{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:1998:CJCFA5LP73PGS72LVYGNLIHZB6","short_pith_number":"pith:CJCFA5LP","schema_version":"1.0","canonical_sha256":"124450756ffede697f4bae0cd5a0f90fab045bb00dea0739f884e3e3c6bc944e","source":{"kind":"arxiv","id":"astro-ph/9808089","version":1},"attestation_state":"computed","paper":{"title":"Iron line profiles including emission from within the innermost stable orbit of a black hole accretion disc","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A.C.Fabian, A.J. Young, R.R. Ross","submitted_at":"1998-08-10T16:33:21Z","abstract_excerpt":"Reynolds & Begelman (1997) have recently proposed a model in which the broad and extremely redshifted iron line seen during a deep minimum of the light curve of the Seyfert 1 galaxy MCG-6-30-15 originates from matter spiralling into a Schwarzschild black hole, contrary to previous claims that the black hole may be spinning rapidly (Iwasawa et al 1996; Dabrowski et al 1997). Here we calculate in detail the X-ray spectrum produced by their model using the full reflected continuum emission, including absorption features. This calculation takes into account the doppler and relativistic effects. Fo"},"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":"astro-ph/9808089","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"1998-08-10T16:33:21Z","cross_cats_sorted":[],"title_canon_sha256":"2804dfeb3e9d7d1ead6663277a8145c6c49a63f128f7f1759f341c3641441284","abstract_canon_sha256":"98fe928f39695e1fe3876b4c138978ae8bdfce99d67f90a537a024dd74d31e8e"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:06:55.296885Z","signature_b64":"snc8yItz1YethtN7VKhw4jFnc4gtD+BmGJ+R98RCWTXBZHIfkZCXyc6p2tZqijaio5+PuFBGVBju4BPq33ZPAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"124450756ffede697f4bae0cd5a0f90fab045bb00dea0739f884e3e3c6bc944e","last_reissued_at":"2026-07-04T16:06:55.296485Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:06:55.296485Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Iron line profiles including emission from within the innermost stable orbit of a black hole accretion disc","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A.C.Fabian, A.J. Young, R.R. Ross","submitted_at":"1998-08-10T16:33:21Z","abstract_excerpt":"Reynolds & Begelman (1997) have recently proposed a model in which the broad and extremely redshifted iron line seen during a deep minimum of the light curve of the Seyfert 1 galaxy MCG-6-30-15 originates from matter spiralling into a Schwarzschild black hole, contrary to previous claims that the black hole may be spinning rapidly (Iwasawa et al 1996; Dabrowski et al 1997). Here we calculate in detail the X-ray spectrum produced by their model using the full reflected continuum emission, including absorption features. This calculation takes into account the doppler and relativistic effects. Fo"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/9808089","kind":"arxiv","version":1},"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/astro-ph/9808089/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":"astro-ph/9808089","created_at":"2026-07-04T16:06:55.296533+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/9808089v1","created_at":"2026-07-04T16:06:55.296533+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/9808089","created_at":"2026-07-04T16:06:55.296533+00:00"},{"alias_kind":"pith_short_12","alias_value":"CJCFA5LP73PG","created_at":"2026-07-04T16:06:55.296533+00:00"},{"alias_kind":"pith_short_16","alias_value":"CJCFA5LP73PGS72L","created_at":"2026-07-04T16:06:55.296533+00:00"},{"alias_kind":"pith_short_8","alias_value":"CJCFA5LP","created_at":"2026-07-04T16:06:55.296533+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2411.14338","citing_title":"Morphology of Relativistically Broadened Line Emission from Axisymmetric Equatorial Accretion Disks","ref_index":60,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/CJCFA5LP73PGS72LVYGNLIHZB6","json":"https://pith.science/pith/CJCFA5LP73PGS72LVYGNLIHZB6.json","graph_json":"https://pith.science/api/pith-number/CJCFA5LP73PGS72LVYGNLIHZB6/graph.json","events_json":"https://pith.science/api/pith-number/CJCFA5LP73PGS72LVYGNLIHZB6/events.json","paper":"https://pith.science/paper/CJCFA5LP"},"agent_actions":{"view_html":"https://pith.science/pith/CJCFA5LP73PGS72LVYGNLIHZB6","download_json":"https://pith.science/pith/CJCFA5LP73PGS72LVYGNLIHZB6.json","view_paper":"https://pith.science/paper/CJCFA5LP","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/9808089&json=true","fetch_graph":"https://pith.science/api/pith-number/CJCFA5LP73PGS72LVYGNLIHZB6/graph.json","fetch_events":"https://pith.science/api/pith-number/CJCFA5LP73PGS72LVYGNLIHZB6/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/CJCFA5LP73PGS72LVYGNLIHZB6/action/timestamp_anchor","attest_storage":"https://pith.science/pith/CJCFA5LP73PGS72LVYGNLIHZB6/action/storage_attestation","attest_author":"https://pith.science/pith/CJCFA5LP73PGS72LVYGNLIHZB6/action/author_attestation","sign_citation":"https://pith.science/pith/CJCFA5LP73PGS72LVYGNLIHZB6/action/citation_signature","submit_replication":"https://pith.science/pith/CJCFA5LP73PGS72LVYGNLIHZB6/action/replication_record"}},"created_at":"2026-07-04T16:06:55.296533+00:00","updated_at":"2026-07-04T16:06:55.296533+00:00"}