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HI gas in higher density regions of the intergalactic medium
http://hdl.handle.net/10091/17259
http://hdl.handle.net/10091/17259d154afe0-d8bd-4684-92b6-a09c7c457210
名前 / ファイル | ライセンス | アクション |
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2004_AJ_128_2954.pdf (915.9 kB)
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Item type | 学術雑誌論文 / Journal Article(1) | |||||
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公開日 | 2013-12-02 | |||||
タイトル | ||||||
言語 | en | |||||
タイトル | HI gas in higher density regions of the intergalactic medium | |||||
言語 | ||||||
言語 | eng | |||||
キーワード | ||||||
主題 | galaxies : ISM, intergalactic medium, quasars : absorption lines | |||||
資源タイプ | ||||||
資源 | http://purl.org/coar/resource_type/c_6501 | |||||
タイプ | journal article | |||||
著者 |
Misawa, T
× Misawa, T× Tytler, D× Iye, M× Paschos, P× Norman, M× Kirkman, D× O'Meara, J× Suzuki, N× Kashikawa, N |
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信州大学研究者総覧へのリンク | ||||||
氏名 | Misawa, T | |||||
URL | http://soar-rd.shinshu-u.ac.jp/profile/ja.ypchuUkV.html | |||||
出版者 | ||||||
出版者 | UNIV CHICAGO PRESS | |||||
引用 | ||||||
内容記述タイプ | Other | |||||
内容記述 | ASTRONOMICAL JOURNAL. 128(6):2954-2961 (2004) | |||||
書誌情報 |
ASTRONOMICAL JOURNAL 巻 128, 号 6, p. 2954-2961, 発行日 2004-12 |
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抄録 | ||||||
内容記述タイプ | Abstract | |||||
内容記述 | Using H I absorption alone, we attempt to separate H I absorption lines in quasar spectra into two categories: higher density lines (HDLs) and lower density lines (LDLs), and we discuss the difference in their physical properties. We deblend and fit all H I lines with Voigt profiles and make an unbiased sample of H I lines covering a wide column density range (12<log N-H I [cm(-2)]<19). To reduce the influence of line blending, we simultaneously fit several Lyman series lines. As a result of a two-point correlation analysis, we found that higher column density H I lines are clustering at Deltav<200 km s(-1), whereas lower ones cluster at &UDelta;v<100 km s(-1). We define HDLs as H I lines with 15<log N-H I<19 and all H I lines within 200 km s(-1) of a line with log N-H I>15 and LDLs as all others with 12<log N-H I<15. We found that the HDLs have smaller minimum b-values for a given column density than the LDLs. This difference is successfully reproduced by our hydrodynamic simulation. The LDLs seem to be cool or shock-heated diffuse intergalactic medium gas, whereas the HDLs are likely to be cooler dense gas near to galaxies. | |||||
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 | 0004-6256 | |||||
書誌レコードID | ||||||
収録物識別子タイプ | NCID | |||||
収録物識別子 | AA00552749 | |||||
DOI | ||||||
識別子タイプ | DOI | |||||
関連識別子 | https://doi.org/10.1086/425879 | |||||
関連名称 | 10.1086/425879 | |||||
権利 | ||||||
権利情報 | Copyright© 2004 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 | |||||
WoS | ||||||
表示名 | Web of Science | |||||
URL | http://gateway.isiknowledge.com/gateway/Gateway.cgi?&GWVersion=2&SrcAuth=ShinshuUniv&SrcApp=ShinshuUniv&DestLinkType=FullRecord&DestApp=WOS&KeyUT=000225417500029 |