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三谷 烈史

ミタニ タケフミ  (Takefumi MITANI)

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 太陽系科学研究系 助教
学位
修士(理学)(東京大学)
博士(理学)(東京大学)
J-GLOBAL ID
201901006861784502
researchmap会員ID
B000359529

研究キーワード

 8

研究分野

 1

経歴

 5

学歴

 3

委員歴

 1

論文

 83
  • Masahito Nosé, Keisuke Hosokawa, Reiko Nomura, Mariko Teramoto, Kazushi Asamura, Yoshizumi Miyoshi, Takefumi Mitani, Takeshi Sakanoi, Taku Namekawa, Takeshi Kawano, Yoshihiro Iwanaga, Shunichi Tatematsu, Masafumi Hirahara, Alexa Halford, Mykhaylo Shumko, Marc R. Lessard, Kristina Lynch, Nicholaos Paschalidis, Allison N. Jaynes, Matthew G. McHarg
    Journal of Geophysical Research: Space Physics 129(6) 2024年5月31日  
    Abstract We made observations of magnetic field variations in association with pulsating auroras with the magneto‐impedance sensor magnetometer (MIM) carried by the Loss through Auroral Microburst Pulsations (LAMP) sounding rocket that was launched at 11:27:30 UT on 5 March 2022 from Poker Flat Research Range, Alaska. At an altitude of 200–250 km, MIM detected clear enhancements of the magnetic field by 15–25 nT in both the northward and westward components. From simultaneous observations with the ground all‐sky camera, we found that the footprint of LAMP at the 100 km altitude was located near the center of a pulsating auroral patch. The auroral patch had a dimension of ∼90 km in latitude and ∼25 km in longitude, and its major axis was inclined toward northwest. These observations were compared with results of a simple model calculation, in which local electron precipitation into the thin‐layer ionosphere causes an elliptical auroral patch. The conductivity within the patch is enhanced in the background electric field and as a result, the magnetic field variations are induced around the auroral patch. The model calculation results can explain the MIM observations if the electric field points toward southeast and one of the model parameters is adjusted. We conclude that the pulsating auroral patch in this event was associated with a one‐pair field‐aligned current that consists of downward (upward) currents at the poleward (equatorward) edge of the patch. This current structure is maintained even if the auroral patch is latitudinally elongated.
  • T. Namekawa, T. Mitani, K. Asamura, Y. Miyoshi, K. Hosokawa, M. Lessard, C. Moser, A. J. Halford, T. Sakanoi, M. Kawamura, M. Nose, R. Nomura, M. Teramoto, M. Shumko, K. A. Lynch, A. N. Jaynes, M. G. McHarg
    Geophysical Research Letters 2023年12月28日  査読有り
  • Vladimir Borisovich Belakhovsky, Vyacheslav A. Pilipenko, Elizaveta E. Antonova, Yoshizumi Miyoshi, Yoshiya Kasahara, Satoshi Kasahara, Nana Higashio, Iku Shinohara, Tomoaki Hori, Shoya Matsuda, Shoichiro Yokota, Takeshi Takashima, Mitani Takefumi, Kunihiro Keika, Satoko Nakamura
    Earth, Planets and Space 75(1) 2023年12月21日  
    Abstract Variations of relativistic electron fluxes (E ≥ 1 MeV) and wave activity in the Earth magnetosphere are studied to determine the contribution of different acceleration mechanisms of the outer radiation belt electrons: ULF mechanism, VLF mechanism, and adiabatic acceleration. The electron fluxes were measured by Arase satellite and geostationary GOES satellites. The ULF power index is used to characterize the magnetospheric wave activity in the Pc5 range. To characterize the VLF wave activity in the magnetosphere, we use data from PWE instrument of Arase satellite. We consider some of the most powerful magnetic storms during the Arase era: May 27–29, 2017; September 7–10, 2017; and August 25–28, 2018. Also, non-storm intervals with a high solar wind speed before and after these storms for comparison are analyzed. Magnitudes of relativistic electron fluxes during these magnetic storms are found to be greater than that during non-storm intervals with high solar wind streams. During magnetic storms, the flux intensity maximum shifts to lower L-shells compared to intervals without magnetic storms. For the considered events, the substorm activity, as characterized by AE index, is found to be a necessary condition for the increase of relativistic electron fluxes, whereas a high solar wind speed alone is not sufficient for the relativistic electron growth. The enhancement of relativistic electron fluxes by 1.5–2 orders of magnitude is observed 1–3 days after the growth of the ULF index and VLF emission power. The growth of VLF and ULF wave powers coincides with the growth of substorm activity and occurs approximately at the same time. Both mechanisms operate at the first phase of electron acceleration. At the second phase of electron acceleration, the mechanism associated with the injection of electrons into the region of the magnetic field weakened by the ring current and their subsequent betatron acceleration during the magnetic field restoration can work effectively. Graphical Abstract
  • Sandeep Kumar, Y. Miyoshi, V. Jordanova, L. M. Kistler, I. Park, C. Jun, T. Hori, K. Asamura, Shreedevi P. R, S. Yokota, S. Kasahara, Y. Kazama, S.‐Y. Wang, Sunny W. Y. Tam, Tzu‐Fang Chang, T. Mitani, N. Higashio, K. Keika, A. Matsuoka, S. Imajo, I. Shinohara
    Journal of Geophysical Research: Space Physics 2023年9月4日  
    Abstract Using Arase observations of the inner magnetosphere during 26 CIR‐driven geomagnetic storms with minimum Sym‐H between ‐33 and ‐86 nT, we investigated ring current pressure development of ions (H+, He+, O+) and electron during prestorm, main, early recovery and late recovery phases as a function of L‐shell and magnetic local time. It is found that during the main and early recovery phase of the storms the ion pressure is asymmetric in the inner magnetosphere, leading to a strong partial ring current. The ion pressure becomes symmetric during the late recovery phase. H+ ions with energies of ∼20‐50 keV and ∼50‐100 keV contribute more to the ring current pressure during the main phase and early/late recovery phase, respectively. O+ ions with energies of ∼10‐20 keV contribute significantly during main and early recovery phase. These are consistent with previous studies. The electron pressure was found to be asymmetric during the main, early recovery and late recovery phase. The electron pressure peaks from midnight to the dawn sector. Electrons with energy of <50 keV contribute to the ring current pressure during the main and early recovery phase of the storms. Overall, the electron contribution to the total ring current is found to be ∼11% during the main and early recovery phases. However, the electron contribution is found to be significant (∼22%) in the 03‐09 MLT sector during the main and early recovery phase. The results indicate an important role of electrons in the ring current build up. This article is protected by copyright. All rights reserved.
  • Yoshizumi Miyoshi, Yuto Katoh, Shinji Saito, Takefumi Mitani, Takeshi Takashima
    Solar-Terrestrial Environmental Prediction 115-137 2023年2月1日  
もっとみる

MISC

 139
  • 長谷部信行, 鳥居祥二, 片岡淳, 唐牛譲, 山下直之, 武田侑子, 森田幹雄, 小林進悟, 晴山慎, 三谷烈史, 高島健, 小林正規, 荒井朋子, D’USTON Claude, KIM Kyeong Ja, BRUECKNER Johannes
    宇宙科学技術連合講演会講演集(CD-ROM) 53rd 1J02 2009年  
  • 田中智, 飯島祐一, 大嶽久志, 木村淳, 倉本圭, 三谷烈史, 小川和律
    日本鉱物科学会年会講演要旨集 2009 29 2009年  
  • 西村夏奈, 高島健, 平原聖文, 三谷烈史, 小林光吉
    地球電磁気・地球惑星圏学会総会及び講演会予稿集(CD-ROM) 126th ROMBUNNO.B009-P019 2009年  
  • 小林光吉, 高島健, 平原聖文, 三谷烈史, 笠原慧
    地球電磁気・地球惑星圏学会総会及び講演会予稿集(CD-ROM) 126th ROMBUNNO.B006-15 2009年  
  • 森田幹雄, 長谷部信行, 鳥居祥二, 片岡淳, 唐牛譲, 早津佳那子, 武田侑子, 長岡央, 三谷烈史, 小林進悟, 晴山慎, 飯島祐一, 高島健, 小林正規, 荒井朋子, D’USTON C, GASNAULT O, 山下直之, KIM K. J, DOHM J. M
    太陽系科学シンポジウム講演集録(CD-ROM) 31st ROMBUNNO.12GATSU21NICHI,14 2009年  
  • 上田剛, 榎戸輝揚, 中澤知洋, 三谷烈史, 高島健, 坂野井健, 氏家恵理子, 笠羽康正, 吉田和哉, 高橋幸弘, 森國城, 牧島一夫
    日本物理学会講演概要集 63(2) 94-94 2008年8月25日  
  • 高島健, 三谷烈史, 中嶋大, 松浦大介, 内堀幸夫, 北村尚
    NIRS-M (National Inst. of Radiological Sciences) (214) 213-215 2008年6月  
  • 高島健, 柳町朋樹, 平原聖文, 三谷烈史, 浅村和史, 海老原祐輔, 三好由純, 関華奈子, 小笠原桂一, 笠原慧
    搭載機器基礎開発実験経費・宇宙科学推進戦略的開発研究経費実績報告書 2006 70-73 2008年3月  
  • 榎戸輝揚, 三谷烈史, 中澤知洋, 牧島一夫, 坂野井健, 高島健, 吉田和哉, 高橋幸弘
    地球電磁気・地球惑星圏学会総会及び講演会予稿集(CD-ROM) 124th ROMBUNNO.B005-26 2008年  
  • 三谷 烈史
    遊・星・人 : 日本惑星科学会誌 16(3) 239-241 2007年9月25日  
  • 高島健, 三谷烈史, 小笠原圭一, 内堀幸夫, 北村尚
    NIRS-M (National Inst. of Radiological Sciences) (203) 222-223 2007年6月  
  • Takahashi, T., Abe, K., Endo, M., Endo, Y., Ezoe, Y., Fukazawa, Y., Hamaya, M., Hirakurl, S., Hong, S., Horii, M., Inoue, H., Isobe, N., Itoh, T., Iyomoto, N., Kamae, T., Kasama, D., Kataoka, J., Kato, H., Kawaharada, M., Kawano, N., Kawashima, K., Kawasoe, S., Klshishita, T., Kltaguchi, T., Kobayashi, Y., Kokubun, M., Kotoku, J., Kouda, M., Kubota, A., Kuroda, Y., Madejski, G., Makishima, K., Masukawa, K., Matsumoto, Y., Mitani, T., Miyawaki, R., Mizuno, T., Mori, K., Mori, M., Murashima, M., Murakami, T., Nakazawa, K., Niko, H., Nomachi, M., Okada, Y., Ohno, M., Oonuki, K., Ota, N., Ozawa, H., Sato, G., Shinoda, S., Sugiho, M., Suzuki, M., Taguchi, K., Takahashi, H., Takahashi, I., Takeda, S., Tamura, K.-I., Tamura, T., Tanaka, T., Tanihata, C., Tashiro, M., Terada, Y., Tominaga, S., Uchiyama, Y., Watanabe, S., Yamaoka, K., Yanagida, T., Yonetoku, D.
    Publications of the Astronomical Society of Japan 59(1 SPEC. ISS.) 2007年4月8日  
    The Hard X-ray Detector (HXD) on board Suzaku covers a wide energy range from 10keV to 600 keV by the combination of silicon PIN diodes and GSO scintillators. The HXD is designed to achieve an extremely low in-orbit background based on a combination of new techniques, including the concept of a well-type active shield counter. With an effective area of 142cm 2 at 20keV and 273cm 2 at 150keV, the background level at sea level reached ∼ 1 × 10 -5 cts s -1 cm -2 keV -1 at 30 keV for the PIN diodes, and ∼ 2 × 10 -5 cts s -1 cm -2 keV -1 at 100keV, and ∼ 7 × 10 -6 cts s -1 cm -2 keV -1 at 200keV for the phoswich counter. Tight active shielding of the HXD results in a large array of guard counters surrounding the main detector parts. These anti-coincidence counters, made of ∼ 4cm thick BGO crystals, have a large effective area for sub-MeV to MeV x-rays. They work as an excellent y-ray burst monitor with limited angular resolution (∼ 5°). The on-board signal-processing system and the data transmitted to the ground are also described. © 2007. Astronomical Society of Japan.
  • Kokubun, M., Makishima, K., Takahashi, T., Murakami, T., Tashiro, M., Fukazawa, Y., Kamae, T., Madejski, G.M., Nakazawa, K., Yamaoka, K., Terada, Y., Yonetoku, D., Watanabe, S., Tamagawa, T., Mizuno, T., Kubota, A., Isobe, N., Takahashi, I., Sato, G., Takahashi, H., Hong, S., Kawaharada, M., Kawano, N., Mitani, T., Murashima, M., Suzuki, M., Abe, K., Miyawaki, R., Ohno, M., Tanaka, T., Yanagida, T., Itoh, T., Ohnuki, K., Tamura, K.-I., Endo, Y., Hirakuri, S., Hiruta, T., Kitaguchi, T., Kishishita, T., Sugita, S., Takahashi, T., Takeda, S., Enoto, T., Hirasawa, A., Katsuta, J., Matsumura, S., Onda, K., Sato, M., Ushio, M., Ishikawa, S.-N., Murase, K., Odaka, H., Suzuki, M., Yaji, Y., Yamada, S., Yamasaki, T., Yuasa, T.
    Publications of the Astronomical Society of Japan 59(1 SPEC. ISS.) 2007年4月8日  
    The in-orbit performance and calibration of the Hard X-ray Detector (HXD) on board the X-ray astronomy satellite Suzaku are described. Its basic performances, including a wide energy bandpass of 10-600 keV, energy resolutions of ∼ 4 keV (FWHM) at 40 keV and ∼ 11% at 511 keV, and a high background rejection efficiency, have been confirmed by extensive in-orbit calibrations. The long-term gains of PIN-Si diodes have been stable within 1% for half a year, and those of scintillators have decreased by 5-20%. The residual non-X-ray background of the HXD is the lowest among past non-imaging hard X-ray instruments in energy ranges of 15-70 and 150-500 keV. We provide accurate calibrations of energy responses, angular responses, timing accuracy of the HXD, and relative normalizations to the X-ray CCD cameras using multiple observations of the Crab Nebula. © 2007. Astronomical Society of Japan.
  • 岡田達明, 三谷烈史, 澤井秀次郎, 水野貴秀, 福田盛介, 久保田孝
    日本惑星科学会秋季講演会予稿集 2007 134-134 2007年  
    比較的安価な小型月着陸実験機でピンポイントに月面の目標地点に着陸し，科学探査を行う小型ミッションを検討している．観測機器の重量制限，ミッション期間が最長で月の昼間に限定，月の表側のみに着陸可能など，制約は多い．しかし，単目的でも小回りの利く探査は，大型で高価な周回衛星や着陸機と相補的な役割を果たすことができ，さらに将来の惑星表面探査への技術ステップとしても重要性は高い．本研究では、小型月着陸機による探査構想とミッション候補の検討、搭載機器の可能性を検討した結果を報告する。
  • 岡田達明, 白井慶, 山本幸生, 荒井武彦, 小川和律, 白石浩章, 岩崎正統, 岩崎正統, 川村太一, 森戸久貴, 三谷烈史, 加藤学
    日本惑星科学会秋季講演会予稿集 2007 133-133 2007年  
    「かぐや（セレーネ）」搭載蛍光エックス線分光計（XRS）による月面元素分析手法の開発を進めている．本報告では、その手法の概要について紹介する．特に，われわれは月表面のラフネスによる蛍光X線強度への影響とその補正方法について検討してきている．ラフネスには２種類あり，X線吸収長程度の微小凹凸による影響と，より大きな地形的凹凸による影響がある．さらに，鉱物サイズが無視できないことによる効果も検討している．これらを定式化することが大量データで解析する上で重要であり，それらの検討を進めている．その現状についても紹介する．
  • 三谷烈史, 岡田達明, 高島健, 渡辺伸, 高橋忠幸
    日本惑星科学会秋季講演会予稿集 2007 132-132 2007年  
    月・惑星の起源や進化を解き明かす際、その元素組成・分布を明らかにすることは、最も基本的かつ重要な観測である。高精度ガンマ線分光計をローバーへ搭載することにより、細かな地形に応じた元素地図が取得できる。これを実現するために、我々は小型で高いエネルギー分解能を実現できるテルル化カドミウム半導体を用いたガンマ線検出器の開発を進めている。本発表では検出器の基礎的な特性と搭載機器の基礎設計について紹介する。
  • 三谷烈史, 高橋忠幸, 中澤知洋, 佐藤悟朗, 久保田あや, MARKWARDT Craig, TUELLER Jack, PARSONS Ann, BARTHELMY Scott, GEHRELS Neil
    日本天文学会年会講演予稿集 2006 61 2006年2月20日  
  • 斉藤孝男, 植野優, 片岡淳, 河合誠之, 高島健, 田中孝明, 三谷烈史, 高橋忠幸
    日本天文学会年会講演予稿集 2005 323 2005年8月20日  
  • 佐藤 悟朗, 高橋 忠幸, 中澤 知洋, 三谷 烈史, 田代 信, 鈴木 雅也, Gehrels Neil, Hullinger Derek, Parsons Ann, 坂本 貴紀, the Swift team
    日本物理学会講演概要集 60(2) 29-29 2005年8月19日  
  • 田代 信, 高橋 忠幸, 中澤 知洋, 佐藤 悟朗, 鈴木 雅也, 三谷 烈史, Gehrels Neil, the Swift team
    日本物理学会講演概要集 60(2) 29-29 2005年8月19日  
  • 大貫宏祐, 岸下徹一, 高橋忠幸, 武田伸一郎, 田中孝明, 中沢知洋, 三谷烈史, 渡辺伸
    応用物理学関係連合講演会講演予稿集 52nd(1) 161 2005年3月29日  
  • 武田 伸一郎, 田中 孝明, 三谷 烈史, 渡辺 伸, 大貫 宏祐, 中澤 知洋, 高橋 忠幸, 田島 宏康, 深沢 泰司, 澤本 直之
    日本物理学会講演概要集 60(1) 87-87 2005年3月4日  
  • 岸下徹一, 高橋忠幸, 田中孝明, 中澤知洋, 三谷烈史, 渡辺伸, 寺田幸功, 川原田円, 国分紀秀, 高橋勲, 二河久子, 宮脇良平
    日本天文学会年会講演予稿集 2005 251 2005年2月20日  
  • 寺田幸功, 渡辺伸, 尾崎正伸, 大野雅功, 鈴木雅也, 伊藤健, 内山泰伸, 久保信, 佐藤悟朗, 高橋勲, 川原田円, 村島未生, 宮脇良平, 柳田健之, 三谷烈史, 田中孝明, 川埜直美, 洪秀徴, 牧島一夫, 高橋忠幸, 村上敏夫, 田代信, 深沢泰司, 国分紀秀, 中澤知洋, 山岡和貴, 米徳大輔
    日本天文学会年会講演予稿集 2005 251 2005年2月20日  
  • Kousuke Oonuki, Takaaki Tanaka, Shin Watanabe, Shin'ichiro Takeda, Kazuhiro Nakazawa, Takefumi Mitani, Tadayuki Takahashi, Hiroyasu Tajima, Yasushi Fukazawa, Masaharu Nomachi
    Proceedings of SPIE - The International Society for Optical Engineering 5922 1-11 2005年  
    We have been developed Si/CdTe semiconductor Compton telescope to explore the universe in the energy band from several 10 keV to a few MeV. In our Si/CdTe Compton telescope, a stacked thin CdTe pixel detector is a key component to achieve higher detection efficiency for MeV gamma-rays maintaining high energy resolution. In this paper, results from a prototype stacked CdTe pixel detector are reported, which consists of three layers of CdTe pixel detectors and one CdTe pixel detector at their side. With this prototype detector, we succeeded in Compton reconstruction of images and spectra in the energy band from 122 keV to 662 keV. The energy resolution (FWHM) of reconstructed spectra is 7.3 keV at 511 keV and 3.1 keV at 122 keV, respectively.
  • Shin Watanabe, Takaaki Tanaka, Kazuhiro Nakazawa, Takefumi Mitani, Kousuke Oonuki, Tadayuki Takahashi, Takeshi Takashima, Hiroyasu Tajima, Yasushi Fukazawa, Masaharu Nomachi, Shin Kubo, Mitsunobu Onishi, Yoshikatsu Kuroda
    IEEE Nuclear Science Symposium Conference Record 7 4286-4290 2004年12月1日  
    We are developing a Compton camera based on Si and CdTe semiconductor imaging devices with high energy resolution. In this paper, results from the most recent prototype are reported. The Compton camera consists of six stacked double-sided Si Strip detectors and CdTe pixel detectors, which are read out with low noise analog ASICs, VA32TAs. We obtained Compton reconstructed images and spectra of line gamma-rays from 80 keV to 662 keV. The energy resolution (FWHM) is 10 keV and 16 keV at 356 keV and 511 keV, respectively. © 2004 IEEE.
  • Ryohei Miyawaki, Hisako Niko, Yuu Okada, Motohide Kokubun, Kazuo Makishima, Hitoshi Negoro, Jun'ichi Kotoku, Yukikatsu Terada, Takaaki Tanaka, Takefumi Mitani, Kazuhiro Nakazawa, Tadayuki Takahashi, Ryoichi Ohno, Minoru Funaki, Yoshikatsu Kuroda, Kei Genba, Mitsunobu Onishi
    IEEE Nuclear Science Symposium Conference Record 7 4392-4396 2004年12月1日  
    Employing Fourier-synthesis optics and one-dimensional position-sensitive detectors, we are developing a novel hard X-ray imager which can work in the ∼10 keV to ∼200 keV range either as a telescope or a microscope. As the detection part of our imager, we have developed a strip detector made of Schottky CdTe diode, with its cathode divided into 64 channels of 150 μm pitch. Electrodes of all channels are gold-stud bonded to a fanout board, and connected to low noise analog ASIC. We read out signals from all channels simultaneously. As the grid optics elements, one-dimensional modulation collimator grids of 1 mm thick tungsten have been manufactured, with 10 grid pitches ranging from 0.2 mm to 2 mm with harmonic ratios. Combining the CdTe strip detector and the modulation collimators, we have verified hard X-ray imaging performance of this system. Specifically, by observing an241Am source, we have successfully obtained an image in the 10-70 keV range. © 2004 IEEE.
  • H. Tajima, T. Kamae, G. Madejski, T. Mitani, K. Nakazawa, T. Tanaka, T. Takahashi, S. Watanabe, Y. Fukazawa, T. Ikagawa, J. Kataoka, M. Kokubun, K. Makishima, Y. Terada, M. Nomachi, M. Tashiro
    IEEE Nuclear Science Symposium Conference Record 1 314-321 2004年12月1日  
    The Soft Gamma-ray Detector (SGD) on board NeXT (Japanese future high energy astrophysics mission) is a Compton telescope with narrow field of view (FOV), which utilizes Compton kinematics to enhance its background rejection capabilities. It is realized as a hybrid semiconductor gamma-ray detector which consists of silicon and CdTe (Cadmium Telluride) detectors. It can detect photons in a wide energy band (0.05-1 MeV) at a background level of 5 × 10-7counts/s/cm2/keV; the silicon layers are required to improve the performance at a lower energy band (<0.3 MeV). Excellent energy resolution is the key feature of the SGD, allowing to achieve both high angular resolution and good background rejection capability. An additional capability of the SGD, its ability to measure gamma-ray polarization opens up a new window to study properties of astronomical objects. We will present the development of key technologies to realize the SGD; high quality CdTe, low noise front-end ASIC and bump bonding tecnology. Energy resolutions of 1.7 keV (FWHM) for CdTe pixel detectors and 1.1 keV for Si strip detectors have been measured. We also present the validation of MC simulation used to evaluate the performance of the SGD. © 2004 IEEE.
  • 村島未生, 川原田円, 国分紀秀, 岡田祐, 牧島一夫, 井上北斗, 小林謙仁, 三谷烈史, 中沢知洋, 高橋忠幸, HONG Soojing, 寺田幸功, 宮坂浩正, 山岡和貴, 川添哲志
    宇宙航空研究開発機構研究開発報告 JAXA-RR- (04-004) 26P 2004年12月1日  
  • M Kokubun, K Abe, Y Ezoe, Y Fukazawa, S Hong, H Inoue, T Itoh, T Kamae, D Kasama, M Kawaharada, N Kawano, K Kawashima, S Kawasoe, Y Kobayashi, J Kotoku, M Kouda, A Kubota, GM Madejski, K Makishima, T Mitani, H Miyasaka, R Miyawaki, K Mori, M Mori, T Murakami, MM Murashima, K Nakazawa, H Niko, M Nomachi, M Ohno, Y Okada, K Oonuki, G Sato, M Suzuki, H Takahashi, Takahashi, I, T Takahashi, K Tamura, T Tanaka, M Tashiro, Y Terada, S Tominaga, S Watanabe, K Yamaoka, T Yanagida, D Yonetoku
    IEEE TRANSACTIONS ON NUCLEAR SCIENCE 51(5) 1991-1996 2004年10月  
    We summarize significant improvements which have been achived in the development of Astro-E2 Hard X-ray Detector (HXD-II). An expanded energy range and better energy resolution have been achieved from progresses in device materials and redesigning of the front-end electronics. An improved estimation for the detector background in orbit has also been conducted based upon results from our proton irradiation experiment. The sensitivity of HXD-II can be expected to reach an order of 10(-6) [c s(-1) keV(-1) cm(-2)].
  • T Takashima, T Mitani, K Nakazawa, H Tajima, T Takahashi, T Tanaka, S Uno, Y Uchihori, H Kitamura
    IEEE TRANSACTIONS ON NUCLEAR SCIENCE 51(5) 2004-2007 2004年10月  
    We are developing a medium energy particle detector in a high-count rate environment, in order to solve the acceleration mechanism and the process of high-energy particles in the collision less plasma shock region in the space. The key observation is to measure the maximum energy of accelerated particles correctly. It is important to reduce the pile-up events, in order to measure the correct maximum energy. The new developed detector for the high-count rate environment consists of the double-sided silicon strip detector (DSSD) and the readout Application Specific Integrated Circuit (ASIC) chips VA32TA, made by IDEA. The performance of the new DSSD system for charged particles was tested using proton beams with an energy of 6 MeV from the medium-energy accelerator in the Heavy Ion Medical Accelerator in Chiba (HIMAC) of the National Institute for Radiological Science. The result is that the new DSSD system works well and has high performance in detecting not only X-rays, but also charged particles. It is certain that this new DSSD system can measure the correct energy of incident particles in high-count rate environments using the accelerator.
  • 大貫 宏祐, 田中 孝明, 三谷 烈史, 渡辺 伸, 岸下 徹一, 武田 伸一郎, 中澤 知洋, 高橋 忠幸
    日本物理学会講演概要集 59(2) 63-63 2004年8月25日  
  • 澤本 直之, 中本 達也, 深沢 泰司, 大杉 節, 田島 宏康, 田中 孝明, 三谷 烈史, 渡辺 伸, 中澤 知洋, 高橋 忠幸, 大山 博史
    日本物理学会講演概要集 59(2) 75-75 2004年8月25日  
  • 田中 孝明, 渡辺 伸, 三谷 烈史, 大貫 宏祐, 中澤 知洋, 高橋 忠幸, 田島 宏康, 澤本 直之, 深沢 泰司, 中村 秀仁, 能町 正治
    日本物理学会講演概要集 59(2) 75-75 2004年8月25日  
  • 中澤 知洋, 高橋 忠幸, 渡辺 伸, 佐藤 悟朗, 三谷 烈史, 田中 孝明, 大貫 宏祐, 田村 健一, 岸下 徹一, 武田 伸一郎, 蛭田 達郎
    日本物理学会講演概要集 59(2) 75-75 2004年8月25日  
  • 中本 達也, 深沢 泰司, 澤本 直之, 三谷 烈史, 田中 孝明, 田島 宏康, 高橋 忠幸, 中澤 和洋
    日本物理学会講演概要集 59(1) 89-89 2004年3月3日  
  • 川原田 円, 村島 未生, 伊藤 健, 二河 久子, 宮脇 良平, 柳田 健之, 国分 紀秀, 牧島 一夫, 三谷 烈史, 田中 孝明, 大貫 宏佑, 田村 健一, 中澤 知洋, 高橋 忠幸, 川埜 直美, 河嶋 健吾, 深沢 泰司, 鈴木 雅也, 阿部 圭一, 田代 信
    日本物理学会講演概要集 59(1) 89-89 2004年3月3日  
  • 田中 孝明, 三谷 烈史, 中澤 知洋, 大貫 宏祐, 佐藤 悟朗, 高橋 忠幸, 渡辺 伸, 田島 宏康, 中村 秀仁, 能町 正治, 中本 達也, 深沢 泰司
    日本物理学会講演概要集 59(1) 90-90 2004年3月3日  
  • 宮脇 良平, 二河 久子, 岡田 祐, 古徳 純一, 国分 紀秀, 牧島 一夫, 田中 孝明, 三谷 烈史, 中澤 知洋, 高橋 忠幸, 根来 均, 寺田 幸功
    日本物理学会講演概要集 59(1) 89-89 2004年3月3日  
  • 中沢知洋, 高橋忠幸, 渡辺伸, 佐藤悟朗, 小林謙仁, 三谷烈史, 井上北斗, 田中孝明, 大貫宏祐
    UTNL-R(東京大学大学院工学系研究科附属原子力工学研究施設) (0433) 11-12 2004年2月2日  
  • 三谷 烈史, 大貫 宏裕, 小林 謙仁
    宇宙科学シンポジウム 4 617-620 2004年1月8日  
  • K Oonuki, H Inoue, K Nakazawa, T Mitani, T Tanaka, T Takahashi, CMH Chen, WR Cook, FA Harrison
    HIGH-ENERGY DETECTORS IN ASTRONOMY 5501 218-228 2004年  
    We have developed a large CdTe pixel detector with dimensions of 23.7 x 13.0 mm(2) and a pixel size of 448 x 448 mum(2). The detector is based on recent technologies of an uniform CdTe single crystal, a two-dimensional ASIC, and stud bump-bonding to connect pixel electrodes on the CdTe surface to the ASIC. Good spectra are obtained from 1051 pixels out of total 1056 pixels. When we operate the detector at -50degreesC, the energy resolution is 0.67 keV and 0.99 keV at 14 keV and 60 keV, respectively. Week-long stability of the detector is confirmed at operating temperatures of both -50degreesC and -20degreesC. The detector also shows high uniformity: the peak positions for all pixels agree to within 0.82%, and the average of the energy resolution is 1.04 keV at a temperature of -50degreesC. When we normalized the peak area by the total counts detected by each pixel, a variation of 2.1% is obtained.
  • M Kawaharada, SJ Hong, MM Murashima, M Kokubun, T Itoh, K Makishima, R Miyawaki, H Niko, T Yanagida, T Mitani, K Nakazawa, K Oonuki, T Takahashi, KI Tamura, T Tanaka, Y Terada, Y Fukazawa, N Kawano, K Kawashima, M Ohno, K Yamaoka, K Abe, M Suzuki, M Tashiro, D Yonetoku, T Murakami
    HIGH-ENERGY DETECTORS IN ASTRONOMY 5501 286-295 2004年  
    The Hard X-ray Detector (HXD-II), one of instruments onboard the Astro-E2 satellite to be launched in February 2005, is in the final stage of its development. The HXD-II probes the universe in the energy range of 10-600 keV with a sensitivity by an order of magnitude better than those of previous missions. The assembly of the HXD-II completed in January 2004, followed by a series of pre-launch qualification tests. As a result, the design goals of the HXD-II have been met. These include; a background level of 5x10(-6) counts/s/keV/cm(2) at 200 keV for GSO and 1x10(-5) counts/s/keV/cm(2) at 30 keV for PIN; energy resolutions of 2.9 keV (PIN diode, at 59.5 keV) and 10% (GSO scintillator, at 662 keV); and low energy thresholds of 10 keV for PIN diodes and 30 keV for GSO scintillators. The measured background predicts a continuum sensitivity of a few x10(-6) photons/s/keV/cm(2). Anti-Counter units surrounding the HXD-II provide 50 keV-5 MeV information on gamma-ray bursts and bright X-ray transients.
  • T Tanaka, T Mitani, S Watanabe, K Nakazawa, K Oonuki, G Sato, T Takahashi, KI Tamura, H Tajima, H Nakamura, M Nomachi, T Nakamoto, Y Fukazawa
    HIGH-ENERGY DETECTORS IN ASTRONOMY 5501 229-240 2004年  
    We are developing a Compton telescope based on high resolution Si and CdTe imaging devices in order to obtain a high sensitivity astrophysical observation in sub-MeV gamma-ray region. In this paper, recent results from the prototype Si/CdTe semiconductor Compton telescope are reported. The Compton telescope consists of a double-sided Si strip detector (DSSD) and CdTe pixel detectors, combined with low noise analog LSI, VA32TA. With this detector, we obtained Compton reconstructed images and spectra from line gamma-rays ranging from 81 keV up to 356 keV. The energy resolution is 3.8 keV and 7.9 keV at 122 keV and 356 keV, respectively, and the angular resolution is 9.9degrees and 5.7degrees at 122 keV and 356 keV, respectively.
  • Y Fukazawa, T Nakamoto, N Sawamoto, S Uno, T Ohsugi, H Tajima, T Takahashi, T Mitani, T Tanaka, K Nakazawa
    HIGH-ENERGY DETECTORS IN ASTRONOMY 5501 197-207 2004年  
    A Semiconductor Multiple-Compton Telescope (SMCT) is expected to proceed a high-sensitivity soft gamma-ray observation in the energy range of 0.1-20 MeV. Double-sided silicon strip detector (DSSD) is one of key technologies for constructing SMCT, as well as the high-stopping semiconductor CdTe, because of its high energy resolution and high scattering efficiency. We have developed a low-noise system of DSSD and frontend LSI for SMCT, by optimizing geometrical structures of DSSD. We have thus obtained an energy resolution of 1.3 keV (FWHM) for 60 keV and 122 keV at -10degreesC in the multi-channel reading. Gamma-ray responses such as image flatness and charge splittings were found to be not problematic. We also demonstrated that our system achieved the good angular resolution close to the Doppler-broadening limit in the Compton imaging by two DSSDs.
  • H Tajima, G Madejski, T Mitani, T Tanaka, H Nakamura, K Nakazawa, T Takahashi, Y Fukazawa, T Kamae, M Kokubun, D Marlow, M Nomachi, EDE Silva
    UV AND GAMMA-RAY SPACE TELESCOPE SYSTEMS, PTS 1 AND 2 5488 561-571 2004年  
    Compton telescope is a promising technology to achieve very high sensitivity in the soft gamma-ray band (0.1-10 MeV) by utilizing Compton kinematics. Compton kinematics also enables polarization measurement which will open new windows to study gamma-ray production mechanism in the universe. CdTe and Si semiconductor technologies are key technologies to realize the Compton telescope in which their high energy resolution is crucial for high angular resolution and back-round rejection capability. We have assembled a prototype module using a double-sided silicon strip detector and CdTe pixel detectors. In this paper, we present expected polarization performance of a proposed mission (NeXT/SGD). We also report results from polarization measurements using polarized synchrotron light and validation of EGS4 MC simulation.
  • 大貫宏祐, 井上北斗, 高橋忠幸, 田中孝明, 田村健一, 三谷烈史, 中澤知洋, CHEN Hubert, COOK Walter, HARRISON Fiona
    日本天文学会年会講演予稿集 2004 262 2004年  
  • 村島未生, 川原田円, 二河久子, 宮脇良平, 高橋勲, 国分紀秀, 牧島一夫, 三谷烈史, 渡辺伸, 中澤知洋, 川埜直美, 鈴木雅也, 田代信, 寺田幸功
    日本天文学会年会講演予稿集 2004 248 2004年  
  • 五十川知子, 片岡淳, 斎藤孝男, 谷津陽一, 倉本祐輔, 河合誠之, 深沢泰司, 高橋忠幸, 三谷烈史, 石川嘉隆
    日本天文学会年会講演予稿集 2004 260 2004年  
  • 三谷烈史, 武田伸一郎, 岸下徹一, 大貫宏祐, 田中孝明, 佐藤悟朗, 渡辺伸, 中澤知洋, 高橋忠幸
    日本天文学会年会講演予稿集 2004 262 2004年  

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