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  2. 前田 良知

前田 良知

マエダ ヨシトモ  (Yoshitomo Maeda)

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 助教
総合研究大学院大学 宇宙観測科学講座 飛翔体天文学分野 助教
学位
博士(理学)(1998年3月 京都大学)
修士(理学)(1995年3月 京都大学)
研究者番号
80342624
ORCID ID
 https://orcid.org/0000-0002-9099-5755
J-GLOBAL ID
202001011170717781
researchmap会員ID
R000011919

論文

 222
  • Yohko Tsuboi, Koichiro Akasu, Noboru Nemoto, Tomokage Yoneyama, Marina Yoshimoto, Kotaro Fukushima, Katsuhiro Hayashi, Yoshiaki Kanemaru, Shoji Ogawa, Tessei Yoshida, Marc Audard, Ehud Behar, Shun Inoue, Yuiko Ishihara, Takayoshi Komura, Yoshitomo Maeda, Misaki Mizumoto, Masayoshi Nobukawa, Katja Pottschmidt, Megumi Shidatsu, Yukikatsu Terada, Yuichi Terashima, Hiroyuki Uchida
    Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray 236-236 2024年8月21日  
  • Yoshiaki Kanemaru, Ryo Iizuka, Yoshitomo Maeda, Takashi Okajima, Takayuki Hayashi, Kazuhiro Kiyokane, Yuto Nihei, Takashi Kominato, Manabu Ishida, Chikara Natsukari, Shin Watanabe, Kosuke Sato, Yukikatsu Terada, Katsuhiro Hayashi, Chris Baluta, Tessei Yoshida, Akio Hoshino, Shoji Ogawa, Kotaro Fukushima, Hiromitsu Takahashi, Masayoshi Nobukawa, Tsunefumi Mizuno, Kazuhiro Nakazawa, Shin'ichiro Uno, Ken Ebisawa, Satoshi Eguchi, Satoru Katsuda, Aya Kubota, Naomi Ota, Megumi Shidatsu, Atsushi Tanimoto, Yuichi Terashima, Yohko Tsuboi, Yuusuke Uchida, Hideki Uchiyama, Shigeo Yamauchi, Yoneyama Tomokage, Satoshi Yamada, Nagomi Uchida, Rie Sato, Matt Holland, Michael Loewenstein, Eric D. Miller, Tahir Yaqoob, Robert S. Hill, Trisha F. Doyle, Efrain Perez-Solis, Morgan D. Waddy, Mark Mekosh, Joseph B. Fox, Makoto S. Tashiro, Kenichi Toda, Hironori Maejima
    Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray 224-224 2024年8月21日  
  • Keisuke Tamura, Takayuki Hayashi, Rozenn Boissay-Malaquin, Takashi Okajima, Toshiki Sato, Megan E. Eckart, Maurice A. Leutenegger, Tahir Yaqoob, Koji Mori, Manabu Ishida, Yoshitomo Maeda, Hiroshi Tomida, Hiroshi Nakajima, Hirofumi Noda, Hiroyuki Uchida, Hiromasa Suzuki, Shogo B. Kobayashi, Tomokage Yoneyama, Kouichi Hagino, Kumiko K. Nobukawa, Takaaki Tanaka, Hiroshi Murakami, Hideki Uchiyama, Masayoshi Nobukawa, Tessei Yoshida, Hironori Matsumoto, Takeshi Go Tsuru, Makoto Yamauchi, Isamu Hatsukade, Hirokazu Odaka, Takayoshi Kohmura, Kazutaka Yamaoka, Yoshiaki Kanemaru, Junko S. Hiraga, Tadayasu Dotani, Masanobu Ozaki, Hiroshi Tsunemi, Keitaro Miyazaki, Kohei Kusunoki, Yoshinori Otsuka, Haruhiko Yokosu, Wakana Yonematsu, Kazuhiro Ichikawa, Hanako Nakano, Reo Takemoto, Tsukasa Matsushima, Yoh Asahina, Masahiro Fukuda, Marina Yoshimoto, Kohei Shima, Mio Aoyagi, Yuma Aoki, Yamato Ito, Daiki Aoki, Kaito Fujisawa, Yasuyuki Shimizu, Mayu Higuchi, Kiyoshi Hayashida, Aurora Simionescud, Eric Miller, Laura Brenneman
    Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray 59-59 2024年8月21日  
  • M. Aoyagi, R.G. Bose, S. Chun, E. Gau, K. Hu, K. Ishiwata, N.K. Iyer, F. Kislat, M. Kiss, K. Klepper, H. Krawczynski, L. Lisalda, Y. Maeda, F. af Malmborg, H. Matsumoto, A. Miyamoto, T. Miyazawa, M. Pearce, B.F. Rauch, N. Rodriguez Cavero, S. Spooner, H. Takahashi, Y. Uchida, A.T. West, K. Wimalasena, M. Yoshimoto
    Astroparticle Physics 158 102944-102944 2024年6月  査読有り
  • Mikio Morii, Yoshitomo Maeda, Hisamitsu Awaki, Kouichi Hagino, Manabu Ishida, Koji Mori
    Publications of the Astronomical Society of Japan 2024年2月9日  査読有り
    Abstract We develop a new deconvolution method to recover the precise Crab Nebula image taken by the Hitomi HXT, suppressing the artifact due to the bright Crab pulsar. We extend the Richardson–Lucy method, introducing two components corresponding to the nebula and pulsar with regularization for smoothness and flux, respectively, and performing simultaneous deconvolution of multi-pulse-phase images. The structures, including the torus and jets, seen in the deconvolved nebula image at the lowest energy band of 3.6–15 keV appear consistent with those identified in the high-resolution Chandra X-ray image. Above 15 keV, we confirm NuSTAR’s findings that the nebula size decreases in higher energy bands. We find that the north-east side of the nebula is fainter in higher energy bands. Our deconvolution method is applicable for any telescope images of faint diffuse objects containing a bright point source.
もっとみる

MISC

 37
  • 高橋, 弘充, ABARR, Quin, 青柳, 美緒, 朝倉, 一統, 粟木, 久光, BARING, Matthew, BOSE, Richard, BRAUN, Dana, DE, GERONIMO Gianluigi, DOWKNOTT, Paul, ELLIOT, John, 榎戸, 輝揚, ERRAND, Manel, 深沢, 泰司, 古澤, 彰浩, GADSON, Thomas, GAU, Epharaim, GUARINO, Victor, 郡司, 修一, 袴田, 知宏, 萩原, 涼太, HALL, Kenny, 花岡, 真帆, HARMON, Keon, 服部, 兼吾, 林田, 清, HEATWOLE, Scott, HOSSEN, Arman, 井出, 峻太郎, 今村, 竜太, 今里, 郁弥, 今澤, 遼, 石橋, 和紀, 石田, 学, 石倉, 彩美, 石渡, 幸太, IYER, Nirmal Kumar, KISLAT, Fabian, MOZSI, Kiss, 亀谷, 紀香, 鴨川, 航, 北口, 貴雄, KOTSIFAKIS, David, KRAWCZYNSK, Henric, LANZI, James, LISALDA, Lindsey, 前田, 良知, 松下, 友亮, 眞武, 寛人, 松本, 浩典, 峯田, 大晴, 宮本, 明日香, 宮澤, 拓也, 水野, 恒史, 中庭, 望, 野田, 博文, 大出, 優一, 岡島, 崇, 岡崎, 貴樹, PASTRANI, Izabella, PEARCE, Mark, PETERSON, Zachary, PUDY, Chris, RAUCH, Brian, RYDE, Felix, 斎藤, 芳隆, 佐久間, 翔太郎, 佐藤, 淳矢, 澤上, 拳明, SHREEVES, Chris, SIMBURGER, Garry, SNOW, Carl, SPOONER, Sean, STANA, Theodor-Adrian, STUCHLIK, David, 鈴木, 瞳, 武尾, 舞, 玉川, 徹, 田村, 啓輔, 常深, 博, 内田, 和海, 内田, 悠介, VINCENT, Brett, WEST, Andrew, WULF, Eric, 米山, 友景, 善本, 真梨那, TAKAHASHI, Hiromitsu, AOYAGI, Mio, ASAKURA, Kazunori, AWAKI, Hisamitsu, ENOTO, Teruaki, FUKAZAWA, Yasushi, FURUZAWA, Akihiro, GUNJI, Shuichi, HAKAMADA, Tomohiro, HAGIWARA, Ryota, HANAOKA, Maho, HATTORI, Kengo, HAYASHIDA, Kiyoshi, IDE, Shuntaro, IMAMURA, Ryuta, IMAZATO, Fumiya, IMAZAWA, Ryo, ISHIBASHI, Kazunori, ISHIDA, Manabu, ISHIKURA, Ayami, ISHIWATARI, Kota, MOZI, Kiss, KAMETANI, Norika, KAMOGAWA, Wataru, KITAGUCHI, Takao, KOTSUIFAKIS, David, KRAWCZYNSKI, Henric, MAEDA, Yoshitomo, MATSUSHITA, Yusuke, MATAKE, Hiroto, MATSUMOTO, Hironori, MINETA, Taisei, MIYAMOTO, Asuka, MIYAZAWA, Takuya, MIZUNO, Tsunefumi, NAKANIWA, Nozomi, NODA, Hirofumi, ODE, Yuichi, OKAJIMA, Takashi, OKAZAKI, Kouki, PURDY, Chris, RAUNCH, Brian, SAITO, Yoshitaka, SAKUMA, Shotaro, SATO, Junya, SAWAGAMI, Kenmei, SUZUKI, Hitomi, TAKEO, Mai, TAMAGAWA, Toru, TAMURA, Keisuke, TSUNEMI, Hiroshi, UCHIDA, Nagomi, UCHIDA, Yuusuke, YONEYAMA, Tomokage, YOSHIMOTO, Marina
    大気球シンポジウム: 2022年度 = Balloon Symposium: 2022 2022年11月  
    大気球シンポジウム 2022年度（2022年11月7-8日. ハイブリッド開催（JAXA相模原キャンパス& オンライン)) Balloon Symposium 2022 (November 7-8, 2022. Hybrid(in-person & online) Conference (Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS)), Sagamihara, Kanagawa Japan 著者人数: 87名 資料番号: SA6000177030 レポート番号: isas22-sbs-030
  • 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  
  • 野田博文, 林田清, 林田清, 冨田洋, 森浩二, 森浩二, 田中孝明, 内田裕之, 鶴剛, 中嶋大, 松本浩典, 岡島崇, 石田学, 前田良知, 村上弘志, 山内誠, 廿日出勇, 信川正順, 信川久実子, 幸村孝由, 萩野浩一, 小林翔悟, 平賀純子, 内山秀樹, 山岡和貴, 尾崎正伸, 堂谷忠靖, 常深博
    日本物理学会講演概要集(CD-ROM) 75(1) 2020年  
  • 佐藤浩介, 内田悠介, 大橋隆哉, 石崎欣尚, 江副祐一郎, 山田真也, 山崎典子, 中島裕貴, 満田和久, 石田学, 前田良知, 三石郁之, 田原譲, 藤本龍一, 鶴剛, 太田直美, 大里健, 中島真也, 藤田裕, 永井大輔, 吉川耕司, 河合誠之, 松下恭子, 一戸悠人
    日本天文学会年会講演予稿集 2020 2020年  
  • 信川正順, 山内茂雄, 内山秀樹, 信川久実子, 村上弘志, 鶴剛, 前田良知, 野田博文
    日本天文学会年会講演予稿集 2020 2020年  
  • 松本浩典, 山崎典子, 満田和久, 篠崎慶亮, 前田良知, 粟木久光, 坪井陽子, 江副祐一郎, 山口弘悦, 佐藤浩介, 中嶋大, 深沢泰司, 大橋隆哉, 上田佳宏, 寺島雄一, 太田直美, 馬場彩, 海老沢研, 寺田幸功, 鶴剛, 常深博
    日本天文学会年会講演予稿集 2020 2020年  
  • 佐藤浩介, 大橋隆哉, 石橋欣尚, 江副祐一郎, 藤田裕, 山崎典子, 石田学, 前田良知, 満田和久, 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 2020 2020年  
  • 野田博文, 林田清, 林田清, 冨田洋, 森浩二, 森浩二, 田中孝明, 内田裕之, 鶴剛, 中嶋大, 松本浩典, 岡島崇, 吉田鉄生, 石田学, 前田良知, 村上弘志, 山内誠, 廿日出勇, 信川正順, 信川久実子, 幸村孝由, 萩野浩一, 小林翔悟, 平賀純子, 内山秀樹, 山岡和貴, 尾崎正伸, 堂谷忠靖, 常深博
    日本物理学会講演概要集(CD-ROM) 75(2) 2020年  
  • 田中孝明, 林田清, 冨田洋, 森浩二, 内田裕之, 鶴剛, 中嶋大, 野田博文, 松本浩典, 岡島崇, 石田学, 前田良知, 村上弘志, 山内誠, 廿日出勇, 信川正順, 信川久実子, 幸村孝由, 萩野浩一, 小林翔悟, 平賀純子, 内山秀樹, 山岡和貴, 尾崎正伸, 堂谷忠靖, 常深博
    日本物理学会講演概要集(CD-ROM) 74(1) 2019年  
  • 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, 中島裕貴, 満田和久, 石田学, 前田良知, 三石郁之, 田原譲, 藤本龍一, 鶴剛, 太田直美, 大里健, 中島真也, 藤田裕, 永井大輔, 吉川耕司, 河合誠之
    日本天文学会年会講演予稿集 2019 2019年  
  • 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, 藤田裕, 永井大輔, 吉川耕司, 河合誠之
    日本天文学会年会講演予稿集 2019 2019年  
  • 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 2018年  
  • 一戸悠人, 飯塚亮, 井上翔太, 上田周太朗, 太田直美, 北山哲, 佐藤浩介, 田中桂悟, 田村隆幸, 辻本匡弘, 藤本龍一, 前田良知
    日本天文学会年会講演予稿集 2017 2017年  
  • 上田周太朗, 飯塚亮, 一戸悠人, 井上翔太, 太田直美, 北山哲, 佐藤浩介, 田中桂悟, 田村隆幸, 辻本匡弘, 藤本龍一, 前田良知
    日本天文学会年会講演予稿集 2017 2017年  
  • 石村 康生, 仙場 淳彦, 秋田 剛, 鳥阪 綾子, 田中 宏明, 山川 宏, 宮下 朋之, 河野 太郎, 馬場 満久, 小川 博之, 岡崎 峻, 後藤 健, 嶋田 岳史, 旗持 天, 村田 泰宏, 前田 良知, 石田 学, 岩田 直子, 柴野 靖子, 高精度伸展式光学架台の研究開発メンバー, Ishimura Kosei, Senba Atsuko, Akita Tsuyoshi, Torisaka Ayako, Tanaka. Hiroaki, Yamakawa Hiroshi, Miyashita Tomoyuki, Kawano Taro, Baba Mitsuhisa, Ogawa Hiroyuki, Okazaki Shun, Goto Ken, Shimada Takeshi, Murata Yasuhiro, Maeda Yoshitomo, Ishida Manabu, Iwata Naoko, Shibano Yasuko, R&D member of Precise Extensible Optical Bench
    第32回宇宙構造・材料シンポジウム：講演集録 = Proceedings of 32nd Symposium on Aerospace Structure and Materials 2016年12月  
    第32回宇宙構造・材料シンポジウム（2016年12月9日. 宇宙航空研究開発機構宇宙科学研究所 (JAXA)(ISAS)), 相模原市, 神奈川県資料番号: SA6000087012レポート番号: A11
  • 飯塚 亮, 石田 学, 前田 良知
    宇宙科学技術連合講演会講演集 57 5p 2013年10月9日  
  • Yoshitomo Maeda, Tadayuki Takahashi, Kazuhisa Mitsuda, Richard Kelley
    Acta Polytechnica 53(1) 803-806 2013年  
    A review of the Astro-H mission is presented here on behalf of the Astro-H collaboration. 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). One of the main uniquenesses of the ASTRO-H satellite is the high sensitivity and imaging capability of the wide energy band from 0.3 keV to 600 keV. The coverage is achieved by combining the four instruments of the SXS, SXI, HXI, and SGD. The other main uniqueness is a spectroscopic capability not only for a point-like source but also for an extended source with high spectral resolution of ΔE~4÷7eV of SXS. Using the unique powers of these instruments, ASTRO-H will address unresolved issues in high-energy astrophysics. © Czech Technical University in Prague, 2013.
  • 吉村 昂泰, 高坂 達郎, 粟木 久光, 黄木 景二, 石田 学, 前田 良知, 古澤 彰浩, 宮澤 拓也, 山根 伸幸, 加藤 大佳, 国枝 秀世
    Dynamics & Design Conference 2011 "706-1"-"706-8" 2011年9月5日  
    In the present paper, vibration properties of mirror foils installed in a hard X-ray telescope (HXT) on-board a satellite were investigated. Vibration tests and FEM analysis of mirror foils installed in the part model of HXT were conducted. From the experimental results, it appeared that the mirror had resonant frequencies at 64, 73 and 11 OHz. The modal shapes of 64 and 73Hz showed that the maximum amplitude appeared at edges of the foil. On the other hand, vibration amplitude became maximum at the center in the modal shape of 11 OHz. Experimental results of frequency responses of these modes agreed well with analytical results except around 64Hz. It is considered that the resonant mode of 64Hz was strongly affected by nonlinear characteristics of friction constraint between the foils and HXT housing.
  • V. A. Dogiel, V. A. Dogiel, K. S. Cheng, D. O. Chernyshoy, V. Tatisoheff, C. M. Ko, W. H. Ip, M. Kokubun, Y. Maeda, K. Mitsuda
    Journal of the Physical Society of Japan 78 133-137 2009年6月16日  
    We assume that the energy source in the Galactic Center is the black hole Sgr A, which becomes active when a star is captured in a rate of ∼ 10-5yr-1. During the active phase relativistic protons with a characteristic energy ∼ 6 x 1052erg per capture are ejected. We suppose that the annihilation of secondary positrons produced by proton-proton collisions is observed as the 511 keV line flux from the Galactic bulge. Though these positron are generated with relatively high energies (> 30 MeV), our model satisfy the criterion derived by Beacom and Yiiksel based on the COMPTEL data in the range 1-30 MeV. From our estimations it follows also that a flux of gamma-ray de-excitation lines ∼ 2.5 x 10-5 ph cm-2 s-1 in the range below 8 MeV is produced by the relativistic protons in the Galactic center. A specific line is the one at 1.809 MeV from radioactivity of 26 Al. The predicted quasi-stationary flux of the 26Al 1.809 MeV line from the 1° x 1 central region is < 10-6 ph cm-2 s-1. We conclude also the the thermal 6.5 keV X-ray flux and the non-thermal hard X-ray flux in the range 14-40 keV observed by SUZAKU is emitted by subrelativistic protons produced by accretion processes. © 2009 The Physical Society of Japan.
  • I. Mitsuishi, Y. Ezoe, M. Koshiishi, M. Mita, Y. Maeda, N. Y. Yamasaki, K. Mitsuda, T. Shirata, T. Hayashi, T. Takano, R. Maeda
    2008 IEEE/LEOS INTERNATIONAL CONFERENCE ON OPTICAL MEMS AND NANOPHOTONICS 104-105 2008年  査読有り
    X-ray reflectivity of an ultra light-weight X-ray optic using MEMS technologies was measured in two different energies (0.28 keV and 1.49 keV). The obtained reflectivities can be understood by considering the mirror surface structures.
  • 輿石 真樹, 江副 祐一郎, 三田 信, 前田 良知, 満田 和久, 大澤 武幸, 鈴木 真樹, 星野 晶夫, 石崎 欣尚, 高野 貴之, 前田 龍太郎
    日本物理学会講演概要集 62(2) 116-116 2007年8月21日  
  • Mori Hideyuki, Iizuka Ryo, Shibata Ryo, HABA Yoshito, HAYAKAWA Akira, HAYASHI Atsushi, INOUE Chiaki, INOUE Hirohiko, ISHIDA Manabu, ITOH Akiharu, ITOH Kei, KUNIEDA Hideyo, MAEDA Yoshitomo, MISAKI Kazutami, NAITOU Masataka, OKADA Shunsaku, SHIMIZU Tomoo, YOKOYAMA Yushi
    PASJ : publications of the Astronomical Society of Japan 57(1) 245-257 2005年2月25日  
  • K Ebisawa, Beckmann, V, TJL Courvoisier, P Dubath, H Kaneda, Y Maeda, S Yamauchi, E Nishihara
    ASTRONOMISCHE NACHRICHTEN 324(1-2) 158-158 2003年  
    We have carried out a deep X-ray observation on a typical Galactic plane<br /> region with the Chandra ACIS-I instrument with unprecedented sensitivity and<br /> spatial resolution, and detected 274 unidentified X-ray point sources in the<br /> \~500 arcmin2 region. In order to identify these new X-ray sources, we have<br /> carried out a near infrared follow-up observation using ESO/NTT infrared camera<br /> on 2002/7/28 and 2002/7/29. Initial results are briefly reported.
  • Masaaki Sakano, Katsuji Koyama, Hiroshi Murakami, Yoshitomo Maeda, Shigeo Yamauchi
    Astrophysical Journal Supplement Series 138(1) 19-34 2002年1月1日  
    The ASCA satellite made 107 pointing observations on a 5 x 5 deg^2 region<br /> around the center of our Milky Way Galaxy (the Galactic Center) from 1993 to<br /> 1999. In the X-ray images of the 0.7--3 keV or 3--10 keV bands, we found 52<br /> point sources and a dozen diffuse sources. All the point sources are uniformly<br /> fitted with an absorbed power-law model. For selected bright sources, Sgr A*,<br /> AX J1745.6-2901, A 1742-294, SLX 1744-300, GRO J1744-28, SLX 1737-282, GRS<br /> 1734-292, AX J1749.2-2725, KS 1741-293, GRS 1741.9-2853, and an unusual flare<br /> source XTE J1739-302, we present further detailed spectral and timing analyses,<br /> and discuss their nature.<br /> The dozen extended X-ray sources comprise radio supernova remnants, giant<br /> molecular clouds, and some new discoveries. Most show emission lines from<br /> either highly ionized atoms or low-ionized irons.<br /> The X-ray spectra were fitted with either a thin thermal or power-law model.<br /> This paper summarizes the results and provides the ASCA X-ray source catalogue<br /> in the Galactic Center region.
  • K Ebisawa, Y Maeda, H Kaneda, S Yamauchi
    SCIENCE 293(5535) 1633-1635 2001年8月  
    The Galactic plane is a strong emitter of hard x-rays (2 to 10 kiloelectron volts), and the emission forms a narrow continuous ridge. The currently known hard x-ray sources are far too few to explain the ridge x-ray emission, and the fundamental question of whether the ridge emission is ultimately resolved into numerous dimmer discrete sources or truly diffuse emission has not yet been settled. In order to obtain a decisive answer, using the Chandra X-ray Observatory, we carried out the deepest hard x-ray survey of a Galactic plane region that is devoid of known x-ray point sources. We detected at least 36 new hard x-ray point sources in addition to strong diffuse emission within a 17' by 17' field of view. The surface density of the point sources is comparable to that at high Galactic latitudes after the effects of Galactic absorption are considered. Therefore, most of these point sources are probably extragalactic, presumably active galaxies seen through the Galactic disk. The Galactic ridge hard x-ray emission is diffuse, which indicates omnipresence within the Galactic plane of a hot plasma, the energy density of which is more than one order of magnitude higher than any other substance in the interstellar space.
  • H Murakami, K Koyama, Y Maeda, M Sakano
    NEW CENTURY OF X-RAY ASTRONOMY 251 310-311 2001年  
    We present a Chandra observation of the giant molecular cloud Sgr B2 at the Galactic center region. We detected diffuse X-ray emission and 17 point sources in the cloud. The diffuse emission shows a strong 6.4 keV line from neutral iron, and is prominent on the Galactic center side. These features support the "X-ray Reflection Nebula" hypothesis, in which the cloud is irradiated by an external X-ray source in the direction of the Galactic center and emits fluorescent and scattered X-rays.
  • M Sakano, K Koyama, H Murakami, Y Maeda, S Yamauchi
    NEW CENTURY OF X-RAY ASTRONOMY 251 314-315 2001年  
    Front the ASCA X-ray point-source list in the Galactic center 5 x 5 degree(2) region, we found the clear correlation between the position of the sources and the absorption. This fact implies that the major part of the absorption is due to the cold interstellar matter (ISM) in the line of sight. Using the correlation, we estimate the distribution of the cold ISM. We also found that the ratio of numbers of high mass binaries to low mass binaries is significantly smaller than that in the whole Galaxy or SMC, which implies that the past starburst activity in the Galactic center region was rather quiet.
  • Koyama Katsuji, Maeda Yoshitomo, Yamauchi Shigeo, MAEDA Yoshitomo, YAMAUCHI Shigeo
    PASJ : publications of the Astronomical Society of Japan 52(6) 1141-1145 2000年12月1日  
  • Tanaka Yasuo, Koyama Katsuji, Maeda Yoshitomo, SONOBE Takashi
    PASJ : publications of the Astronomical Society of Japan 52(4) L25-L30 2000年8月25日  
  • H Murakami, K Koyama, Y Maeda, M Sakano, M Nishiuchi, M Tsujimoto
    BROAD BAND X-RAY SPECTRA OF COSMIC SOURCES 25(3-4) 579-582 2000年  
    We present the ASCA results of imaging spectroscopy of the giant molecular cloud Sgr B2. The X-ray spectrum is found to be very peculiar; it exhibits a strong emission line at 6.4 keV, a low energy cutoff below 4 keV and a pronounced edge-structure at 7.1 keV. The X-ray image is extended and its peak position is shifted in the direction of the Galactic center by about 1-2 arcminute from the core of the molecular cloud. The X-ray spectrum and morphology are well reproduced by a scenario that X-rays from a source located at the Galactic center side are scattered by the molecular cloud Sgr B2, and come into our line of sight. Thus Sgr B2 may be called an X-ray reflection nebula. (C) 2000 COSPAR. Published by Elsevier Science Ltd.
  • M Nishiuchi, K Koyama, Y Maeda, T Dotani, K Asai, Y Ueda, K Mitsuda, F Nagase, H Inoue, C Kouveliotou
    BROAD BAND X-RAY SPECTRA OF COSMIC SOURCES 25(3-4) 391-394 2000年  
    The ASCA results of the bursting X-ray pulsar GRO J1744-28 are reported. The observations were made twice, in February 1996 and March 1997. We detected 12 and 17 Type II bursts during the two observations, with mean bursting intervals of about 27 min and 37 min. Each burst is followed by an intensity dip with the depleted flux depending on the burst fluence. The energy spectra are approximated by an absorbed power law with additional structure around 6-7 keV, which is most probably due to iron and maybe reproduced by the disk line model with additional broadening mechanism. The absorption column is constant ((5 - 6) x 10(22) cm(-2)), independent of the observation dates and emission phase (persistent, burst and dip). This means the source may be actually located near the galactic center (8.5kpc). (C) 2000 COSPAR. Published by Elsevier Science Ltd.
  • M Nishiuchi, K Koyama, Y Maeda, K Asai, T Dotani, H Inoue, K Mitsuda, F Nagase, Y Ueda, C Kouveliotou
    ASTROPHYSICAL JOURNAL 517(1) 436-448 1999年5月  
    We report the ASCA results of the bursting X-ray pulsar GRO J1744-28, which was observed in 1996 February and 1997 March. The source flux in the 2-10 keV band was 2.0 x 10(-8) ergs s(-1) cm(2) in 1996 and 5.0 x 10(-9) ergs s(-1) cm2 in 1997. We detected 12 and 17 type II bursts during type two observations, with mean bursting intervals of about 27 min and 37 min. Each burst is followed by an intensity dip with the depleted flux depending on the burst fluence. The energy spectra are approximated by an absorbed power law with additional structure around 6-7 keV. The constant absorption column, (5-6) x 10(22) cm(-2), independent of the observation dates and emission phases (persistent, burst, and dir) is interpreted as an interstellar absorption. The source may be actually located near the Galactic center, at a distance of 8.5 kpc. The structure in the energy spectrum at 6 7 keV is most probably due to iron and may be reproduced by a disk line model with additional broadening mechanism.
  • Astronomische Nachrichten 320(4-5) 330-330 1999年  
  • 前田 良知, 鶴 剛, 粟木 久光
    日本物理学会講演概要集 52(1) 82-82 1997年3月17日  
  • Maeda Yoshitomo, Koyama Katsuji, Sakano Masaaki, TAKESHIMA Toshiaki, YAMAUCHI Shigeo
    PASJ : publications of the Astronomical Society of Japan 48(3) 417-423 1996年6月25日  
  • Koyama Katsuji, Maeda Yoshitomo, Sonobe Takashi, TAKESHIMA Toshiaki, TANAKA Yasuo, YAMAUCHI Shigeo
    PASJ : publications of the Astronomical Society of Japan 48(2) 249-255 1996年  

講演・口頭発表等

 5
  • 前田良知
    Optics & Photonics Japan 2023シンポジウム 『X線・EUV結像光学のフロンティア』 2023年11月29日  招待有り
  • Maeda, Yoshitomo, Morii, Mikio, Ishida, Manabu, Hisamitsu, Awaki, Hagino, Koichi
    44th COSPAR Scientific Assembly 2022年
  • 前田良知, the XRISM PV, Eta Carinae team
    nuclear burning in massive stars – towards the formation of binary black holes – 2021年7月28日
  • Yoshitomo Maeda, Quincy Abarr, Hisamitsu Awaki, Matthew Baring, Richard Bose, Dana Braun, Gianluigi De Geronimo, Paul Dowkontt, John W. Elliot, Teruaki Enoto, Manel Errando, Yasushi Fukazawa, Akihiro Furuzawa, Thomas A. Gadson, Ephraim Gau, Victor Guarino, Shuichi Gunji, Kenny E. Hall, Keon D. Harmon, Kengo Hattori, Kiyoshi Hayashida, Scott E. Heatwole, Arman Hossen, Fumiya Imazato, Kazunori Ishibashi, Manabu Ishida, Nirmal Iyer, Fabian Kislat, Mózsi Kiss, Takao Kitaguchi, David P. Kotsifakis, Henric Krawczynski, James R. Lanzi, Lindsey Lisalda, Hiroto Matake, Hironori Matsumoto, Taisei Mineta, Takuya Miyazawa, Tsunefumi Mizuno, Takashi Okajima, Nozomi Nakaniwa, Izabella Pastrani, Mark Pearce, Zachary Peterson, Chris Purdy, Brian Rauch, Felix Ryde, Yoshitaka Saito, Chris Shreeves, Garry Simburger, Carl Snow, Sean Spooner, Theodor-Adrian Stana, David W. Stuchlik, Hiromitsu Takahashi, Tomoshi Takeda, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Hiroshi Tsunemi, Nagomi Uchida, Yuusuke Uchida, Keisuke Uchiyama, Brett Vincent, Andrew T. West, Eric Wulf, Yuto Yoshida, Ryuya Yamamoto
    Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray 2020年12月19日
  • Yoshitomo Maeda
    The 15th Symposium of Japanese Research Community on X-ray Imaging Optics 2019年10月26日  招待有り

担当経験のある科目(授業)

 6
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所属学協会

 4

共同研究・競争的資金等の研究課題

 11
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社会貢献活動

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