{"_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": "\u51fa\u7248\u30bf\u30a4\u30d7", "attribute_value_mlt": [{"subitem_version_resource": "http://purl.org/coar/version/c_970fb48d4fbd8a85", "subitem_version_type": "VoR"}]}, "item_6_biblio_info_6": {"attribute_name": "\u66f8\u8a8c\u60c5\u5831", "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": "\u6284\u9332", "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\u003clog N-H I [cm(-2)]\u003c19). 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\u003c200 km s(-1), whereas lower ones cluster at \u0026UDelta;v\u003c100 km s(-1). We define HDLs as H I lines with 15\u003clog N-H I\u003c19 and all H I lines within 200 km s(-1) of a line with log N-H I\u003e15 and LDLs as all others with 12\u003clog N-H I\u003c15. 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": "\u8cc7\u6e90\u30bf\u30a4\u30d7\uff08\u30b3\u30f3\u30c6\u30f3\u30c4\u306e\u7a2e\u985e\uff09", "attribute_value_mlt": [{"subitem_description": "Article", "subitem_description_type": "Other"}]}, "item_6_description_5": {"attribute_name": "\u5f15\u7528", "attribute_value_mlt": [{"subitem_description": "ASTRONOMICAL JOURNAL. 128(6):2954-2961 (2004)", "subitem_description_type": "Other"}]}, "item_6_link_3": {"attribute_name": "\u4fe1\u5dde\u5927\u5b66\u7814\u7a76\u8005\u7dcf\u89a7\u3078\u306e\u30ea\u30f3\u30af", "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_text": "Web of Science", "subitem_link_url": "http://gateway.isiknowledge.com/gateway/Gateway.cgi?\u0026GWVersion=2\u0026SrcAuth=ShinshuUniv\u0026SrcApp=ShinshuUniv\u0026DestLinkType=FullRecord\u0026DestApp=WOS\u0026KeyUT=000225417500029"}]}, "item_6_publisher_4": {"attribute_name": "\u51fa\u7248\u8005", "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": "\u6a29\u5229", "attribute_value_mlt": [{"subitem_rights": "Copyright\u00a9 2004 The American Astronomical Society"}]}, "item_6_select_64": {"attribute_name": "\u8457\u8005\u7248\u30d5\u30e9\u30b0", "attribute_value_mlt": [{"subitem_select_item": "publisher"}]}, "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_39": {"attribute_name": "NII ISSN", "attribute_value_mlt": [{"subitem_source_identifier": "0004-6256", "subitem_source_identifier_type": "ISSN"}]}, "item_6_source_id_40": {"attribute_name": "\u66f8\u8a8c\u30ec\u30b3\u30fc\u30c9ID", "attribute_value_mlt": [{"subitem_source_identifier": "AA00552749", "subitem_source_identifier_type": "NCID"}]}, "item_6_text_69": {"attribute_name": "wosonly authkey", "attribute_value_mlt": [{"subitem_text_value": "galaxies : ISM; intergalactic medium; quasars : absorption lines"}]}, "item_6_text_70": {"attribute_name": "wosonly keywords", "attribute_value_mlt": [{"subitem_text_value": "LY-ALPHA FOREST; HIGH-REDSHIFT GALAXIES; LYMAN-LIMIT ABSORPTION; HIGH-RESOLUTION SPECTROSCOPY; COSMOLOGICAL BARYON DENSITY; HYDROGEN ABUNDANCE RATIO; DARK-MATTER COSMOLOGY; C-IV-ABSORPTION; DEUTERIUM ABUNDANCE; PHYSICAL-PROPERTIES"}]}, "item_6_textarea_68": {"attribute_name": "wosonly abstract", "attribute_value_mlt": [{"subitem_textarea_value": "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\u003clog N-H I [cm(-2)]\u003c19). 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\u003c200 km s(-1), whereas lower ones cluster at \u0026UDelta;v\u003c100 km s(-1). We define HDLs as H I lines with 15\u003clog N-H I\u003c19 and all H I lines within 200 km s(-1) of a line with log N-H I\u003e15 and LDLs as all others with 12\u003clog N-H I\u003c15. 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."}]}, "item_creator": {"attribute_name": "\u8457\u8005", "attribute_type": "creator", "attribute_value_mlt": [{"creatorNames": [{"creatorName": "Misawa,  T"}], "nameIdentifiers": [{"nameIdentifier": "45878", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Tytler,  D"}], "nameIdentifiers": [{"nameIdentifier": "45879", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Iye,  M"}], "nameIdentifiers": [{"nameIdentifier": "45880", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Paschos,  P"}], "nameIdentifiers": [{"nameIdentifier": "45881", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Norman,  M"}], "nameIdentifiers": [{"nameIdentifier": "45882", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Kirkman,  D"}], "nameIdentifiers": [{"nameIdentifier": "45883", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "O\u0027Meara,  J"}], "nameIdentifiers": [{"nameIdentifier": "45884", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Suzuki,  N"}], "nameIdentifiers": [{"nameIdentifier": "45885", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Kashikawa,  N"}], "nameIdentifiers": [{"nameIdentifier": "45886", "nameIdentifierScheme": "WEKO"}]}]}, "item_files": {"attribute_name": "\u30d5\u30a1\u30a4\u30eb\u60c5\u5831", "attribute_type": "file", "attribute_value_mlt": [{"accessrole": "open_date", "date": [{"dateType": "Available", "dateValue": "2015-09-28"}], "displaytype": "detail", "download_preview_message": "", "file_order": 0, "filename": "2004_AJ_128_2954.pdf", "filesize": [{"value": "915.9 kB"}], "format": "application/pdf", "future_date_message": "", "is_thumbnail": false, "licensetype": "license_note", "mimetype": "application/pdf", "size": 915900.0, "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": "\u30ad\u30fc\u30ef\u30fc\u30c9", "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": "\u8a00\u8a9e", "attribute_value_mlt": [{"subitem_language": "eng"}]}, "item_resource_type": {"attribute_name": "\u8cc7\u6e90\u30bf\u30a4\u30d7", "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": "\u30bf\u30a4\u30c8\u30eb", "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": ["1544/1545"], "permalink_uri": "http://hdl.handle.net/10091/17259", "pubdate": {"attribute_name": "PubDate", "attribute_value": "2013-12-02"}, "publish_date": "2013-12-02", "publish_status": "0", "recid": "15849", "relation": {}, "relation_version_is_last": true, "title": ["HI gas in higher density regions of the intergalactic medium"], "weko_shared_id": -1}