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The Physical Conditions of the Intrinsic N V Narrow Absorption Line Systems of Three Quasars
http://hdl.handle.net/10091/10715
http://hdl.handle.net/10091/10715012aac26-b932-4ce1-8133-981ffd84a761
名前 / ファイル | ライセンス | アクション |
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PHYSICAL_CONDITIONS_INTRINSIC.pdf (1.2 MB)
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Item type | 学術雑誌論文 / Journal Article(1) | |||||
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公開日 | 2010-10-19 | |||||
タイトル | ||||||
言語 | en | |||||
タイトル | The Physical Conditions of the Intrinsic N V Narrow Absorption Line Systems of Three Quasars | |||||
言語 | ||||||
言語 | eng | |||||
キーワード | ||||||
主題 | quasars: absorption lines, quasars: individual (HE0130-4021, Q1009+2956, HS1700+6416) | |||||
資源タイプ | ||||||
資源 | http://purl.org/coar/resource_type/c_6501 | |||||
タイプ | journal article | |||||
著者 |
Wu, Jian
× Wu, Jian× Charlton, Jane C.× Misawa, Toru× Eracleous, Michael× Ganguly, Rajib |
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信州大学研究者総覧へのリンク | ||||||
氏名 | Misawa, Toru | |||||
URL | http://soar-rd.shinshu-u.ac.jp/profile/ja.ypchuUkV.html | |||||
出版者 | ||||||
出版者 | IOP PUBLISHING LTD | |||||
引用 | ||||||
内容記述タイプ | Other | |||||
内容記述 | The Astrophysical Journal. 722(2):997-1012 (2010) | |||||
書誌情報 |
The Astrophysical Journal 巻 722, 号 2, p. 997-1012, 発行日 2010-10-20 |
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抄録 | ||||||
内容記述タイプ | Abstract | |||||
内容記述 | We employ detailed photoionization models to infer the physical conditions of intrinsic narrow absorption line systems found in high-resolution spectra of three quasars at z = 2.6-3.0. We focus on a family of intrinsic absorbers characterized by N V lines that are strong relative to the Lyα lines. The inferred physical conditions are similar for the three intrinsic N V absorbers, with metallicities greater than 10 times the solar value (assuming a solar abundance pattern), and with high ionization parameters (log U ~ 0). Thus, we conclude that the unusual strength of the N V lines results from a combination of partial coverage, a high ionization state, and high metallicity. We consider whether dilution of the absorption lines by flux from the broad emission line region can lead us to overestimate the metallicities and we find that this is an unlikely possibility. The high abundances that we infer are not surprising in the context of scenarios in which metal enrichment takes place very early on in massive galaxies. We estimate that the mass outflow rate in the absorbing gas (which is likely to have a filamentary structure) is less than a few M_ yr−1 under the most optimistic assumptions, although it may be embedded in a much hotter, more massive outflow. | |||||
資源タイプ(コンテンツの種類) | ||||||
内容記述タイプ | Other | |||||
内容記述 | Article | |||||
ISSN | ||||||
収録物識別子タイプ | ISSN | |||||
収録物識別子 | 0004-637X | |||||
書誌レコードID | ||||||
収録物識別子タイプ | NCID | |||||
収録物識別子 | AA00553253 | |||||
DOI | ||||||
識別子タイプ | DOI | |||||
関連識別子 | https://doi.org/10.1088/0004-637X/722/2/997 | |||||
関連名称 | 10.1088/0004-637X/722/2/997 | |||||
権利 | ||||||
権利情報 | Copyright (c) 2010 The American Astronomical Society | |||||
出版タイプ | ||||||
出版タイプ | VoR | |||||
出版タイプResource | http://purl.org/coar/version/c_970fb48d4fbd8a85 |