{"created":"2021-03-01T06:27:20.829600+00:00","id":19821,"links":{},"metadata":{"_buckets":{"deposit":"8231ea9b-1bb9-4296-ba0c-1f35adc165bb"},"_deposit":{"id":"19821","owners":[],"pid":{"revision_id":0,"type":"depid","value":"19821"},"status":"published"},"_oai":{"id":"oai:nagoya.repo.nii.ac.jp:00019821","sets":["879:1183:1640:1731"]},"author_link":["58045","58046","58047","58048","58049","58050","58051","58052","58053","58054"],"item_1615768549627":{"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_9_biblio_info_6":{"attribute_name":"書誌情報","attribute_value_mlt":[{"bibliographicIssueDates":{"bibliographicIssueDate":"1965-03-25","bibliographicIssueDateType":"Issued"},"bibliographicPageEnd":"48","bibliographicPageStart":"35","bibliographicVolumeNumber":"12","bibliographic_titles":[{"bibliographic_title":"Proceedings of the Research Institute of Atmospherics, Nagoya University","bibliographic_titleLang":"en"}]}]},"item_9_description_4":{"attribute_name":"抄録","attribute_value_mlt":[{"subitem_description":"The observations at 9.4 Ge/s of Cygnus A, Taurus A, Orion Nebula and Omega Nebula have been made with the 2. 2' fan beam of the 16-element interferometer and the maser amplifier. Cygnus A has also been observed with the 0.7' fan beam of the compound interferometer. The maser amplifier for radio astronomical observations has been developed, with special emphasis on the high stable performance and the convenience of adjustment and handling in the field installations. The voltage-gain band-width product is about 100 Mc/s, the noise temperature is 40 K and the gain instability is 0.1 db up to 30 minutes and 0.2 db up to 2 hours. The brightness distributions, sizes and flux densities of the radio sources have been compared with the results of the earlier observations. Flux densities of the sources have been derived from that of the sun, comparing the areas under the drift-curves of the sources with that of the sun. The results of flux density measurements show that our scale of flux density at 9.4 Gc/s of the solar observations is nearly equal to the average scale of the galactic or extragalactic observations.","subitem_description_language":"en","subitem_description_type":"Abstract"}]},"item_9_identifier_60":{"attribute_name":"URI","attribute_value_mlt":[{"subitem_identifier_type":"HDL","subitem_identifier_uri":"http://hdl.handle.net/2237/21875"}]},"item_9_publisher_32":{"attribute_name":"出版者","attribute_value_mlt":[{"subitem_publisher":"The Research Institute of Atmospherics, Nagoya University","subitem_publisher_language":"en"}]},"item_9_select_15":{"attribute_name":"著者版フラグ","attribute_value_mlt":[{"subitem_select_item":"publisher"}]},"item_9_source_id_7":{"attribute_name":"ISSN（print）","attribute_value_mlt":[{"subitem_source_identifier":"0077-264X","subitem_source_identifier_type":"PISSN"}]},"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":"TANAKA, Haruo","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"58045","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"KAKINUMA, Takakiyo","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"58046","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"YAMASHITA, Takashi","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"58047","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"UCHIDA, Hidenari","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"58048","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"INABA, Humio","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"58049","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"TSURU, Hiroshi","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"58050","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"TAKAHASHI, Kenichi","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"58051","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"YOSHIKAWA, Syogo","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"58052","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"HOZUMI, Hidekichi","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"58053","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"HAYASHI, Hiromi","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"58054","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":"2018-02-21"}],"displaytype":"detail","filename":"proria_12_35.pdf","filesize":[{"value":"1.9 MB"}],"format":"application/pdf","licensetype":"license_note","mimetype":"application/pdf","url":{"label":"proria_12_35.pdf","objectType":"fulltext","url":"https://nagoya.repo.nii.ac.jp/record/19821/files/proria_12_35.pdf"},"version_id":"4f1a9c9c-6f88-44de-aed0-005bff872652"}]},"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":"OBSERVATIONS OF RADIO SOURCES AT 9.4 GC/S WITH MASER AND HIGH-RESOLUTION INTERFEROMETER","item_titles":{"attribute_name":"タイトル","attribute_value_mlt":[{"subitem_title":"OBSERVATIONS OF RADIO SOURCES AT 9.4 GC/S WITH MASER AND HIGH-RESOLUTION INTERFEROMETER","subitem_title_language":"en"}]},"item_type_id":"9","owner":"1","path":["1731"],"pubdate":{"attribute_name":"PubDate","attribute_value":"2015-05-12"},"publish_date":"2015-05-12","publish_status":"0","recid":"19821","relation_version_is_last":true,"title":["OBSERVATIONS OF RADIO SOURCES AT 9.4 GC/S WITH MASER AND HIGH-RESOLUTION INTERFEROMETER"],"weko_creator_id":"1","weko_shared_id":-1},"updated":"2023-01-26T05:13:03.757612+00:00"}