{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:2346U55TNXROC4PWB55NHXEACZ","short_pith_number":"pith:2346U55T","schema_version":"1.0","canonical_sha256":"d6f9ea77b36de2e171f60f7ad3dc801645c7f34502ae927dd280885d906d0f4d","source":{"kind":"arxiv","id":"2310.17908","version":2},"attestation_state":"computed","paper":{"title":"On the Doublet Flux Ratio of Mg II Resonance Lines in and Around Galaxies","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Kwang-Il Seon","submitted_at":"2023-10-27T05:57:04Z","abstract_excerpt":"Observations of metallic doublet emission lines, particularly Mg II 2796, 2803, provide crucial information for understanding galaxies and their circumgalactic medium. This study explores the effects of resonant scattering on the Mg II doublet lines and the stellar continuum in spherical and cylindrical geometries. Our findings show that under certain circumstances, resonance scattering can cause an increase in the doublet flux ratio and the escaping flux of the lines beyond what are expected in optically thin spherical media. As expected, the doublet ratio is consistently lower than the intri"},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":false,"formal_links_present":false},"canonical_record":{"source":{"id":"2310.17908","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.GA","submitted_at":"2023-10-27T05:57:04Z","cross_cats_sorted":[],"title_canon_sha256":"a71fb7fdc8907f5291da3e6ac7d0865fd1ce659cadcbdae6b076960dd3e350e3","abstract_canon_sha256":"fbffe25e252459a1d2ae1d520d68564845547acd4dbc66b282aa19e27bda951e"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T08:31:42.786332Z","signature_b64":"0ySGpfrGbzy3Ie0SF543Q+phKNFU2QSJmAXU363rMkpX3F8CIm/KaglLlbz0XSybpDo6YhfL3zYP2ZlH2JUWAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d6f9ea77b36de2e171f60f7ad3dc801645c7f34502ae927dd280885d906d0f4d","last_reissued_at":"2026-07-05T08:31:42.785846Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T08:31:42.785846Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"On the Doublet Flux Ratio of Mg II Resonance Lines in and Around Galaxies","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Kwang-Il Seon","submitted_at":"2023-10-27T05:57:04Z","abstract_excerpt":"Observations of metallic doublet emission lines, particularly Mg II 2796, 2803, provide crucial information for understanding galaxies and their circumgalactic medium. This study explores the effects of resonant scattering on the Mg II doublet lines and the stellar continuum in spherical and cylindrical geometries. Our findings show that under certain circumstances, resonance scattering can cause an increase in the doublet flux ratio and the escaping flux of the lines beyond what are expected in optically thin spherical media. As expected, the doublet ratio is consistently lower than the intri"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2310.17908","kind":"arxiv","version":2},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2310.17908/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"},"aliases":[{"alias_kind":"arxiv","alias_value":"2310.17908","created_at":"2026-07-05T08:31:42.785905+00:00"},{"alias_kind":"arxiv_version","alias_value":"2310.17908v2","created_at":"2026-07-05T08:31:42.785905+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2310.17908","created_at":"2026-07-05T08:31:42.785905+00:00"},{"alias_kind":"pith_short_12","alias_value":"2346U55TNXRO","created_at":"2026-07-05T08:31:42.785905+00:00"},{"alias_kind":"pith_short_16","alias_value":"2346U55TNXROC4PW","created_at":"2026-07-05T08:31:42.785905+00:00"},{"alias_kind":"pith_short_8","alias_value":"2346U55T","created_at":"2026-07-05T08:31:42.785905+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2502.01742","citing_title":"Constraining the geometry of the gas surrounding a typical galaxy at $z = 3.4$ with Ly$\\alpha$ polarization","ref_index":72,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/2346U55TNXROC4PWB55NHXEACZ","json":"https://pith.science/pith/2346U55TNXROC4PWB55NHXEACZ.json","graph_json":"https://pith.science/api/pith-number/2346U55TNXROC4PWB55NHXEACZ/graph.json","events_json":"https://pith.science/api/pith-number/2346U55TNXROC4PWB55NHXEACZ/events.json","paper":"https://pith.science/paper/2346U55T"},"agent_actions":{"view_html":"https://pith.science/pith/2346U55TNXROC4PWB55NHXEACZ","download_json":"https://pith.science/pith/2346U55TNXROC4PWB55NHXEACZ.json","view_paper":"https://pith.science/paper/2346U55T","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2310.17908&json=true","fetch_graph":"https://pith.science/api/pith-number/2346U55TNXROC4PWB55NHXEACZ/graph.json","fetch_events":"https://pith.science/api/pith-number/2346U55TNXROC4PWB55NHXEACZ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/2346U55TNXROC4PWB55NHXEACZ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/2346U55TNXROC4PWB55NHXEACZ/action/storage_attestation","attest_author":"https://pith.science/pith/2346U55TNXROC4PWB55NHXEACZ/action/author_attestation","sign_citation":"https://pith.science/pith/2346U55TNXROC4PWB55NHXEACZ/action/citation_signature","submit_replication":"https://pith.science/pith/2346U55TNXROC4PWB55NHXEACZ/action/replication_record"}},"created_at":"2026-07-05T08:31:42.785905+00:00","updated_at":"2026-07-05T08:31:42.785905+00:00"}