{"created":"2023-06-20T15:07:18.173215+00:00","id":36663,"links":{},"metadata":{"_buckets":{"deposit":"89868743-aafe-4723-a541-88929e31a583"},"_deposit":{"created_by":1,"id":"36663","owners":[1],"pid":{"revision_id":0,"type":"depid","value":"36663"},"status":"published"},"_oai":{"id":"oai:jaxa.repo.nii.ac.jp:00036663","sets":["1887:1890","1896:1898:1899:1991"]},"author_link":["424160"],"item_9_biblio_info_10":{"attribute_name":"書誌情報","attribute_value_mlt":[{"bibliographicIssueDates":{"bibliographicIssueDate":"2000-12","bibliographicIssueDateType":"Issued"},"bibliographicPageEnd":"106","bibliographicPageStart":"99","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":"With the advent of ISO, mid-infrared spectroscopy has become sensitive enoughfor detailed analyses of sizeable samples of galaxies. Mid-infrared aromatic emission features aredetected strongly and ubiquitously in star forming galaxies. They are absent close to an activegalactic nucleus but can be strong on larger scales of the AGN host, in particular, if there is intensecircumnuclear star formation. Through their nebular emission, hot star populations can be studiedin dusty environments like starburst galaxies. Starbursts seem to be normal in their hot star initialmass function but short lived due to strong negative feedback. The rich fine structure and coronalline spectrum of active galaxies can be used to reconstruct the otherwise unobservable extremeultraviolet emission of the AGN. Mid-infrared emission lines and continuum features provide newdiagnostics to discriminate between starburst and AGN activity in obscured galaxies. Using thesetools, most ultraluminous infrared galaxies are found to be predominantly starburst powered.Trends can be searched for in a larger sample of ULIRGs. The fraction of AGNs increases withluminosity above ～ 3 ×1012L, but there is no obvious trend for ULIRGs to be more AGN-likewith more advanced merger phase.","subitem_description_type":"Other"}]},"item_9_description_32":{"attribute_name":"資料番号","attribute_value_mlt":[{"subitem_description":"資料番号: SA4588054000","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":"Max-Planck-Institut für extraterrestrische Physik"}]},"item_creator":{"attribute_name":"著者","attribute_type":"creator","attribute_value_mlt":[{"creatorNames":[{"creatorName":"Dieter, LUTZ","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":"SA4588054.pdf","filesize":[{"value":"463.0 kB"}],"format":"application/pdf","licensetype":"license_note","mimetype":"application/pdf","url":{"label":"SA4588054.pdf","url":"https://jaxa.repo.nii.ac.jp/record/36663/files/SA4588054.pdf"},"version_id":"6e71b77f-27d8-4c82-8d58-7fab56fb270a"}]},"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":"departmental bulletin paper","resourceuri":"http://purl.org/coar/resource_type/c_6501"}]},"item_title":"ISO Spectroscopy of ULIRGs and AGN: Lessons for Future Missions","item_titles":{"attribute_name":"タイトル","attribute_value_mlt":[{"subitem_title":"ISO Spectroscopy of ULIRGs and AGN: Lessons for Future Missions","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":"36663","relation_version_is_last":true,"title":["ISO Spectroscopy of ULIRGs and AGN: Lessons for Future Missions"],"weko_creator_id":"1","weko_shared_id":-1},"updated":"2023-06-20T22:51:45.941231+00:00"}