{"created":"2021-03-01T06:18:51.072597+00:00","id":15849,"links":{},"metadata":{"_buckets":{"deposit":"24f08e70-139a-4d36-8486-a53189b03548"},"_deposit":{"id":"15849","owners":[],"pid":{"revision_id":0,"type":"depid","value":"15849"},"status":"published"},"_oai":{"id":"oai:soar-ir.repo.nii.ac.jp:00015849","sets":["1544:1545"]},"author_link":["45878","45879","45880","45881","45882","45883","45884","45885","45886"],"item_1628147817048":{"attribute_name":"出版タイプ","attribute_value_mlt":[{"subitem_version_resource":"http://purl.org/coar/version/c_970fb48d4fbd8a85","subitem_version_type":"VoR"}]},"item_6_biblio_info_6":{"attribute_name":"書誌情報","attribute_value_mlt":[{"bibliographicIssueDates":{"bibliographicIssueDate":"2004-12","bibliographicIssueDateType":"Issued"},"bibliographicIssueNumber":"6","bibliographicPageEnd":"2961","bibliographicPageStart":"2954","bibliographicVolumeNumber":"128","bibliographic_titles":[{"bibliographic_title":"ASTRONOMICAL JOURNAL"}]}]},"item_6_description_20":{"attribute_name":"抄録","attribute_value_mlt":[{"subitem_description":"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.","subitem_description_type":"Abstract"}]},"item_6_description_30":{"attribute_name":"資源タイプ（コンテンツの種類）","attribute_value_mlt":[{"subitem_description":"Article","subitem_description_type":"Other"}]},"item_6_description_5":{"attribute_name":"引用","attribute_value_mlt":[{"subitem_description":"ASTRONOMICAL JOURNAL. 128(6):2954-2961 (2004)","subitem_description_type":"Other"}]},"item_6_link_3":{"attribute_name":"信州大学研究者総覧へのリンク","attribute_value_mlt":[{"subitem_link_text":"Misawa, T","subitem_link_url":"http://soar-rd.shinshu-u.ac.jp/profile/ja.ypchuUkV.html"}]},"item_6_link_67":{"attribute_name":"WoS","attribute_value_mlt":[{"subitem_link_url":"http://gateway.isiknowledge.com/gateway/Gateway.cgi?&GWVersion=2&SrcAuth=ShinshuUniv&SrcApp=ShinshuUniv&DestLinkType=FullRecord&DestApp=WOS&KeyUT=000225417500029"}]},"item_6_publisher_4":{"attribute_name":"出版者","attribute_value_mlt":[{"subitem_publisher":"UNIV CHICAGO PRESS"}]},"item_6_relation_48":{"attribute_name":"DOI","attribute_value_mlt":[{"subitem_relation_name":[{"subitem_relation_name_text":"10.1086/425879"}],"subitem_relation_type_id":{"subitem_relation_type_id_text":"https://doi.org/10.1086/425879","subitem_relation_type_select":"DOI"}}]},"item_6_rights_62":{"attribute_name":"権利","attribute_value_mlt":[{"subitem_rights":"Copyright© 2004 The American Astronomical Society"}]},"item_6_source_id_35":{"attribute_name":"ISSN","attribute_value_mlt":[{"subitem_source_identifier":"0004-6256","subitem_source_identifier_type":"ISSN"}]},"item_6_source_id_40":{"attribute_name":"書誌レコードID","attribute_value_mlt":[{"subitem_source_identifier":"AA00552749","subitem_source_identifier_type":"NCID"}]},"item_creator":{"attribute_name":"著者","attribute_type":"creator","attribute_value_mlt":[{"creatorNames":[{"creatorName":"Misawa,  T"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"Tytler,  D"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"Iye,  M"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"Paschos,  P"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"Norman,  M"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"Kirkman,  D"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"O'Meara,  J"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"Suzuki,  N"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"Kashikawa,  N"}],"nameIdentifiers":[{}]}]},"item_files":{"attribute_name":"ファイル情報","attribute_type":"file","attribute_value_mlt":[{"accessrole":"open_date","date":[{"dateType":"Available","dateValue":"2015-09-28"}],"displaytype":"detail","filename":"2004_AJ_128_2954.pdf","filesize":[{"value":"915.9 kB"}],"format":"application/pdf","licensetype":"license_note","mimetype":"application/pdf","url":{"label":"2004_AJ_128_2954.pdf","url":"https://soar-ir.repo.nii.ac.jp/record/15849/files/2004_AJ_128_2954.pdf"},"version_id":"a57e83cc-6c5e-43bd-ade4-479aa064cd3b"}]},"item_keyword":{"attribute_name":"キーワード","attribute_value_mlt":[{"subitem_subject":"galaxies : ISM","subitem_subject_scheme":"Other"},{"subitem_subject":"intergalactic medium","subitem_subject_scheme":"Other"},{"subitem_subject":"quasars : absorption lines","subitem_subject_scheme":"Other"}]},"item_language":{"attribute_name":"言語","attribute_value_mlt":[{"subitem_language":"eng"}]},"item_resource_type":{"attribute_name":"資源タイプ","attribute_value_mlt":[{"resourcetype":"journal article","resourceuri":"http://purl.org/coar/resource_type/c_6501"}]},"item_title":"HI gas in higher density regions of the intergalactic medium","item_titles":{"attribute_name":"タイトル","attribute_value_mlt":[{"subitem_title":"HI gas in higher density regions of the intergalactic medium","subitem_title_language":"en"}]},"item_type_id":"6","owner":"1","path":["1545"],"pubdate":{"attribute_name":"PubDate","attribute_value":"2013-12-02"},"publish_date":"2013-12-02","publish_status":"0","recid":"15849","relation_version_is_last":true,"title":["HI gas in higher density regions of the intergalactic medium"],"weko_creator_id":"1","weko_shared_id":-1},"updated":"2022-12-14T04:01:45.006752+00:00"}