{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:QLU5SEUJ5KLPRWUFY6S4THSVGH","short_pith_number":"pith:QLU5SEUJ","schema_version":"1.0","canonical_sha256":"82e9d91289ea96f8da85c7a5c99e5531ca839bbdda39b07ddeba2daade0a00a4","source":{"kind":"arxiv","id":"1810.07706","version":3},"attestation_state":"computed","paper":{"title":"Effective Field Theory of Black Hole Quasinormal Modes in Scalar-Tensor Theories","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","gr-qc"],"primary_cat":"hep-th","authors_text":"Enrico Trincherini, Gabriele Franciolini, Lam Hui, Luca Santoni, Riccardo Penco","submitted_at":"2018-10-17T18:00:15Z","abstract_excerpt":"The final ringdown phase in a coalescence process is a valuable laboratory to test General Relativity and potentially constrain additional degrees of freedom in the gravitational sector. We introduce here an effective description for perturbations around spherically symmetric spacetimes in the context of scalar-tensor theories, which we apply to study quasi-normal modes for black holes with scalar hair. We derive the equations of motion governing the dynamics of both the polar and the axial modes in terms of the coefficients of the effective theory. Assuming the deviation of the background fro"},"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":"1810.07706","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"hep-th","submitted_at":"2018-10-17T18:00:15Z","cross_cats_sorted":["astro-ph.CO","gr-qc"],"title_canon_sha256":"84d3d35ce9cf5a69c07737e1d00add3a4dfe94a617a1e6c90b3c3588235f7f97","abstract_canon_sha256":"c8f73179f811045d5840e8b14a20bd19db131e6ce6c4cbd8bdd2f494189493e4"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-17T23:50:23.378606Z","signature_b64":"T7gK5GWFSgHTMofDrjvxqVc2WaO3MEnJ9p08E+nAQk8oQJReRp3q7kxBa8CFJXgLPQpgUG54w9BY2C5H77pwCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"82e9d91289ea96f8da85c7a5c99e5531ca839bbdda39b07ddeba2daade0a00a4","last_reissued_at":"2026-05-17T23:50:23.378116Z","signature_status":"signed_v1","first_computed_at":"2026-05-17T23:50:23.378116Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Effective Field Theory of Black Hole Quasinormal Modes in Scalar-Tensor Theories","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","gr-qc"],"primary_cat":"hep-th","authors_text":"Enrico Trincherini, Gabriele Franciolini, Lam Hui, Luca Santoni, Riccardo Penco","submitted_at":"2018-10-17T18:00:15Z","abstract_excerpt":"The final ringdown phase in a coalescence process is a valuable laboratory to test General Relativity and potentially constrain additional degrees of freedom in the gravitational sector. We introduce here an effective description for perturbations around spherically symmetric spacetimes in the context of scalar-tensor theories, which we apply to study quasi-normal modes for black holes with scalar hair. We derive the equations of motion governing the dynamics of both the polar and the axial modes in terms of the coefficients of the effective theory. Assuming the deviation of the background fro"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1810.07706","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":"1810.07706","created_at":"2026-05-17T23:50:23.378201+00:00"},{"alias_kind":"arxiv_version","alias_value":"1810.07706v3","created_at":"2026-05-17T23:50:23.378201+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1810.07706","created_at":"2026-05-17T23:50:23.378201+00:00"},{"alias_kind":"pith_short_12","alias_value":"QLU5SEUJ5KLP","created_at":"2026-05-18T12:32:46.962924+00:00"},{"alias_kind":"pith_short_16","alias_value":"QLU5SEUJ5KLPRWUF","created_at":"2026-05-18T12:32:46.962924+00:00"},{"alias_kind":"pith_short_8","alias_value":"QLU5SEUJ","created_at":"2026-05-18T12:32:46.962924+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":4,"sample":[{"citing_arxiv_id":"2511.12580","citing_title":"Dynamical Tidal Response of Non-rotating Black Holes: Connecting the MST Formalism and Worldline EFT","ref_index":181,"is_internal_anchor":true},{"citing_arxiv_id":"2512.22728","citing_title":"Probing higher curvature gravity via ringdown with overtones","ref_index":10,"is_internal_anchor":true},{"citing_arxiv_id":"2603.22398","citing_title":"Stable black hole solutions with cosmological hair","ref_index":79,"is_internal_anchor":true},{"citing_arxiv_id":"2603.23634","citing_title":"Testing Dark Energy with Black Hole Ringdown","ref_index":33,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/QLU5SEUJ5KLPRWUFY6S4THSVGH","json":"https://pith.science/pith/QLU5SEUJ5KLPRWUFY6S4THSVGH.json","graph_json":"https://pith.science/api/pith-number/QLU5SEUJ5KLPRWUFY6S4THSVGH/graph.json","events_json":"https://pith.science/api/pith-number/QLU5SEUJ5KLPRWUFY6S4THSVGH/events.json","paper":"https://pith.science/paper/QLU5SEUJ"},"agent_actions":{"view_html":"https://pith.science/pith/QLU5SEUJ5KLPRWUFY6S4THSVGH","download_json":"https://pith.science/pith/QLU5SEUJ5KLPRWUFY6S4THSVGH.json","view_paper":"https://pith.science/paper/QLU5SEUJ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1810.07706&json=true","fetch_graph":"https://pith.science/api/pith-number/QLU5SEUJ5KLPRWUFY6S4THSVGH/graph.json","fetch_events":"https://pith.science/api/pith-number/QLU5SEUJ5KLPRWUFY6S4THSVGH/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/QLU5SEUJ5KLPRWUFY6S4THSVGH/action/timestamp_anchor","attest_storage":"https://pith.science/pith/QLU5SEUJ5KLPRWUFY6S4THSVGH/action/storage_attestation","attest_author":"https://pith.science/pith/QLU5SEUJ5KLPRWUFY6S4THSVGH/action/author_attestation","sign_citation":"https://pith.science/pith/QLU5SEUJ5KLPRWUFY6S4THSVGH/action/citation_signature","submit_replication":"https://pith.science/pith/QLU5SEUJ5KLPRWUFY6S4THSVGH/action/replication_record"}},"created_at":"2026-05-17T23:50:23.378201+00:00","updated_at":"2026-05-17T23:50:23.378201+00:00"}