{"_buckets": {"deposit": "8e5fac86-292a-4c06-b14d-b961310cc330"}, "_deposit": {"id": "28403", "owners": [], "pid": {"revision_id": 0, "type": "depid", "value": "28403"}, "status": "published"}, "_oai": {"id": "oai:nagoya.repo.nii.ac.jp:00028403", "sets": ["2028"]}, "author_link": ["92963", "92964", "92965", "92966", "92967", "92968", "92969", "92970", "92971", "92972", "92973", "92974", "92975", "92976", "92977", "92978"], "item_10_biblio_info_6": {"attribute_name": "書誌情報", "attribute_value_mlt": [{"bibliographicIssueDates": {"bibliographicIssueDate": "2019-05-01", "bibliographicIssueDateType": "Issued"}, "bibliographicIssueNumber": "1", "bibliographicPageStart": "37", "bibliographicVolumeNumber": "876", "bibliographic_titles": [{"bibliographic_title": "The Astrophysical Journal", "bibliographic_titleLang": "en"}]}]}, "item_10_description_4": {"attribute_name": "抄録", "attribute_value_mlt": [{"subitem_description": "We present a detailed morphological study of TeV gamma-rays, synchrotron radiation, and interstellar gas in the young Type Ia supernova remnant (SNR) RCW 86. We find that the interstellar atomic gas shows good spatial correlation with the gamma-rays, indicating that the TeV gamma-rays from RCW 86 are likely predominantly of hadronic origin. In contrast, the spatial correlation between the interstellar molecular cloud and the TeV gamma-rays is poor in the southeastern shell of the SNR. We argue that this poor correlation can be attributed to the low-energy cosmic rays (~1 TeV) not penetrating into the dense molecular cloud due to an enhancement of the turbulent magnetic field around the dense cloud of ~10–100 μG. We also find that the southwestern shell, which is bright in both synchrotron X-ray and radio continuum radiation, shows a significant gamma-ray excess compared with the interstellar proton column density, suggesting that leptonic gamma-rays via inverse Compton scattering possibly contribute alongside the hadronic gamma-rays. The total cosmic-ray energies of the young TeV gamma-ray SNRs—RX J1713.7−3946, Vela Jr, HESS J1731−347, and RCW 86—are roughly similar, which indicates that cosmic rays can be accelerated in both the core-collapse and Type Ia supernovae. The total energy of cosmic rays derived using the gas density, ~1048–1049 erg, gives a safe lower limit due mainly to the low filling factor of interstellar gas within the shell.", "subitem_description_language": "en", "subitem_description_type": "Abstract"}]}, "item_10_publisher_32": {"attribute_name": "出版者", "attribute_value_mlt": [{"subitem_publisher": "IOP publishing", "subitem_publisher_language": "en"}]}, "item_10_relation_11": {"attribute_name": "DOI", "attribute_value_mlt": [{"subitem_relation_type": "isVersionOf", "subitem_relation_type_id": {"subitem_relation_type_id_text": "https://doi.org/10.3847/1538-4357/ab108f", "subitem_relation_type_select": "DOI"}}]}, "item_10_rights_12": {"attribute_name": "権利", "attribute_value_mlt": [{"subitem_rights": "© 2019. The American Astronomical Society", "subitem_rights_language": "en"}]}, "item_10_select_15": {"attribute_name": "著者版フラグ", "attribute_value_mlt": [{"subitem_select_item": "publisher"}]}, "item_10_source_id_61": {"attribute_name": "ISSN（print）", "attribute_value_mlt": [{"subitem_source_identifier": "1538-4357", "subitem_source_identifier_type": "PISSN"}]}, "item_1615787544753": {"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_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": "Sano, H.", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "92963", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Rowell, G.", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "92964", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Reynoso, E. M.", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "92965", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Jung-Richardt, I.", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "92966", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Yamane, Y.", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "92967", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Nagaya, T.", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "92968", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Yoshiike, S.", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "92969", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Hayashi, K.", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "92970", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Torii, K.", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "92971", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Maxted, N.", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "92972", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Mitsuishi, I.", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "92973", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Inoue, T.", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "92974", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Inutsuka, S.", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "92975", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Yamamoto, H.", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "92976", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Tachihara, K.", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "92977", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Fukui, Y.", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "92978", "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": "2019-08-20"}], "displaytype": "detail", "download_preview_message": "", "file_order": 0, "filename": "Sano_2019_ApJ_876_37.pdf", "filesize": [{"value": "8.3 MB"}], "format": "application/pdf", "future_date_message": "", "is_thumbnail": false, "licensetype": "license_note", "mimetype": "application/pdf", "size": 8300000.000000001, "url": {"label": "Sano_2019_ApJ_876_37", "objectType": "fulltext", "url": "https://nagoya.repo.nii.ac.jp/record/28403/files/Sano_2019_ApJ_876_37.pdf"}, "version_id": "c0e70c73-6ec5-450e-8fc0-5c388372a3f3"}]}, "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": "Possible Evidence for Cosmic-Ray Acceleration in the Type Ia SNR RCW 86: Spatial Correlation between TeV Gamma-Rays and Interstellar Atomic Protons", "item_titles": {"attribute_name": "タイトル", "attribute_value_mlt": [{"subitem_title": "Possible Evidence for Cosmic-Ray Acceleration in the Type Ia SNR RCW 86: Spatial Correlation between TeV Gamma-Rays and Interstellar Atomic Protons", "subitem_title_language": "en"}]}, "item_type_id": "10", "owner": "1", "path": ["2028"], "permalink_uri": "http://hdl.handle.net/2237/00030596", "pubdate": {"attribute_name": "PubDate", "attribute_value": "2019-08-20"}, "publish_date": "2019-08-20", "publish_status": "0", "recid": "28403", "relation": {}, "relation_version_is_last": true, "title": ["Possible Evidence for Cosmic-Ray Acceleration in the Type Ia SNR RCW 86: Spatial Correlation between TeV Gamma-Rays and Interstellar Atomic Protons"], "weko_shared_id": -1}