{"created":"2023-06-20T15:07:18.271533+00:00","id":36665,"links":{},"metadata":{"_buckets":{"deposit":"eeacd63d-b034-41fb-b80a-c8d0b07a7276"},"_deposit":{"created_by":1,"id":"36665","owners":[1],"pid":{"revision_id":0,"type":"depid","value":"36665"},"status":"published"},"_oai":{"id":"oai:jaxa.repo.nii.ac.jp:00036665","sets":["1887:1890","1896:1898:1899:1991"]},"author_link":["424166","424164","424165"],"item_9_biblio_info_10":{"attribute_name":"書誌情報","attribute_value_mlt":[{"bibliographicIssueDates":{"bibliographicIssueDate":"2000-12","bibliographicIssueDateType":"Issued"},"bibliographicPageEnd":"122","bibliographicPageStart":"115","bibliographicVolumeNumber":"14","bibliographic_titles":[{},{"bibliographic_title":"The Institute of Space and Astronautical Science report. S.P. : Mid- and Far-Infrared Astronomy and Future Space Mission","bibliographic_titleLang":"en"}]}]},"item_9_description_17":{"attribute_name":"抄録（英）","attribute_value_mlt":[{"subitem_description":"Infrared (IR) dust emission from galaxies is frequently used as an indicator of starformation rate (SFR). However, the effect of dust-to-gas ratio, or amount of dust, on the con-version law from IR luminosity to SFR has not been considered. In this paper, we present aconvenient formula including the effect. In order to obtain the dependence of the dust-to-gasratio, we extend the formula derived in our previous paper, in which a theoretical formula con-verting IR luminosity to SFR was derived. That formula was expressed as SFR=(M yr-1) ={3.3 ×10-10(1-η)/(0.4 - 0.2f + 0.6ε)}(LIR=L), where f is the fraction of ionizing photons ab-sorbed by hydrogen, εis the effciency of dust absorption for nonionizing photons, ηis the cirrusfraction of observed dust luminosity, and LIR is the observed luminosity of dust emission in the8-1000-μm range. Throughout the current discussion, we construct an algorithm to relate f andε, both of which depend on the dust-to-gas ratio, to the metallicity, by adopting a galactic relationbetween dust-to-gas ratio and metallicity. Thus, we estimate the metallicity dependence of ourformula. We apply the result to the cosmic star formation history and find that the comoving SFRat z ～ 3 calculated from previous empirical formulae is underestimated by the factor of 4. Finally,we comment on the HII/L2 mission (SPICA).","subitem_description_type":"Other"}]},"item_9_description_32":{"attribute_name":"資料番号","attribute_value_mlt":[{"subitem_description":"資料番号: SA4588073000","subitem_description_type":"Other"}]},"item_9_publisher_8":{"attribute_name":"出版者","attribute_value_mlt":[{"subitem_publisher":"宇宙科学研究所"}]},"item_9_publisher_9":{"attribute_name":"出版者（英）","attribute_value_mlt":[{"subitem_publisher":"Institute of Space and Astronautical Science"}]},"item_9_source_id_21":{"attribute_name":"ISSN","attribute_value_mlt":[{"subitem_source_identifier":"0288-433X","subitem_source_identifier_type":"ISSN"}]},"item_9_source_id_24":{"attribute_name":"書誌レコードID","attribute_value_mlt":[{"subitem_source_identifier":"AA10455137","subitem_source_identifier_type":"NCID"}]},"item_9_text_7":{"attribute_name":"著者所属（英）","attribute_value_mlt":[{"subitem_text_language":"en","subitem_text_value":"Department of Astronomy, Faculty of Science, Kyoto University"},{"subitem_text_language":"en","subitem_text_value":"Department of Astronomy, Faculty of Science, Kyoto University"},{"subitem_text_language":"en","subitem_text_value":"Department of Astronomy, Faculty of Science, Kyoto University"}]},"item_creator":{"attribute_name":"著者","attribute_type":"creator","attribute_value_mlt":[{"creatorNames":[{"creatorName":"HIRASHITA, Hiroyuki","creatorNameLang":"en"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"INOUE, Akio K.","creatorNameLang":"en"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"KAMAYA, Hideyuki","creatorNameLang":"en"}],"nameIdentifiers":[{}]}]},"item_files":{"attribute_name":"ファイル情報","attribute_type":"file","attribute_value_mlt":[{"accessrole":"open_date","date":[{"dateType":"Available","dateValue":"2020-01-24"}],"displaytype":"detail","filename":"SA4588073.pdf","filesize":[{"value":"235.3 kB"}],"format":"application/pdf","licensetype":"license_note","mimetype":"application/pdf","url":{"label":"SA4588073.pdf","url":"https://jaxa.repo.nii.ac.jp/record/36665/files/SA4588073.pdf"},"version_id":"fb255705-443b-475d-b03c-a509140b6a96"}]},"item_language":{"attribute_name":"言語","attribute_value_mlt":[{"subitem_language":"jpn"}]},"item_resource_type":{"attribute_name":"資源タイプ","attribute_value_mlt":[{"resourcetype":"departmental bulletin paper","resourceuri":"http://purl.org/coar/resource_type/c_6501"}]},"item_title":"Chemical Evolution and Far-Infrared Emission of Galaxies","item_titles":{"attribute_name":"タイトル","attribute_value_mlt":[{"subitem_title":"Chemical Evolution and Far-Infrared Emission of Galaxies","subitem_title_language":"en"}]},"item_type_id":"9","owner":"1","path":["1890","1991"],"pubdate":{"attribute_name":"公開日","attribute_value":"2015-03-26"},"publish_date":"2015-03-26","publish_status":"0","recid":"36665","relation_version_is_last":true,"title":["Chemical Evolution and Far-Infrared Emission of Galaxies"],"weko_creator_id":"1","weko_shared_id":-1},"updated":"2023-06-20T22:51:42.079345+00:00"}