{"@context":{"@vocab":"https://cir.nii.ac.jp/schema/1.0/","rdfs":"http://www.w3.org/2000/01/rdf-schema#","dc":"http://purl.org/dc/elements/1.1/","dcterms":"http://purl.org/dc/terms/","foaf":"http://xmlns.com/foaf/0.1/","prism":"http://prismstandard.org/namespaces/basic/2.0/","cinii":"http://ci.nii.ac.jp/ns/1.0/","datacite":"https://schema.datacite.org/meta/kernel-4/","ndl":"http://ndl.go.jp/dcndl/terms/","jpcoar":"https://github.com/JPCOAR/schema/blob/master/2.0/"},"@id":"https://cir.nii.ac.jp/crid/1360004234658672000.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1093/mnras/stu2738"}},{"identifier":{"@type":"URI","@value":"http://academic.oup.com/mnras/article-pdf/448/2/1240/9503614/stu2738.pdf"}},{"identifier":{"@type":"DOI","@value":"10.25916/sut.26227793.v1"}},{"identifier":{"@type":"DOI","@value":"10.25916/sut.26227793"}},{"identifier":{"@type":"DOI","@value":"10.25916/sut.26227793.v2"}},{"identifier":{"@type":"HANDLE","@value":"1959.3/393404"}}],"resourceType":"学術雑誌論文(journal article)","dc:title":[{"@value":"Large-scale environment of z ∼ 5.7 C iv absorption systems –II. Spectroscopy of Lyman α emitters★"}],"description":[{"notation":[{"@value":"The flow of baryons to and from a galaxy, which is fundamental for galaxy formation and evolution, can be studied with galaxy-metal absorption system pairs. Our search for galaxies around C IV absorption systems at z ˜ 5.7 showed an excess of photometric Lyman α emitter (LAE) candidates in the fields J1030+0524 and J1137+3549. Here, we present spectroscopic follow-up of 33 LAEs in both fields. In the first field, three out of the five LAEs within 10h-1 projected comoving Mpc from the C IV system are within ±500 km s-1 from the absorption at z_{C IV}=5.7242± 0.0001. The closest candidate (LAE 103027+052419) is robustly confirmed at 212.8^{+14}_{-0.4}h^{-1} physical kpc from the C IV system. In the second field, the LAE sample is selected at a lower redshift (Δz ˜ 0.04) than the C IV absorption system as a result of the filter transmission and, thus, do not trace its environment. The observed properties of LAE 103027+052419 indicate that it is near the high-mass end of the LAE distribution, probably having a large H I column density and large-scale outflows. Therefore, our results suggest that the C IV system is likely produced by a star-forming galaxy which has been injecting metals into the intergalactic medium since z > 6. Thus, the C IV system is either produced by LAE 103027+052419, implying that outflows can enrich larger volumes at z > 6 than at z ˜ 3.5, or an undetected dwarf galaxy. In either case, C IV systems like this one trace the ionized intergalactic medium at the end of cosmic hydrogen reionization and may trace the sources of the ionizing flux density."}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380004234658672128","@type":"Researcher","foaf:name":[{"@value":"C. Gonzalo Díaz"}]},{"@id":"https://cir.nii.ac.jp/crid/1380004234658672000","@type":"Researcher","foaf:name":[{"@value":"Emma V. Ryan-Weber"}]},{"@id":"https://cir.nii.ac.jp/crid/1380004234658672002","@type":"Researcher","foaf:name":[{"@value":"Jeff Cooke"}]},{"@id":"https://cir.nii.ac.jp/crid/1420564276163282176","@type":"Researcher","personIdentifier":[{"@type":"KAKEN_RESEARCHERS","@value":"40724662"},{"@type":"NRID","@value":"1000040724662"},{"@type":"NRID","@value":"9000018553043"},{"@type":"NRID","@value":"9000408809834"}],"foaf:name":[{"@value":"Yusei Koyama"}]},{"@id":"https://cir.nii.ac.jp/crid/1380004234658672001","@type":"Researcher","foaf:name":[{"@value":"Masami Ouchi"}]}],"contributor":[{"@id":"https://cir.nii.ac.jp/crid/1891147691091135104","@type":"Researcher","foaf:name":[{"@value":"Swinburne University of Technology"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"00358711"},{"@type":"EISSN","@value":"13652966"}],"prism:publicationName":[{"@value":"Monthly Notices of the Royal Astronomical Society"}],"dc:publisher":[{"@value":"Oxford University Press (OUP)"}],"prism:publicationDate":"2015-02-12","prism:volume":"448","prism:number":"2","prism:startingPage":"1240","prism:endingPage":"1270"},"reviewed":"false","dcterms:accessRights":"http://purl.org/coar/access_right/c_abf2","url":[{"@id":"http://academic.oup.com/mnras/article-pdf/448/2/1240/9503614/stu2738.pdf"}],"createdAt":"2015-02-12","modifiedAt":"2019-08-20","foaf:topic":[{"@id":"https://cir.nii.ac.jp/all?q=Cosmology%20and%20extragalactic%20astronomy","dc:title":"Cosmology and extragalactic astronomy"},{"@id":"https://cir.nii.ac.jp/all?q=Astrophysics%20-%20Astrophysics%20of%20Galaxies","dc:title":"Astrophysics - Astrophysics of Galaxies"},{"@id":"https://cir.nii.ac.jp/all?q=520","dc:title":"520"}],"project":[{"@id":"https://cir.nii.ac.jp/crid/1040282257293107328","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"26800107"},{"@type":"JGN","@value":"JP26800107"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-26800107/"}],"notation":[{"@language":"ja","@value":"ミクロな視点で解き明かす銀河団銀河の形成史"},{"@language":"en","@value":"Microscopic views of cluster galaxy formation"}]}],"relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1360001114131869952","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"The First Galaxies"}]},{"@id":"https://cir.nii.ac.jp/crid/1360011144217942784","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"DEMOGRAPHICS AND PHYSICAL PROPERTIES OF GAS OUTFLOWS/INFLOWS AT 0.4 <<i>z</i>< 1.4"}]},{"@id":"https://cir.nii.ac.jp/crid/1360011146203593472","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"THE HETDEX PILOT SURVEY. 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