup&gt cm&lt sup&gt -2&lt /sup&gt s&lt sup&gt -1&lt /sup&gt keV&lt sup&gt -1&lt /sup&gt for continuum. © 1993 IEEE
  • T. Takahashi, S. Gunji, M. Hirayama, T. Kamae, S. Miyazaki, Y. Sekimoto, T. Tamura, M. Tanaka, N. Y. Yamasaki, T. Yamagami, M. Nomachi, H. Murakami
    IEEE Transactions on Nuclear Science 40(4) 890-898 1993年  査読有り
    We have developed a low background hard X-ray/gamma-ray telescope (Welcome-1) for balloon-borne experiments in the energy range from 40 keV to 800–1000 keV. The detector is based on newly developed well-type phoswich counters. In the first well-type phoswich counter, GSO(Ce) (Gd&lt inf&gt 2&lt /inf&gt SiO&lt inf&gt 5&lt /inf&gt doped with Ce) is used as the detection part and CsI(T1) as the shielding part. Welcome-1 consists of 64 GSO/CsI well-type phoswich counters assembled in the “compound-eye” configuration and the effective area is 740 cm&lt sup&gt 2&lt /sup&gt at 122 keV and 222 cm&lt sup&gt 2&lt /sup&gt at 511 keV line. The well-type phoswich counter and the compound eye configuration reduces background significantly both external and internal and allows us a high signal-to-noise ratio in balloon-borne experiments. The data from the detector is taken by the versatile data acquisition system based on the VME computer specially designed for balloon-borne experiments. In the system, the arrival time of each event is recorded by the clock system which utilizes GPS satellite. The background levels at an altitude of 4.5g/cm&lt sup&gt 2&lt /sup&gt are 1×10&lt sup&gt -4&lt /sup&gt /cm&lt sup&gt 2&lt /sup&gt /s/keV at 122 keV. Crab nebula has been observed with the signal to background ratio better than unity between 100 and 200 keV. In this paper, the desine of the telescope and the flight performace are presented. © 1993 IEEE
  • T. Kamae, T. Takahashi, M. Tanaka, S. Gunji, S. Miyazaki, T. Tamura, Y. Sekimoto, N. Yamaoka, J. Nishimura, N. Yajima, T. Yamagami, M. Nomachi, H. Murakami, M. Nakagawa, A. Neri
    Advances in Space Research 13(2) 165-168 1993年  査読有り
    We have developed a new kind of phoswich counters that will be capable of detecting low flux hard X-rays/gamma-rays from astronomical objects. The new phoswich counter consists of a small inorganic scintillator with a fast decay time (the detection part) glued to the interior bottom surface of a rectangular well-shaped block of another inorganic scintillator with a slow decay time (the shielding part). Here, the well-shaped shielding part acts as an active collimator as well as an active shield. We have built a detector system consisting of 64 such phoswich counters: newly developed scintillator (GSO) is used for the detection part and CsI(Tl) is used for the shielding part. The total geometrical area of the 64 detection parts is about 740cm2 and its 3σ sensitivity is expected to reach below 10-5cm-2s-1keV-1 up to 700keV. With several improvements such detectors will be able to detect hard X-rays/gamma-rays at a flux level around 10-6cm-2s-1keV-1 upto 2 MeV. © 1992.
  • H. Murakami, S. Gunji, M. Hirayama, T. Kamae, S. Miyazaki, Y. Sekimoto, T. Takahashi, T. Tamura, M. Tanaka, N. Yamaoka, T. Yamagami, M. Nomachi, K. Mori
    IEEE Transactions on Nuclear Science 39(5) 1316-1320 1992年  査読有り
    We have developed a simple pulse shape discriminator (PSD) for applications where a large number of channels are used within limited space and electric power. In the PSD, the output signal from a photomultiplier is differentiated and integrated to form a triple-polar pulse. The time interval between the first and second zero crossings depends on the decay time of the scintillation light. The circuit selects signals from the proper scintillator by using this interval. By this method, we can significantly reduce the effect of time slewing in the low energy region. We have successfully operated sixty four channels of the PSD in a balloon borne hard X-ray experiment. © 1992 IEEE
  • GUNJI, S, KAMAE, T, MIYAZAKI, S, et al.
    ASTROPHYSICAL JOURNAL 397(2) 1992年  査読有り

MISC

 187
  • 佐藤浩介, 大橋隆哉, 石崎欣尚, 江副祐一郎, 藤田裕, 山崎典子, 石田学, 前田良知, 満田和久, 中島裕貴, 三石郁之, 田原譲, 藤本龍一, 鶴剛, 太田直美, 大里健, 永井大輔, 吉川耕司, 河合誠之, 松下恭子, 山田真也, 一戸悠人, 内田悠介
    日本天文学会年会講演予稿集 2021 2021年  
  • 佐藤浩介, 山崎典子, 石田学, 前田良知, 満田和久, 三石郁之, 田原譲, 石崎欣尚, 江副祐一郎, 藤田裕, 藤本龍一, 鶴剛, 大里健, 太田直美, 永井大輔, 吉川耕司, 河合誠之, 松下恭子, 山田真也, 一戸悠人, 内田悠介, 中島裕貴, 中島裕貴
    日本天文学会年会講演予稿集 2021 2021年  
  • Masashi Hazumi, Peter A. Ade, Alexandre Adler, Erwan Allys, Kam Arnold, Didier Auguste, Jonathan Aumont, Ragnhild Aurlien, Jason Austermann, Carlo Baccigalupi, Anthony J. Banday, R. Banjeri, Rita B. Barreiro, Soumen Basak, Jim Beall, Dominic Beck, Shawn Beckman, Juan Bermejo, Paolo de Bernardis, Marco Bersanelli, Julien Bonis, Julian Borrill, Francois Boulanger, Sophie Bounissou, Maksym Brilenkov, Michael Brown, Martin Bucher, Erminia Calabrese, Paolo Campeti, Alessandro Carones, Francisco J. Casas, Anthony Challinor, Victor Chan, Kolen Cheung, Yuji Chinone, Jean F. Cliche, Loris Colombo, Fabio Columbro, Javier Cubas, Ari Cukierman, David Curtis, Giuseppe D'Alessandro, Nadia Dachlythra, Marco De Petris, Clive Dickinson, Patricia Diego-Palazuelos, Matt Dobbs, Tadayasu Dotani, Lionel Duband, Shannon Duff, Jean M. Duval, Ken Ebisawa, Tucker Elleflot, Hans K. Eriksen, Josquin Errard, Thomas Essinger-Hileman, Fabio Finelli, Raphael Flauger, Cristian Franceschet, Unni Fuskeland, Mathew Galloway, Ken Ganga, Jian R. Gao, Ricardo Genova-Santos, Martina Gerbino, Massimo Gervasi, Tommaso Ghigna, Eirik Gjerløw, Marcin L. Gradziel, Julien Grain, Frank Grupp, Alessandro Gruppuso, Jon E. Gudmundsson, Tijmen de Haan, Nils W. Halverson, Peter Hargrave, Takashi Hasebe, Masaya Hasegawa, Makoto Hattori, Sophie Henrot-Versillé, Daniel Herman, Diego Herranz, Charles A. Hill, Gene Hilton, Yukimasa Hirota, Eric Hivon, Renee A. Hlozek, Yurika Hoshino, Elena de la Hoz, Johannes Hubmayr, Kiyotomo Ichiki, Teruhito Iida, Hiroaki Imada, Kosei Ishimura, Hirokazu Ishino, Greg Jaehnig, Tooru Kaga, Shingo Kashima, Nobuhiko Katayama, Akihiro Kato, Takeo Kawasaki, Reijo Keskitalo, Theodore Kisner, Yohei Kobayashi, Nozomu Kogiso, Alan Kogut, Kazunori Kohri, Eiichiro Komatsu, Kunimoto Komatsu, Kuniaki Konishi, Nicoletta Krachmalnicoff, Ingo Kreykenbohm, Chao-Lin L. Kuo, Akihiro Kushino, Luca Lamagna, Jeff V. Lanen, Massimiliano Lattanzi, Adrian T. Lee, Clément Leloup, François Levrier, Eric Linder, Thibaut Louis, Gemma Luzzi, Thierry Maciaszek, Bruno Maffei, Davide Maino, Muneyoshi Maki, Stefano Mandelli, Enrique Martinez-Gonzalez, Silvia Masi, Tomotake Matsumura, Aniello Mennella, Marina Migliaccio, Yuto Minami, Kazuhisa Mitsuda, Joshua Montgomery, Ludovic Montier, Gianluca Morgante, Baptiste Mot, Yasuhiro Murata, John A. Murphy, Makoto Nagai, Yuya Nagano, Taketo Nagasaki, Ryo Nagata, Shogo Nakamura, Toshiya Namikawa, Paolo Natoli, Simran Nerval, Toshiyuki Nishibori, Haruki Nishino, Fabio Noviello, Créidhe O'Sullivan, Hideo Ogawa, Hiroyuki Ogawa, Shugo Oguri, Hiroyuki Ohsaki, Izumi S. Ohta, Norio Okada, Nozomi Okada, Luca Pagano, Alessandro Paiella, Daniela Paoletti, Guillaume Patanchon, Julien Peloton, Francesco Piacentini, Giampaolo Pisano, Gianluca Polenta, Davide Poletti, Thomas Prouvé, Giuseppe Puglisi, Damien Rambaud, Christopher Raum, Sabrina Realini, Martin Reinecke, Mathieu Remazeilles, Alessia Ritacco, Gilles Roudil, Jose A. Rubino-Martin, Megan Russell, Haruyuki Sakurai, Yuki Sakurai, Maura Sandri, Manami Sasaki, Giorgio Savini, Douglas Scott, Joseph Seibert, Yutaro Sekimoto, Blake Sherwin, Keisuke Shinozaki, Maresuke Shiraishi, Peter Shirron, Giovanni Signorelli, Graeme Smecher, Samantha Stever, Radek Stompor, Hajime Sugai, Shinya Sugiyama, Aritoki Suzuki, Junichi Suzuki, Trygve L. Svalheim, Eric Switzer, Ryota Takaku, Hayato Takakura, Satoru Takakura, Yusuke Takase, Youichi Takeda, Andrea Tartari, Ellen Taylor, Yutaka Terao, Harald Thommesen, Keith L. Thompson, Ben Thorne, Takayuki Toda, Maurizio Tomasi, Mayu Tominaga, Neil Trappe, Matthieu Tristram, Masatoshi Tsuji, Masahiro Tsujimoto, Carole Tucker, Joe Ullom, Gerard Vermeulen, Patricio Vielva, Fabrizio Villa, Michael Vissers, Nicola Vittorio, Ingunn Wehus, Jochen Weller, Benjamin Westbrook, Joern Wilms, Berend Winter, Edward J. Wollack, Noriko Y. Yamasaki, Tetsuya Yoshida, Junji Yumoto, Mario Zannoni, Andrea Zonca
    Space Telescopes and Instrumentation 2020: Optical, Infrared, and Millimeter Wave 2020年12月21日  
  • Ryota Takaku, Shaul Hanany, Yurika Hoshino, Hiroaki Imada, Hirokazu Ishino, Nobuhiko Katayama, Kunimoto Komatsu, Kuniaki Konishi, Makoto Kuwata Gonokami, Tomotake Matsumura, Kazuhisa Mitsuda, Haruyuki Sakurai, Yuki Sakurai, Qi Wen, Noriko Yamasaki, Karl Young, Junji Yumoto
    Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X 2020年12月16日  
  • Yutaro Sekimoto, Peter Ade, Alexandre Adler, Erwan Allys, Kam Arnold, Didier Auguste, Jonathan Aumont, Ragnhild Aurlien, Jason Austermann, Carlo Baccigalupi, Anthony Banday, Ranajoy Banerji, Rita Barreiro, Soumen Basak, Jim Beall, Dominic Beck, Shawn Beckman, Juan Bermejo, Paolo de Bernardis, Marco Bersanelli, Julien Bonis, Julian Borrill, Francois Boulanger, Sophie Bounissou, Maksym Brilenkov, Michael Brown, Martin Bucher, Erminia Calabrese, Paolo Campeti, Alessandro Carones, Francisco Casas, Anthony Challinor, Victor Chan, Kolen Cheung, Yuji Chinone, Jean Cliche, Loris Colombo, Fabio Columbro, Javier Cubas, Ari Cukierman, David Curtis, Giuseppe D'Alessandro, Nadia Dachlythra, Marco De Petris, Clive Dickinson, Patricia Diego-Palazuelos, Matt Dobbs, Tadayasu Dotani, Lionel Duband, Shannon Duff, Jean Duval, Ken Ebisawa, Tucker Elleflot, Hans Eriksen, Josquin Errard, Thomas Essinger-Hileman, Fabio Finelli, Raphael Flauger, Cristian Franceschet, Unni Fuskeland, Mathew Galloway, Ken Ganga, Jian Gao, Ricardo Genova-Santos, Martina Gerbino, Massimo Gervasi, Tommaso Ghigna, Eirik Gjerløw, Marcin Gradziel, Julien Grain, Frank Grupp, Alessandro Gruppuso, Jon Gudmundsson, Tijmen de Haan, Nils Halverson, Peter Hargrave, Takashi Hasebe, Masaya Hasegawa, Makoto Hattori, Masashi Hazumi, Sophie Henrot-Versillé, Daniel Herman, Diego Herranz, Charles Hill, Gene Hilton, Yukimasa Hirota, Eric hivon, Renee Hlozek, Yurika Hoshino, Elena de la Hoz, Johannes Hubmayr, Kiyotomo Ichiki, Teruhito iida, Hiroaki Imada, Kosei Ishimura, Hirokazu Ishino, Greg Jaehnig, Tooru Kaga, Shingo Kashima, Nobuhiko Katayama, Akihiro Kato, Takeo Kawasaki, Reijo Keskitalo, Theodore Kisner, Yohei Kobayashi, Nozomu Kogiso, Alan Kogut, Kazunori Kohri, Eiichiro Komatsu, Kunimoto Komatsu, Kuniaki Konishi, Nicoletta Krachmalnicoff, Ingo Kreykenbohm, Chao-Lin Kuo, Akihiro Kushino, Luca Lamagna, Jeff Lanen, Massimiliano Lattanzi, Adrien Lee, Clément Leloup, François Levrier, Eric Linder, Thibaut Louis, Gemma Luzzi, Thierry Maciaszek, Bruno Maffei, Davide Maino, Muneyoshi Maki, Stefano Mandelli, Enrique Martinez-Gonzalez, Silvia Masi, Tomotake Matsumura, Aniello Mennella, Marina Migliaccio, Yuto Minanmi, Kazuhisa Mitsuda, Josua Montgomery, Ludovic Montier, Gianluca Morgante, Baptise Mot, Yasuhiro Murata, John Murphy, Makoto Nagai, Yuya Nagano, Takeo Nagasaki, Ryo Nagata, Shogo Nakamura, Toshiya Namikawa, Paolo Natoli, Simran Nerval, Toshiyuki Nishibori, Haruki Nishino, Créidhe O'Sullivan, Hideo Ogawa, Hiroyuki Ogawa, Shogo Oguri, Hiroyuki Osaki, Izumi Ohta, Norio Okada, Nozomi Okada, Luca Pagano, Alessandro Paiella, Daniela Paoletti, Guillaume Patanchon, Julien Peloton, Francesco Piacentini, Giampaolo Pisano, Gianluca Polenta, Davide Poletti, Thomas Prouvé, Giuseppe Puglisi, Damien Tambaud, Christopher Raum, Sabrina Realini, Martin Reinecke, Mathieu Remazeilles, Alessa Ritacco, Gilles Roudil, Jose Rubino-Martin, Megan Russell, Haruyuki Sakurai, Yuki Sakurai, Maura Sandri, Manami Sasaki, Giorgio Savini, Douglas Scott, Joseph Seibert, Blake Sherwin, Keisuke Shinozaki, Maresuke Shiraishi, Peter Shirron, Giovanni Signorelli, Graeme Smecher, Samantha Stever, Radek Stompor, Hajime Sugai, Shinya Sugiyama, aritoki Suzuki, Junichi Suzuki, Trygve Svalheim, Eric Switzer, Ryota Takaku, hayato Takakura, satoru Takakura, Yusuke Takase, Youichi Takeda, Andrea Tartari, Ellen Taylor, Yutaka Terao, Harald Thommesen, Keith L. Thompson, Ben Thorne, Takayuki Toda, Maurizio Tomasi, Mayu Tominaga, Neil Trappe, Matthieu Tristram, Masatoshi Tsuji, Masahiro Tsujimoto, Carole Tucker, Joe Ullom, Gerard Vermeulen, Patricio Vielva, Fabrizio Villa, Michael Vissers, Nicola Vittorio, Ingunn Wehus, Jochen Weller, Benjamin Westbrook, Joern Wilms, Berend Winter, Edward Wollack, Noriko Y. Yamasaki, Tetsuya Yoshida, Junji Yumoto, Mario Zannoni, Andrea Zonca
    Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X 2020年12月16日  
もっとみる

担当経験のある科目(授業)

 1

所属学協会

 3

共同研究・競争的資金等の研究課題

 21
もっとみる

教育内容やその他の工夫

 1
  • 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

 8
  • 年度
    2018年度(FY2018)
    博士課程学生数
    1
    修士課程学生数
    1
  • 年度
    2019年度(FY2019)
    博士課程学生数
    1
    修士課程学生数
    3
  • 年度
    2020年度(FY2020)
    博士課程学生数
    1
    修士課程学生数
    3
  • 年度
    2018年度(FY2018)
    博士課程学生数
    1
    修士課程学生数
    1
  • 年度
    2019年度(FY2019)
    博士課程学生数
    1
    修士課程学生数
    3
  • 年度
    2020年度(FY2020)
    博士課程学生数
    1
    修士課程学生数
    3
  • 年度
    2022年度(FY2022)
    博士課程学生数
    3
    修士課程学生数
    2
  • 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

 6
  • 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 laser
    DOI
    http://doi.org/10.1063/5.0022765
  • 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 microcalorimeters
    DOI
    http://doi.org/10.1063/5.0016333
  • 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 converter
    DOI
    http://doi.org/10.1007/s10909-019-02257-9
  • 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 Field
    DOI
    http://doi.org/10.1088/1475-7516/2020/02/011
  • 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 Background
    DOI
    http://doi.org/10.1093/pasj/psv081
  • 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 253
    DOI
    http://doi.org/10.1093/pasj/65.2.44

● 専任大学名

 1
  • 専任大学名
    東京大学（University of Tokyo)

● 所属する所内委員会

 1
  • 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
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