{"created":"2021-03-01T06:32:47.410120+00:00","id":24807,"links":{},"metadata":{"_buckets":{"deposit":"37e16477-126a-40c7-95bf-24dd32a6a93a"},"_deposit":{"id":"24807","owners":[],"pid":{"revision_id":0,"type":"depid","value":"24807"},"status":"published"},"_oai":{"id":"oai:nagoya.repo.nii.ac.jp:00024807","sets":["336:695:696"]},"author_link":["73771","73772","73773","73774","73775","73776","73777","73778","73779","73780","73781","73782","73783","73784","73785"],"item_10_biblio_info_6":{"attribute_name":"書誌情報","attribute_value_mlt":[{"bibliographicIssueDates":{"bibliographicIssueDate":"2017-07-10","bibliographicIssueDateType":"Issued"},"bibliographicIssueNumber":"2","bibliographicPageEnd":"138","bibliographicPageStart":"138","bibliographicVolumeNumber":"843","bibliographic_titles":[{"bibliographic_title":"Astrophysical Journal","bibliographic_titleLang":"en"}]}]},"item_10_description_4":{"attribute_name":"抄録","attribute_value_mlt":[{"subitem_description":"We study the properties of dark matter halos that contain star-forming galaxies at 1.43 ≤ z ≤ 1.74, using the FMOS-COSMOS survey. The sample consists of 516 objects with a detection of the Hα emission line, which represent the star forming population at this epoch, having a stellar mass range of 10^9.57 ≤ M */M ⊙ lesssim 10^11.4 and a star-formation rate range of 15 lesssim SFR/(M ⊙ yr^−1) lesssim ^600. We measure the projected two-point correlation function while carefully taking into account observational biases, and find a significant clustering amplitude at scales of 0.04–10 h ^−1 cMpc, with a correlation length r0 =5.26-0.62^+0.75h^-1cMpc and a bias b =2.44-0.32^+0.38. We interpret our clustering measurement using a halo occupation distribution model. The sample galaxies appear to reside in halos with mass Mh=4.71-1.62^+1.19×10^12h^-1,M⊙ on average, which will likely become present-day halos of mass M h (z = 0) ~ 2 × 10^13 h ^−1 M ⊙, equivalent to the typical halo mass scale of galaxy groups. We then confirm the decline of the stellar-to-halo mass ratio at M h < 10^12 M ⊙, finding M */M h ≈ 5 × 10^−3 at M h = 7. 5 × 10^11 M ⊙, which is lower by a factor of 2–4 than those measured at higher masses (M h ~ 10^12–13 M ⊙). Finally, we use our results to illustrate the future capabilities of Subaru's Prime-Focus Spectrograph, a next-generation instrument that will provide strong constraints on the galaxy-formation scenario by obtaining precise measurements of galaxy clustering at z>1.","subitem_description_language":"en","subitem_description_type":"Abstract"}]},"item_10_identifier_60":{"attribute_name":"URI","attribute_value_mlt":[{"subitem_identifier_type":"DOI","subitem_identifier_uri":"http://doi.org/10.3847/1538-4357/aa789d"},{"subitem_identifier_type":"HDL","subitem_identifier_uri":"http://hdl.handle.net/2237/27029"}]},"item_10_publisher_32":{"attribute_name":"出版者","attribute_value_mlt":[{"subitem_publisher":"IOP publishing","subitem_publisher_language":"en"}]},"item_10_relation_11":{"attribute_name":"DOI","attribute_value_mlt":[{"subitem_relation_type":"isVersionOf","subitem_relation_type_id":{"subitem_relation_type_id_text":"https://doi.org/10.3847/1538-4357/aa789d","subitem_relation_type_select":"DOI"}}]},"item_10_rights_12":{"attribute_name":"権利","attribute_value_mlt":[{"subitem_rights":"© 2017. The American Astronomical Society","subitem_rights_language":"en"}]},"item_10_select_15":{"attribute_name":"著者版フラグ","attribute_value_mlt":[{"subitem_select_item":"publisher"}]},"item_10_source_id_7":{"attribute_name":"ISSN","attribute_value_mlt":[{"subitem_source_identifier":"0004-637X","subitem_source_identifier_type":"PISSN"}]},"item_1615787544753":{"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_access_right":{"attribute_name":"アクセス権","attribute_value_mlt":[{"subitem_access_right":"open access","subitem_access_right_uri":"http://purl.org/coar/access_right/c_abf2"}]},"item_creator":{"attribute_name":"著者","attribute_type":"creator","attribute_value_mlt":[{"creatorNames":[{"creatorName":"Kashino, Daichi","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"73771","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"More, Surhud","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"73772","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"Silverman, John D.","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"73773","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"Daddi, Emanuele","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"73774","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"Renzini, Alvio","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"73775","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"Sanders, David B.","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"73776","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"Rodighiero, Giulia","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"73777","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"Puglisi, Annagrazia","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"73778","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"Kajisawa, Masaru","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"73779","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"Valentino, Francesco","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"73780","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"Kartaltepe, Jeyhan S.","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"73781","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"Fèvre, Olivier Le","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"73782","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"Nagao, Tohru","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"73783","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"Arimoto, Nobuo","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"73784","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"Sugiyama, Naoshi","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"73785","nameIdentifierScheme":"WEKO"}]}]},"item_files":{"attribute_name":"ファイル情報","attribute_type":"file","attribute_value_mlt":[{"accessrole":"open_date","date":[{"dateType":"Available","dateValue":"2018-02-22"}],"displaytype":"detail","filename":"pdf.pdf","filesize":[{"value":"2.7 MB"}],"format":"application/pdf","licensetype":"license_note","mimetype":"application/pdf","url":{"label":"pdf.pdf","objectType":"fulltext","url":"https://nagoya.repo.nii.ac.jp/record/24807/files/pdf.pdf"},"version_id":"62b41ea5-d1da-4008-92ec-4b4c9cdae45b"}]},"item_keyword":{"attribute_name":"キーワード","attribute_value_mlt":[{"subitem_subject":"galaxies: evolution","subitem_subject_scheme":"Other"},{"subitem_subject":"galaxies: formation","subitem_subject_scheme":"Other"},{"subitem_subject":"galaxies: halos","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":"The FMOS-COSMOS Survey of Star-forming Galaxies at Z ~ 1.6. V: Properties of Dark Matter Halos Containing Hα Emitting Galaxies","item_titles":{"attribute_name":"タイトル","attribute_value_mlt":[{"subitem_title":"The FMOS-COSMOS Survey of Star-forming Galaxies at Z ~ 1.6. V: Properties of Dark Matter Halos Containing Hα Emitting Galaxies","subitem_title_language":"en"}]},"item_type_id":"10","owner":"1","path":["696"],"pubdate":{"attribute_name":"PubDate","attribute_value":"2017-10-11"},"publish_date":"2017-10-11","publish_status":"0","recid":"24807","relation_version_is_last":true,"title":["The FMOS-COSMOS Survey of Star-forming Galaxies at Z ~ 1.6. V: Properties of Dark Matter Halos Containing Hα Emitting Galaxies"],"weko_creator_id":"1","weko_shared_id":-1},"updated":"2023-01-16T04:13:41.392480+00:00"}