ログイン
言語:

WEKO3

  • トップ
  • コミュニティ
  • ランキング
AND
To
lat lon distance
To

Field does not validate



インデックスリンク

インデックスツリー

メールアドレスを入力してください。

WEKO

One fine body…

WEKO

One fine body…

アイテム

{"_buckets": {"deposit": "79af9f89-aa9e-46b6-ba47-97ecf9f467c2"}, "_deposit": {"id": "15851", "owners": [], "pid": {"revision_id": 0, "type": "depid", "value": "15851"}, "status": "published"}, "_oai": {"id": "oai:soar-ir.repo.nii.ac.jp:00015851", "sets": ["1544:1545"]}, "author_link": ["45894", "45895", "45896", "45897", "45898", "45899"], "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": "2002-04", "bibliographicIssueDateType": "Issued"}, "bibliographicIssueNumber": "4", "bibliographicPageEnd": "1863", "bibliographicPageStart": "1847", "bibliographicVolumeNumber": "123", "bibliographic_titles": [{"bibliographic_title": "ASTRONOMICAL JOURNAL"}]}]}, "item_6_description_20": {"attribute_name": "\u6284\u9332", "attribute_value_mlt": [{"subitem_description": "We present a modest survey of quasar metal line absorption systems at redshifts 2.3-4.5. Relatively high signal-to-noise ratio (similar to25 pixel(-1)) spectra of 18 quasars at 2 Angstrom FWHM resolution show many absorption systems with strong metal lines in the region redward of the Lyalpha emission lines. We conducted a systematic search and found 55 C IV doublets, 19 Si IV doublets, three Mg II doublets, and seven N v doublets. The present data alone hint that the number of C IV absorption doublets per unit redshift, N(z), decreases with increasing redshift for 2.3 \u003c z \u003c 4.5 but at only the 1-2 sigma level, for either an Einstein de Sitter model (Lambda = 0) or a flat universe with Lambda = 0.7. When we combine our sample with published data that extend to lower redshifts, we detect evolution at the 1-4 sigma level, depending on the cosmological model and the strength of the C IV lines. There are fewer C IV systems per unit z with increasing z, and the systems with stronger C IV lines evolve much faster. At z similar or equal to 2.4, C IV with W \u003e 0.3 Angstrom are approximately 55% of all C IV systems with W \u003e 0.15 Angstrom, but by z similar or equal to 4 that percentage is less than 37%. Similar conclusions were reached by Sargent, Boksenberg, \u0026 Steidel and by Steidel, primarily at lower redshifts. However, we measure approximately twice the density of C IV systems at 2.3 \u003c z \u003c 3.8 with W \u003e 0.15 Angstrom that was reported by Steidel. The probability that our sample and previous samples come from the same distribution is only similar to2%. But this could be a statistical accident because it is an a posteriori comparison. We believe that the systems that we report are real, and we have no other explanation for this difference. For Si IV absorption lines, there is a 1 sigma hint of evolution with the same sense. In contrast, Lyalpha and Mg II systems are known to show evolution of the opposite sense with more absorbers at larger redshifts. The physical cause of this difference may be a mixture of ionization and chemical evolution effects.", "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. 123(4):1847-1863 (2002)", "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=000174756400004"}]}, "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": "10.1086/339313"}], "subitem_relation_type_id": {"subitem_relation_type_id_text": "https://doi.org/10.1086/339313", "subitem_relation_type_select": "DOI"}}]}, "item_6_rights_62": {"attribute_name": "\u6a29\u5229", "attribute_value_mlt": [{"subitem_rights": "Copyright\u00a9 2002 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 : abundances; galaxies : evolution; quasars : absorption lines"}]}, "item_6_text_70": {"attribute_name": "wosonly keywords", "attribute_value_mlt": [{"subitem_text_value": "MG-II ABSORPTION; HIGH-RESOLUTION; HIGH-REDSHIFT; EVOLUTION; SAMPLE; SPECTRA; QSOS; ALPHA"}]}, "item_6_textarea_68": {"attribute_name": "wosonly abstract", "attribute_value_mlt": [{"subitem_textarea_value": "We present a modest survey of quasar metal line absorption systems at redshifts 2.3-4.5. Relatively high signal-to-noise ratio (similar to25 pixel(-1)) spectra of 18 quasars at 2 Angstrom FWHM resolution show many absorption systems with strong metal lines in the region redward of the Lyalpha emission lines. We conducted a systematic search and found 55 C IV doublets, 19 Si IV doublets, three Mg II doublets, and seven N v doublets. The present data alone hint that the number of C IV absorption doublets per unit redshift, N(z), decreases with increasing redshift for 2.3 \u003c z \u003c 4.5 but at only the 1-2 sigma level, for either an Einstein de Sitter model (Lambda = 0) or a flat universe with Lambda = 0.7. When we combine our sample with published data that extend to lower redshifts, we detect evolution at the 1-4 sigma level, depending on the cosmological model and the strength of the C IV lines. There are fewer C IV systems per unit z with increasing z, and the systems with stronger C IV lines evolve much faster. At z similar or equal to 2.4, C IV with W \u003e 0.3 Angstrom are approximately 55% of all C IV systems with W \u003e 0.15 Angstrom, but by z similar or equal to 4 that percentage is less than 37%. Similar conclusions were reached by Sargent, Boksenberg, \u0026 Steidel and by Steidel, primarily at lower redshifts. However, we measure approximately twice the density of C IV systems at 2.3 \u003c z \u003c 3.8 with W \u003e 0.15 Angstrom that was reported by Steidel. The probability that our sample and previous samples come from the same distribution is only similar to2%. But this could be a statistical accident because it is an a posteriori comparison. We believe that the systems that we report are real, and we have no other explanation for this difference. For Si IV absorption lines, there is a 1 sigma hint of evolution with the same sense. In contrast, Lyalpha and Mg II systems are known to show evolution of the opposite sense with more absorbers at larger redshifts. The physical cause of this difference may be a mixture of ionization and chemical evolution effects."}]}, "item_creator": {"attribute_name": "\u8457\u8005", "attribute_type": "creator", "attribute_value_mlt": [{"creatorNames": [{"creatorName": "Misawa,  T"}], "nameIdentifiers": [{"nameIdentifier": "45894", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Tytler,  D"}], "nameIdentifiers": [{"nameIdentifier": "45895", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Iye,  M"}], "nameIdentifiers": [{"nameIdentifier": "45896", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Storrie-Lombardi,  LJ"}], "nameIdentifiers": [{"nameIdentifier": "45897", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Suzuki,  N"}], "nameIdentifiers": [{"nameIdentifier": "45898", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Wolfe,  AM"}], "nameIdentifiers": [{"nameIdentifier": "45899", "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": "2002_AJ_123_1847.pdf", "filesize": [{"value": "638.2 kB"}], "format": "application/pdf", "future_date_message": "", "is_thumbnail": false, "licensetype": "license_note", "mimetype": "application/pdf", "size": 638200.0, "url": {"label": "2002_AJ_123_1847.pdf", "url": "https://soar-ir.repo.nii.ac.jp/record/15851/files/2002_AJ_123_1847.pdf"}, "version_id": "7cb03dbe-230b-42fb-9c9a-e747caec9c91"}]}, "item_keyword": {"attribute_name": "\u30ad\u30fc\u30ef\u30fc\u30c9", "attribute_value_mlt": [{"subitem_subject": "galaxies : abundances", "subitem_subject_scheme": "Other"}, {"subitem_subject": "galaxies : evolution", "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": "C IV and other metal absorption line systems in 18 z=4 quasars", "item_titles": {"attribute_name": "\u30bf\u30a4\u30c8\u30eb", "attribute_value_mlt": [{"subitem_title": "C IV and other metal absorption line systems in 18 z=4 quasars", "subitem_title_language": "en"}]}, "item_type_id": "6", "owner": "1", "path": ["1544/1545"], "permalink_uri": "http://hdl.handle.net/10091/17257", "pubdate": {"attribute_name": "PubDate", "attribute_value": "2013-12-02"}, "publish_date": "2013-12-02", "publish_status": "0", "recid": "15851", "relation": {}, "relation_version_is_last": true, "title": ["C IV and other metal absorption line systems in 18 z=4 quasars"], "weko_shared_id": -1}
  1. 100 全学教育機構
  2. 1001 学術論文

C IV and other metal absorption line systems in 18 z=4 quasars

http://hdl.handle.net/10091/17257
7c006db2-c269-4772-b87d-c8e7614ab559
名前 / ファイル ライセンス アクション
2002_AJ_123_1847.pdf 2002_AJ_123_1847.pdf (638.2 kB)
Item type 学術雑誌論文 / Journal Article(1)
公開日 2013-12-02
タイトル
言語 en
タイトル C IV and other metal absorption line systems in 18 z=4 quasars
言語
言語 eng
キーワード
主題Scheme Other
主題 galaxies : abundances
キーワード
主題Scheme Other
主題 galaxies : evolution
キーワード
主題Scheme Other
主題 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

WEKO 45894

Misawa, T

Search repository
Tytler, D

× Tytler, D

WEKO 45895

Tytler, D

Search repository
Iye, M

× Iye, M

WEKO 45896

Iye, M

Search repository
Storrie-Lombardi, LJ

× Storrie-Lombardi, LJ

WEKO 45897

Storrie-Lombardi, LJ

Search repository
Suzuki, N

× Suzuki, N

WEKO 45898

Suzuki, N

Search repository
Wolfe, AM

× Wolfe, AM

WEKO 45899

Wolfe, AM

Search repository
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. 123(4):1847-1863 (2002)
書誌情報 ASTRONOMICAL JOURNAL

巻 123, 号 4, p. 1847-1863, 発行日 2002-04
抄録
内容記述タイプ Abstract
内容記述 We present a modest survey of quasar metal line absorption systems at redshifts 2.3-4.5. Relatively high signal-to-noise ratio (similar to25 pixel(-1)) spectra of 18 quasars at 2 Angstrom FWHM resolution show many absorption systems with strong metal lines in the region redward of the Lyalpha emission lines. We conducted a systematic search and found 55 C IV doublets, 19 Si IV doublets, three Mg II doublets, and seven N v doublets. The present data alone hint that the number of C IV absorption doublets per unit redshift, N(z), decreases with increasing redshift for 2.3 < z < 4.5 but at only the 1-2 sigma level, for either an Einstein de Sitter model (Lambda = 0) or a flat universe with Lambda = 0.7. When we combine our sample with published data that extend to lower redshifts, we detect evolution at the 1-4 sigma level, depending on the cosmological model and the strength of the C IV lines. There are fewer C IV systems per unit z with increasing z, and the systems with stronger C IV lines evolve much faster. At z similar or equal to 2.4, C IV with W > 0.3 Angstrom are approximately 55% of all C IV systems with W > 0.15 Angstrom, but by z similar or equal to 4 that percentage is less than 37%. Similar conclusions were reached by Sargent, Boksenberg, & Steidel and by Steidel, primarily at lower redshifts. However, we measure approximately twice the density of C IV systems at 2.3 < z < 3.8 with W > 0.15 Angstrom that was reported by Steidel. The probability that our sample and previous samples come from the same distribution is only similar to2%. But this could be a statistical accident because it is an a posteriori comparison. We believe that the systems that we report are real, and we have no other explanation for this difference. For Si IV absorption lines, there is a 1 sigma hint of evolution with the same sense. In contrast, Lyalpha and Mg II systems are known to show evolution of the opposite sense with more absorbers at larger redshifts. The physical cause of this difference may be a mixture of ionization and chemical evolution effects.
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
関連識別子
識別子タイプ DOI
関連識別子 https://doi.org/10.1086/339313
関連名称
関連名称 10.1086/339313
権利
権利情報 Copyright© 2002 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=000174756400004
戻る
0
views
See details
Views

Versions

Ver.1 2021-03-01 10:12:19.100107
Show All versions

Share

Mendeley CiteULike Twitter Facebook Print Addthis

Cite as

Export

OAI-PMH
  • OAI-PMH JPCOAR
  • OAI-PMH DublinCore
  • OAI-PMH DDI
Other Formats
  • JSON
  • BIBTEX

Confirm


Powered by CERN Data Centre & Invenio


Powered by CERN Data Centre & Invenio