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X-Ray Measurements of the Field and Particle Energy Distributions in the West Lobe of the Radio Galaxy NGC 1316 (Fornax A)
https://sucra.repo.nii.ac.jp/records/13456
https://sucra.repo.nii.ac.jp/records/134568523d47b-6bd3-4f88-bd1b-4063f6127904
名前 / ファイル | ライセンス | アクション |
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A1002926.pdf (226.3 kB)
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Item type | 学術雑誌論文 / Journal Article(1) | |||||
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公開日 | 2009-07-29 | |||||
タイトル | ||||||
タイトル | X-Ray Measurements of the Field and Particle Energy Distributions in the West Lobe of the Radio Galaxy NGC 1316 (Fornax A) | |||||
言語 | ||||||
言語 | eng | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | galaxies : individual (NGC 1316) magnetic fields | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | radiation mechanisms : nonthermal radio continuum : galaxies | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | X-rays : galaxies | |||||
資源タイプ | ||||||
資源タイプ識別子 | http://purl.org/coar/resource_type/c_6501 | |||||
資源タイプ | journal article | |||||
著者 |
田代, 信
× 田代, 信 |
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著者 ローマ字 | ||||||
Tashiro, Makoto | ||||||
著者 ローマ字 | ||||||
Makishima, K | ||||||
著者 ローマ字 | ||||||
Iyomoto, N | ||||||
著者 ローマ字 | ||||||
Isobe, N | ||||||
著者 ローマ字 | ||||||
Kaneda, H | ||||||
著者 所属 | ||||||
埼玉大学大学院理工学研究科物質科学部門 | ||||||
著者 所属(別言語) | ||||||
Graduate School of Science and Engineering, Saitama University | ||||||
書誌情報 |
The Astrophysical Journal 巻 546, 号 1, p. L19-L23, 発行日 2001 |
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年月次 | ||||||
2001-1 | ||||||
出版者名 | ||||||
出版者 | American Astronomical Society | |||||
ISSN | ||||||
収録物識別子タイプ | ISSN | |||||
収録物識別子 | 0004637X | |||||
DOI | ||||||
関連タイプ | isVersionOf | |||||
識別子タイプ | DOI | |||||
関連識別子 | info:doi/10.1086/318057 | |||||
関連サイト | ||||||
内容記述タイプ | Other | |||||
内容記述 | http://www.iop.org/EJ/abstract/1538-4357/546/1/L19/ | http://www.iop.org/EJ/abstract/1538-4357/546/1/L19/ | |||||
抄録 | ||||||
内容記述タイプ | Abstract | |||||
内容記述 | A follow-up X-ray study was made of the west lobe of the radio galaxy Fornax A (NGC 1316) that was based on new ASCA observations made in 1997 for 98 ks and that incorporated the previous observation in 1994 for 39 ks. The 0.7-10 keV spectrum of the emission can be described by a power law with an energy index of 0.74 +/- 0.10 which agrees with the synchrotron radio index of 0.9 +/- 0.2. Therefore, the X-rays are reconfirmed to arise via the inverse Compton scattering of the cosmic microwave photons, as Kaneda et al. and Feigelson et al. concluded. The surface brightness of the inverse Compton X-rays exhibits a relatively flat distribution over the west lobe, indicative of an approximately spherical emissivity distribution with a radius of similar to 11 ' (75 kpc). In contrast, the 1.4 GHz radio image by Ekers et al. exhibits a rim-brightened surface brightness, consistent with a shell-like emissivity distribution whose inner and outer boundaries are 4 ' and 11 ', respectively. These morphological differences between radio and X-rays suggest that the relativistic electrons are distributed homogeneously over the lobe volume, whereas the magnetic field is amplified toward the lobe rim region. | |||||
注記 | ||||||
内容記述タイプ | Other | |||||
内容記述 | arXiv:astro-ph/0010503v1 http://arxiv.org/abs/astro-ph/0010503 |
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版 | ||||||
[著者版] | ||||||
著者版フラグ | ||||||
出版タイプ | AM | |||||
出版タイプResource | http://purl.org/coar/version/c_ab4af688f83e57aa | |||||
資源タイプ | ||||||
内容記述タイプ | Other | |||||
内容記述 | text | |||||
フォーマット | ||||||
内容記述タイプ | Other | |||||
内容記述 | application/pdf | |||||
作成日 | ||||||
日付 | 2009-07-28 | |||||
日付タイプ | Created | |||||
アイテムID | ||||||
A1002926 |