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Suzaku observation of the unidentified gamma-ray source TeV J2032+4130
https://jaxa.repo.nii.ac.jp/records/4953
https://jaxa.repo.nii.ac.jp/records/49533e7b98a9-7cfa-4435-b71b-ecc53711382e
名前 / ファイル | ライセンス | アクション |
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64574021.pdf (296.1 kB)
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Item type | 会議発表論文 / Conference Paper(1) | |||||
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公開日 | 2015-03-26 | |||||
タイトル | ||||||
言語 | en | |||||
タイトル | Suzaku observation of the unidentified gamma-ray source TeV J2032+4130 | |||||
言語 | ||||||
言語 | eng | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | acceleration of particles - X-rays: individual (TeV J2032+4130) - X-rays: ISM - pulsars: individual (PSR J2032+4127) | |||||
資源タイプ | ||||||
資源タイプ識別子 | http://purl.org/coar/resource_type/c_5794 | |||||
資源タイプ | conference paper | |||||
著者 |
村上, 弘志
× 村上, 弘志× 北本, 俊二× Murakami, Hiroshi× Kitamoto, Shunji |
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著者所属 | ||||||
立教大学理学部物理学科 | ||||||
著者所属 | ||||||
立教大学理学部物理学科 | ||||||
著者所属(英) | ||||||
en | ||||||
Department of Physics, Rikkyo University | ||||||
著者所属(英) | ||||||
en | ||||||
Department of Physics, Rikkyo University | ||||||
出版者 | ||||||
出版者 | 宇宙航空研究開発機構 | |||||
出版者(英) | ||||||
出版者 | Japan Aerospace Exploration Agency (JAXA) | |||||
書誌情報 |
宇宙航空研究開発機構特別資料: en : JAXA Special Publication: The Energetic Cosmos; from Suzaku to ASTRO-H 巻 JAXA-SP-09-008E, p. 54-55, 発行日 2010-02-26 |
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会議概要(会議名, 開催地, 会期, 主催者等)(英) | ||||||
内容記述タイプ | Other | |||||
内容記述 | The 3rd Suzaku international Conference "Energetic Cosmos : from Suzaku to ASTRO-H" (June 29-July 2, 2009. Grand Park Otaru Hotel), Otaru, Hokkaido Japan | |||||
抄録(英) | ||||||
内容記述タイプ | Other | |||||
内容記述 | We observed the first unidentified TeV gamma-ray source TeV J2032+4130 with Suzaku. With the high sensitivity for detection of diffuse X-ray emission, we found a structure in the TeV emitting region, which is coincident with a gamma-ray pulsar. By subtracting the contribution of point sources estimated by Chandra observation, we obtained X-ray spectrum of diffuse component. The spectrum can be reproduced by a power-law model with a photon index of approximately 2, and an X-ray flux of 2 x 10(exp -13) erg s(exp -1) cm(exp -2). The ratio of the gamma-ray flux to the X-ray flux is approximately 10. If the origin of TeV gamma-ray is inverse Compton scattering of microwave background by TeV electrons, which are responsible to synchrotron emission, this ratio corresponds to the magnetic field of approximately 1 micro-G. | |||||
内容記述(英) | ||||||
内容記述タイプ | Other | |||||
内容記述 | Meeting sponsors: The University of Tokyo, The Institute of Physical and Chemical Research, The Japan Society for the Promotion of Science | |||||
ISSN | ||||||
収録物識別子タイプ | ISSN | |||||
収録物識別子 | 1349-113X | |||||
書誌レコードID | ||||||
収録物識別子タイプ | NCID | |||||
収録物識別子 | AA11984031 | |||||
資料番号 | ||||||
内容記述タイプ | Other | |||||
内容記述 | 資料番号: AA0064574021 | |||||
レポート番号 | ||||||
内容記述タイプ | Other | |||||
内容記述 | レポート番号: JAXA-SP-09-008E |