{"created":"2023-06-20T13:22:38.064681+00:00","id":3294,"links":{},"metadata":{"_buckets":{"deposit":"fe7c1e54-ca66-43a4-a027-058233c79764"},"_deposit":{"created_by":21,"id":"3294","owners":[21],"pid":{"revision_id":0,"type":"depid","value":"3294"},"status":"published"},"_oai":{"id":"oai:ir.soken.ac.jp:00003294","sets":["1:274"]},"author_link":["750","754","752","743","745","744","734","746","751","748","753","749","738","747"],"item_10001_biblio_info_7":{"attribute_name":"書誌情報","attribute_value_mlt":[{"bibliographicIssueDates":{"bibliographicIssueDate":"2003-10","bibliographicIssueDateType":"Issued"},"bibliographicIssueNumber":"5","bibliographicPageEnd":"L64","bibliographicPageStart":"L61","bibliographicVolumeNumber":"55","bibliographic_titles":[{"bibliographic_title":"Publications of the Astronomical Society of Japan "},{"bibliographic_title":"Publications of the Astronomical Society of Japan ","bibliographic_titleLang":"en"}]}]},"item_10001_creator_3":{"attribute_name":"著者別名","attribute_type":"creator","attribute_value_mlt":[{"creatorNames":[{"creatorName":"池内, 了"}],"nameIdentifiers":[{},{},{}]}]},"item_10001_description_19":{"attribute_name":"フォーマット","attribute_value_mlt":[{"subitem_description":"application/pdf","subitem_description_type":"Other"}]},"item_10001_description_5":{"attribute_name":"抄録","attribute_value_mlt":[{"subitem_description":"Supernova remnants ( = SNR) are suggested to be sites of cosmic-ray acceleration. In particular, it has been an issue of keen interest whether cosmic ray protons are being accelerated in a SNR which emits TeV γ-rays. A crucial observational test for this is to find dense molecular gas towards the SNR, because such molecular gas can best verify the existence of cosmic-ray protons via pion decay to γ-rays. Here, we show that new high-resolution mm-wave observations of interstellar CO molecule have revealed molecular gas at 1kpc distance interacting with the TeV γ-ray SNR G 347.3 - 0.5, and that a molecular cloud of ˜ 200 solar masses is clearly associated with the TeV γ-ray peak, providing strong evidence for proton acceleration. We have estimated the total energy of accelerated protons to be ˜ 1048 erg, which corresponds to an acceleration efficiency of ˜ 0.001, posing an observational constraint on the proton acceleration. ","subitem_description_type":"Abstract"}]},"item_10001_publisher_8":{"attribute_name":"出版者","attribute_value_mlt":[{"subitem_publisher":"The Astronomical Society of Japan"}]},"item_10001_relation_14":{"attribute_name":"DOI","attribute_value_mlt":[{"subitem_relation_name":[{"subitem_relation_name_text":"10.1093/pasj/55.5.L61"}],"subitem_relation_type":"isIdenticalTo","subitem_relation_type_id":{"subitem_relation_type_id_text":"https://doi.org/10.1093/pasj/55.5.L61","subitem_relation_type_select":"DOI"}}]},"item_10001_relation_17":{"attribute_name":"関連サイト","attribute_value_mlt":[{"subitem_relation_name":[{"subitem_relation_name_text":"Copyright"}],"subitem_relation_type_id":{"subitem_relation_type_id_text":"http://pasj.asj.or.jp/info/subscription.html","subitem_relation_type_select":"URI"}}]},"item_10001_rights_15":{"attribute_name":"権利","attribute_value_mlt":[{"subitem_rights":"\u0001© 2003. The Astronomical Society of Japan."}]},"item_10001_source_id_9":{"attribute_name":"ISSN","attribute_value_mlt":[{"subitem_source_identifier":"00046264","subitem_source_identifier_type":"ISSN"}]},"item_10001_version_type_20":{"attribute_name":"著者版フラグ","attribute_value_mlt":[{"subitem_version_resource":"http://purl.org/coar/version/c_970fb48d4fbd8a85","subitem_version_type":"VoR"}]},"item_creator":{"attribute_name":"著者","attribute_type":"creator","attribute_value_mlt":[{"creatorNames":[{"creatorName":"FUKUI, Yasuo"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"MORIGUCHI, Yoshiaki"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"TAMURA, Keisuke"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"YAMAMOTO, Hiroaki"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"TAWARA, Yuzuru"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"MIZUNO, Norikazu"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"ONISHI, Toshikazu"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"MIZUNO, Akira"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"UCHIYAMA, Yasunobu"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"HIRAGA, Junko"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"TAKAHASHI, Tadayuki"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"YAMASHITA, Koujin"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"IKEUCHI, Satoru"}],"nameIdentifiers":[{}]}]},"item_files":{"attribute_name":"ファイル情報","attribute_type":"file","attribute_value_mlt":[{"accessrole":"open_date","date":[{"dateType":"Available","dateValue":"2012-12-17"}],"displaytype":"simple","filename":"55052495.pdf","filesize":[{"value":"432.0 kB"}],"format":"application/pdf","licensetype":"license_11","mimetype":"application/pdf","url":{"label":"55052495","url":"https://ir.soken.ac.jp/record/3294/files/55052495.pdf"},"version_id":"aaba90f1-1ba6-4ee7-b18b-6f625a7d1fe8"}]},"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":"Discovery of Interacting Molecular Gas toward the TeV Gamma-Ray Peak of the SNR G 347.3-0.5","item_titles":{"attribute_name":"タイトル","attribute_value_mlt":[{"subitem_title":"Discovery of Interacting Molecular Gas toward the TeV Gamma-Ray Peak of the SNR G 347.3-0.5"},{"subitem_title":"Discovery of Interacting Molecular Gas toward the TeV Gamma-Ray Peak of the SNR G 347.3-0.5","subitem_title_language":"en"}]},"item_type_id":"10001","owner":"21","path":["95","274"],"pubdate":{"attribute_name":"公開日","attribute_value":"2012-12-13"},"publish_date":"2012-12-13","publish_status":"0","recid":"3294","relation_version_is_last":true,"title":["Discovery of Interacting Molecular Gas toward the TeV Gamma-Ray Peak of the SNR G 347.3-0.5"],"weko_creator_id":"21","weko_shared_id":21},"updated":"2023-06-20T14:11:59.394099+00:00"}