{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2007:BVDFQNQ2JZQF4RSX2TTU4MFSA7","short_pith_number":"pith:BVDFQNQ2","schema_version":"1.0","canonical_sha256":"0d4658361a4e605e4657d4e74e30b207db6d9f7a944c69492af253b7ee3c61cf","source":{"kind":"arxiv","id":"gr-qc/0701086","version":2},"attestation_state":"computed","paper":{"title":"Mining information from binary black hole mergers: a comparison of estimation methods for complex exponentials in noise","license":"","headline":"","cross_cats":["astro-ph"],"primary_cat":"gr-qc","authors_text":"Emanuele Berti, Jose A. Gonzalez, Ulrich Sperhake, Vitor Cardoso","submitted_at":"2007-01-16T19:56:35Z","abstract_excerpt":"The ringdown phase following a binary black hole merger is usually assumed to be well described by a linear superposition of complex exponentials (quasinormal modes). In the strong-field conditions typical of a binary black hole merger, non-linear effects may produce mode coupling. Artificial mode coupling can also be induced by the black hole's rotation, if the radiation field is expanded in terms of spin-weighted spherical (rather than spheroidal) harmonics. Observing deviations from linear black hole perturbation theory requires optimal fitting techniques to extract ringdown parameters from"},"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":"gr-qc/0701086","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"gr-qc","submitted_at":"2007-01-16T19:56:35Z","cross_cats_sorted":["astro-ph"],"title_canon_sha256":"f2554af979dde5f12a4e3c2926c3516dd3173170112beaa93dc7348d960040b4","abstract_canon_sha256":"cf39d46b30f306cef3f583580e3d9c74b1ff755613df3ed1e2775fe270990f85"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:16:38.304071Z","signature_b64":"eKdfXiO/5SsJsqAoCwIzE2JxYX7LPAFTEQXYCNAtQEQHn1Mzqh7+rnRihkH0DG7D/JjjAOVD1awJg3GmhgL+DQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"0d4658361a4e605e4657d4e74e30b207db6d9f7a944c69492af253b7ee3c61cf","last_reissued_at":"2026-07-04T15:16:38.303509Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:16:38.303509Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Mining information from binary black hole mergers: a comparison of estimation methods for complex exponentials in noise","license":"","headline":"","cross_cats":["astro-ph"],"primary_cat":"gr-qc","authors_text":"Emanuele Berti, Jose A. Gonzalez, Ulrich Sperhake, Vitor Cardoso","submitted_at":"2007-01-16T19:56:35Z","abstract_excerpt":"The ringdown phase following a binary black hole merger is usually assumed to be well described by a linear superposition of complex exponentials (quasinormal modes). In the strong-field conditions typical of a binary black hole merger, non-linear effects may produce mode coupling. Artificial mode coupling can also be induced by the black hole's rotation, if the radiation field is expanded in terms of spin-weighted spherical (rather than spheroidal) harmonics. Observing deviations from linear black hole perturbation theory requires optimal fitting techniques to extract ringdown parameters from"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"gr-qc/0701086","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/gr-qc/0701086/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":"gr-qc/0701086","created_at":"2026-07-04T15:16:38.303572+00:00"},{"alias_kind":"arxiv_version","alias_value":"gr-qc/0701086v2","created_at":"2026-07-04T15:16:38.303572+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.gr-qc/0701086","created_at":"2026-07-04T15:16:38.303572+00:00"},{"alias_kind":"pith_short_12","alias_value":"BVDFQNQ2JZQF","created_at":"2026-07-04T15:16:38.303572+00:00"},{"alias_kind":"pith_short_16","alias_value":"BVDFQNQ2JZQF4RSX","created_at":"2026-07-04T15:16:38.303572+00:00"},{"alias_kind":"pith_short_8","alias_value":"BVDFQNQ2","created_at":"2026-07-04T15:16:38.303572+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2606.29704","citing_title":"Quasibound states of a charged Dirac field around regular black holes","ref_index":57,"is_internal_anchor":true},{"citing_arxiv_id":"2601.16016","citing_title":"Nonlinear tails of massive scalar fields around a black hole","ref_index":51,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/BVDFQNQ2JZQF4RSX2TTU4MFSA7","json":"https://pith.science/pith/BVDFQNQ2JZQF4RSX2TTU4MFSA7.json","graph_json":"https://pith.science/api/pith-number/BVDFQNQ2JZQF4RSX2TTU4MFSA7/graph.json","events_json":"https://pith.science/api/pith-number/BVDFQNQ2JZQF4RSX2TTU4MFSA7/events.json","paper":"https://pith.science/paper/BVDFQNQ2"},"agent_actions":{"view_html":"https://pith.science/pith/BVDFQNQ2JZQF4RSX2TTU4MFSA7","download_json":"https://pith.science/pith/BVDFQNQ2JZQF4RSX2TTU4MFSA7.json","view_paper":"https://pith.science/paper/BVDFQNQ2","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=gr-qc/0701086&json=true","fetch_graph":"https://pith.science/api/pith-number/BVDFQNQ2JZQF4RSX2TTU4MFSA7/graph.json","fetch_events":"https://pith.science/api/pith-number/BVDFQNQ2JZQF4RSX2TTU4MFSA7/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/BVDFQNQ2JZQF4RSX2TTU4MFSA7/action/timestamp_anchor","attest_storage":"https://pith.science/pith/BVDFQNQ2JZQF4RSX2TTU4MFSA7/action/storage_attestation","attest_author":"https://pith.science/pith/BVDFQNQ2JZQF4RSX2TTU4MFSA7/action/author_attestation","sign_citation":"https://pith.science/pith/BVDFQNQ2JZQF4RSX2TTU4MFSA7/action/citation_signature","submit_replication":"https://pith.science/pith/BVDFQNQ2JZQF4RSX2TTU4MFSA7/action/replication_record"}},"created_at":"2026-07-04T15:16:38.303572+00:00","updated_at":"2026-07-04T15:16:38.303572+00:00"}