{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:NYVT727MQXWTJ3WJZVMYPGNQEM","short_pith_number":"pith:NYVT727M","schema_version":"1.0","canonical_sha256":"6e2b3febec85ed34eec9cd598799b023396246e96765f1964467708f388b625b","source":{"kind":"arxiv","id":"2510.01001","version":3},"attestation_state":"computed","paper":{"title":"GW250114 reveals black hole horizon signatures","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","hep-ph"],"primary_cat":"gr-qc","authors_text":"Ling Sun, Neil Lu, Ornella J. Piccinni, Sizheng Ma, Yanbei Chen","submitted_at":"2025-10-01T15:08:26Z","abstract_excerpt":"The horizon of a black hole, the \"surface of no return\", is characterized by its rotation frequency $\\Omega_H$ and surface gravity $\\kappa$. A striking signature is that any infalling object appears to orbit at $\\Omega_H$ due to frame dragging, while its emitted signals decay exponentially at a rate set by $\\kappa$ as a consequence of gravitational redshift. Recent theoretical work predicts that the merger phase of gravitational waves from binary black hole coalescences carries direct imprints of the remnant horizon's properties, via a \"direct wave\" component that (i) oscillates near $2\\Omega_"},"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":"2510.01001","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2025-10-01T15:08:26Z","cross_cats_sorted":["astro-ph.HE","hep-ph"],"title_canon_sha256":"0828182b7555b3c19e8eece0367c877fc4bdb8900083dfaf1b77149b15b161fc","abstract_canon_sha256":"db22c333011166ad2e13bf349606780e6a6c35090e3572656c67a7cc35fe2a82"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-26T01:03:16.278875Z","signature_b64":"AuRzLyRENG61SsFKwQUUCwNWfePCwKP2RagzFxXnJve+EQGbeKnCs7Z3MjAxS/t8zlBRiN+GJiLUbMoVYfstDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"6e2b3febec85ed34eec9cd598799b023396246e96765f1964467708f388b625b","last_reissued_at":"2026-05-26T01:03:16.278014Z","signature_status":"signed_v1","first_computed_at":"2026-05-26T01:03:16.278014Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"GW250114 reveals black hole horizon signatures","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","hep-ph"],"primary_cat":"gr-qc","authors_text":"Ling Sun, Neil Lu, Ornella J. Piccinni, Sizheng Ma, Yanbei Chen","submitted_at":"2025-10-01T15:08:26Z","abstract_excerpt":"The horizon of a black hole, the \"surface of no return\", is characterized by its rotation frequency $\\Omega_H$ and surface gravity $\\kappa$. A striking signature is that any infalling object appears to orbit at $\\Omega_H$ due to frame dragging, while its emitted signals decay exponentially at a rate set by $\\kappa$ as a consequence of gravitational redshift. Recent theoretical work predicts that the merger phase of gravitational waves from binary black hole coalescences carries direct imprints of the remnant horizon's properties, via a \"direct wave\" component that (i) oscillates near $2\\Omega_"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2510.01001","kind":"arxiv","version":3},"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/2510.01001/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":"2510.01001","created_at":"2026-05-26T01:03:16.278139+00:00"},{"alias_kind":"arxiv_version","alias_value":"2510.01001v3","created_at":"2026-05-26T01:03:16.278139+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2510.01001","created_at":"2026-05-26T01:03:16.278139+00:00"},{"alias_kind":"pith_short_12","alias_value":"NYVT727MQXWT","created_at":"2026-05-26T01:03:16.278139+00:00"},{"alias_kind":"pith_short_16","alias_value":"NYVT727MQXWTJ3WJ","created_at":"2026-05-26T01:03:16.278139+00:00"},{"alias_kind":"pith_short_8","alias_value":"NYVT727M","created_at":"2026-05-26T01:03:16.278139+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":4,"sample":[{"citing_arxiv_id":"2605.11283","citing_title":"Black Hole Binary Detection Landscape for the Laser Interferometer Lunar Antenna (LILA): Signal-to-Noise Calculations & Science Cases","ref_index":176,"is_internal_anchor":true},{"citing_arxiv_id":"2605.03576","citing_title":"Ringdown Analysis of GW250114 with Orthonormal Modes","ref_index":28,"is_internal_anchor":true},{"citing_arxiv_id":"2604.08680","citing_title":"Prompt Response from Plunging Sources in Schwarzschild Spacetime","ref_index":51,"is_internal_anchor":true},{"citing_arxiv_id":"2604.17558","citing_title":"Deterministic Trust Regions for Finite-Window Black-Hole Spectroscopy in GW250114","ref_index":30,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/NYVT727MQXWTJ3WJZVMYPGNQEM","json":"https://pith.science/pith/NYVT727MQXWTJ3WJZVMYPGNQEM.json","graph_json":"https://pith.science/api/pith-number/NYVT727MQXWTJ3WJZVMYPGNQEM/graph.json","events_json":"https://pith.science/api/pith-number/NYVT727MQXWTJ3WJZVMYPGNQEM/events.json","paper":"https://pith.science/paper/NYVT727M"},"agent_actions":{"view_html":"https://pith.science/pith/NYVT727MQXWTJ3WJZVMYPGNQEM","download_json":"https://pith.science/pith/NYVT727MQXWTJ3WJZVMYPGNQEM.json","view_paper":"https://pith.science/paper/NYVT727M","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2510.01001&json=true","fetch_graph":"https://pith.science/api/pith-number/NYVT727MQXWTJ3WJZVMYPGNQEM/graph.json","fetch_events":"https://pith.science/api/pith-number/NYVT727MQXWTJ3WJZVMYPGNQEM/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/NYVT727MQXWTJ3WJZVMYPGNQEM/action/timestamp_anchor","attest_storage":"https://pith.science/pith/NYVT727MQXWTJ3WJZVMYPGNQEM/action/storage_attestation","attest_author":"https://pith.science/pith/NYVT727MQXWTJ3WJZVMYPGNQEM/action/author_attestation","sign_citation":"https://pith.science/pith/NYVT727MQXWTJ3WJZVMYPGNQEM/action/citation_signature","submit_replication":"https://pith.science/pith/NYVT727MQXWTJ3WJZVMYPGNQEM/action/replication_record"}},"created_at":"2026-05-26T01:03:16.278139+00:00","updated_at":"2026-05-26T01:03:16.278139+00:00"}