{"_buckets": {"deposit": "df7993bd-10f3-4ce3-9224-f6a784c341a1"}, "_deposit": {"created_by": 1, "id": "31747", "owners": [1], "pid": {"revision_id": 0, "type": "depid", "value": "31747"}, "status": "published"}, "_oai": {"id": "oai:jaxa.repo.nii.ac.jp:00031747", "sets": ["1890", "1910"]}, "author_link": ["406051", "406048", "406050", "406052", "406053", "406054", "406049", "406047"], "item_9_alternative_title_2": {"attribute_name": "その他のタイトル（英）", "attribute_value_mlt": [{"subitem_alternative_title": "Balloon Observations of Galactic Infrared Radiations"}]}, "item_9_biblio_info_10": {"attribute_name": "書誌情報", "attribute_value_mlt": [{"bibliographicIssueDates": {"bibliographicIssueDate": "1977-09", "bibliographicIssueDateType": "Issued"}, "bibliographicIssueNumber": "3_B", "bibliographicPageEnd": "843", "bibliographicPageStart": "823", "bibliographicVolumeNumber": "13", "bibliographic_titles": [{"bibliographic_title": "東京大学宇宙航空研究所報告"}]}]}, "item_9_description_16": {"attribute_name": "抄録", "attribute_value_mlt": [{"subitem_description": "視野1°角の気球望遠鏡により波長2.4μmにおいて我々の銀河系の観測を行い,銀経l=350°～30°,銀緯|b|O°の領域の表面輝度の分布を得た その輝度分布は,銀経方向に約15゜,銀線緯方向に約7.5°の広がりを持ち,かつl≦10゜に鋭い輝度の集中を示すBulge成分と銀河面上での輝度分布がl=10°～30゜において平坦でその幅が約4°と非常に狭いDisk成分に大別することができる.微細構造としてl=355゜,b=0°の位置に広がった赤外線源を発見した.→観測された輝度分布には,銀河中心方向に星間塵によると思われる強い吸収が認められた.吸収を受けない前の輝度分布をアンドロメダ星雲との類似性から仮定して,星間塵の分布を求めてみると,CO分子の観測で見出された5Kpc Ringに伴なう大量のダスト以外に,銀河中心に集中したダストが存在することが予想される.これらの結果をもとに,銀河系内における星とダストの分布について1つのモデルを組立て,種々の観測結果との比較を試みる.", "subitem_description_type": "Abstract"}]}, "item_9_description_32": {"attribute_name": "資料番号", "attribute_value_mlt": [{"subitem_description": "資料番号: SA0124784000", "subitem_description_type": "Other"}]}, "item_9_publisher_8": {"attribute_name": "出版者", "attribute_value_mlt": [{"subitem_publisher": "東京大学宇宙航空研究所"}]}, "item_9_source_id_21": {"attribute_name": "ISSN", "attribute_value_mlt": [{"subitem_source_identifier": "0563-8100", "subitem_source_identifier_type": "ISSN"}]}, "item_9_source_id_24": 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