{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2011:VUM6PVJB3H424LOX43P5FIGEQ3","short_pith_number":"pith:VUM6PVJB","schema_version":"1.0","canonical_sha256":"ad19e7d521d9f9ae2dd7e6dfd2a0c486ea4da44ad1ec8742f0d42d8d82c742a3","source":{"kind":"arxiv","id":"1107.0854","version":3},"attestation_state":"computed","paper":{"title":"Black-hole hair loss: learning about binary progenitors from ringdown signals","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"B. S. Sathyaprakash (Cardiff), Ioannis Kamaretsos (Cardiff), Mark Hannam (Cardiff), Sascha Husa (Palma)","submitted_at":"2011-07-05T12:10:38Z","abstract_excerpt":"Perturbed Kerr black holes emit gravitational radiation, which (for the practical purposes of gravitational-wave astronomy) consists of a superposition of damped sinusoids termed quasi-normal modes. The frequencies and time-constants of the modes depend only on the mass and spin of the black hole - a consequence of the no-hair theorem. It has been proposed that a measurement of two or more quasi-normal modes could be used to confirm that the source is a black hole and to test if general relativity continues to hold in ultra-strong gravitational fields. In this paper we propose a practical appr"},"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":"1107.0854","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2011-07-05T12:10:38Z","cross_cats_sorted":[],"title_canon_sha256":"f926e57e814aae2f6129ab0838da32987493d5d36479033cf25ae5dd21d05d81","abstract_canon_sha256":"5e1ecc07750535b6a20f4a2bc685c63832d41cc6843234396bed9d43e6fd584a"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T03:23:23.497871Z","signature_b64":"JZ+Jw2epuu1Xv/LpPgt9kUy72vQ8B9oz+LqeHj4F8xNF1hV0JS3nL1fzk/AGUVD8QpP6vG4vUYkr0R3pYvO/AQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ad19e7d521d9f9ae2dd7e6dfd2a0c486ea4da44ad1ec8742f0d42d8d82c742a3","last_reissued_at":"2026-05-18T03:23:23.497187Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T03:23:23.497187Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Black-hole hair loss: learning about binary progenitors from ringdown signals","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"B. S. Sathyaprakash (Cardiff), Ioannis Kamaretsos (Cardiff), Mark Hannam (Cardiff), Sascha Husa (Palma)","submitted_at":"2011-07-05T12:10:38Z","abstract_excerpt":"Perturbed Kerr black holes emit gravitational radiation, which (for the practical purposes of gravitational-wave astronomy) consists of a superposition of damped sinusoids termed quasi-normal modes. The frequencies and time-constants of the modes depend only on the mass and spin of the black hole - a consequence of the no-hair theorem. It has been proposed that a measurement of two or more quasi-normal modes could be used to confirm that the source is a black hole and to test if general relativity continues to hold in ultra-strong gravitational fields. In this paper we propose a practical appr"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1107.0854","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":""},"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":"1107.0854","created_at":"2026-05-18T03:23:23.497309+00:00"},{"alias_kind":"arxiv_version","alias_value":"1107.0854v3","created_at":"2026-05-18T03:23:23.497309+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1107.0854","created_at":"2026-05-18T03:23:23.497309+00:00"},{"alias_kind":"pith_short_12","alias_value":"VUM6PVJB3H42","created_at":"2026-05-18T12:26:44.992195+00:00"},{"alias_kind":"pith_short_16","alias_value":"VUM6PVJB3H424LOX","created_at":"2026-05-18T12:26:44.992195+00:00"},{"alias_kind":"pith_short_8","alias_value":"VUM6PVJB","created_at":"2026-05-18T12:26:44.992195+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":4,"sample":[{"citing_arxiv_id":"2508.21216","citing_title":"Persistence of post-Newtonian amplitude structure in binary black hole mergers","ref_index":27,"is_internal_anchor":true},{"citing_arxiv_id":"2303.15923","citing_title":"Science with the Einstein Telescope: a comparison of different designs","ref_index":168,"is_internal_anchor":true},{"citing_arxiv_id":"1905.00869","citing_title":"Testing the no-hair theorem with GW150914","ref_index":30,"is_internal_anchor":true},{"citing_arxiv_id":"1903.04467","citing_title":"Tests of General Relativity with the Binary Black Hole Signals from the LIGO-Virgo Catalog GWTC-1","ref_index":74,"is_internal_anchor":true},{"citing_arxiv_id":"2112.06861","citing_title":"Tests of General Relativity with GWTC-3","ref_index":276,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/VUM6PVJB3H424LOX43P5FIGEQ3","json":"https://pith.science/pith/VUM6PVJB3H424LOX43P5FIGEQ3.json","graph_json":"https://pith.science/api/pith-number/VUM6PVJB3H424LOX43P5FIGEQ3/graph.json","events_json":"https://pith.science/api/pith-number/VUM6PVJB3H424LOX43P5FIGEQ3/events.json","paper":"https://pith.science/paper/VUM6PVJB"},"agent_actions":{"view_html":"https://pith.science/pith/VUM6PVJB3H424LOX43P5FIGEQ3","download_json":"https://pith.science/pith/VUM6PVJB3H424LOX43P5FIGEQ3.json","view_paper":"https://pith.science/paper/VUM6PVJB","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1107.0854&json=true","fetch_graph":"https://pith.science/api/pith-number/VUM6PVJB3H424LOX43P5FIGEQ3/graph.json","fetch_events":"https://pith.science/api/pith-number/VUM6PVJB3H424LOX43P5FIGEQ3/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/VUM6PVJB3H424LOX43P5FIGEQ3/action/timestamp_anchor","attest_storage":"https://pith.science/pith/VUM6PVJB3H424LOX43P5FIGEQ3/action/storage_attestation","attest_author":"https://pith.science/pith/VUM6PVJB3H424LOX43P5FIGEQ3/action/author_attestation","sign_citation":"https://pith.science/pith/VUM6PVJB3H424LOX43P5FIGEQ3/action/citation_signature","submit_replication":"https://pith.science/pith/VUM6PVJB3H424LOX43P5FIGEQ3/action/replication_record"}},"created_at":"2026-05-18T03:23:23.497309+00:00","updated_at":"2026-05-18T03:23:23.497309+00:00"}