{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2005:XG6W3FUL5JCCPLFHSHCKYOGUCS","short_pith_number":"pith:XG6W3FUL","schema_version":"1.0","canonical_sha256":"b9bd6d968bea4427aca791c4ac38d414a1dc2e16ab9f165a43e6eb8fa425d903","source":{"kind":"arxiv","id":"astro-ph/0508302","version":2},"attestation_state":"computed","paper":{"title":"Estimating the Spin of Stellar-Mass Black Holes via Spectral Fitting of the X-ray Continuum","license":"","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph","authors_text":"Jeffrey E. McClintock, Li-Xin Li, Ramesh Narayan, Rebecca Shafee, Ronald A. Remillard, Shane W. Davis","submitted_at":"2005-08-14T15:20:01Z","abstract_excerpt":"We fit X-ray spectral data in the thermal dominant or high soft state of two dynamically confirmed black holes, GRO J1655-40 and 4U 1543-47, and estimate the dimensionless spin parameters a* = a/M of the two holes. For GRO J1655-40, using a spectral hardening factor computed for a non-LTE relativistic accretion disk, we estimate a* ~ 0.75 and ~ 0.65-0.75, respectively, from ASCA and RXTE data. For 4U 1543-47, we estimate a* ~ 0.75-0.85 from RXTE data. Thus, neither black hole has a spin approaching the theoretical maximum a* = 1."},"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/0508302","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2005-08-14T15:20:01Z","cross_cats_sorted":["gr-qc"],"title_canon_sha256":"e48726a0d222bf91e0a60beda684f3bf9ea81224949619dd5c1a63894e8b7610","abstract_canon_sha256":"b9ef24b112065447accc23383ba797a1c2b45e4df799e87ec680021a0de22ad9"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T17:15:00.555218Z","signature_b64":"ZSjz/y6w15MklnyjDerhxI1+KifFhvEu8GsKg1RfxJ3qzw9Q4Rv1X965peeZ3QRJlfhA35WZXb272ps1s9EXDw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"b9bd6d968bea4427aca791c4ac38d414a1dc2e16ab9f165a43e6eb8fa425d903","last_reissued_at":"2026-07-04T17:15:00.554726Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T17:15:00.554726Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Estimating the Spin of Stellar-Mass Black Holes via Spectral Fitting of the X-ray Continuum","license":"","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph","authors_text":"Jeffrey E. McClintock, Li-Xin Li, Ramesh Narayan, Rebecca Shafee, Ronald A. Remillard, Shane W. Davis","submitted_at":"2005-08-14T15:20:01Z","abstract_excerpt":"We fit X-ray spectral data in the thermal dominant or high soft state of two dynamically confirmed black holes, GRO J1655-40 and 4U 1543-47, and estimate the dimensionless spin parameters a* = a/M of the two holes. For GRO J1655-40, using a spectral hardening factor computed for a non-LTE relativistic accretion disk, we estimate a* ~ 0.75 and ~ 0.65-0.75, respectively, from ASCA and RXTE data. For 4U 1543-47, we estimate a* ~ 0.75-0.85 from RXTE data. Thus, neither black hole has a spin approaching the theoretical maximum a* = 1."},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0508302","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/astro-ph/0508302/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/0508302","created_at":"2026-07-04T17:15:00.554785+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0508302v2","created_at":"2026-07-04T17:15:00.554785+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0508302","created_at":"2026-07-04T17:15:00.554785+00:00"},{"alias_kind":"pith_short_12","alias_value":"XG6W3FUL5JCC","created_at":"2026-07-04T17:15:00.554785+00:00"},{"alias_kind":"pith_short_16","alias_value":"XG6W3FUL5JCCPLFH","created_at":"2026-07-04T17:15:00.554785+00:00"},{"alias_kind":"pith_short_8","alias_value":"XG6W3FUL","created_at":"2026-07-04T17:15:00.554785+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.20317","citing_title":"Simulation-Based Prediction of Black Hole Fe K$\\alpha$ Line Profiles","ref_index":11,"is_internal_anchor":true},{"citing_arxiv_id":"1501.07274","citing_title":"Testing General Relativity with Present and Future Astrophysical Observations","ref_index":263,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/XG6W3FUL5JCCPLFHSHCKYOGUCS","json":"https://pith.science/pith/XG6W3FUL5JCCPLFHSHCKYOGUCS.json","graph_json":"https://pith.science/api/pith-number/XG6W3FUL5JCCPLFHSHCKYOGUCS/graph.json","events_json":"https://pith.science/api/pith-number/XG6W3FUL5JCCPLFHSHCKYOGUCS/events.json","paper":"https://pith.science/paper/XG6W3FUL"},"agent_actions":{"view_html":"https://pith.science/pith/XG6W3FUL5JCCPLFHSHCKYOGUCS","download_json":"https://pith.science/pith/XG6W3FUL5JCCPLFHSHCKYOGUCS.json","view_paper":"https://pith.science/paper/XG6W3FUL","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0508302&json=true","fetch_graph":"https://pith.science/api/pith-number/XG6W3FUL5JCCPLFHSHCKYOGUCS/graph.json","fetch_events":"https://pith.science/api/pith-number/XG6W3FUL5JCCPLFHSHCKYOGUCS/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/XG6W3FUL5JCCPLFHSHCKYOGUCS/action/timestamp_anchor","attest_storage":"https://pith.science/pith/XG6W3FUL5JCCPLFHSHCKYOGUCS/action/storage_attestation","attest_author":"https://pith.science/pith/XG6W3FUL5JCCPLFHSHCKYOGUCS/action/author_attestation","sign_citation":"https://pith.science/pith/XG6W3FUL5JCCPLFHSHCKYOGUCS/action/citation_signature","submit_replication":"https://pith.science/pith/XG6W3FUL5JCCPLFHSHCKYOGUCS/action/replication_record"}},"created_at":"2026-07-04T17:15:00.554785+00:00","updated_at":"2026-07-04T17:15:00.554785+00:00"}