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  2. 藤本 龍一

藤本 龍一

フジモト リュウイチ  (Ryuichi Fujimoto)

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
総合研究大学院大学 先端学術院 宇宙科学コース 教授
東京工業大学 理学院 特定教授
学位
博士（理学）(東京大学)
修士(東京大学)
研究者番号
20280555
ORCID ID
 https://orcid.org/0000-0002-2374-7073
J-GLOBAL ID
200901095989600566
researchmap会員ID
1000363020

X線マイクロカロリメータを用いた極低温精密X線分光装置の開発に取り組み，2023年9月打ち上げのXRISM衛星に搭載されたResolve観測装置として実現しました．

研究指導のテーマとしては，(1) XRISM衛星による精密X線分光観測データを解析し，銀河団ガスの運動を調べて，宇宙の大規模構造形成過程の理解を深める，(2) 宇宙マイクロ波背景放射の偏光観測を目指すLiteBIRD衛星を見据えた実験的研究を行なう等．特定の自然現象について理解を深めると同時に，複雑な自然現象の背景にある物理法則に至る過程を，実験・解析手法とともにしっかりと身につけてもらいたいと考えています．

研究キーワード

 6

研究分野

 2

経歴

 8
もっとみる

学歴

 4

委員歴

 2

受賞

 2

論文

 155
  • Hishi, U., Fujimoto, R., Kunihisa, T., Takakura, S., Mitsude, T., Kamiya, K., Kotake, M., Hoshino, A., Shinozaki, K.
    Journal of Low Temperature Physics 176(5-6) 2014年  
  • Mitsuishi, I., Ezoe, Y., Ishikawa, K., Ohashi, T., Fujimoto, R., Mitsuda, K., Tsunematsu, S., Yoshida, S., Kanao, K., Murakami, M., Dipirro, M., Shirron, P.
    Cryogenics 64 2014年  
  • Sato, Y., Sawada, K., Shinozaki, K., Sugita, H., Nishibori, T., Sato, R., Mitsuda, K., Yamasaki, N.Y., Takei, Y., Goto, K., Nakagawa, T., Fujimoto, R., Kikuchi, K., Murakami, M., Tsunematsu, S., Ootsuka, K., Kanao, K., Narasaki, K.
    Cryogenics 64 2014年  
  • Mitsuda, K., Kelley, R.L., Boyce, K.R., Brown, G.V., Costantini, E., Di Pirro, M.J., Ezoe, Y., Fujimoto, R., Gendreau, K.C., Den Herder, J.-W., Hoshino, A., Ishisaki, Y., Kilbourne, C.A., Kitamoto, S., McCammon, D., Murakami, M., Murakami, H., Ogawa, M., Ohashi, T., Okamoto, A., Paltani, S., Pohl, M., Porter, F.S., Sato, Y., Shinozaki, K., Shirron, P.J., Sneiderman, G.A., Sugita, H., Szymkowiak, A., Takei, Y., Tamagawa, T., Tashiro, M., Terada, Y., Tsujimoto, M., De Vries, C., Yamasaki, N.Y.
    Journal of Low Temperature Physics 167(5-6) 2012年  
  • Hoshino, A., Yatsu, T., Kunihisa, T., Koi, N., Notsuke, M., Fujimoto, R., Yamamoto, R., Shinozaki, K.
    Journal of Low Temperature Physics 167(3-4) 2012年  
  • Ezoe, Y., Fujimoto, R., Yamasaki, N.Y., Mitsuda, K., Ohashi, T., Ishikawa, K., Oishi, S., Miyoshi, Y., Terada, N., Futaana, Y., Porter, F.S., Brown, G.V.
    Astronomische Nachrichten 333(4) 2012年  
  • Seta, H., Tashiro, M.S., Ishisaki, Y., Tsujimoto, M., Shimoda, Y., Abe, Y., Yasuda, T., Takeda, S., Asahina, M., Hiyama, Y., Yamaguchi, S., Terada, Y., Boyce, K.R., Porter, F.S., Kilbourne, C.A., Kelley, R.L., Fujimoto, R., Takei, Y., Mitsuda, K., Matsuda, K., Masukawa, K.
    IEEE Transactions on Nuclear Science 59(2) 2012年  
  • Ezoe, Y., Ishikawa, K., Ohashi, T., Yamaguchi, H., Mitsuda, K., Fujimoto, R., Murakami, M., Kanao, K., Yoshida, S., Tsunematsu, S., Dipirro, M., Shirron, P.
    Cryogenics 52(4-6) 2012年  
  • Sato, Y., Shinozaki, K., Sugita, H., Mitsuda, K., Yamasaki, N.Y., Takei, Y., Nakagawa, T., Fujimoto, R., Murakami, M., Tsunematsu, S., Otsuka, K., Yoshida, S., Kanao, K., Narasaki, K.
    Cryogenics 52(4-6) 2012年  
  • den Herder, J.-W., Piro, L., Ohashi, T., Kouveliotou, C., Hartmann, D.H., Kaastra, J.S., Amati, L., Andersen, M.I., Arnaud, M., Att{\'e}ia, J.-L., B, ler, S., Barbera, M., Barcons, X., Barthelmy, S., Basa, S., Basso, S., Boer, M., Branchini, E., Br, uardi-Raymont, G., Borgani, S., Boyarsky, A., Brunetti, G., Budtz-Jorgensen, C., Burrows, D., Butler, N., Campana, S., Caroli, E., Ceballos, M., Christensen, F., Churazov, E., Comastri, A., Colasanti, L., Cole, R., Content, R., Corsi, A., Costantini, E., Conconi, P., Cusumano, G., de Plaa, J., De Rosa, A., Del Santo, M., Di Cosimo, S., De Pasquale, M., Doriese, R., Ettori, S., Evans, P., Ezoe, Y., Ferrari, L., Finger, H., Figueroa-Feliciano, T., Friedrich, P., Fujimoto, R., Furuzawa, A., Fynbo, J., Gatti, F., Galeazzi, M., Gehrels, N., Gendre, B., Ghirl, a, G., Ghisellini, G., Gilfanov, M., Giommi, P., Girardi, M., Grindlay, J., Cocchi, M., Godet, O., Guedel, M., Haardt, F., den Hartog, R., Hepburn, I., Hermsen, W., Hjorth, J., Hoekstra, H., Holl, , A., Hornstrup, A., van der Horst, A., Hoshino, A., in{'}t Z, , J., Irwin, K., Ishisaki, Y., Jonker, P., Kitayama, T., Kawahara, H., Kawai, N., Kelley, R., Kilbourne, C., de Korte, P., Kusenko, A., Kuvvetli, I., Labanti, M., Macculi, C., Maiolino, R., Hesse, M.M., Matsushita, K., Mazzotta, P., McCammon, D., M{\'e}ndez, M., Mignani, R., Mineo, T., Mitsuda, K., Mushotzky, R., Molendi, S., Moscardini, L., Natalucci, L., Nicastro, F., O{'}Brien, P., Osborne, J., Paerels, F., Page, M., Paltani, S., Pedersen, K., Perinati, E., Ponman, T., Pointecouteau, E., Predehl, P., Porter, S., Rasmussen, A., Rauw, G., R{\"o}ttgering, H., Roncarelli, M., Rosati, P., Quadrini, E., Ruchayskiy, O., Salvaterra, R., Sasaki, S., Sato, K., Savaglio, S., Schaye, J., Sciortino, S., Shaposhnikov, M., Sharples, R., Shinozaki, K., Spiga, D., Sunyaev, R., Suto, Y., Takei, Y., Tanvir, N., Tashiro, M., Tamura, T., Tawara, Y., Troja, E., Tsujimoto, M., Tsuru, T., Ubertini, P., Ullom, J., Ursino, E., Verbunt, F., van de Voort, F., Viel, M., Wachter, S., Watson, D., Weisskopf, M., Werner, N., White, N., Willingale, R., Wijers, R., Yamasaki, N., Yoshikawa, K., Zane, S.
    Experimental Astronomy 34(2) 2012年  
  • Ezoe, Y., Ishikawa, K., Ohashi, T., Yamasaki, N.Y., Mitsuda, K., Fujimoto, R., Miyoshi, Y., Terada, N., Uchiyama, Y., Futaana, Y.
    Advances in Space Research 47(3) 2011年  
  • J. W. Den Herder, R. L. Kelley, K. Mitsuda, L. Piro, S. R. Bandler, P. Bastia, K. R. Boyce, M. Bruin, J. A. Chervenak, L. Colasanti, W. B. Doriese, M. DiPirro, M. E. Eckart, Y. Ezoe, E. Figueroa-Feliciano, L. Ferrari, R. Fujimoto, F. Gatti, K. C. Gendreau, L. Gottardi, R. Den Hartog, G. C. Hilton, H. Hoevers, K. D. Irwin, Y. Ishisaki, A. Kashani, C. A. Kilbourne, P. De Korte, J. Van, Der Kuur, C. MacCuli, T. Mineo, J. H. Nieland, T. Ohashi, S. Paltani, E. Perinati, F. S. Porter, P. J. Shirron, S. J. Smith, Y. Takei, M. Tashiro, G. Torrioli, M. Tsujimoto, H. Van Weers, N. Y. Yamasaki
    Proceedings of SPIE - The International Society for Optical Engineering 7732 2010年10月19日  
    One of the instruments on the International X-ray Observatory (IXO), under study with NASA, ESA and JAXA, is the X-ray Microcalorimeter Spectrometer (XMS). This instrument, which will provide high spectral resolution images, is based on X-ray micro-calorimeters with Transition Edge Sensor (TES) with absorbers that consist of metal and semimetal layers and a multiplexed SQUID readout. The requirements for this instrument are demanding. In the central array (40 x 40 pixels) an energy resolution of < 2.5 eV is required, whereas the energy resolution of the outer array is more relaxed (∼ 10 eV) but the detection elements have to be a factor 16 larger in order to keep the number of read-out channels acceptable for a cryogenic instrument. Due to the large collection area of the IXO optics, the XMS instrument must be capable of processing high counting rates, while maintaining the spectral resolution and a low deadtime. In addition, an anti-coincidence detector is required to suppress the particle-induced background. In this paper we will summarize the instrument status and performance. We will describe the results of design studies for the focal plane assembly and the cooling systems. Also the system and its required spacecraft resources will be given. © 2010 SPIE.
  • Ryuichi Fujimoto, Kazuhisa Mitsuda, Noriko Yamasaki, Yoh Takei, Masahiro Tsujimoto, Hiroyuki Sugita, Yoichi Sato, Keisuke Shinozaki, Atsushi Okamoto, Takaya Ohashi, Yoshitaka Ishisaki, Yuichiro Ezoe, Kumi Ishikawa, Masahide Murakami, Shunji Kitamoto, Hiroshi Murakami, Toru Tamagawa, Madoka Kawaharada, Hiroya Yamaguchi, Kosuke Sato, Akio Hoshino, Kenichi Kanao, Seiji Yoshida, Mikio Miyaoka, Michael DiPirro, Peter Shirron, Gary Sneiderman, Richard L. Kelley, F. Scott Porter, Caroline A. Kilbourne, John Crow, Andrea Mattern, Ali Kashani, Dan McCammon
    SPACE TELESCOPES AND INSTRUMENTATION 2010: ULTRAVIOLET TO GAMMA RAY 7732(9) 488-493 2010年  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. The detector array is cooled down to 50 mK using a 3-stage adiabatic demagnetization refrigerator (ADR). The cooling chain from room temperature to the ADR heat-sink is composed of superfluid liquid He, a He-4 Joule-Thomson cryocooler, and 2-stage Stirling cryocoolers. It is designed to keep 30 L of liquid He for more than 3 years in the nominal case. It is also designed with redundant subsystems throughout from room temperature to the ADR heat-sink, to alleviate failure of a single cryocooler or loss of liquid He.
  • F. S. Porter, J. S. Adams, G. V. Brown, J. A. Chervenak, M. P. Chiao, R. Fujimoto, Y. Ishisaki, R. L. Kelley, C. A. Kilbourne, D. McCammon, K. Mitsuda, T. Ohashi, A. E. Szymkowiak, Y. Takei, M. Tashiro, N. Yamasaki
    Proceedings of SPIE - The International Society for Optical Engineering 7732 2010年  査読有り
    The Soft X-ray Spectrometer (SXS) instrument on the Astro-H observatory is based on a 36 pixel x-ray calorimeter array cooled to 50 mK in a sophisticated spaceflight cryostat. The SXS is a true spatial-spectral instrument, where each spatially discrete pixel functions as a high-resolution spectrometer. Here we discuss the SXS detector subsystem that includes the detector array, the anticoincidence detector, the first stage amplifiers, the thermal and mechanical staging of the detector, and the cryogenic bias electronics. The design of the SXS detector subsystem has significant heritage from the Suzaku/XRS instrument but has some important modifications that increase performance margins and simplify the focal plane assembly. Notable improvements include x-ray absorbers with significantly lower heat capacity, improved load resistors, improved thermometry, and a decreased sensitivity to thermal radiation. These modifications have yielded an energy resolution of 3.5-4.0 eV FWHM at 6 keV for representative devices in the laboratory, giving considerable margin against the 7 eV instrument requirement. We expect similar performance in flight. © 2010 SPIE.
  • Fujimoto Ryuichi, Sato Kosuke, Wada Akane, Yatsu Takahiro, Hoshino Akio, Murakami Toshio, Shinozaki Keisuke
    AIP Conference Proceedings 1279 309-311 2010年1月1日  
    金沢大学理工研究域数物科学系An X-ray microcalorimeter is a non-dispersive spectrometer that measures the energy of an incident X-ray photon as a temperature rise. Operated at < 0.1 K, it achieves very high resolving power. We are developing X-ray microcalorimeters for future γ-ray burst observations, and are now setting up a compact adiabatic demagnetization refrigerator (ADR) for X-ray microcalorimeter operations. We fabricated a paramagnetic salt pill, and integrated it with a superconducting magnet and a heat-switch in a dedicated He cryostat. By applying a magnetic field of 2.6 T at the bath temperature of 1.8 K, it achieved 0.1 K. The attainable temperature and the hold time were, however, limited due to unexpected heat load. We also successfully measured a resistance-temperature characteristics of a superconducting transition edge. © 2010 American Institute of Physics.
  • Kazuhisa Mitsuda, Richard L. Kelley, Kevin R. Boyce, Gregory V. Brown, Elisa Costantini, Michael J. DiPirro, 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, Hiroya Yamaguchi, Noriko Y. Yamasaki
    Proceedings of SPIE - The International Society for Optical Engineering 7732 2010年  査読有り
    We present the science and an overview of the Soft X-ray Spectrometer onboard the ASTRO-H mission with emphasis on the detector system. 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′ filed 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. © 2010 SPIE.
  • Ezoe, Y., Ebisawa, K., Yamasaki, N.Y., Mitsuda, K., Yoshitake, H., Terada, N., Miyoshi, Y., Fujimoto, R.
    Publications of the Astronomical Society of Japan 62(4) 981-986 2010年  
    We report on the detection of a time variable O VII line emission in a deep 100 ks 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 (similar to 4 sigma) correlation with the solar-wind O7+ 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.
  • Shinozaki, K., Mitsuda, K., Yamasaki, N.Y., Takei, Y., Masui, K., Asano, K., Ohashi, T., Ezoe, Y., Ishisaki, Y., Fujimoto, R., Sato, K., Kanao, K., Yoshida, S.
    Cryogenics 50(9) 2010年  
  • Fujimoto Ryuichi, Mitsuda Kazuhisa, Yamasaki Noriko, Takei Yoh, Tsujimoto Masahiro, Sugita Hiroyuki, Sato Yoichi, Shinozaki Keisuke, Ohashi Takaya, Ishisaki Yoshitaka, Ezoe Yuichiro, Murakami Masahide, Kitamoto Shunji, Murakami Hiroshi, Tamagawa Toru, Kawaharada Madoka, Yamaguchi Hiroya, Sato Kosuke, Kanao Kenichi, Yoshida Seiji, DiPirro Mike, Shirron Peter, Sneiderman Gary, Kelley Richard L., Porter F. Scott, Kilbourne Caroline A., Crow John, Mattern Andrea, Kashani Ali, McCammon Dan, Herder Jan-Willem den
    Cryogenics 50(9) 488-493 2010年  
    金沢大学理工研究域数物科学系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.
  • Sato, Y., Sugita, H., Mitsuda, K., Nakagawa, T., Fujimoto, R., Murakami, M., Otsuka, K., Tsunematsu, S., Kanao, K., Narasaki, K.
    Cryogenics 50(9) 500-506 2010年  
    The Soft X-ray Spectrometer (SXS) is a high-resolution spectrometer with an X-ray micro-calorimeter array onboard the Japanese X-ray astronomy satellite Astro-H, planned for launch in 2013. The micro-calorimeter is operated at cryogenic temperature of 50 mK provided by the Adiabatic Demagnetization Refrigerator (ADR) with a heat sink of 1.3 K liquid helium stored in the SXS Dewar. To extend the liquid helium lifetime to over 3 years in orbit, two types of mechanical cryocoolers are installed: 20 K-class double-staged Stirling (2ST) coolers and a 1 K-class Joule-Thomson (JT) cooler. Improvement of mechanical cryocoolers has been investigated and verified for higher reliability and cooling performance. The engineering model (EM) of upgraded mechanical cryocoolers was fabricated for a long lifetime test. The required cooling power of 200 mW at 20K for the 2ST cooler and 10 mW at 1.7 K for the JT cooler are achieved by EM test. (c) 2010 Elsevier Ltd. All rights reserved.
  • Ishikawa, K., Ezoe, Y., Yamaguchi, H., Mitsuishi, I., Yoshitake, H., Mitsuda, K., Fujimoto, R., Ohashi, T., Murakami, M., Kanao, K.-I., Yoshida, S., Tsunematsu, S., Dipirro, M., Shirron, P.
    Cryogenics 50(9) 2010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.
  • Yoshino, T., Mitsuda, K., Yamasaki, N.Y., Takei, Y., Hagihara, T., Masui, K., Bauer, M., McCammon, D., Fujimoto, R., Wang, Q.D., Yao, Y.
    Publications of the Astronomical Society of Japan 61(4) 2009年  
  • Kazuhisa Mitsuda, Noriko Y. Yamasaki, Keisuke Shinozaki, Yoh Takei, Takao Nakagawai, Hiroyuki Sugitai, Yohichi Satoh, Ryuichi Fujimoto, Takaya Ohashi, Yoshitaka Ishisaki, Yuichiro Ezoe, Masahide Murakami, Makoto Tashiro, Yukikatsu Terada, Shunji Kitamoto, Toru Tamagawa, Madoka Kawaharada, Tatehiro Mihara, Richard L. Kelley, Caroline A. Kilbourne, F. Scott Porter, Peter J. Shirron, Michael J. Dipirro, Dan Mccammon, Jan-Willem Den Herder
    Proceedings of SPIE - The International Society for Optical Engineering 7011 2008年  査読有り
    The Soft X-ray Spectrometer (SXS) onboard the NeXT (New exploration X-ray Telescope) is an X-ray spectrometer utilizing an X-ray microcalorimeter array. Combined with the soft X-ray telescope of 6 m focal length, the instrument will have a ∼ 290cm2 effective at 6.7 keV. With the large effective area and the energy resolution as good as 6 eV (FWHM), the instrument is very suited for the high-resolution spectroscopy of iron K emission line. One of the major scientific objectives of SXS is to determine turbulent and/or macroscopic motions of the hot gas in clusters of galaxies of up to z ∼ 1. The instruments will use 6 × 6 or 8 × 8 format microcalorimeter array which is similar to that of Suzaku XRS. The detector will be cooled to a cryogenic temperature of 50 mK by multi-stage cooling system consisting of adiabatic demagnetization refrigerator, super fluid He, a 3He Joule Thomson cooler, and double-stage Stirling cycle cooler.
  • J. W. Den Herder, R. Kelley, D. Mccammon, K. Mitsuda, H. Aarts, C. V. Van Baren, M. Buntov, E. Churazov, E. Costantini, J. Cottam, L. Dubbeldam, Y. Ezoe, P. Friedrichs, R. Fujimoto, M. Gilvanov, Y. Ishisaki, J. Kaastra, C. Kilbourne, K. Kuntz, R. Mushotzky, M. Murakami, T. Nakagawa, T. Ohashi, M. Pavlinsky, R. Petre, Scott Porter, P. Predehl, Y. Sato, N. Semea, K. Shinozaki, R. Smith, S. Snowden, R. Sunyaev, H. Sugita, Y. Takei, A. Tkachenko, J. Vink, C. P. De Vries, N. White, N. Yamasaki, F. Zwart
    Proceedings of SPIE - The International Society for Optical Engineering 7011 2008年  
    Spatially resolved X-ray spectroscopy with high spectral resolution allows the study of astrophysical processes in extended sources with unprecedented sensitivity. This includes the measurement of abundances, temperatures, densities, ionisation stages as well as turbulence and velocity structures in these sources. An X-ray calorimeter is planned for the Russian mission Spektr Röntgen-Gamma (SRG), to be launched in 2011. During the first half year (pointed phase) it will study the dynamics and composition of of the hot gas in massive clusters of galaxies and in supernova remnants (SNR). During the survey phase it will produce the first all sky maps of line-rich spectra of the interstellar medium (ISM). Spectral analysis will be feasible for typically every 5° × 5° region on the sky. Considering the very short time-scale for the development of this instrument it consists of a combination of well developed systems. For the optics an extra eROSITA mirror, also part of the Spektr-RG payload, will be used. The detector will be based on spare parts of the detector flown on Suzaku combined with a rebuild of the electronics and the cooler will be based on the design for the Japanese mission NeXT. In this paper we will present the science and give an overview of the instrument.
  • K. Shinozaki, K. Mitsuda, N. Y. Yamasaki, Y. Takei, M. Dipirro, Y. Ezoe, R. Fujimoto, J. W. Den Herder, M. Hirabayashi, Y. Ishisaki, K. Kanao, M. Kawaharada, R. Kelley, C. Kilbourne, S. Kitamoto, D. McCammon, T. Mihara, M. Murakami, T. Nakagawa, T. Ohashi, F. S. Porter, Y. Satoh, P. Shirron, H. Sugita, T. Tamagawa, M. Tashiro, S. Yoshida
    Proceedings of SPIE - The International Society for Optical Engineering 7011 2008年  
    The SXS (Soft X-ray Spectrometer) onboard the coming Japanese X-ray satellite NeXT (New Exploration Xray Telescope) and the SXC (Spectrum-RG X-ray Calorimeter) in Spectrum-RG mission are microcalorimeter array spectrometers which will achieve high spectral resolution of ~ 6 eV in 0.3-10.0 keV energy band. These spectrometers are well-suited to address key problems in high-energy astrophysics. To achieve these high spectral sensitivities, these detectors require to be operated under 50 mK by using very efficient cooling systems including adiabatic demagnetization refrigerator (ADR). For both missions, we propose a two-stage series ADR as a cooling system below 1 K, in which two units of ADR consists of magnetic cooling material, a superconducting magnet, and a heat switch are operated step by step. Three designs of the ADR are proposed for SXS/SXC. In all three designs, ADR can attain the required hold time of 23 hours at 50 mK and cooling power of 0.4μW with a low magnetic fields (1.5/1.5 Tesla or 2.0/3.0 Tesla) in a small configuration (180 mmφ× 319 mm in length). We also fabricated a new portable refrigerator for a technology investigation of two-stage ADR. Two units of ADR have been installed at the bottom of liquid He tank. By using this dewar, important technologies such as an operation of two-stage cooling cycle, tight temperature control less than 1 μK (in rms) stability, a magnetic shielding, saltpills, and gas-gap heat switches are evaluated.
  • Tadayuki Takahashi, Richard Kelley, Kazuhisa Mitsuda, Hideyo Kunieda, Robert Petre, Nicholas White, Tadayasu Dotani, Ryuichi Fujimoto, Yasushi Fukazawa, Kiyoshi Hayashida, Manabu Ishida, Yoshitaka Ishisaki, Motohide Kokubun, Kazuo Makishima, Katsuji Koyama, Greg M. Madejski, Koji Mori, Richard Mushotzky, Kazuhiro Nakazawa, Yasushi Ogasaka, Takaya Ohashi, Masanobu Ozaki, Hiroyasu Tajima, Makoto Tashiro, Yukikatsu Terada, Hiroshi Tsunemi, Takeshi Go Tsuru, Yoshihiro Ueda, Noriko Yamasaki, Shin Watanabe
    Proceedings of SPIE - The International Society for Optical Engineering 7011 2008年  
    The NeXT (New exploration X-ray Telescope), the new Japanese X-ray Astronomy Satellite following Suzakii, is an international X-ray mission which is currently planed for launch in 2013. NeXT is a combination of wide band X-ray spectroscopy (3-80 keV) provided by multi-layer coating, focusing hard X-ray mirrors and hard X-ray imaging detectors, and high energy-resolution soft X-ray spectroscopy (0.3-10 keV) provided by thin-foil X-ray optics and a micro-calorimeter array. The mission will also carry an X-ray CCD camera as a focal plane detector for a soft X-ray telescope and a non-focusing soft gamma-ray detector. With these instruments, NeXT covers very wide energy range from 0.3 keV to 600 keV. The micro-calorimeter system will be developed by international collaboration lead by ISAS/JAXA and NASA. The simultaneous broad bandpass, coupled with high spectral resolution of ΔE ∼7 eV by the micro-calorimeter will enable a wide variety of important science themes to be pursued.
  • Miller, E.D., Tsunemi, H., Bautz, M.W., McCammon, D., Fujimoto, R., Hughes, J.P., Katsuda, S., Kokubun, M., Mitsuda, K., Porter, F.S., Takei, Y., Tsuboi, Y., Yamasaki, N.Y.
    Publications of the Astronomical Society of Japan 60(SPEC. ISS. 1) 2008年  
  • Kimura, S., Masui, K., Takei, Y., Mitsuda, K., Yamasaki, N.Y., Fujimoto, R., Morooka, T., Nakayama, S.
    Journal of Low Temperature Physics 151(3-4 PART 2) 2008年  
  • Uchiyama Yasunobu, Maeda Yoshitomo, Ebara Masatoshi, FUJIMOTO Ryuichi, ISHISAKI Yoshitaka, ISHIDA Manabu, IIZUKA Ryo, USHIO Masayoshi, INOUE Hirohiko, OKADA Shunsaku, MORI Hideyuki, OZAKI Masanobu
    PASJ : publications of the Astronomical Society of Japan 60(SPEC. ISS. 1) S35-S41 2008年  
  • Shirai, H., Fukazawa, Y., Sasada, M., Ohno, M., Yonetoku, D., Yokota, S., Fujimoto, R., Murakami, T., Terashima, Y., Awaki, H., Ikeda, S., Ozawa, M., Tsuru, T.G.
    Publications of the Astronomical Society of Japan 60(SPEC. ISS. 1) 2008年  
  • T. Dotani, K. Mitsuda, M. Bautz, H. Inoue, R. L. Kelley, K. Koyama, H. Kunieda, K. Makishima, Y. Ogawara, R. Petre, T. Takahashi, H. Tsunemi, N. E. White, N. Anabuki, L. Angelini, K. Arnaud, H. Awaki, A. Bamba, K. Boyce, G. V. Brown, K. -W. Chan, J. Cottam, J. Doty, K. Ebisawa, Y. Ezoe, A. C. Fabian, E. Figueroa, R. Fujimoto, Y. Fukazawa, T. Furusho, A. Furuzawa, K. Gendreau, R. E. Griffiths, Y. Haba, K. Hamaguchi, l. Harrus, G. Hasinger, I. Hatsukade, K. Hayashida, P. J. Henry, J. S. Hiraga, S. S. Holt, A. Hornschemeier, J. P. Hughes, U. Hwang, M. Ishida, Y. Ishisaki, N. Isobe, M. Itoh, N. Iyomoto, S. M. Kahn, T. Kamae, H. Katagiri, J. Kataoka, H. Katayama, N. Kawai, M. Kawaharada, C. Kilbourne, K. Kinugasa, S. Kissel, S. Kitamoto, M. Kohama, T. Kohmura, M. Kokubun, T. Kotani, J. Kotoku, A. Kubota, G. M. Madejski, Y. Maeda, F. Makino, A. Markowitz, C. Matsumoto, H. Matsumoto, M. Matsuoka, K. Matsushita, D. McCammon, T. Mihara, K. Misaki, E. Miyata, T. Mizuno, K. Mori, H. Mori, M. Morii, H. Moseley, K. Mukai, H. Murakami, T. Murakami, R. Mushotzky, F. Nagase, M. Namiki, H. Negoro, K. Nakazawa, J. A. Nousek, T. Okajima, Y. Ogasaka, T. Ohashi, T. Oshima, N. Ota, M. Ozaki, H. Ozawa, A. N. Parmar, W. D. Pence, F. Scott Porter, J. N. Reeves, G. R. Ricker, L. Sakurai, W. T. Sanders, A. Senda, P. Serlemitsos, R. Shibata, K. Shinozaki, Y. Soong, R. Smith, M. Suzuki, A. E. Szymkowiak, H. Takahashi, Y. Takei, T. Tamagawa, K. Tamura, T. Tamura, Y. Tanaka, M. Tashiro, Y. Tawara, Y. Terada, Y. Terashima, H. Tomida, K. Torii, Y. Tsuboi, Y. Tsujimoto, T. Tsuru, M. J. L. Turner, Y. Uchiyama, Y. Ueda, S. Ueno, M. Ueno, S. Uno, Y. Urata, S. Watanabe, N. Yamamoto, K. Yamaoka, N. Y. Yamasaki, K. Yamashita, M. Yamauchi, S. Yajmauchi, T. Yaqoob, D. Yonetoku, A. Yoshida
    2007 IEEE NUCLEAR SCIENCE SYMPOSIUM CONFERENCE RECORD, VOLS 1-11 2526-+ 2007年  査読有り
    We report in-flight status of the X-ray detectors on board the Suzaku observatory, the 5th X-ray astronomy satellite of Japan launched on July 10, 2005. Suzaku is equipped with two types of instruments: one is the X-ray Imaging Spectrometers (XISs) and the other is Hard X-ray Detector (HXD). XIS utilizes the X-ray CCD camera in combination with the grazing-incidence X-ray telescope. HXD is a non-imaging, hybrid detector utilizing Si PIN diodes and GSO/BGO phoswich counters. Suzaku takes a low-earth, circular orbit with an altitude of 560 km and an inclination of 31 deg. This means that Suzaku goes through the south atlantic anomaly about 1/3 of its revolutions. This has a large impact on the in-flight performance of XIS and HXD, which is reported in detail in the present paper.
  • Y. Fukazawa, H. Shirai, M. Ohno, D. Yonetoku, S. Yokota, T. Murakami, K. Iwasawa, Y. Terashima, H. Awaki, T. Tsuru, M. Ozawa, R. Fujimoto
    CENTRAL ENGINE OF ACTIVE GALACTIC NUCLEI 373 165-+ 2007年  査読有り
    Here we report the preliminary results on the Suzaku observations of the Seyfert 2 galaxy NGC 4388. The longest high-sensitibity wide-band Xray observation of this object for the first time revealed the time variability of spectra and the complex Fe-K line features.
  • Takei, Y., Henry, J.P., Finoguenov, A., Mitsuda, K., Tamura, T., Fujimoto, R., Briel, U.G.
    Astrophysical Journal 655(2 I) 2007年  
  • Mitsuda, K., Bautz, M., Inoue, H., Kelley, R.L., Koyama, K., Kunieda, H., Makishima, K., Ogawara, Y., Petre, R., Takahashi, T., Tsunemi, H., White, N.E., Anabuki, N., Angelini, L., Arnaud, K., Awaki, H., Bamba, A., Boyce, K., Brown, G.V., Chan, K.-W., Cottam, J., Dotani, T., Doty, J., Ebisawa, K., Ezoe, Y., Fabian, A.C., Figueroa, E., Fujimoto, R., Fukazawa, Y., Furusho, T., Furuzawa, A., Gendreau, K., Griffiths, R.E., Haba, Y., Hamaguchi, K., Harrus, I., Hasinger, G., Hatsukade, I., Hayashida, K., Henry, P.J., Hiraga, J.S., Holt, S.S., Hornschemeier, A., Hughes, J.P., Hwang, U., Ishida, M., Ishisaki, Y., Isobe, N., Itoh, M., Iyomoto, N., Kahn, S.M., Kamae, T., Katagiri, H., Kataoka, J., Katayama, H., Kawai, N., Kllbourne, C., Kinugasa, K., Klssel, S., Kitamoto, S., Kohama, M., Kohmura, T., Kokubun, M., Kotani, T., Kotoku, J., Kubota, A., Madejski, G.M., Maeda, Y., Makino, F., Markowitz, A., Matsumoto, C., Matsumoto, H., Matsuoka, M., Matsushita, K., Mccammon, D., Mihara, T., Misakl, K., Miyata, E., Mizuno, T., Mori, K., Mori, H., Morii, M., Moseley, H., Mukai, K., Murakami, H., Murakami, T., Mushotzky, R., Nagase, F., Namiki, M., Negoro, H., Nakazawa, K., Nousek, J.A., Okajima, T., Ogasaka, Y., Ohashi, T., Oshima, T., Ota, N., Ozaki, M., Ozawa, H., Parmar, A.N., Pence, W.D., Porter, F.S., Reeves, J.N., Ricker, G.R., Sakurai, I., Sanders, W.T., Senda, A., Serlemitsos, P., Shibata, R., Soong, Y., Smith, R., Suzuki, M., Szymkowiak, A.E., Takahashi, H., Tamagawa, T., Tamura, K., Tamura, T., Tanaka, Y., Tashiro, M., Tawara, Y., Terada, Y., Terashima, Y., Tomida, H., Torii, K., Tsuboi, Y., Tsujimoto, M., Tsuru, T.G., Turner, M.J.L., Ueda, Y., Ueno, S., Ueno, M., Uno, S., Urata, Y., Watanabe, S., Yamamoto, N., Yamaoka, K., Yamasaki, N.Y., Yamashita, K., Yamauchi, M., Yamauchi, S., Yaqoob, T., Yonetoku, D., Yoshida, A.
    Publications of the Astronomical Society of Japan 59(1 SPEC. ISS.) 2007年  
    High-sensitivity wide-band X-ray spectroscopy is the key feature of the Suzaku X-ray observatory, launched on 2005 July 10. This paper summarizes the spacecraft, in-orbit performance, operations, and data processing that are related to observations. The scientific instruments, the high-throughput X-ray telescopes, X-ray CCD cameras, non-imaging hard X-ray detector are also described. © 2007. Astronomical Society of Japan.
  • Takei, Y., Ohashi, T., Henry, J.P., Mitsuda, K., Fujimoto, R., Tamura, T., Yamasaki, N.Y., Hayashida, K., Tawa, N., Matsushita, K., Bautz, M.W., Hughes, J.P., Madejski, G.M., Kelley, R.L., Arnaud, K.A.
    ESO Astrophysics Symposia 2007 2007年  
  • Fujimoto Ryuichi, Mitsuda Kazuhisa, McCammon Dan, TAKEI Yoh, BAUER Michael, ISHISAKI Yoshitaka, PORTER F. Scott, YAMAGUCHI Hiroya, HAYASHIDA Kiyoshi, YAMASAKI Noriko Y.
    Progress of theoretical physics. Supplement 59(169) 71-74 2007年  
    During the Suzaku north ecliptic pole observation of 2005 September 2-4, a long-term enhancement was observed, and the C VI 4p to 1s transition line at 459eV was apparently detected. The observed line intensity is comparable to that of the C VI 2p to 1s line at 367eV. This is strong evidence for the charge-exchange process. In addition, O VII, O VIII, Ne X, and Mg XI lines showed clear enhancements. There are also features in the 750-900eV range that could be due to some combination of Fe-L lines, higher order transitions of O VIII (3p to 1s and 6p to 1s), and a Ne IX line. From the correlation of the X-ray intensity with solar-wind flux on time scales of about half a day, and from the short-term (～10 minutes) variations of the X-ray intensity, these lines most likely arise from solar-wind heavy ions interacting with neutral material in the Earth's magnetosheath.
  • ISHISAKI Yoshitaka, MAEDA Yoshitomo, FUJIMOTO Ryuichi, OZAKI Masanobu, EBISAWA Ken, TAKAHASHI Tadayuki, UEDA Yoshihiro, OGASAKA Yasushi, PTAK Andrew, MUKAI Koji, HAMAGUCHI Kenji, HIRAYAMA Masaharu, KOTANI Taro, KUBO Hidetoshi, SHIBATA Ryo, EBARA Masatoshi, FURUZAWA Akihiro, IIZUKA Ryo, INOUE Hirohiko, MORI Hideyuki, OKADA Shunsaku, YOKOYAMA Yushi, MATSUMOTO Hironori, NAKAJIMA Hiroshi, YAMAGUCHI Hiroya, ANABUKI Naohisa, TAWA Noriaki, NAGAI Masaaki, KATSUDA Satoru, HAYASHIDA Kiyoshi, BAMBA Aya, MILLER Eric D., SATO Kosuke, YAMASAKI Noriko Y.
    PASJ : publications of the Astronomical Society of Japan 59(1 SPEC. ISS.) S113-S132 2007年  
  • Smith, R.K., Bautz, M.W., Edgar, R.J., Fujimoto, R., Hamaguchi, K., Hughes, J.P., Ishida, M., Kelley, R., Kllbourne, C.A., Kuntz, K.D., McCammon, D., Miller, E., Mitsuda, K., Mukai, K., Plucinsky, P.P., Porter, F.S., Snowden, S.L., Takei, Y., Terada, Y., Tsuboi, Y., Yamasaki, N.Y.
    Publications of the Astronomical Society of Japan 59(1 SPEC. ISS.) 2007年  
  • Shirron, P.J., DiPirro, M.J., Panek, J., Kelley, R., Mitsuda, K., Fujimoto, R., Hirabayashi, M., McCammon, D.
    Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 559(2) 2006年  
  • Yoshino, T., Yoshida, K., Hagihara, T., Sato, K., Morita, U., Ishisaki, Y., Fujimoto, R., Yamasaki, N.Y., Mitsuda, K.
    Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 559(2) 2006年  
  • Fujimoto, R., Mitsuda, K., Hirabayashi, M., Narasaki, K., Breon, S., Boyle, R., DiPirro, M., Volz, S.M., Kelley, R.L.
    Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 559(2) 2006年  
  • Ota, N., Inada, N., Oguri, M., Mitsuda, K., Richards, G.T., Suto, Y., Brandt, W.N., Castander, F.J., Fujimoto, R., Hall, P.B., Keeton, C.R., Nichol, R.C., Schneider, D.P., Eisenstein, D.E., Frieman, J.A., Turner, E.L., Minezaki, T., Yoshi, Y.
    Astrophysical Journal 647(1 I) 215-221 2006年  
    We present results from Chandra observations of SDSS J1004+4112, a strongly lensed quasar system with a maximum image separation of 15''. All four bright images of the quasar, as well as resolved X-ray emission originating from the lensing cluster, are clearly detected. The emission from the lensing cluster extends out to approximately 1'5. We measure the bolometric X-ray luminosity and temperature of the lensing cluster to be 4.7; 10(44) ergs s(-1) and 6.4 keV, consistent with the luminosity-temperature relation for distant clusters. The mass estimated from the X-ray observation shows excellent agreement with the mass derived from gravitational lensing. The X-ray flux ratios of the quasar images differ markedly from the optical flux ratios, and the combined X-ray spectrum of the images possesses an unusually strong Fe K alpha emission line, both of which are indicative of microlensing.
  • Kilbourne, C.A., Boyce, K.R., Brown, G.V., Cottam, J., Figueroa-Feliciano, E., Fujimoto, R., Furusho, T., Ishisaki, Y., Kelley, R.L., McCammon, D., Mitsuda, K., Morita, U., Porter, F.S., Ota, N., Saab, T., Takei, Y., Yamamoto, M.
    Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 559(2) 2006年  
  • Cottam, J., Boyce, K.R., Brown, G.V., Fujimoto, R., Furusho, T., Ishisaki, Y., Kelley, R.L., Kilbourne, C.A., McCammon, D., Mitsuda, K., Morita, U., Ota, N., Porter, F.S., Saab, T., Takei, Y., Yamamoto, M.
    Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 559(2) 2006年  
  • Ota, N., Boyce, K.R., Brown, G.V., Cottam, J., Fujimoto, R., Furusho, T., Ishisaki, Y., Kelley, R.L., Kilbourne, C.A., McCammon, D., Mitsuda, K., Morita, U., Porter, F.S., Takei, Y., Yamamoto, M.
    Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 559(2) 2006年  
  • Morita, U., Yamakawa, Y., Fujimori, T., Ishisaki, Y., Ohashi, T., Takei, Y., Yoshida, K., Yoshino, T., Mitsuda, K., Yamasaki, N.Y., Fujimoto, R., Sato, H., Minoura, Y., Takahashi, N., Homma, T., Shoji, S., Kuroda, Y., Onishi, M.
    Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 559(2) 2006年  
  • A Hayakawa, C Inoue, Y Ishisaki, M Ishida, T Ohashi, T Furusho, NY Yamasaki, R Fujimoto, K Mitsuda, K Misaki, Y Maeda, H Kunieda
    OPTICS FOR EUV, X-RAY AND GAMMA-RAY ASTRONOMY 5168 364-375 2004年  査読有り
    X-Ray Spectrometer (XRS) is the microcalorimeter onboard the X-ray astronomy satellite Astro-E2 which is scheduled to be launched early in 2005. For the XRS to achieve its best energy resolution of 6 eV at 6 keV, X-ray intensity should be limited up to several c s(-1) pixel(-1). The filter wheel (FW) is the instrument to reduce incident X-ray intensity on the XRS using extinction filters. The FW consists of a stepping motor, extinction filters, and a filter disk which has six mounting positions for the extinction filters. Among the six mounting points, two are used for Neutral Density (ND) filters, another two are for Beryllium (Be) filters, and the other two are remained open. The biggest modification from Astro-E is that we attach radioisotopes of Fe-55 and Ca-41 on the filter disk, which illuminate the XRS pixels to monitor the gain in orbit. We present here the mechanical design of the FW especially on improvements from Astro-E, and the results of our calibration measurements on X-ray transmission of the extinction filters.
  • Y Ishisaki, T Ohashi, T Oshima, U Morita, K Shinozaki, K Sato, K Mitsuda, NY Yamasaki, R Fujimoto, Y Takei, H Sato, N Takahashi, T Homma, T Osaka
    HIGH-ENERGY DETECTORS IN ASTRONOMY 5501 123-134 2004年  
    We are developing a superconducting transition-edge sensor (TES) microcalorimeter array for the Diffuse Intergalactic Oxygen Surveyor (DIOS) mission. DIOS is a relatively small Japanese X-ray mission which will study large-scale distribution of the warm-hot intergalactic medium (WHIM) using O-VII and O-VIII emission lines. The satellite weighs about 400 kg equipped with a four-reflection X-ray telescope (FXT) and a TES microcalorimeter array (XSA). The design goal of the observing system is an effective area larger than 100 cm 2 at the oxygen line energy, a field of view about 50 arcmin square, and an energy resolution about 2 eV in the energy range of 0.3-1 keV. The TES microcalorimeter array provides the large field of view and good energy resolution at the same time. We plan to install an array comprising 16 x 16 pixels with an overall size of 1 cm square, which is cooled with a cryogen-free cooler. Pixels are readout by multiplexing signals using a multi-input SQUID amplifier, with each input connected to a TES microcalorimeter which is AC biased with a different frequency. We report the design and present status of the XSA system development.
  • Kudo, H., Nakamura, T., Arakawa, T., Ohtsuka, S., Izumi, T., Shoji, S., Sato, S., Kobayashi, H., Mori, K., Homma, T., Osaka, T., Mitsuda, K., Yamasaki, N.Y., Fujimoto, R., Iyomoto, N., Oshima, T., Futamoto, K., Takei, Y., Ichitsubo, T., Fujimori, T., Ishisaki, Y., Morita, U., Koga, T., Sato, K., Ohashi, T., Kuroda, Y., Onishi, M., Otake, K., Beppu, F.
    Sensors and Actuators, A: Physical 114(2-3) 2004年  

MISC

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  • 佐藤浩介, 大橋隆哉, 石崎欣尚, 江副祐一郎, 山田真也, 山崎典子, 満田和久, 石田学, 前田良知, 田原譲, 三石郁之, 藤本龍一, 鶴剛, 太田直美, 大里健, 中島真也
    日本天文学会年会講演予稿集 2018 225 2018年8月20日  
  • Alle, S.W., Aharonian, F., Akamatsu, H., Akimoto, F., Allen, S.W., Angelini, L., Audard, M., Awaki, H., Axelsson, M., Bamba, A., Bautz, M.W., Blandford, R., Brenneman, L.W., Brown, G.V., Bulbul, E., Cackett, E.M., Chernyakova, M., Chiao, M.P., Coppi, P.S., Costantini, E., De Plaa, J., De Vries, C.P., Den Herder, J.-W., Done, C., Dotani, T., Ebisawa, K., Eckart, M.E., Enoto, T., Ezoe, Y., Fabian, A.C., Ferrigno, C., Foster, A.R., Fujimoto, R., Fukazawa, Y., Furuzawa, A., Galeazzi, M., Gallo, L.C., Gandhi, P., Giustini, M., Goldwurm, A., Gu, L., Guainazzi, M., Haba, Y., Hagino, K., Hamaguchi, K., Harrus, I.M., Hatsukade, I., Hayashi, K., Hayashi, T., Hayashida, K., Hiraga, J.S., Hornschemeier, A., Hoshino, A., Hughes, J.P., Ichinohe, Y., Iizuka, R., Inoue, H., Inoue, Y., Ishida, M., Ishikawa, K., Ishisaki, Y., Iwai, M., Kaastra, J., Kallman, T., Kamae, T., Kataoka, J., Katsuda, S., Kawai, N., Kelley, R.L., Kilbourne, C.A., Kitaguchi, T., Kitamoto, S., Kitayama, T., Kohmura, T., Kokubun, M., Koyama, K., Koyama, S., Kretschmar, P., Krimm, H.A., Kubota, A., Kunieda, H., Laurent, P., Lee, S.-H., Leutenegger, M.A., Limousin, O.O., Loewenstein, M., Long, K.S., Lumb, D., Madejski, G., Maeda, Y., Maier, D., Makishima, K., Markevitch, M., Matsumoto, H., Matsushita, K., Mccammon, D., Mcnamara, B.R., Mehdipour, M., Miller, E.D., Miller, J.M., Mineshige, S., Mitsuda, K., Mitsuishi, I., Miyazawa, T., Mizuno, T., Mori, H., Mori, K., Mukai, K., Murakami, H., Mushotzky, R.F., Nakagawa, T., Nakajima, H., Nakamori, T., Nakashima, S., Nakazawa, K., Nobukawa, K.K., Nobukawa, M., Noda, H., Odaka, H., Ohashi, T., Ohno, M., Okajima, T., Ota, N., Ozaki, M., Paerels, F., Paltani, S., Petre, R., Pinto, C., Porter, F.S., Pottschmidt, K., Reynolds, C.S., Safi-Harb, S., Saito, S., Sakai, K., Sasaki, T., Sato, G., Sato, K., Sato, R., Sawada, M., Schartel, N., Serlemtsos, P.J., Seta, H., Shidatsu, M., Simionescu, A., Smith, R.K., Soong, Y., Stawarz, Ł., Sugawara, Y., Sugita, S., Szymkowiak, A., Tajima, H., Takahashi, H., Takahashi, T., Takeda, S., Takei, Y., Tamagawa, T., Tamura, T., Tanaka, T., Tanaka, Y., Tanaka, Y.T., Tashiro, M.S., Tawara, Y., Terada, Y., Terashima, Y., Tombesi, F., Tomida, H., Tsuboi, Y., Tsujimoto, M., Tsunemi, H., Suru, T.G., Uchida, H., Uchiyama, H., Uchiyama, Y., Ueda, S., Ueda, Y., Uno, S., Urry, C.M., Ursino, E., Watanabe, S., Werner, N., Wilkins, D.R., Williams, B.J., Yamada, S., Yamaguchi, H., Yamaoka, K., Yamasaki, N.Y., Yamauchi, M., Yamauchi, S., Yaqoob, T., Yatsu, Y., Yonetoku, D., Zhuravleva, I., Zoghbi, A., Nakaniwa, N.
    Publications of the Astronomical Society of Japan 70(2) 2018年  
    We report a Hitomi observation of IGR J16318-4848, a high-mass X-ray binary<br /> system with an extremely strong absorption of N_H~10^{24} cm^{-2}. Previous<br /> X-ray studies revealed that its spectrum is dominated by strong fluorescence<br /> lines of Fe as well as continuum emission. For physical and geometrical insight<br /> into the nature of the reprocessing material, we utilize the high spectroscopic<br /> resolving power of the X-ray microcalorimeter (the soft X-ray spectrometer;<br /> SXS) and the wide-band sensitivity by the soft and hard X-ray imager (SXI and<br /> HXI) aboard Hitomi. Even though photon counts are limited due to unintended<br /> off-axis pointing, the SXS spectrum resolves Fe K{\alpha_1} and K{\alpha_2}<br /> lines and puts strong constraints on the line centroid and width. The line<br /> width corresponds to the velocity of 160^{+300}_{-70} km s^{-1}. This<br /> represents the most accurate, and smallest, width measurement of this line made<br /> so far from any X-ray binary, much less than the Doppler broadening and shift<br /> expected from speeds which are characteristic of similar systems. Combined with<br /> the K-shell edge energy measured by the SXI and HXI spectra, the ionization<br /> state of Fe is estimated to be in the range of Fe I--IV. Considering the<br /> estimated ionization parameter and the distance between the X-ray source and<br /> the absorber, the density and thickness of the materials are estimated. The<br /> extraordinarily strong absorption and the absence of a Compton shoulder<br /> component is confirmed. These characteristics suggest reprocessing materials<br /> which are distributed in a narrow solid angle or scattering primarily with warm<br /> free electrons or neutral hydrogen.
  • Aharonian, F., Akamatsu, H., Akimoto, F., Allen, S.W., Angelini, L., Audard, M., Awaki, H., Axelsson, M., Bamba, A., Bautz, M.W., Blandford, R., Brenneman, L.W., Brown, G.V., Bulbul, E., Cackett, E.M., Chernyakova, M., Chiao, M.P., Coppi, P.S., Costantini, E., De Plaa, J., De Vries, C.P., Den Herder, J.-W., Done, C., Dotani, T., Ebisawa, K., Eckart, M.E., Enoto, T., Ezoe, Y., Fabian, A.C., Ferrigno, C., Foster, A.R., Fujimoto, R., Fukazawa, Y., Furuzawa, A., Galeazzi, M., Gallo, L.C., Gandhi, P., Giustini, M., Goldwurm, A., Gu, L., Guainazzi, M., Haba, Y., Hagino, K., Hamaguchi, K., Harrus, I.M., Hatsukade, I., Hayashi, K., Hayashi, T., Hayashida, K., Hiraga, J.S., Hornschemeier, A., Hoshino, A., Hughes, J.P., Ichinohe, Y., Iizuka, R., Inoue, H., Inoue, Y., Ishida, M., Ishikawa, K., Ishisaki, Y., Iwai, M., Kaastra, J., Kallman, T., Kamae, T., Kataoka, J., Katsuda, S., Kawai, N., Kelley, R.L., Kilbourne, C.A., Kitaguchi, T., Kitamoto, S., Kitayama, T., Kohmura, T., Kokubun, M., Koyama, K., Koyama, S., Kretschmar, P., Krimm, H.A., Kubota, A., Kunieda, H., Laurent, P., Lee, S.-H., Leutenegger, M.A., Limousin, O., Loewenstein, M., Long, K.S., Lumb, D., Madejski, G., Maeda, Y., Maier, D., Makishima, K., Markevitch, M., Matsumoto, H., Matsushita, K., McCammon, D., McNamara, B.R., Mehdipour, M., Miller, E.D., Miller, J.M., Mineshige, S., Mitsuda, K., Mitsuishi, I., Miyazawa, T., Mizuno, T., Mori, H., Mori, K., Mukai, K., Murakami, H., Mushotzky, R.F., Nakagawa, T., Nakajima, H., Nakamori, T., Nakashima, S., Nakazawa, K., Nobukawa, K.K., Nobukawa, M., Noda, H., Odaka, H., Ohashi, T., Ohno, M., Okajima, T., Ota, N., Ozaki, M., Paerels, F., Paltani, S., Petre, R., Pinto, C., Porter, F.S., Pottschmidt, K., Reynolds, C.S., Safi-Harb, S., Saito, S., Sakai, K., Sasaki, T., Sato, G., Sato, K., Sato, R., Sawada, M., Schartel, N., Serlemtsos, P.J., Seta, H., Shidatsu, M., Simionescu, A., Smith, R.K., Soong, Y., Stawarz, L., Sugawara, Y., Sugita, S., Szymkowiak, A., Tajima, H., Takahashi, H., Takahashi, T., Takeda, S., Takei, Y., Tamagawa, T., Tamura, T., Tanaka, T., Tanaka, Y., Tanaka, Y.T., Tashiro, M.S., Tawara, Y., Terada, Y., Terashima, Y., Tombesi, F., Tomida, H., Tsuboi, Y., Tsujimoto, M., Tsunemi, H., Tsuru, T.G., Uchida, H., Uchiyama, H., Uchiyama, Y., Ueda, S., Ueda, Y., Uno, S., Urry, C.M., Ursino, E., Watanabe, S., Werner, N., Wilkins, D.R., Williams, B.J., Yamada, S., Yamaguchi, H., Yamaoka, K., Yamasaki, N.Y., Yamauchi, M., Yamauchi, S., Yaqoob, T., Yatsu, Y., Yonetoku, D., Zhuravleva, I., Zoghbi, A., Uchida, Y.
    Publications of the Astronomical Society of Japan 70(6) 2018年  
    We present the results from the Hitomi Soft Gamma-ray Detector (SGD)<br /> observation of the Crab nebula. The main part of SGD is a Compton camera, which<br /> in addition to being a spectrometer, is capable of measuring polarization of<br /> gamma-ray photons. The Crab nebula is one of the brightest X-ray / gamma-ray<br /> sources on the sky, and, the only source from which polarized X-ray photons<br /> have been detected. SGD observed the Crab nebula during the initial test<br /> observation phase of Hitomi. We performed the data analysis of the SGD<br /> observation, the SGD background estimation and the SGD Monte Carlo simulations,<br /> and, successfully detected polarized gamma-ray emission from the Crab nebula<br /> with only about 5 ks exposure time. The obtained polarization fraction of the<br /> phase-integrated Crab emission (sum of pulsar and nebula emissions) is (22.1<br /> $\pm$ 10.6)% and, the polarization angle is 110.7$^o$ + 13.2 / $-$13.0$^o$ in<br /> the energy range of 60--160 keV (The errors correspond to the 1 sigma<br /> deviation). The confidence level of the polarization detection was 99.3%. The<br /> polarization angle measured by SGD is about one sigma deviation with the<br /> projected spin axis of the pulsar, 124.0$^o$ $\pm$0.1$^o$.
  • Aharonian, F., Akamatsu, H., Akimoto, F., Allen, S.W., Angelini, L., Audard, M., Awaki, H., Axelsson, M., Bamba, A., Bautz, M.W., Blandford, R., Brenneman, L.W., Brown, G.V., Bulbul, E., Cackett, E.M., Chernyakova, M., Chiao, M.P., Coppi, P.S., Costantini, E., De Plaa, J., De Vries, C.P., Den Herder, J.-W., Done, C., Dotani, T., Ebisawa, K., Eckart, M.E., Enoto, T., Ezoe, Y., Fabian, A.C., Ferrigno, C., Foster, A.R., Fujimoto, R., Fukazawa, Y., Furukawa, M., Furuzawa, A., Galeazzi, M., Gallo, L.C., Gandhi, P., Giustini, M., Goldwurm, A., Gu, L., Guainazzi, M., Haba, Y., Hagino, K., Hamaguchi, K., Harrus, I.M., Hatsukade, I., Hayashi, K., Hayashi, T., Hayashida, K., Hiraga, J.S., Hornschemeier, A., Hoshino, A., Hughes, J.P., Ichinohe, Y., Iizuka, R., Inoue, H., Inoue, Y., Ishida, M., Ishikawa, K., Ishisaki, Y., Iwai, M., Kaastra, J., Kallman, T., Kamae, T., Kataoka, J., Kato, Y., Katsuda, S., Kawai, N., Kelley, R.L., Kilbourne, C.A., Kitaguchi, T., Kitamoto, S., Kitayama, T., Kohmura, T., Kokubun, M., Koyama, K., Koyama, S., Kretschmar, P., Krimm, H.A., Kubota, A., Kunieda, H., Laurent, P., Lee, S.-H., Leutenegger, M.A., Limousin, O., Loewenstein, M., Long, K.S., Lumb, D., Madejski, G., Maeda, Y., Maier, D., Makishima, K., Markevitch, M., Matsumoto, H., Matsushita, K., McCammon, D., McNamara, B.R., Mehdipour, M., Miller, E.D., Miller, J.M., Mineshige, S., Mitsuda, K., Mitsuishi, I., Miyazawa, T., Mizuno, T., Mori, H., Mori, K., Mukai, K., Murakami, H., Mushotzky, R.F., Nakagawa, T., Nakajima, H., Nakamori, T., Nakashima, S., Nakazawa, K., Nobukawa, K.K., Nobukawa, M., Noda, H., Odaka, H., Ohashi, T., Ohno, M., Okajima, T., Ota, N., Ozaki, M., Paerels, F., Paltani, S., Petre, R., Pinto, C., Porter, F.S., Pottschmidt, K., Reynolds, C.S., Safi-Harb, S., Saito, S., Sakai, K., Sasaki, T., Sato, G., Sato, K., Sato, R., Sawada, M., Schartel, N., Serlemtsos, P.J., Seta, H., Shidatsu, M., Simionescu, A., Smith, R.K., Soong, Y., Stawarz, Ł., Sugawara, Y., Sugita, S., Szymkowiak, A., Tajima, H., Takahashi, H., Takahashi, T., Takeda, S., Takei, Y., Tamagawa, T., Tamura, T., Tanaka, T., Tanaka, Y., Tanaka, Y.T., Tashiro, M.S., Tawara, Y., Terada, Y., Terashima, Y., Tombesi, F., Tomida, H., Tsuboi, Y., Tsujimoto, M., Tsunemi, H., Tsuru, T.G., Uchida, H., Uchiyama, H., Uchiyama, Y., Ueda, S., Ueda, Y., Uno, S., Urry, C.M., Ursino, E., Watanabe, S., Werner, N., Wilkins, D.R., Williams, B.J., Yamada, S., Yamaguchi, H., Yamaoka, K., Yamasaki, N.Y., Yamauchi, M., Yamauchi, S., Yaqoob, T., Yatsu, Y., Yonetoku, D., Zhuravleva, I., Zoghbi, A.
    Publications of the Astronomical Society of Japan 70(2) 2018年  
    The present paper investigates the temperature structure of the X-ray<br /> emitting plasma in the core of the Perseus cluster using the 1.8--20.0 keV data<br /> obtained with the Soft X-ray Spectrometer (SXS) onboard the Hitomi Observatory.<br /> A series of four observations were carried out, with a total effective exposure<br /> time of 338 ks and covering a central region $\sim7&#039;$ in diameter. The SXS was<br /> operated with an energy resolution of $\sim$5 eV (full width at half maximum)<br /> at 5.9 keV. Not only fine structures of K-shell lines in He-like ions but also<br /> transitions from higher principal quantum numbers are clearly resolved from Si<br /> through Fe. This enables us to perform temperature diagnostics using the line<br /> ratios of Si, S, Ar, Ca, and Fe, and to provide the first direct measurement of<br /> the excitation temperature and ionization temperature in the Perseus cluster.<br /> The observed spectrum is roughly reproduced by a single temperature thermal<br /> plasma model in collisional ionization equilibrium, but detailed line ratio<br /> diagnostics reveal slight deviations from this approximation. In particular,<br /> the data exhibit an apparent trend of increasing ionization temperature with<br /> increasing atomic mass, as well as small differences between the ionization and<br /> excitation temperatures for Fe, the only element for which both temperatures<br /> can be measured. The best-fit two-temperature models suggest a combination of 3<br /> and 5 keV gas, which is consistent with the idea that the observed small<br /> deviations from a single temperature approximation are due to the effects of<br /> projection of the known radial temperature gradient in the cluster core along<br /> the line of sight. Comparison with the Chandra/ACIS and the XMM-Newton/RGS<br /> results on the other hand suggests that additional lower-temperature components<br /> are present in the ICM but not detectable by Hitomi SXS given its 1.8--20 keV<br /> energy band.
  • Aharonian, F., Akamatsu, H., Akimoto, F., Allen, S.W., Angelini, L., Audard, M., Awaki, H., Axelsson, M., Bamba, A., Bautz, M.W., Blandford, R., Brenneman, L.W., Brown, G.V., Bulbul, E., Cackett, E.M., Chernyakova, M., Chiao, M.P., Coppi, P.S., Costantini, E., De Plaa, J., De Vries, C.P., Den Herder, J.-W., Done, C., Dotani, T., Ebisawa, K., Eckart, M.E., Enoto, T., Ezoe, Y., Fabian, A.C., Ferrigno, C., Foster, A.R., Fujimoto, R., Fukazawa, Y., Furuzawa, A., Galeazzi, M., Gallo, L.C., Gandhi, P., Giustini, M., Goldwurm, A., Gu, L., Guainazzi, M., Haba, Y., Hagino, K., Hamaguchi, K., Harrus, I.M., Hatsukade, I., Hayashi, K., Hayashi, T., Hayashida, K., Hell, N., Hiraga, J.S., Hornschemeier, A., Hoshino, A., Hughes, J.P., Ichinohe, Y., Iizuka, R., Inoue, H., Inoue, Y., Ishida, M., Ishikawa, K., Ishisaki, Y., Iwai, M., Kaastra, J., Kallman, T., Kamae, T., Kataoka, J., Katsuda, S., Kawai, N., Kelley, R.L., Kilbourne, C.A., Kitaguchi, T., Kitamoto, S., Kitayama, T., Kohmura, T., Kokubun, M., Koyama, K., Koyama, S., Kretschmar, P., Krimm, H.A., Kubota, A., Kunieda, H., Laurent, P., Lee, S.-H., Leutenegger, M.A., Limousin, O., Loewenstein, M., Long, K.S., Lumb, D., Madejski, G., Maeda, Y., Maier, D., Makishima, K., Markevitch, M., Matsumoto, H., Matsushita, K., McCammon, D., McNamara, B.R., Mehdipour, M., Miller, E.D., Miller, J.M., Mineshige, S., Mitsuda, K., Mitsuishi, I., Miyazawa, T., Mizuno, T., Mori, H., Mori, K., Mukai, K., Murakami, H., Mushotzky, R.F., Nakagawa, T., Nakajima, H., Nakamori, T., Nakashima, S., Nakazawa, K., Nobukawa, K.K., Nobukawa, M., Noda, H., Odaka, H., Ohashi, T., Ohno, M., Okajima, T., Ota, N., Ozaki, M., Paerels, F., Paltani, S., Petre, R., Pinto, C., Porter, F.S., Pottschmidt, K., Reynolds, C.S., Safi-Harb, S., Saito, S., Sakai, K., Sasaki, T., Sato, G., Sato, K., Sato, R., Sawada, M., Schartel, N., Serlemtsos, P.J., Seta, H., Shidatsu, M., Simionescu, A., Smith, R.K., Soong, Y., Stawarz, Ł., Sugawara, Y., Sugita, S., Szymkowiak, A., Tajima, H., Takahashi, H., Takahashi, T., Takeda, S., Takei, Y., Tamagawa, T., Tamura, T., Tanaka, T., Tanaka, Y., Tanaka, Y.T., Tashiro, M.S., Tawara, Y., Terada, Y., Terashima, Y., Tombesi, F., Tomida, H., Tsuboi, Y., Tsujimoto, M., Tsunemi, H., Tsuru, T.G., Uchida, H., Uchiyama, H., Uchiyama, Y., Ueda, S., Ueda, Y., Uno, S., Urry, C.M., Ursino, E., Watanabe, S., Werner, N., Wilkins, D.R., Williams, B.J., Yamada, S., Yamaguchi, H., Yamaoka, K., Yamasaki, N.Y., Yamauchi, M., Yamauchi, S., Yaqoob, T., Yatsu, Y., Yonetoku, D., Zhuravleva, I., Zoghbi, A., Raassen, A.J.J.
    Publications of the Astronomical Society of Japan 70(2) 2018年  
    The Hitomi SXS spectrum of the Perseus cluster, with $\sim$5 eV resolution in<br /> the 2-9 keV band, offers an unprecedented benchmark of the atomic modeling and<br /> database for hot collisional plasmas. It reveals both successes and challenges<br /> of the current atomic codes. The latest versions of AtomDB/APEC (3.0.8), SPEX<br /> (3.03.00), and CHIANTI (8.0) all provide reasonable fits to the broad-band<br /> spectrum, and are in close agreement on best-fit temperature, emission measure,<br /> and abundances of a few elements such as Ni. For the Fe abundance, the APEC and<br /> SPEX measurements differ by 16%, which is 17 times higher than the statistical<br /> uncertainty. This is mostly attributed to the differences in adopted<br /> collisional excitation and dielectronic recombination rates of the strongest<br /> emission lines. We further investigate and compare the sensitivity of the<br /> derived physical parameters to the astrophysical source modeling and<br /> instrumental effects. The Hitomi results show that an accurate atomic code is<br /> as important as the astrophysical modeling and instrumental calibration<br /> aspects. Substantial updates of atomic databases and targeted laboratory<br /> measurements are needed to get the current codes ready for the data from the<br /> next Hitomi-level mission.
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