{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2013:3HAL45VVYZWBGW6L4HKDI7NIWE","short_pith_number":"pith:3HAL45VV","schema_version":"1.0","canonical_sha256":"d9c0be76b5c66c135bcbe1d4347da8b1301ddb91332c9a752db15ee87e724926","source":{"kind":"arxiv","id":"1311.5118","version":2},"attestation_state":"computed","paper":{"title":"Mass Measurements of Stellar and Intermediate Mass Black-Holes","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.HE","authors_text":"J. Casares, P.G. Jonker","submitted_at":"2013-11-20T16:15:12Z","abstract_excerpt":"We discuss the method, and potential systematic effects therein, used for measuring the mass of stellar-mass black holes in X-ray binaries. We restrict our discussion to the method that relies on the validity of Kepler's laws; we refer to this method as the dynamical method. We briefly discuss the implications of the mass distribution of stellar-mass black holes and provide an outlook for future measurements. Further, we investigate the evidence for the existence of intermediate-mass black holes i.e. black holes with masses above 100 Msun, the limit to the black hole mass that can be produced "},"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":"1311.5118","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2013-11-20T16:15:12Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"a041cc37eba7f37d97d36f5de056f33e2af163d0d3a101fec87988b1ddcade3d","abstract_canon_sha256":"868aebb0a76990810a3fdd5728fcdbaad13d9a946f9eca6f6f26a6b6c6b175b9"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:46:12.098003Z","signature_b64":"wDC3hwZMyWRljHXDZhss/2OILIrOZzX+93498MY3aNLM7nASucMrzkUwbrgjjzKs7AblJseEwE50IPsDrl3jCQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d9c0be76b5c66c135bcbe1d4347da8b1301ddb91332c9a752db15ee87e724926","last_reissued_at":"2026-05-18T01:46:12.097309Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:46:12.097309Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Mass Measurements of Stellar and Intermediate Mass Black-Holes","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.HE","authors_text":"J. Casares, P.G. Jonker","submitted_at":"2013-11-20T16:15:12Z","abstract_excerpt":"We discuss the method, and potential systematic effects therein, used for measuring the mass of stellar-mass black holes in X-ray binaries. We restrict our discussion to the method that relies on the validity of Kepler's laws; we refer to this method as the dynamical method. We briefly discuss the implications of the mass distribution of stellar-mass black holes and provide an outlook for future measurements. Further, we investigate the evidence for the existence of intermediate-mass black holes i.e. black holes with masses above 100 Msun, the limit to the black hole mass that can be produced "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1311.5118","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":""},"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":"1311.5118","created_at":"2026-05-18T01:46:12.097420+00:00"},{"alias_kind":"arxiv_version","alias_value":"1311.5118v2","created_at":"2026-05-18T01:46:12.097420+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1311.5118","created_at":"2026-05-18T01:46:12.097420+00:00"},{"alias_kind":"pith_short_12","alias_value":"3HAL45VVYZWB","created_at":"2026-05-18T12:27:32.513160+00:00"},{"alias_kind":"pith_short_16","alias_value":"3HAL45VVYZWBGW6L","created_at":"2026-05-18T12:27:32.513160+00:00"},{"alias_kind":"pith_short_8","alias_value":"3HAL45VV","created_at":"2026-05-18T12:27:32.513160+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2605.11703","citing_title":"GW240925 and GW250207: Astrophysical Calibration of Gravitational-wave Detectors","ref_index":86,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/3HAL45VVYZWBGW6L4HKDI7NIWE","json":"https://pith.science/pith/3HAL45VVYZWBGW6L4HKDI7NIWE.json","graph_json":"https://pith.science/api/pith-number/3HAL45VVYZWBGW6L4HKDI7NIWE/graph.json","events_json":"https://pith.science/api/pith-number/3HAL45VVYZWBGW6L4HKDI7NIWE/events.json","paper":"https://pith.science/paper/3HAL45VV"},"agent_actions":{"view_html":"https://pith.science/pith/3HAL45VVYZWBGW6L4HKDI7NIWE","download_json":"https://pith.science/pith/3HAL45VVYZWBGW6L4HKDI7NIWE.json","view_paper":"https://pith.science/paper/3HAL45VV","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1311.5118&json=true","fetch_graph":"https://pith.science/api/pith-number/3HAL45VVYZWBGW6L4HKDI7NIWE/graph.json","fetch_events":"https://pith.science/api/pith-number/3HAL45VVYZWBGW6L4HKDI7NIWE/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/3HAL45VVYZWBGW6L4HKDI7NIWE/action/timestamp_anchor","attest_storage":"https://pith.science/pith/3HAL45VVYZWBGW6L4HKDI7NIWE/action/storage_attestation","attest_author":"https://pith.science/pith/3HAL45VVYZWBGW6L4HKDI7NIWE/action/author_attestation","sign_citation":"https://pith.science/pith/3HAL45VVYZWBGW6L4HKDI7NIWE/action/citation_signature","submit_replication":"https://pith.science/pith/3HAL45VVYZWBGW6L4HKDI7NIWE/action/replication_record"}},"created_at":"2026-05-18T01:46:12.097420+00:00","updated_at":"2026-05-18T01:46:12.097420+00:00"}