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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

 257
  • Kenichiro Nagayoshi, Kazuhiro Sakai, Kazuhisa Mitsuda, Noriko Y. Yamasaki, Yoh Takei, Keisuke Maehata, Naoko Iyomoto, Shohei Ezaki, Akira Takano, Makoto Maeda, Toru Hara
    IEICE Transactions on Electronics E98C(3) 186-191 2015年3月1日  査読有り
    Three-dimensionally assembled TES X-ray microcalorimeter arrays may be utilized for three purposes: (1) to obtain wide X-ray energy coverage of TES microcalorimeters, (2) to distinguish charged particle events from X-ray events, (3) to reconstruct Compton-scattering geometry for hard X-ray Compton cameras. We have designed and fabricated three-dimensionally assembled array of the minimum format i.e. 2 × 2 × 2 array in order to obtain a good energy resolution in a wide energy range of 0.5-20 keV and a high maximum counting rate of 2000 cps for energy dispersive X-ray spectrometer (EDS) system for a transmission electron microscope (TEM). Although we could not obtain required energy resolution because of a problem in the refrigerator system, we confirmed the operation of the three-dimensional array.
  • K. Maehata, N. Iyomoto, Y. Yamanaka, T. Ito, T. Hara, K. Mitsuda, N. Y. Yamasaki, K. Tanaka
    Journal of Superconductivity and Novel Magnetism 28(3) 1161-1165 2015年2月25日  査読有り
    A compact dry 3He- 4He dilution refrigerator (DR) was developed for operation of a superconducting transition edge sensor (TES) microcalorimeter x-ray detector mounted on a transmission electron microscope. A Gifford-McMahon (GM)-type mechanical cryocooler was used as a DR pre-cooler to operate the TES microcalorimeter without consuming liquid helium. To reduce the noise and vibrations generated by the GM cryocooler, the DR was separated from the cryocooler in a split system that allows a remote helium cooling loop to pre-cool the DR. In the DR unit, the dilution components of the still, the heat exchangers, and the cascade pair of mixing chambers were assembled into a compact cylinder. A snout made from an oxygen-free copper rod was attached to the DR mixing chamber for placement of the TES microcalorimeter x-ray detector. The lowest temperature and the cooling power in the mixing chamber were measured to be 87 mK and 20 μW at 100 mK, respectively. The DR unit was shown to maintain the temperature on top of the snout such that it was below the temperature required for multi-pixel-array TES microcalorimeter x-ray detector operation.
  • Takayuki Tamura, Ryo Iizuka, Yoshitomo Maeda, Kazuhisa Mitsuda, Noriko Y. Yamasaki
    Publications of the Astronomical Society of Japan 67(2) 231-2316 2015年1月27日  査読有り
    We present the results from deep Suzaku observations of the central region of the Perseus cluster. Bulbul et al. (2014, ApJ, 789, 13) reported the detection by XMM-Newton instruments of an unidentified X-ray emission line at an energy around 3.5 keV in spectra for the Perseus and other clusters. They argued for a possibility of the decay of sterile neutrino, a dark matter candidate. We examine Suzaku X-ray Imaging Spectrometer (XIS) spectra of the Perseus cluster for evidence in the 3.5 keV line and other possible dark matter features in the 2-6 keV energy band. In order to search for and constrain a weak line feature with the XIS, observations of the Crab Nebula are used to evaluate the system's effective area. We found no line feature at the claimed position with a systematic line flux upper limit at a half (1.5 eV in line equivalent width) of the claimed best-fitting value by Bulbul et al. (2014). We discuss this inconsistency in terms of instrumental calibration errors and modeling of continuum emission. Future prospects for high-energy resolution spectroscopy with ASTRO-H are presented.
  • K. Maehata, T. Hara, T. Ito, Y. Yamanaka, K. Tanaka, K. Mitsuda, N. Y. Yamasaki
    Cryogenics 61 86-91 2014年5月  査読有り
    A dry 3He-4He dilution refrigerator (DR) was developed for a superconducting transition edge sensor (TES) microcalorimeter installed on a transmission electron microscope. This system could be used for energy dispersive X-ray spectroscopy (EDS) with an excellent energy resolution. A Gifford-McMahon (GM)-type mechanical cryocooler was used as a pre-cooler for the DR to ensure liquid helium was not consumed during operation. To reduce sound and vibrations generated by the GM cryocooler, the DR was separated from the GM cryocooler in a split system. The TES microcalorimeter was glued onto the top of a copper rod referred to as the snout, which was attached to the mixing chamber of the DR. The cooling power in the mixing chamber was 30 μW at 105 mK. The lowest temperature in the mixing chamber was 74 mK, and that at top of the snout was 86 mK. An energy resolution of 7.6 eV full width at half maximum for Si Kα X-rays of 1.74 keV was obtained by TES microcalorimeter EDS performed with the transmission electron microscope. © 2014 Elsevier Ltd. All rights reserved.
  • I. Mitsuishi, H. Kawahara, N. Sekiya, S. Sasaki, T. Sousbie, N. Y. Yamasaki
    Astrophysical Journal 783(2) 2014年3月10日  査読有り
    We performed five pointing observations with Suzaku to search for hot gases associated with the junctions of galaxy filaments where no significant diffuse X-ray sources were previously detected. We discovered X-ray sources successfully in all five regions including merging groups of galaxies, Suzaku J0957+2610 and Suzaku J1134+2105, and analyzed two bright sources in each field. Spectral analysis indicates that three sources originate from X-ray diffuse halos associated with optically bright galaxies or groups of galaxies with kT ∼ 0.6-0.8 keV. The three other sources are possibly group- and cluster-scale X-ray halos with temperatures of ∼1 keV and ∼4 keV, respectively while the others are compact object origins such as active galactic nuclei. All of the three observed intracluster media within the junctions of the galaxy filaments previously found are involved in ongoing mergers. Thus, we demonstrate that deep X-ray observations at the filament junctions identified by galaxy surveys are a powerful means to explore previously undetected growing halos in a hierarchical structure. © 2014. The American Astronomical Society. All rights reserved.
  • T. Tamura, N. Y. Yamasaki, R. Iizuka, Y. Fukazawa, K. Hayashida, S. Ueda, K. Matsushita, K. Sato, K. Nakazawa, N. Ota, M. Takizawa
    Astrophysical Journal 782(1) 2014年2月10日  査読有り
    We present the results from Suzaku observations of the Perseus Cluster, which is relatively close, the brightest in the X-ray sky, and a relaxed object with a cool core. A number of exposures of central regions and offset pointing with the X-ray Imaging Spectrometer cover a region within radii of 20′-30′. The central data are used to evaluate the instrumental energy-scale calibration with accuracy confirmed to within around 300 km s -1 by the spatial and temporal variation of the instruments. These deep and well-calibrated data are used to measure X-ray redshifts of the intracluster medium. A hint of gas bulk motion, with radial velocity of about -(150-300) km s-1 relative to the main system, was found at 2′-4′ (45-90 kpc) west of the cluster center, where an X-ray excess and a cold front were found previously. No other velocity structure was discovered. Over spatial scales of 50-100 kpc and within 200 kpc radii of the center, the gas-radial-velocity variation is below 300 km s-1, while over scales of 400 kpc within 600 kpc radii, the variation is below 600 km s-1. These X-ray redshift distributions are compared spatially with those of optical member galaxies for the first time in galaxy clusters. Based on X-ray line widths, gas turbulent velocities within these regions are also constrained within 1000-3000 km s-1. These results of gas dynamics in the core and larger scales in association with cluster merger activities are discussed, and the future potential of high-energy resolution spectroscopy with ASTRO-H is considered. © 2014. The American Astronomical Society. All rights reserved..
  • Kosuke Sato, Kyoko Matsushita, Noriko Y. Yamasaki, Shin Sasaki, Takaya Ohashi
    Publications of the Astronomical Society of Japan 66(5) 2014年  査読有り
    We report properties of the intracluster medium (ICM) in Abell 1246 to the virial radius (r&lt inf&gt 200&lt /inf&gt ) and further outside as observed with Suzaku. The ICM emission is clearly detected to r&lt inf&gt 200&lt /inf&gt , and we derive profiles of electron temperature, density, entropy, and clustermass based on the spectral analysis. The temperature shows variation from ∼7 keV at the central region to ∼2.5 keV around r&lt inf&gt 200&lt /inf&gt . The total mass in r500 is (4.3 ± 0.4) × 1014 M&lt inf&gt ⊙&lt /inf&gt , assuming hydrostatic equilibrium. At r &gt r&lt inf&gt 500&lt /inf&gt , the hydrostatic mass starts to decline and we therefore employ the total mass within r&lt inf&gt 200&lt /inf&gt based on a weak-lens mass profile obtained from a sample of lower-mass clusters. This yields a gasmass fraction at r&lt inf&gt 200&lt /inf&gt consistent with the cosmic baryon fraction, i.e., ∼17%. The entropy profile indicates a flatter slope than that of the numerical simulation, particularly in r &gt r&lt inf&gt 500&lt /inf&gt . These tendencies are similar to those of other clusters observed with Suzaku. We detect no significant ICM emission outside of r&lt inf&gt 200&lt /inf&gt , and 2σ upper limits of redshifted O VII and O VIII line intensities are constrained to be less than 2.9 and 5.6 × 10&lt sup&gt -7&lt /sup&gt photons cm&lt sup&gt -2&lt /sup&gt s&lt sup&gt -1&lt /sup&gt arcmin&lt sup&gt -2&lt /sup&gt , respectively. The O VII line upper limit indicates n&lt inf&gt H&lt /inf&gt &lt 4.7 × 10&lt sup&gt -5&lt /sup&gt cm&lt sup&gt -3&lt /sup&gt (Z/0.2 Z&lt inf&gt ⊙&lt /inf&gt )&lt sup&gt -1/2&lt /sup&gt (L/20 Mpc)&lt sup&gt -1/2&lt /sup&gt , which corresponds to an overdensity, δ &lt 160 (Z/0.2 Z&lt inf&gt ⊙&lt /inf&gt )&lt sup&gt -1/2&lt /sup&gt (L/20 Mpc)&lt sup&gt -1/2&lt /sup&gt .
  • Kazuhiro Sakai, Yangsen Yao, Kazuhisa Mitsuda, Noriko Y. Yamasaki, Q. Daniel Wang, Yoh Takei, Dan McCammon
    Publications of the Astronomical Society of Japan 66(4) 2014年  査読有り
    We present a structural study of the hot ISM in the Galactic halo along the sight line toward the bright active galactic nucleus Mkn 421. The OVII and OVIII absorption lines were measured with the LowEnergy Transmission Grating Spectrograph aboard Chandra toward Mkn 421 the OVII and OVIII emission lines were observed in the adjacent fields of the line of sight with the X-ray Imaging Spectrometer aboard Suzaku. We jointly analyzed the absorption and emission spectra while assuming exponential distributions of the gas temperature and density from the Galactic plane, and constrained the temperature and density at the plane to be (3.2+0.6 -0.7) × 106 K and (1.2+0.5-0.4) × 10-3 cm-3, with a scale heights of 1.6+1.7 -0.7 kpc and &gt 2.8 kpc, respectively. The results are consistent with those obtained in the LMC X-3 direction and the PKS 2155-304 direction, describing a thick disk-like hot gas with its height of a few kpc from the Galactic plane. © The Author 2014.
  • Y. Ishisaki, Y. Enokijima, Y. Ezoe, T. Ohashi, H. Akamatsu, R. Yamamoto, Y. Takei, K. Mitsuda, N. Y. Yamasaki, S. Yamada
    Journal of Low Temperature Physics 176(3-4) 344-349 2014年  査読有り
    We have developed Ti/Au bilayer transition-edge sensor (TES) microcalorimeters for future X-ray astrophysical satellite missions such as DIOS. One possible concern on the space use of TES microcalorimeters is its radiation tolerance. We have evaluated the performance of a Ti/Au bilayer (30/40 nm thick) TES microcalorimeter with 1.5 μ m thick Au absorber, before and after irradiation of 150 MeV proton beam with a total dose of 10 krad, corresponding to 10 years in the low Earth orbit. No significant changes on transition temperature, sensitivity, normal resistance, and critical current were observed. The energy resolution for 5.9 keV X-rays was 5.6 ± 0.3 eV (FWHM) after the irradiation, which was slightly worse than 5.1 ± 0.3 eV before the irradiation. We consider that our TES has sufficient radiation tolerance in orbit. © 2014 Springer Science+Business Media New York.
  • R. Yamamoto, K. Sakai, Y. Takei, N. Y. Yamasaki, K. Mitsuda
    Journal of Low Temperature Physics 176(3-4) 453-458 2014年  査読有り
    Frequency division multiplexing (FDM) is a promising approach to read out a large format transition-edge sensor (TES) array for future astrophysical missions. We constructed a four channel FDM readout system using baseband feedback in the MHz band. We demonstrated the principle of our FDM method with an actual TES array, a multiplexing SQUID and LC band-pass filters under 100 mK. The resonant frequencies of LC filters were consistent with the design value with an accuracy of better than 3 %. We successfully obtained X-ray pulses from two TESs simultaneously but the energy resolution was degraded to about 100 eV at 5.9 keV and crosstalk effects were observed. The origin of the crosstalk effects is investigated by modified setups. Based on comparative experiments and numerical calculations, we conclude that the non-linearity of the SQUID is the cause of some of the crosstalk effects. Unlike the regular crosstalk effect from the adjoining channels, the crosstalk effect due to non-linearity observed in this paper occurs in all channels. Solving these problems will help us to obtain FDM readout with sufficient energy resolution. © 2014 Springer Science+Business Media New York.
  • Norio Sekiya, Noriko Y. Yamasaki, Kazuhisa Mitsuda, Yoh Takei
    Publications of the Astronomical Society of Japan 66(2) 2014年  査読有り
    The quantitative measurement of O VII line intensity is a powerful method for understanding the soft X-ray diffuse background. By systematically analyzing the O VII line intensity in 145 high-latitude Suzaku/XIS observations, the flux of O I fluorescent line in the XIS spectrum, contaminating the O VII line, is found to have an increasing trend with time especially after 2011. For these observations, the O VII line intensity would be overestimated unless taking into consideration the O I fluorescent line contamination. Since the O I line emission originates from solar X-rays, this increase suggests that the flux of incident solar X-rays at the O I fluorescence energy tend to be larger than that in the early phase of Suzaku observations (2005-2010). © 2014 The Author.
  • T. Matsumura, Y. Akiba, J. Borrill, Y. Chinone, M. Dobbs, H. Fuke, A. Ghribi, M. Hasegawa, K. Hattori, M. Hattori, M. Hazumi, W. Holzapfel, Y. Inoue, K. Ishidoshiro, H. Ishino, H. Ishitsuka, K. Karatsu, N. Katayama, I. Kawano, A. Kibayashi, Y. Kibe, K. Kimura, N. Kimura, K. Koga, M. Kozu, E. Komatsu, A. Lee, H. Matsuhara, S. Mima, K. Mitsuda, K. Mizukami, H. Morii, T. Morishima, S. Murayama, M. Nagai, R. Nagata, S. Nakamura, M. Naruse, K. Natsume, T. Nishibori, H. Nishino, A. Noda, T. Noguchi, H. Ogawa, S. Oguri, I. Ohta, C. Otani, P. Richards, S. Sakai, N. Sato, Y. Sato, Y. Sekimoto, A. Shimizu, K. Shinozaki, H. Sugita, T. Suzuki, A. Suzuki, O. Tajima, S. Takada, S. Takakura, Y. Takei, T. Tomaru, Y. Uzawa, T. Wada, H. Watanabe, M. Yoshida, N. Yamasaki, T. Yoshida, K. Yotsumoto
    Journal of Low Temperature Physics 176(5-6) 733-740 2014年  査読有り
    LiteBIRD is a next-generation satellite mission to measure the polarization of the cosmic microwave background (CMB) radiation. On large angular scales the B-mode polarization of the CMB carries the imprint of primordial gravitational waves, and its precise measurement would provide a powerful probe of the epoch of inflation. The goal of LiteBIRD is to achieve a measurement of the characterizing tensor to scalar ratio r to an uncertainty of δr = 0.001. In order to achieve this goal we will employ a kilo-pixel superconducting detector array on a cryogenically cooled sub-Kelvin focal plane with an optical system at a temperature of 4 K. We are currently considering two detector array options transition edge sensor (TES) bolometers and microwave kinetic inductance detectors. In this paper we give an overview of LiteBIRD and describe a TES-based polarimeter designed to achieve the target sensitivity of 2 μK arcmin over the frequency range 50-320 GHz. © 2014 Springer Science+Business Media New York.
  • Yoichi Sato, Kenichiro Sawada, Keisuke Shinozaki, Hiroyuki Sugita, Toshiyuki Nishibori, Ryota Sato, Kazuhisa Mitsuda, Noriko Y. Yamasaki, Yoh Takei, Ken Goto, Takao Nakagawa, Ryuichi Fujimoto, Kenichi Kikuchi, Masahide Murakami, Shoji Tsunematsu, Kiyomi Ootsuka, Kenichi Kanao, Katsuhiro Narasaki
    Cryogenics 64 182-188 2014年  査読有り
    Astro-H is the Japanese X-ray astronomy satellite to be launched in 2015. The Soft X-ray Spectrometer (SXS) on board Astro-H is a high energy resolution spectrometer utilizing an X-ray micro-calorimeter array, which is operated at 50 mK by the ADR with the 30 liter superfluid liquid helium. The mechanical cryocoolers, 4 K-class Joule Thomson (JT) cooler and 20 K-class double-staged Stirling (2ST) cooler, are key components of the SXS cooling system to extend the lifetime of LHe cryogen beyond 3 years as required. Higher reliability was therefore investigated with higher cooling capability based on the heritage of existing cryocoolers. As the task of assessing further reliability dealt with the pipe-choking phenomena by contaminant solidification of the on-orbit SMILES JT cryocooler, outgassing from materials and component parts used in the cryocoolers was measured quantitatively to verify the suppression of carbon dioxide gas by their storage process and predict the total accumulated carbon dioxide for long-term operation. A continuous running test to verify lifetime using the engineering model (EM) of the 4 K-JT cooler is underway, having operated for a total of 720 days as of June 2013 and showing no remarkable change in cooling performance. During the current development phase, prototype models (PM) of the cryocoolers were installed to the test SXS dewar (EM) to verify the overall cooling performance from room temperature to 50 mK. During the EM dewar test, the requirement to reduce the transmitted vibration from the 2ST cooler compressor was recognized as mitigating the thermal instability of the SXS microcalorimeter at 50 mK.
  • K. Maehata, N. Iyomoto, M. Maeda, S. Ezaki, A. Takano, S. Matsumura, T. Hara, K. Mitsuda, N. Y. Yamasaki, K. Tanaka
    Journal of Low Temperature Physics 176(3-4) 578-583 2014年  査読有り
    A four-pixel-array superconducting transition-edge sensor (TES) microcalorimeter with a mushroom-shaped absorber was developed for energy dispersive spectroscopy performed on a transmission electron microscope. The TES consists of a bilayer of Au/Ti with either a 120- or 50-nm thickness. The absorber is made from a Au layer and its stem is deposited in the center of the TES surface. A Ta22O5 insulating layer of 100-nm thickness is inserted between the overhang region of the absorber and the TES surface. Two types of microcalorimeter were fabricated with differing absorber thicknesses of 0.5 and 5.0 μ m. An energy resolution of 15 eV FWHM with 5.9-keV X-rays was obtained using the 0.5- μ m-type microcalorimeter. © 2014 Springer Science+Business Media New York.
  • K. Sakai, Y. Takei, R. Yamamoto, N. Y. Yamasaki, K. Mitsuda, M. Hidaka, S. Nagasawa, S. Kohjiro, T. Miyazaki
    Journal of Low Temperature Physics 176(3-4) 400-407 2014年  査読有り
    We are developing frequency-division multiplexing (FDM) systems with baseband feedback for TES X-ray microcalorimeter arrays for use with the DIOS mission. To meet the requirement of limited cooling capacity at cryogenic temperatures, we developed low-power and FDM-optmized dc-SQUIDs. To make maximum use of the SQUIDs, we also developed digital electronics using FPGA evaluation boards and ADC/DAC FMC daughter cards, and evaluated signal-to-noise ratios and gain-bandwidth products. © 2014 Springer Science+Business Media New York.
  • Hiroshi Yoshitake, Kazuhiro Sakai, Kazuhisa Mitsuda, Noriko Y. Yamasaki, Yoh Takei, Ryo Yamamoto
    Publications of the Astronomical Society of Japan 65(2) 2013年4月25日  査読有り
    Long-term time variabilities of the OVII (0.57 keV) emission in the soft X-ray diffuse background were studied using six Suzaku annual observations of the blank sky towards the Lockman Hole made from 2006 to 2011. After time intervals in which the emission was enhanced on time scales of a few tens of ks were removed, the OVII intensity was found to be constant from 2006 to 2009 within 90% statistical errors. The intensity in 2010 and 2011 was higher by 2-3 LU (= photons s-1 cm-2 sr-1) than the earlier values. The most plausible origin of the fast variable component is Solar wind charge exchange (SWCX). The intensity increase is not positively correlated with the proton flux at the L1 point. Since all of the observations were made in the same season of a year, the variation cannot be explained by parallax of the SWCX-induced X-ray emission from the Heliosphere. We consider that it is related to geometrical changes of slow and fast solar wind structures associated with the 11 year solar activity. The observed variation was compared with that expected from the SWCX-induced X-ray emission model. © 2013 Astronomical Society of Japan.
  • MITSUISHI Ikuyuki, YAMASAKI Noriko Y., TAKEI Yoh
    Publications of the Astronomical Society of Japan 65(2) 44-1-12 2013年  査読有り
  • Ikuyuki Mitsuishi, Yuichiro Ezoe, Kensuke Ishizu, Teppei Moriyama, Makoto Mita, Noriko Y. Yamasaki, Kazuhisa Mitsuda, Yoshiaki Kanamori, Kohei Morishita, Kazuo Nakajima
    Sensors and Actuators, A: Physical 188 411-416 2012年12月  査読有り
    We report on our first X-ray imaging test of our novel ultra-lightweight and high-resolution MEMS X-ray optics for future space astronomical missions. We have fabricated a single-stage test optic made of Si from a Si (1 1 1) wafer with a thickness of 300 μm. We conducted a dry etching and made 20 μm line and space through holes to use their side walls for X-ray mirrors. We have smoothed the side walls by annealing and plastically bending the wafer to a spherical shape with a curvature of radius of 1000 mm.We have irradiated Al Kα 1.49 keV to the test optic and, for the first time, have verified X-ray focusing. An evaluated angular resolution ranged from 26 to 130 arcmin, which is two orders of magnitude worse than our goal of 15 arcsec. We found that this degraded resolution is mainly due to a large surface roughness of the side walls &gt 10 μm scale and possibly the deformation process. An estimated X-ray reflectivity was also an order of magnitude lower than the theoretical value assuming flat side walls. We concluded that this could be due to the loss of the reflective area by the rough surface. Therefore, the future improvement on the large scale surface roughness is indispensable for the better angular resolution and effective area. © 2012 Elsevier B.V. All rights reserved.
  • Jan-Willem den Herder, Luigi Piro, Takaya Ohashi, Chryssa Kouveliotou, Dieter H. Hartmann, Jelle S. Kaastra, L. Amati, M. I. Andersen, M. Arnaud, J. L. Attéia, S. Bandler, M. Barbera, X. Barcons, S. Barthelmy, S. Basa, S. Basso, M. Boer, E. Branchini, G. Branduardi-Raymont, S. Borgani, A. Boyarsky, G. Brunetti, C. Budtz-Jorgensen, D. Burrows, N. Butler, S. Campana, E. Caroli, M. Ceballos, F. Christensen, E. Churazov, A. Comastri, L. Colasanti, R. Cole, R. Content, A. Corsi, E. Costantini, P. Conconi, G. Cusumano, J. de Plaa, A. De Rosa, M. Del Santo, S. Di Cosimo, M. De Pasquale, R. Doriese, S. Ettori, P. Evans, Y. Ezoe, L. Ferrari, H. Finger, T. Figueroa-Feliciano, P. Friedrich, R. Fujimoto, A. Furuzawa, J. Fynbo, F. Gatti, M. Galeazzi, N. Gehrels, B. Gendre, G. Ghirlanda, G. Ghisellini, M. Gilfanov, P. Giommi, M. Girardi, J. Grindlay, M. Cocchi, O. Godet, M. Guedel, F. Haardt, R. den Hartog, I. Hepburn, W. Hermsen, J. Hjorth, H. Hoekstra, A. Holland, A. Hornstrup, A. van der Horst, A. Hoshino, J. in't Zand, K. Irwin, Y. Ishisaki, P. Jonker, T. Kitayama, H. Kawahara, N. Kawai, R. Kelley, C. Kilbourne, P. de Korte, A. Kusenko, I. Kuvvetli, M. Labanti, C. Macculi, R. Maiolino, M.Mas Hesse, K. Matsushita, P. Mazzotta, D. McCammon, M. Méndez, R. Mignani, T. Mineo, K. Mitsuda, R. Mushotzky, S. Molendi, L. Moscardini, L. Natalucci, F. Nicastro, P. O'Brien, J. Osborne, F. Paerels, M. Page, S. Paltani, K. Pedersen, E. Perinati, T. Ponman, E. Pointecouteau, P. Predehl, S. Porter, A. Rasmussen, G. Rauw, H. Röttgering, M. Roncarelli, P. Rosati, E. Quadrini, O. Ruchayskiy, R. Salvaterra, S. Sasaki, K. Sato, S. Savaglio, J. Schaye, S. Sciortino, M. Shaposhnikov, R. Sharples, K. Shinozaki, D. Spiga, R. Sunyaev, Y. Suto, Y. Takei, N. Tanvir, M. Tashiro, T. Tamura, Y. Tawara, E. Troja, M. Tsujimoto, T. Tsuru, P. Ubertini, J. Ullom, E. Ursino, F. Verbunt, F. van de Voort, M. Viel, S. Wachter, D. Watson, M. Weisskopf, N. Werner, N. White, R. Willingale, R. Wijers, N. Yamasaki, K. Yoshikawa, S. Zane
    Experimental Astronomy 34(2) 519-549 2012年10月  査読有り
    ORIGIN is a proposal for the M3 mission call of ESA aimed at the study of metal creation from the epoch of cosmic dawn. Using high-spectral resolution in the soft X-ray band, ORIGIN will be able to identify the physical conditions of all abundant elements between C and Ni to red-shifts of z = 10, and beyond. The mission will answer questions such as: When were the first metals created? How does the cosmic metal content evolve? Where do most of the metals reside in the Universe? What is the role of metals in structure formation and evolution? To reach out to the early Universe ORIGIN will use Gamma-Ray Bursts (GRBs) to study their local environments in their host galaxies. This requires the capability to slew the satellite in less than a minute to the GRB location. By studying the chemical composition and properties of clusters of galaxies we can extend the range of exploration to lower redshifts (z ~0. 2). For this task we need a high-resolution spectral imaging instrument with a large field of view. Using the same instrument, we can also study the so far only partially detected baryons in the Warm-Hot Intergalactic Medium (WHIM). The less dense part of the WHIM will be studied using absorption lines at low redshift in the spectra for GRBs. The ORIGIN mission includes a Transient Event Detector (coded mask with a sensitivity of 0. 4 photon/cm2/s in 10 s in the 5-150 keV band) to identify and localize 2000 GRBs over a five year mission, of which ~65 GRBs have a redshift &gt 7. The Cryogenic Imaging Spectrometer, with a spectral resolution of 2. 5 eV, a field of view of 30 arcmin and large effective area below 1 keV has the sensitivity to study clusters up to a significant fraction of the virial radius and to map the denser parts of the WHIM (factor 30 higher than achievable with current instruments). The payload is complemented by a Burst InfraRed Telescope to enable onboard red-shift determination of GRBs (hence securing proper follow up of high-z bursts) and also probes the mildly ionized state of the gas. Fast repointing is achieved by a dedicated Controlled Momentum Gyro and a low background is achieved by the selected low Earth orbit. © 2011 Springer Science+Business Media B.V.
  • K. Maehata, N. Iyomoto, T. Yasumune, M. Maeda, S. Matsumura, T. Hara, K. Mitsuda, N. Yamasaki, K. Tanaka
    Journal of Low Temperature Physics 167(3-4) 226-231 2012年6月  査読有り
    A 3×3+1 superconducting transition-edge sensor (TES) microcalorimeter- array has been developed for the energy dispersive spectrometer performed on a transmission electron microscope. For increasing sensitive area, each TES microcalorimeter consisted of a Ti/Au bilayer and a mushroom shaped absorber. The mushroom shaped absorber is made from a Au layer of 0.5 μm thick. Geometrical dimensions of the surface area of the TES and the absorber are 350 μm × 350 μm and 330 μm × 330 μm, respectively. The absorber stem of 150 μm × 150 μm in the cross sectional area is deposited on the center of the TES surface. A Ta2O5 insulating layer of 0.1 μm thick is inserted between the overhang layer of the absorber and the TES surface. One pixel of the TES microcalorimeter was operated for detecting X-ray photons emitted from an 55Fe source. © Springer Science+Business Media, LLC 2012.
  • N. Sekiya, N. Y. Yamasaki, K. Mitsuda, S. Kawasaki, Y. Takei, H. Yoshitake, K. Sakai, K. Sato, K. Maehata, H. Takashima
    Journal of Low Temperature Physics 167(3-4) 435-441 2012年6月  査読有り
    For future X-ray astronomy, a microcalorimeter array that has both megapixel imaging capability and eV-level high energy-resolution is desirable. In order to realize it, thermometers with negligible self-heating, multiplexing readout and close packing are essential components. We propose a novel detector concept, a dielectric microcalorimeter (DMC) and present current design studies. The DMC uses dielectric pixels as thermometers which form LC resonators in GHz band. The signals from many pixels can be easily multiplexed in a similar way to kinetic inductance detectors. The dielectric pixels are easy to be integrated into large and dense arrays. However, dielectrics with temperature-dependent permittivity below 2 K were not known. We evaluated quantum ferroelectric strontium titanate (STO) used in a capacitive thermometer higher than 2 K as a suitable dielectric for the DMC pixels. We fabricated STO capacitors and measured their capacitance from 2 K down to 80 mK. As a result, we found that their capacitive thermometer sensitivity at 100 mK are d logC/d log T ∼ 10-3, and they can be sensitive enough to detect X-ray with a resonator. We report the concepts, the measurement details, expected response to X-ray irradiation and our designs of the DMC. © Springer Science+Business Media, LLC 2012.
  • Yoichi Sato, Keisuke Shinozaki, Hiroyuki Sugita, Kazuhisa Mitsuda, Noriko Y. Yamasaki, Yoh Takei, Takao Nakagawa, Ryuichi Fujimoto, Masahide Murakami, Shoji Tsunematsu, Kiyomi Otsuka, Seiji Yoshida, Kenichi Kanao, Katsuhiro Narasaki
    Cryogenics 52(4-6) 158-164 2012年4月  査読有り
    Astro-H is the Japanese X-ray astronomy satellite planned for launch in 2014. The Soft X-ray Spectrometer (SXS) onboard Astro-H, is a high energy resolution spectrometer utilizing an X-ray micro-calorimeter array, which is operated at 50 mK by the ADR with the 30-L superfluid liquid helium (LHe). The mechanical cryocoolers, 4 K-class Joule Thomson (JT) cooler and 20 K-class double-staged Stirling (2ST) cooler are key components to achieve a LHe lifetime for over 3 years in orbit (5 years as a goal). Based on the existing cryocoolers onboard Akari (2006) and JEM/SMILES (2009), modifications for higher cooling power and reliability had been investigated. In the present development phase, the Engineering Models (EMs) of these upgraded cryocoolers are fabricated to carry out verification tests for cooling performance, mechanical performance and lifetime. Nominal cooling power of 200 mW at 20 K for the 2ST cooler and 40 mW at 4.5 K for the JT cooler were demonstrated with temperature and power margin. Mechanical performance test for the 2ST cooler units proves tolerability for pyro shock and vibration environment of the Astro-H criteria. Continuous running of the 4 K-class JT cooler combined with the 2ST precooler for lifetime test has achieved over 5000 h without any degradation of cooling performance. © 2012 Elsevier Ltd. All rights reserved.
  • Tadayuki Takahashi, Kazuhisa Mitsuda, Richard Kelley, Henri Aarts, Felix Aharonian, Hiroki Akamatsu, Fumie Akimotoe, Steve Allen, Naohisa Anabuki, Lorella Angelini, Keith Arnaud, Makoto Asai, Marc Audard, Hisamitsu Awaki, Philipp Azzarello, Chris Baluta, Aya Bamba, Nobutaka Bando, Mark Bautz, Roger Blandford, Kevin Boyce, Greg Brown, Ed Cackett, Maria Chernyakova, Paolo Coppi, Elisa Costantini, Jelle De Plaa, Jan-Willem Den Herder, Michael DiPirro, Chris Done, Tadayasu Dotani, John Doty, Ken Ebisawa, Megan Eckart, Teruaki Enoto, Yuichiro Ezoe, Andrew Fabian, Carlo Ferrigno, Adam Foster, Ryuichi Fujimoto, Yasushi Fukazawa, Stefan Funk, Akihiro Furuzawa, Massimiliano Galeazzi, Luigi Gallo, Poshak Gandhi, Keith Gendreau, Kirk Gilmore, Daniel Haas, Yoshito Haba, Kenji Hamaguchi, Isamu Hatsukade, Takayuki Hayashi, Kiyoshi Hayashida, Junko Hiraga, Kazuyuki Hirose, Ann Hornschemeier, Akio Hoshino, John Hughes, Una Hwang, Ryo Iizuka, Yoshiyuki Inoue, Kazunori Ishibashi, Manabu Ishida, Kosei Ishimura, Yoshitaka Ishisaki, Masayuki Ito, Naoko Iwat, Naoko Iyomoto, Jelle Kaastr, Timothy Kallman, Tuneyoshi Kamae, Jun Kataoka, Satoru Katsuda, Hajime Kawahara, Madoka Kawaharada, Nobuyuki Kawai, Shigeo Kawasaki, Dmitry Khangaluyan, Caroline Kilbourne, Masashi Kimura, Kenzo Kinugasaa, Shunji Kitamoto, Tetsu Kitayama, Takayoshi Kohmura, Motohide Kokubun, Tatsuro Kosaka, Alex Koujelev, Katsuji Koyama, Hans Krimm, Aya Kubota, Hideyo Kunieda, Stephanie LaMass, Philippe Laurent, Francois Lebrun, Maurice Leutenegger, Olivier Limousin, Michael Loewenstein, Knox Long, David Lumb, Grzegorz Madejski, Yoshitomo Maedaa, Kazuo Makishima, Genevieve Marchand, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammona, Brian McNamara, Jon Miller, Eric Miller, Shin Mineshige, Kenji Minesugi, Ikuyuki Mitsuishi, Takuya Miyazaw, Tsunefumi Mizuno, Hideyuki Mori, Koji Mori, Koji Mukai, Toshio Murakami, Hiroshi Murakami, Richard Mushotzky, Housei Nagano, Ryo Nagino, Takao Nakagaw, Hiroshi Nakajim, Takeshi Nakamori, Kazuhiro Nakazaw, Yoshiharu Namba, Chikara Natsukari, Yusuke Nishiok, Masayoshi Nobukawa, Masaharu Nomachi, Steve O'Dell, Hirokazu Odak, Hiroyuki Ogaw, Mina Ogaw, Keiji Ogi, Takaya Ohashi, Masanori Ohno, Masayuki Ohta, Takashi Okajima, Atsushi Okamotoa, Tsuyoshi Okazaki, Naomi Ota, Masanobu Ozaki, Frits Paerelsb, Stephane Paltanii, Arvind Parmar, Robert Petre, Martin Pohl, F.Scott Porter, Brian Ramsey, Rubens Reis, Christopher Reynolds, Helen Russell, Samar Sa-Harb, Shin-Ichiro Sakai, Hiroaki Sameshima, Jeremy Sanders, Goro Sato, Rie Sato, Yoichi Sato, Kosuke Sato, Makoto Sawada, Peter Serlemitsos, Hiromi Seta, Yasuko Shibano, Maki Shida, Takanobu Shimada, Keisuke Shinozaki, Peter Shirron, Aurora Simionescu, Cynthia Simmons, Randall Smith, Gary Sneiderman, Yang Soong, Lukasz Stawarz, Yasuharu Sugawara, Hiroyuki Sugita, Satoshi Sugit, Andrew Szymkowiak, Hiroyasu Tajim, Hiromitsu Takahashi, Shin-Ichiro Takeda, Yoh Takei, Toru Tamagawa, Takayuki Tamura, Keisuke Tamura, Takaaki Tanaka, Yasuo Tanaka, Makoto Tashiro, Yuzuru Tawara, Yukikatsu Terada, Yuichi Terashima, Francesco Tombesi, Hiroshi Tomida, Yoko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Hiroyuki Uchida, Yasunobu Uchiyam, Hideki Uchiyam, Yoshihiro Ueda, Shiro Ueno, Shinichiro Unobe, Meg Urry, Eugenio Ursino, Cor De Vries, Atsushi Wada, Shin Watanabe, Norbert Werner, Nicholas White, Takahiro Yamada, Shinya Yamada, Hiroya Yamaguchi, Noriko Yamasaki, Shigeo Yamauchi, Makoto Yamauchi, Yoichi Yatsuag, Daisuke Yonetok, Atsumasa Yoshida, Takayuki Yuasa
    Proceedings of SPIE - The International Society for Optical Engineering 8443 2012年  
    The joint JAXA/NASA ASTRO-H mission is the sixth in a series of highly successful X-ray missions initiated by the Institute of Space and Astronautical Science (ISAS). ASTRO-H will investigate the physics of the highenergy universe via a suite of four instruments, covering a very wide energy range, from 0.3 keV to 600 keV. These instruments include a high-resolution, high-Throughput spectrometer sensitive over 0.3-12 keV with high spectral resolution of ?E 5 7 eV, enabled by a micro-calorimeter array located in the focal plane of thin-foil X-ray optics hard X-ray imaging spectrometers covering 5-80 keV, located in the focal plane of multilayer-coated, focusing hard X-ray mirrors a wide-field imaging spectrometer sensitive over 0.4-12 keV, with an X-ray CCD camera in the focal plane of a soft X-ray telescope and a non-focusing Compton-camera type soft gamma-ray detector, sensitive in the 40-600 keV band. The simultaneous broad bandpass, coupled with high spectral resolution, will enable the pursuit of a wide variety of important science themes. © 2012 SPIE.
  • 前畑 京介, 前田 亮, 江崎 翔平, 高野 彬, 伊豫本 直子, 松村 晶, 原 徹, 満田 和久, 山崎 典子, 田中 啓一
    日本原子力学会 年会・大会予稿集 2012 77-77 2012年  
    我々は透過型電子顕微鏡に搭載するエネルギー分散型X線検出器として、超伝導転移端温度センサー(TES)型X線検出器の開発研究を展開している。本研究では、4ピクセル配置のTES型X線検出器を試作した。個々のピクセルは、TESの全面を厚さ0.5μmのAu吸収体層が覆い、TESとの間に厚さ0.1μmのTa2O5絶縁層が挿入されている。選択した2ピクセルについてX線検出特性を測定した。
  • K. Sakai, K. Mitsuda, N. Y. Yamasaki, Y. Takei, R. Yamamoto, T. Hara, K. Maehata, N. Iyomoto, K. Tanaka
    Journal of Low Temperature Physics 167(5-6) 759-764 2012年  査読有り
    We have been improving our TEM-EDS for elemental microanalysis after a successful achievement of a high energy resolution (7.8 eV at 1.7 keV) using a TES microcalorimeter. The improvements fall into a 3D superconductive wiring and a high-speed processing (∼3,000 cps). We are implementing a 10-ch TES array for higher count rate and a broader dynamic range. The shape of a probe needs to be a small polygonal rod with an approximate size of 1 cm × 1 cm× 10 cm, and hence the placing and wiring of the TES array and read-out circuits at the cryogenic stage were very demanding. We overcame those difficulties by 3D photolithography and electrodeposition. With these new technologies, we developed the OFC probe with solder-plated 3D wiring, and successfully observed a superconductivity at the temperature of liquid helium. As a required count rate per channel is ∼300 cps, the overall system count rate is ∼3,000 cps, which is incomparably higher than before. In the last model, we used an embedded system to process waveforms from a 4-ch 14-bit 1 MS/s ADC due to a small signal bandwidth, but this time we parallelized three identical ADCs and transfer raw waveforms by Ethernet lines to a host to achieve the required system count rate. © Springer Science+Business Media, LLC 2012.
  • MITSUISHI Ikuyuki, GUPTA Anjali, YAMASAKI Noriko Y., TAKEI Yoh, OHASHI Takaya, SATO Kosuke, GALEAZZI Massimiliano, HENRY J. Patrick, KELLEY Richard L.
    PASJ : publications of the Astronomical Society of Japan 64(1) "18-1"-"18-14" 2012年  査読有り
  • Kazuhisa Mitsuda, Richard L. Kelley, Kevin R. Boyce, Gregory V. Brown, Elisa Costantini, Michael J. Di Pirro, Yuichiro Ezoe, Ryuichi Fujimoto, Keith C. Gendreau, Jan-Willem Den Herder, Akio Hoshino, Yoshitaka Ishisaki, Caroline A. Kilbourne, Shunji Kitamoto, Dan McCammon, Masahide Murakami, Hiroshi Murakami, Mina Ogawa, Takaya Ohashi, Atsushi Okamoto, Stéphane Paltani, Martin Pohl, F. Scott Porter, Yoichi Sato, Keisuke Shinozaki, Peter J. Shirron, Gary A. Sneiderman, Hiroyuki Sugita, Andrew Szymkowiak, Yoh Takei, Toru Tamagawa, Makoto Tashiro, Yukikatsu Terada, Masahiro Tsujimoto, Cor De Vries, Noriko Y. Yamasaki
    Journal of Low Temperature Physics 167(5-6) 795-802 2012年  査読有り
    The science and an overview of the Soft X-ray Spectrometer onboard the STRO-H mission are presented. The SXS consists of X-ray focusing mirrors and a microcalorimeter array and is developed by international collaboration lead by JAXA and NASA with European participation. The detector is a 6 × 6 format microcalorimeter array operated at a cryogenic temperature of 50 mK and covers a 3' × 3' field of view of the X-ray telescope of 5.6 m focal length. We expect an energy resolution better than 7 eV (FWHM, requirement) with a goal of 4 eV. The effective area of the instrument will be 225 cm2 at 7 keV by a factor of about two larger than that of the X-ray microcalorimeter on board Suzaku. One of the main scientific objectives of the SXS is to investigate turbulent and/or macroscopic motions of hot gas in clusters of galaxies. © Springer Science+Business Media, LLC 2012.
  • Ikuyuki Mitsuishi, Noriko Y. Yamasaki, Yoh Takei
    Astrophysical Journal Letters 742(2) 2011年12月1日  査読有り
    A bright, nearby edge-on starburst galaxy, NGC253, was studied using the Suzaku, XMM, and Chandra X-ray observatories. With Suzaku and XMM we detected complex line structure of Fe K, which is resolved into three lines (FeI at 6.4keV, FeXXV at 6.7keV, and FeXXVI at 7.0keV) around the center of NGC253. Especially, the FeI and FeXXVI lines are the first clear detections, with a significance of &gt 99.99% and 99.89% estimated by a Monte Carlo procedure. Imaging spectroscopy with Chandra revealed that the emission is distributed in ∼60arcsec2 region around the nucleus, which suggests that the source is not only the buried active galactic nucleus. The flux of highly ionized Fe lines can be explained by the accumulation of 10-1000 supernova remnants that are the result of high star-forming activity, while the FeI line flux is consistent with the fluorescent line emission expected with the molecular clouds in the region. © 2011. The American Astronomical Society. All rights reserved..
  • Keisuke Maehata, Toru Hara, Keiichi Tanaka, Kazuhisa Mitsuda, Noriko Y. Yamasaki, Mitsuaki Ohsaki, Shigemasa Ohta, Takuji Itoh, Yoshihiro Yamanaka
    Proceedings of the 25th Workshop on Radiation Detectors and Their Uses 1-10 2011年  
  • Hagihara, Toshishige, Yamasaki, Noriko Y., Mitsuda, Kazuhisa, Takei, Yoh, Sakai, Kazuhiro, Yao, Yangsen, Wang, Q. Daniel, McCammon, Dan
    Publications of the Astronomical Society of Japan 63 S889-S901 2011年  査読有り
    We present a detailed spectroscopic study of the hot gas toward the galactic bulge along the 4U 1820-303 sight line by a combination analysis of emission and absorption spectra. In addition to the absorption lines of O VII K alpha, O VII K beta, O VIII K alpha, and Ne IV K alpha by Chandra LTGS, as shown by previous studies. Suzaku clearly detected the emission lines of O VII, O VIII, Ne IX, and Ne X from the vicinity. We used simplified plasma models with constant temperature and density. An evaluation of the background and foreground emission was carefully performed, including the stellar X-ray contribution based on the recent X-ray observational results and the stellar distribution simulator. If we assume that one plasma component exists in front of 4U 1820-303 and the other one at the back, the obtained temperatures are T = (1.7 +/- 0.2) x 10(6) K for the front-side plasma and T = (3.9(-0.3)(+0.4)) x 10(6) K for the back-side. This scheme is consistent with a hot and thick ISM disk, as suggested by extragalactic source observations and an X-ray bulge around the galactic center.
  • Kosuke Sato, Madoka Kawaharada, Kazuhiro Nakazawa, Kyoko Matsushita, Yoshitaka Ishisaki, Noriko Y. Yamasaki, Takaya Ohashi
    Publications of the Astronomical Society of Japan 62(6) 1445-1454 2010年12月25日  査読有り
    We studied the temperature and metal abundance distributions of the intra-cluster medium (ICM) in a group of galaxies, NGC 1550, observed with Suzaku. NGC 1550 is classified as a fossil group, which has few bright member galaxies, except for the central galaxy. Thus, such a type of galaxy is important to investigate how metals are enriched to the ICM. With the Suzaku XIS instrument, we directly measured not only the Si, S, and Fe lines, but also the O and Mg lines, and obtained those abundances to an outer region of ∼0.5r180 for the first time, and confirmed that the metals in the ICM of such a fossil group are indeed extending to a large radius. We found steeper gradients for the Mg, Si, S, and Fe abundances, while O showed an almost flat abundance distribution. Abundance ratios of α-elements to Fe were similar to those of the other groups and poor clusters. We calculated the number ratio of type II to type Ia supernovae for the ICM enrichment to be 2.9±0.5 within 0.1r180 the value is consistent with those for the other groups and poor clusters observed with Suzaku. We also calculated the metal mass-to-light ratios (MLRs) for Fe, O, and Mg with the B-band and K-band luminosities of the member galaxies of NGC 1550. The derived MLRs are comparable to those of the NGC 5044 group in the r &lt 0.1r180 region, while those of NGC 1550 are slightly higher than those of NGC 5044 in the outer region. © 2010. Astronomical Society of Japan.
  • Keisuke Shinozaki, Kazuhisa Mitsuda, Noriko Y. Yamasaki, Yoh Takei, Kensuke Masui, Kentaro Asano, Takaya Ohashi, Yuichiro Ezoe, Yoshitaka Ishisaki, Ryuichi Fujimoto, Kosuke Sato, Kenichi Kanao, Seiji Yoshida
    Cryogenics 50(9) 597-602 2010年9月  査読有り
    We report a development of a portable dewar with a double-stage ADR in it, and its cooling test results. The purpose of this system is to establish a cooling cycle of double-stage adiabatic demagnetization from 4.2 K to 50 mK, which is strongly desired for future space science missions. In our test dewar, two units of ADR are installed in parallel at the bottom of a liquid He tank. We used 600 g of GGG (Gadolinium Gallium Garnet) for the higher temperature stage (4 Tesla) and ∼90 g of CPA (Chromic Potassium Alum) for the lower temperature stage (3 Tesla). A passive gas-gap heat switch (PGGHS) is used between these two stages, while a mechanical heat switch between the He tank and the GGG stage. Using this system, 50 mK was achieved, and various kinds of cooling cycles with different operating temperatures and different sequences of magnetization were tested. We also evaluated the performance of the PGGHS, and interference of the magnetic field with each other during a stable temperature control. © 2010 Elsevier Ltd. All rights reserved.
  • Ryuichi Fujimoto, Kazuhisa Mitsuda, Noriko Yamasaki, Yoh Takei, Masahiro Tsujimoto, Hiroyuki Sugita, Yoichi Sato, Keisuke Shinozaki, Takaya Ohashi, Yoshitaka Ishisaki, Yuichiro Ezoe, Masahide Murakami, Shunji Kitamoto, Hiroshi Murakami, Toru Tamagawa, Madoka Kawaharada, Hiroya Yamaguchi, Kosuke Sato, Kenichi Kanao, Seiji Yoshida, Mike Dipirro, Peter Shirron, Gary Sneiderman, Richard L. Kelley, F. Scott Porter, Caroline A. Kilbourne, John Crow, Andrea Mattern, Ali Kashani, Dan McCammon, Jan-Willem Den Herder
    Cryogenics 50(9) 488-493 2010年9月  査読有り
    The Soft X-ray Spectrometer (SXS) is a cryogenic high resolution X-ray spectrometer onboard the X-ray astronomy satellite Astro-H which will be launched in 2014. The detector array is cooled down to 50 mK using an adiabatic demagnetization refrigerator (ADR). The cooling chain from the room temperature to the ADR heat-sink is composed of superfluid liquid He, a Joule-Thomson cryocooler, and double-stage Stirling cryocoolers. It is designed to keep 30 l of liquid He for more than 5 years in the normal case, and longer than 3 years even if one of the cryocoolers fails. Cryogen-free operation is also possible in the normal case. It is fully redundant from the room temperature to the ADR heat-sink. © 2010 Elsevier Ltd. All rights reserved.
  • Yuichiro Ezoe, Ken Ebisawa, Noriko Y. Yamasaki, Kazuhisa Mitsuda, Hiroshi Yoshitake, Naoki Terada, Yoshizumi Miyoshi, Ryuichi Fujimoto
    Publications of the Astronomical Society of Japan 62(4) 981-986 2010年8月25日  査読有り
    We report on the detection of a time variable O VII line emission in a deep 100ks Suzaku X-ray Imaging Spectrometer spectrum of the galactic ridge X-ray emission. The observed line intensity is too strong (11 ±2 line unit or photon cm-2 s-1 sr-1) to be emitted inside the heavily obscured galactic disk. It showed a factor of two time variation that showed a significant (∼4σ) correlation with the solar-wind O 7+ ion flux. The high line intensity and good time correlation with the solar wind strongly suggests that it originated from geocoronal solar-wind charge-exchange emission. We discuss the X-ray line intensity while considering a line-of-sight direction and also theoretical distribution models of the neutral hydrogen and solar wind around Earth. Our results indicate that X-ray observations of geocoronal solar-wind charge-exchange emission can be used to constrain these models. © 2010. Astronomical Society of Japan.
  • Yuichiro Ezoe, Ikuyuki Mitsuishi, Utako Takagi, Masaki Koshiishi, Kazuhisa Mitsuda, Noriko Y. Yamasaki, Takaya Ohashi, Fumiki Kato, Susumu Sugiyama, Raul E. Riveros, Hitomi Yamaguchi, Shinya Fujihira, Yoshiaki Kanamori, Kohei Morishita, Kazuo Nakajima, Ryutaro Maeda
    Microsystem Technologies 16(8-9) 1633-1641 2010年8月  査読有り
    We are developing novel ultra light-weight and high-resolution X-ray micro pore optics for space X-ray telescopes. In our method, curvilinear micro pore structures are firstly fabricated by silicon deep reactive ion etching (DRIE) or X-ray LIGA processes. Secondly, side walls of the micro structures are smoothed by magnetic field assisted finishing and/or hydrogen annealing techniques for high reflectivity mirrors. Thirdly, to focus parallel X-ray lights from astronomical objects, these structures are elastically or plastically bent into a spherical shape. Fourthly, the bent structures are stacked to form a multistage X-ray telescope. In this paper, we report on fabrication and X-ray reflection tests of silicon and nickel X-ray mirrors using the DRIE and LIGA processes, respectively. For the first time, X-ray reflections were confirmed on both of the mirrors. Estimated rms roughnesses were 5 nm and 3 nm for the silicon and nickel mirrors, respectively. © 2009 Springer-Verlag.
  • Raul E. Riveros, Hitomi Yamaguchi, Ikuyuki Mitsuishi, Utako Takagi, Yuichiro Ezoe, Fumiki Kato, Susumu Sugiyama, Noriko Yamasaki, Kazuhisa Mitsuda
    Applied Optics 49(18) 3511-3521 2010年6月20日  査読有り
    X-ray astronomy research is often limited by the size, weight, complexity, and cost of functioning x-ray optics. Micropore optics promises an economical alternative to traditional (e.g., glass or foil) x-ray optics however, many manufacturing difficulties prevent micropore optics from being a viable solution. Ezoe et al. introduced microelectromechanical systems(MEMS)micropore optics having curvilinear micropores in 2008. Madeby either deep reactive ion etching or x-ray lithography, electroforming, and molding (LIGA), MEMSmicropore optics suffer from high micropore sidewall roughness (10-30 nm rms) which, by current standards, cannot be improved. In this research, a new alternating magnetic-field-assisted finishing process was developed using a mixture of ferrofluid and microscale abrasive slurry. A machine was built, and a set of working process parameters including alternating frequency, abrasive size, and polishing time was selected. A polishing experiment on a LIGA-fabricated MEMS micropore optic was performed, and a change in micropore sidewall roughness of 9:3 ± 2:5 nm rms to 5:7 ± 0:7 nm rms was measured. An improvement in x-ray reflectancewas also seen. This research shows the feasibility and confirms the effects of this new polishing process on MEMS micropore optics. © 2010 Optical Society of America.
  • Ikuyuki Mitsuishi, Yuichiro Ezoe, Masaki Koshiishi, Makoto Mita, Yoshitomo Maeda, Noriko Y. Yamasaki, Kazuhisa Mitsuda, Takayuki Shirata, Takayuki Hayashi, Takayuki Takano, Ryutaro Maeda
    Applied Optics 49(6) 1007-1011 2010年2月20日  査読有り
    The x-ray reflectivity of an ultralightweight and low-cost x-ray optic using anisotropic wet etching of Si (110) wafers is evaluated at two energies, C Kα 0:28 keV and Al Kα 1:49 keV. The obtained reflectivities at both energies are not represented by a simple planar mirror model considering surface roughness. Hence, an geometrical occultation effect due to step structures upon the etched mirror surface is taken into account. Then, the reflectivities are represented by the theoretical model. The estimated surface roughness at C Kα (∼6nmrms) is significantly larger than ∼1nm at Al Kα. This can be explained by different coherent lengths at two energies. © 2010 Optical Society of America.
  • Toru Hara, Keiichi Tanaka, Keisuke Maehata, Kazuhisa Mitsuda, Noriko Y. Yamasaki, Mitsuaki Ohsaki, Katsuaki Watanabe, Xiuzhen Yu, Takuji Ito, Yoshihiro Yamanaka
    Journal of Electron Microscopy 59(1) 17-26 2010年2月  査読有り
    A new energy dispersive X-ray spectrometer (EDS) with a mi- crocalorimeter detector equipped with a transmission electron microscope (TEM) has been developed for high- accuracy compositional analysis in the nanoscale. A superconducting transition-edge-sensor-type microcalorimeter is applied as the detector. A cryogen-free cooling system, which consists of a mechanical and a dilution refrigerator, is selected to achieve long-term temperature stability. In order to mount these detector and refrigerators on a TEM, the cooling system is specially designed such that these two refrigerators are separated. Also, the detector position and arrangement are carefully designed to avoid adverse affects between the superconductor detector and the TEM lens system. Using the developed EDS system, at present, an energy resolution of 21.92 eV full-width-at-half maximum has been achieved at the Cr Kα line. This value is about seven times better than that of the current typical commercial Si(Li) detector, which is usually around 140 eV. The developed microcalorimeter EDS system can measure a wide energy range, 1-20 keV, at one time with this high energy resolution that can resolve peaks from most of the elements. Although several further developments will be needed to enable practical use, highly accurate compositional analysis with high energy resolution will be realized by this microcalorimeter EDS system.
  • K. Mitsuda, T. Yoshino, N. Y. Yamasaki, Y. Takei, T. Hagihara, K. Masui, M. Bauer, D. McCammon, R. Fujimoto, Q. D. Wang, Y. Yao
    Memorie della Societa Astronomica Italiana, Supplementi - Journal of the Italian Astronomical Society, Supplement 81(1) 69-76 2010年  
    The origins of the soft diffuse X-ray background are discussed basing on recent Suzaku observations. The O vn and O vm intensities of fourteen different fields were determined with Suzaku with relatively small statistical and systematic errors. The Ovu and Ovm intensities show strong correlations: Ovu emission shows an intensity floor at ∼ 2 photons s-1 cm-2 str-1 (LU), while the high-latitude O vm emission shows a tight correlation with excess of O vn emission above the floor, with (O vm intensity) = 0.5 × [(O vn intensity) - 2 LU], suggesting that temperatures averaged over different line-of-sight show a narrow distribution around ∼ 0.2 keV. We consider that the offset intensity of Ovu arises from the Heliospheric solar wind charge exchange, and that the excess O vn (2-7 LU) is emission from more distant parts of the Galaxy, which may be regarded as the halo of our Galaxy. The total bolometric luminosity of this galactic emission is estimated to be 4 × 10-39 erg s-1, and its characteristic temperature may be related to the virial temperature of the Galaxy.
  • Toshishige Hagihara, Yangsen Yao, Noriko Y. Yamasaki, Kazuhisa Mitsuda, Q. Daniel Wang, Yoh Takei, Tomotaka Yoshino, Dan McCAMMON
    Publications of the Astronomical Society of Japan 62(3) 723-733 2010年  査読有り
    We present a detailed spectroscopic study of the hot gas in the Galactic halo toward the direction of a blazer PKS 2155-304 (z = 0.117). The O vil and O vIII absorption lines were measured with the Low and High Energy Transmission Grating Spectrographs aboard Chandra, and the O VII, O vIII, and Ne IX emission lines produced in an adjacent field of the PKS 2155-304 direction were observed with the X-ray Imaging Spectrometer aboard Suzaku. Assuming vertically exponential distributions of the gas temperature and the density, we performed a combined analysis of the absorption and emission data. The gas temperature and the density at the galactic plane were determined to be (2.5+0.3 +0.6) × 106K and (1.4-0.4+0.5) × 10-3cm-3, and the scale heights of the gas temperature and density were 5.6-4.2+7.4 kpc and 2.3 -0.8+0.9kpc, respectively. These values are consistent with those obtained in the LMC X-3 direction. © 2010. Astronomical Society of Japan.
  • Ikuyuki Mitsuishi, Yuichiro Ezoe, Utako Takagi, Kensuke Ishizu, Teppei Moriyama, Takayuki Hayashi, Takuro Sato, Kohei Morishita, Kazuo Nakajima, Noriko Y. Yamasaki, Kazuhisa Mitsuda
    IEEE Journal of Quantum Electronics 46(9) 1309-1312 2010年  査読有り
    We have been developing novel microelectromechanical systems X-ray optics for future satellites. It can be ultra-lightweight and of high-resolution. For the first time, we fabricated a spherical test optics made of silicon. We used the dry etching and hot plastic deformation method. We conducted imaging tests to examine whether it can focus a parallel beam of light. Visible light was selected instead of X-rays because of the convenience of testing. The focusing was confirmed with a fullwidth at half-maximum focal size of 2 arcmin. Since the focus is affected by optical diffraction, a smaller focus can be expected in future X-ray imaging tests. © 2010 IEEE.
  • Sato Kousuke, Kelley Richard L., Takei Yoh, TAMURA Takayuki, YAMASAKI Noriko Y., OHASHI Takaya, GUPTA Anjali, GALEAZZI Massimiliano
    PASJ : publications of the Astronomical Society of Japan 62(6) 1423-1433 2010年  査読有り
  • 原 徹, 田中 啓一, 前畑 京介, 満田 和久, 山崎 典子, 大崎 光明, 大田 繁正
    まてりあ : 日本金属学会会報 48(12) 630-630 2009年12月1日  
  • H. Yoshitake, Y. Ezoe, T. Yoshino, K. Mukai, K. Ishikawa, K. Mitsuda, N. Y. Yamasaki, Y. Ishisaki, H. Akamatsu, R. Maeda, T. Takano
    IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY 19(3) 456-459 2009年6月  査読有り
    We fabricated 16 16 format arrays of 180 square Ti/Au superconducting transition edge X-ray microcalorimeters of which transition temperatures range from 130 to 220 mK. All pixels are wired with Al, and stand on SiO(2) and SiN(x) membranes that work as a weak thermal link. The membrane structure is formed by deep reactive ion etching. Energy resolution of a pixel in the array without a Au absorber was 11 eV (FWHM) at 5.9 keV, while the baseline resolution is about 3.7 eV.
  • L. Piro, J. W. den Herder, T. Ohashi, L. Amati, J. L. Atteia, S. Barthelmy, M. Barbera, D. Barret, S. Basso, M. Boer, S. Borgani, O. Boyarskiy, E. Branchini, G. Branduardi-Raymont, M. Briggs, G. Brunetti, C. Budtz-Jorgensen, D. Burrows, S. Campana, E. Caroli, G. Chincarini, F. Christensen, M. Cocchi, A. Comastri, A. Corsi, V. Cotroneo, P. Conconi, L. Colasanti, G. Cusumano, A. de Rosa, M. Del Santo, S. Ettori, Y. Ezoe, L. Ferrari, M. Feroci, M. Finger, G. Fishman, R. Fujimoto, M. Galeazzi, A. Galli, F. Gatti, N. Gehrels, B. Gendre, G. Ghirlanda, G. Ghisellini, P. Giommi, M. Girardi, L. Guzzo, F. Haardt, I. Hepburn, W. Hermsen, H. Hoevers, A. Holland, J. in't Zand, Y. Ishisaki, H. Kawahara, N. Kawai, J. Kaastra, M. Kippen, P. A. J. de Korte, C. Kouveliotou, A. Kusenko, C. Labanti, R. Lieu, C. Macculi, K. Makishima, G. Matt, P. Mazzotta, D. McCammon, M. Mendez, T. Mineo, S. Mitchell, K. Mitsuda, S. Molendi, L. Moscardini, R. Mushotzky, L. Natalucci, F. Nicastro, P. O'Brien, J. Osborne, F. Paerels, M. Page, S. Paltani, G. Pareschi, E. Perinati, C. Perola, T. Ponman, A. Rasmussen, M. Roncarelli, P. Rosati, O. Ruchayskiy, E. Quadrini, I. Sakurai, R. Salvaterra, S. Sasaki, G. Sato, J. Schaye, J. Schmitt, S. Sciortino, M. Shaposhnikov, K. Shinozaki, D. Spiga, Y. Suto, G. Tagliaferri, T. Takahashi, Y. Takei, Y. Tawara, P. Tozzi, H. Tsunemi, T. Tsuru, P. Ubertini, E. Ursino, M. Viel, J. Vink, N. White, R. Willingale, R. Wijers, K. Yoshikawa, N. Yamasaki
    EXPERIMENTAL ASTRONOMY 23(1) 67-89 2009年3月  
    How structures of various scales formed and evolved from the early Universe up to present time is a fundamental question of astrophysical cosmology. EDGE (Piro et al., 2007) will 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. This enables the study of their star-forming and host galaxy environments 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 (0.1-2.2 eV) with excellent energy resolution (3 eV at 0.6 keV), a Wide-Field Imager (0.3-6 keV) with high angular resolution (HPD = 15") constant over the full 1.4 degree field of view, and a Wide Field Monitor (8-200 keV) with a FOV of A1/4 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 outline the science drivers and describe in more detail the payload of this mission.
  • 常深 博, 林田 清, 山崎 典子, 中澤 知洋, 大橋 隆哉, 深澤 泰司, 鶴 剛
    日本物理学会講演概要集 64 254-254 2009年  
  • R. L. Kelley, S. R. Bandler, W. B. Doriese, Y. Ezoe, R. Fujimoto, L. Gottardi, R. den Hartog, J-W den Herder, H. Hoevers, K. Irwin, Y. Ishisaki, C. A. Kilbourne, P. de Korte, J. van der Kuur, K. Mitsuda, T. Ohashi, L. Piro, F. S. Porter, K. Sato, K. Shinozaki, P. Shirron, S. J. Smith, Y. Takei, P. Whitehouse, N. Y. Yamasaki
    LOW TEMPERATURE DETECTORS LTD 13 1185 757-+ 2009年  査読有り
    The International X-Ray Observatory (IXO) is under formulation by NASA, ESA and JAXA for deployment in 2022. IXO emerged over the last 18 months as the NASA Constellation-X and ESA/JAXA X-Ray Evolving Universe Spectrometer (XEUS) missions were combined. The driving performance requirements for the X-Ray Microcalorimeter Spectrometer (XMS) are a spectral resolution of 2.5 eV over the central 2'x2' in the 0.3-7.0 keV band, and 10 eV to the edge of the 5'x5' field of view (FOV). The XMS is now based on a microcalorimeter array of Transition-Edge Sensor (TES) thermometers with Au/Bi absorbers and a SQUID MUX readout. One of the concepts studied as part of the mission formulation has a core 40x40 array corresponding to a 2'x2' FOV with 3 '' pixels surrounded by an outer, annular 52 x 52 array of 6 '' pixels that extends the field of view to 5.4'x5.4' with better than 10 eV resolution. There are several options for implementing the readout and cooling system of the XMS under study in the US, Europe and Japan. The ADR system will have from two to five stages depending on the performance of the cryocooler. Mechanical coolers with sufficient cooling power at 4K are available now, and similar to 2K coolers are under development. In this paper we give an overview of the XMS instrument, and some of the tradeoffs to be addressed for this observatory instrument.
  • Y. Yao, Q. D. Wang, T. Hagihara, K. Mitsuda, D. McCammon, N. Y. Yamasaki
    Astrophysical Journal 690(1) 143-153 2009年  査読有り
    We present Suzaku spectra of X-ray emission in the fields just off the LMC X-3 sight line. O VII, O VIII, and Ne IX emission lines are clearly detected, suggesting the presence of an optically thin thermal plasma with an average temperature of 2.4 × 106 K. This temperature is significantly higher than that inferred from existing X-ray absorption line data obtained with Chandra grating observations of LMC X-3, strongly suggesting that the gas is not isothermal. We then jointly analyze these data to characterize the spatial and temperature distributions of the gas. Assuming a vertical exponential Galactic disk model, we estimate the gas temperature and density at the Galactic plane and their scale heights as 3.6(2.9, 4.7) × 106 K and 1.4(0.3, 3.4) × 10-3 cm-3 and 1.4(0.2, 5.2) kpc and 2.8(1.0, 6.4) kpc, respectively. This characterization can account for all the O VI line absorption, as observed in a Far Ultraviolet Spectroscopy Explorer spectrum of LMC X-3, but only predicts less than one-tenth of the O VI line emission intensity typically detected at high Galactic latitudes. The bulk of the O VI emission most likely arises at interfaces between cool and hot gases. © 2009. The American Astronomical Society. All rights reserved.
  • MASUI, K, MITSUDA, K, YAMASAKI, NY, et al.
    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 61 2009年  査読有り
  • Y. Takei, N. Y. Yamasaki, W. Hirakoso, S. Kimura, K. Mitsuda
    Superconductor Science and Technology 22(11) 2009年  査読有り
    A microcalorimeter array based on a transition-edge sensor (TES) thermometer is a promising imaging spectrometer for use in future x-ray astronomy missions. A TES microcalorimeter achieves eV energy resolution and an array of &gt 100 pixels also provides a moderate imaging capability. For a large format array, signal multiplexing at the low temperature stage is mandatory in order to reduce heat loads from cold stage preamplifiers and through wirings. We are developing frequency division multiplexing (FDM). In FDM, each TES is ac-biased with a different carrier frequency. Signals from several pixels are summed and then read out by one dc SQUID (superconducting quantum interference device). The maximum number of multiplexed pixels is limited by the bandwidth of a SQUID in a flux-locked loop. Assuming 1m cable length between the room temperature and the cold stage, the bandwidth is only &lt 1MHz with a standard flux-locked loop, due to the delay and phase shift of wirings. We report our development of baseband feedback, a new feedback scheme that overcomes the bandwidth limitation. In baseband feedback, the signal (kHz) from the TES is sent back to the SQUID after the phase of carrier frequency (∼1MHz) has been adjusted. We demonstrated open-loop gain of 8 for 10kHz signal at 5MHz carrier frequency, which indicates the possibility of ∼40-pixel multiplexing of the TES signal. © 2009 IOP Publishing Ltd.

MISC

 189
  • 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

 22
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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