{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2015:7RN3MFDXJHEQAEONYJRNO7D5EI","short_pith_number":"pith:7RN3MFDX","schema_version":"1.0","canonical_sha256":"fc5bb6147749c90011cdc262d77c7d220df80a5adcdab67733a1bec5ac04304d","source":{"kind":"arxiv","id":"1512.03414","version":1},"attestation_state":"computed","paper":{"title":"On the Spin of the Black Hole in IC 10 X-1","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Dominic J. Walton, James F. Steiner, Javier A. Garcia, Jeffrey E. McClintock, Kristin K. Madsen, Matthew J. Middleton, Robin Barnard, Silas G. T. Laycock","submitted_at":"2015-12-10T20:50:29Z","abstract_excerpt":"The compact X-ray source in the eclipsing X-ray binary IC 10 X-1 has reigned for years as ostensibly the most massive stellar-mass black hole, with a mass estimated to be about twice that of its closest rival. However, striking results presented recently by Laycock et al. reveal that the mass estimate, based on emission-line velocities, is unreliable and that the mass of the X-ray source is essentially unconstrained. Using Chandra and NuSTAR data, we rule against a neutron-star model and conclude that IC 10 X-1 contains a black hole. The eclipse duration of IC 10 X-1 is shorter and its depth s"},"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":"1512.03414","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2015-12-10T20:50:29Z","cross_cats_sorted":[],"title_canon_sha256":"6ba8ad3b04a3f77708bf53391f331ce2b9d19adefdb012b4b7e9795293adf82e","abstract_canon_sha256":"28289b6907f6e3e7c44aa29cf38adbf11783d579205f32de65382020d8960de6"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:21:26.033585Z","signature_b64":"M8kvTa+06/I5lwb0btzqW+ZtOR5HtUmXS2GGvk0NmY29j9olAclFCg8tEj6EAIzsB6os0WZU/jy0kPkLuBVbBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"fc5bb6147749c90011cdc262d77c7d220df80a5adcdab67733a1bec5ac04304d","last_reissued_at":"2026-05-18T01:21:26.032917Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:21:26.032917Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"On the Spin of the Black Hole in IC 10 X-1","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Dominic J. Walton, James F. Steiner, Javier A. Garcia, Jeffrey E. McClintock, Kristin K. Madsen, Matthew J. Middleton, Robin Barnard, Silas G. T. Laycock","submitted_at":"2015-12-10T20:50:29Z","abstract_excerpt":"The compact X-ray source in the eclipsing X-ray binary IC 10 X-1 has reigned for years as ostensibly the most massive stellar-mass black hole, with a mass estimated to be about twice that of its closest rival. However, striking results presented recently by Laycock et al. reveal that the mass estimate, based on emission-line velocities, is unreliable and that the mass of the X-ray source is essentially unconstrained. Using Chandra and NuSTAR data, we rule against a neutron-star model and conclude that IC 10 X-1 contains a black hole. The eclipse duration of IC 10 X-1 is shorter and its depth s"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1512.03414","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":""},"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":"1512.03414","created_at":"2026-05-18T01:21:26.033020+00:00"},{"alias_kind":"arxiv_version","alias_value":"1512.03414v1","created_at":"2026-05-18T01:21:26.033020+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1512.03414","created_at":"2026-05-18T01:21:26.033020+00:00"},{"alias_kind":"pith_short_12","alias_value":"7RN3MFDXJHEQ","created_at":"2026-05-18T12:29:10.953037+00:00"},{"alias_kind":"pith_short_16","alias_value":"7RN3MFDXJHEQAEON","created_at":"2026-05-18T12:29:10.953037+00:00"},{"alias_kind":"pith_short_8","alias_value":"7RN3MFDX","created_at":"2026-05-18T12:29:10.953037+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2510.06741","citing_title":"Diagnosing the Properties and Evolutionary Fates of Black Hole and Wolf-Rayet X-ray Binaries as Potential Gravitational Wave Sources for the LIGO-Virgo-KAGRA Network","ref_index":34,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/7RN3MFDXJHEQAEONYJRNO7D5EI","json":"https://pith.science/pith/7RN3MFDXJHEQAEONYJRNO7D5EI.json","graph_json":"https://pith.science/api/pith-number/7RN3MFDXJHEQAEONYJRNO7D5EI/graph.json","events_json":"https://pith.science/api/pith-number/7RN3MFDXJHEQAEONYJRNO7D5EI/events.json","paper":"https://pith.science/paper/7RN3MFDX"},"agent_actions":{"view_html":"https://pith.science/pith/7RN3MFDXJHEQAEONYJRNO7D5EI","download_json":"https://pith.science/pith/7RN3MFDXJHEQAEONYJRNO7D5EI.json","view_paper":"https://pith.science/paper/7RN3MFDX","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1512.03414&json=true","fetch_graph":"https://pith.science/api/pith-number/7RN3MFDXJHEQAEONYJRNO7D5EI/graph.json","fetch_events":"https://pith.science/api/pith-number/7RN3MFDXJHEQAEONYJRNO7D5EI/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/7RN3MFDXJHEQAEONYJRNO7D5EI/action/timestamp_anchor","attest_storage":"https://pith.science/pith/7RN3MFDXJHEQAEONYJRNO7D5EI/action/storage_attestation","attest_author":"https://pith.science/pith/7RN3MFDXJHEQAEONYJRNO7D5EI/action/author_attestation","sign_citation":"https://pith.science/pith/7RN3MFDXJHEQAEONYJRNO7D5EI/action/citation_signature","submit_replication":"https://pith.science/pith/7RN3MFDXJHEQAEONYJRNO7D5EI/action/replication_record"}},"created_at":"2026-05-18T01:21:26.033020+00:00","updated_at":"2026-05-18T01:21:26.033020+00:00"}