{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:JQB7XAVTPDBBFPQIRXP6H5B2HY","short_pith_number":"pith:JQB7XAVT","schema_version":"1.0","canonical_sha256":"4c03fb82b378c212be088ddfe3f43a3e21f7e54fa5431a7e2e3bdf9230e71e07","source":{"kind":"arxiv","id":"2111.02935","version":2},"attestation_state":"computed","paper":{"title":"Apples and Oranges: Comparing black holes in X-ray binaries and gravitational-wave sources","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.HE","authors_text":"Maya Fishbach, Vicky Kalogera","submitted_at":"2021-11-04T15:14:57Z","abstract_excerpt":"The component black holes (BHs) observed in gravitational-wave (GW) binary black hole (BBH) events tend to be more massive and slower spinning than those observed in black hole X-ray binaries (BH-XRBs). Without modeling their evolutionary histories, we investigate whether these apparent tensions in the BH populations can be explained by GW observational selection effects alone. We find that this is indeed the case for the discrepancy between BH masses in BBHs and the observed high-mass X-ray binaries (HMXBs), when we account for statistical uncertainty from the small sample size of just three "},"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":"2111.02935","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2021-11-04T15:14:57Z","cross_cats_sorted":["gr-qc"],"title_canon_sha256":"c1e97734239392c1b4b9cdb8cb304319429e636d514058c6a148997246f2e6f9","abstract_canon_sha256":"20ecf2309e2f041783dc355a60a1519ac2a0bdd6ef2602c1fc14fd3fba40c89e"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T04:17:37.138016Z","signature_b64":"BXhFWeoEok2YZqna7RRzYTluDbRBcxhfbHAmRpjyTWlgl7V3Xcwtj8clAv9fHQy3bBEX1n2erlDY7l+8CKfxCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"4c03fb82b378c212be088ddfe3f43a3e21f7e54fa5431a7e2e3bdf9230e71e07","last_reissued_at":"2026-07-05T04:17:37.137452Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T04:17:37.137452Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Apples and Oranges: Comparing black holes in X-ray binaries and gravitational-wave sources","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.HE","authors_text":"Maya Fishbach, Vicky Kalogera","submitted_at":"2021-11-04T15:14:57Z","abstract_excerpt":"The component black holes (BHs) observed in gravitational-wave (GW) binary black hole (BBH) events tend to be more massive and slower spinning than those observed in black hole X-ray binaries (BH-XRBs). Without modeling their evolutionary histories, we investigate whether these apparent tensions in the BH populations can be explained by GW observational selection effects alone. We find that this is indeed the case for the discrepancy between BH masses in BBHs and the observed high-mass X-ray binaries (HMXBs), when we account for statistical uncertainty from the small sample size of just three "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2111.02935","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/2111.02935/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":"2111.02935","created_at":"2026-07-05T04:17:37.137517+00:00"},{"alias_kind":"arxiv_version","alias_value":"2111.02935v2","created_at":"2026-07-05T04:17:37.137517+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2111.02935","created_at":"2026-07-05T04:17:37.137517+00:00"},{"alias_kind":"pith_short_12","alias_value":"JQB7XAVTPDBB","created_at":"2026-07-05T04:17:37.137517+00:00"},{"alias_kind":"pith_short_16","alias_value":"JQB7XAVTPDBBFPQI","created_at":"2026-07-05T04:17:37.137517+00:00"},{"alias_kind":"pith_short_8","alias_value":"JQB7XAVT","created_at":"2026-07-05T04:17:37.137517+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2607.01317","citing_title":"No Evidence for Superradiant Axions in LIGO-Virgo-KAGRA GWTC-5 Binary Black Hole Spins","ref_index":57,"is_internal_anchor":false},{"citing_arxiv_id":"2311.01300","citing_title":"Waveform Modelling for the Laser Interferometer Space Antenna","ref_index":212,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/JQB7XAVTPDBBFPQIRXP6H5B2HY","json":"https://pith.science/pith/JQB7XAVTPDBBFPQIRXP6H5B2HY.json","graph_json":"https://pith.science/api/pith-number/JQB7XAVTPDBBFPQIRXP6H5B2HY/graph.json","events_json":"https://pith.science/api/pith-number/JQB7XAVTPDBBFPQIRXP6H5B2HY/events.json","paper":"https://pith.science/paper/JQB7XAVT"},"agent_actions":{"view_html":"https://pith.science/pith/JQB7XAVTPDBBFPQIRXP6H5B2HY","download_json":"https://pith.science/pith/JQB7XAVTPDBBFPQIRXP6H5B2HY.json","view_paper":"https://pith.science/paper/JQB7XAVT","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2111.02935&json=true","fetch_graph":"https://pith.science/api/pith-number/JQB7XAVTPDBBFPQIRXP6H5B2HY/graph.json","fetch_events":"https://pith.science/api/pith-number/JQB7XAVTPDBBFPQIRXP6H5B2HY/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/JQB7XAVTPDBBFPQIRXP6H5B2HY/action/timestamp_anchor","attest_storage":"https://pith.science/pith/JQB7XAVTPDBBFPQIRXP6H5B2HY/action/storage_attestation","attest_author":"https://pith.science/pith/JQB7XAVTPDBBFPQIRXP6H5B2HY/action/author_attestation","sign_citation":"https://pith.science/pith/JQB7XAVTPDBBFPQIRXP6H5B2HY/action/citation_signature","submit_replication":"https://pith.science/pith/JQB7XAVTPDBBFPQIRXP6H5B2HY/action/replication_record"}},"created_at":"2026-07-05T04:17:37.137517+00:00","updated_at":"2026-07-05T04:17:37.137517+00:00"}