{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:ITAJSISPNBW735SG4J7N5H62D2","short_pith_number":"pith:ITAJSISP","schema_version":"1.0","canonical_sha256":"44c099224f686dfdf646e27ede9fda1e831c992cc7b016e83f3b8fffb69c0465","source":{"kind":"arxiv","id":"2110.15922","version":2},"attestation_state":"computed","paper":{"title":"High Precision Ringdown Modeling: Multimode Fits and BMS Frames","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","hep-th"],"primary_cat":"gr-qc","authors_text":"Dante A. B. Iozzo, Fran\\c{c}ois H\\'ebert, Harald P. Pfeiffer, Jordan Moxon, Keefe Mitman, Lawrence E. Kidder, Leo C. Stein, Lorena Maga\\~na Zertuche, Mark A. Scheel, Michael Boyle, Neev Khera, Nils Deppe, Nils Vu, Saul A. Teukolsky, William Throwe","submitted_at":"2021-10-29T17:16:46Z","abstract_excerpt":"Quasi-normal mode (QNM) modeling is an invaluable tool for characterizing remnant black holes, studying strong gravity, and testing GR. Only recently have QNM studies begun to focus on multimode fitting to numerical relativity (NR) strain waveforms. As GW observatories become even more sensitive they will be able to resolve higher-order modes. Consequently, multimode QNM fits will be critically important, and in turn require a more thorough treatment of the asymptotic frame at $\\mathscr{I}^+$. The first main result of this work is a method for systematically fitting a QNM model containing many"},"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":"2110.15922","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2021-10-29T17:16:46Z","cross_cats_sorted":["astro-ph.HE","hep-th"],"title_canon_sha256":"15eb1b6c346c74fa908fc216e2922d67d5de4f8637dcaf2107738a865bdc527e","abstract_canon_sha256":"67386717800f4d16e91e8043c3eb72a7f9110fc982a8a2e1ba34e0e805fc803d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T04:22:17.610674Z","signature_b64":"tMizNty4+IenTdKPAq4KoF8YfszZuMCsRE60AzLYBw2oykNE9caIdP9viL6kD5rG3fkKVQFlkI4psYAnL1nECA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"44c099224f686dfdf646e27ede9fda1e831c992cc7b016e83f3b8fffb69c0465","last_reissued_at":"2026-07-05T04:22:17.610188Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T04:22:17.610188Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"High Precision Ringdown Modeling: Multimode Fits and BMS Frames","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","hep-th"],"primary_cat":"gr-qc","authors_text":"Dante A. B. Iozzo, Fran\\c{c}ois H\\'ebert, Harald P. Pfeiffer, Jordan Moxon, Keefe Mitman, Lawrence E. Kidder, Leo C. Stein, Lorena Maga\\~na Zertuche, Mark A. Scheel, Michael Boyle, Neev Khera, Nils Deppe, Nils Vu, Saul A. Teukolsky, William Throwe","submitted_at":"2021-10-29T17:16:46Z","abstract_excerpt":"Quasi-normal mode (QNM) modeling is an invaluable tool for characterizing remnant black holes, studying strong gravity, and testing GR. Only recently have QNM studies begun to focus on multimode fitting to numerical relativity (NR) strain waveforms. As GW observatories become even more sensitive they will be able to resolve higher-order modes. Consequently, multimode QNM fits will be critically important, and in turn require a more thorough treatment of the asymptotic frame at $\\mathscr{I}^+$. The first main result of this work is a method for systematically fitting a QNM model containing many"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2110.15922","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/2110.15922/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":"2110.15922","created_at":"2026-07-05T04:22:17.610246+00:00"},{"alias_kind":"arxiv_version","alias_value":"2110.15922v2","created_at":"2026-07-05T04:22:17.610246+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2110.15922","created_at":"2026-07-05T04:22:17.610246+00:00"},{"alias_kind":"pith_short_12","alias_value":"ITAJSISPNBW7","created_at":"2026-07-05T04:22:17.610246+00:00"},{"alias_kind":"pith_short_16","alias_value":"ITAJSISPNBW735SG","created_at":"2026-07-05T04:22:17.610246+00:00"},{"alias_kind":"pith_short_8","alias_value":"ITAJSISP","created_at":"2026-07-05T04:22:17.610246+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.24816","citing_title":"The Bondi--Sachs gauge, BMS frames, and memory in black hole perturbation theory","ref_index":27,"is_internal_anchor":false},{"citing_arxiv_id":"2605.14078","citing_title":"Properties of natural polynomials for Schwarzschild and Kerr black holes","ref_index":16,"is_internal_anchor":false},{"citing_arxiv_id":"2505.23895","citing_title":"Black hole spectroscopy: from theory to experiment","ref_index":45,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/ITAJSISPNBW735SG4J7N5H62D2","json":"https://pith.science/pith/ITAJSISPNBW735SG4J7N5H62D2.json","graph_json":"https://pith.science/api/pith-number/ITAJSISPNBW735SG4J7N5H62D2/graph.json","events_json":"https://pith.science/api/pith-number/ITAJSISPNBW735SG4J7N5H62D2/events.json","paper":"https://pith.science/paper/ITAJSISP"},"agent_actions":{"view_html":"https://pith.science/pith/ITAJSISPNBW735SG4J7N5H62D2","download_json":"https://pith.science/pith/ITAJSISPNBW735SG4J7N5H62D2.json","view_paper":"https://pith.science/paper/ITAJSISP","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2110.15922&json=true","fetch_graph":"https://pith.science/api/pith-number/ITAJSISPNBW735SG4J7N5H62D2/graph.json","fetch_events":"https://pith.science/api/pith-number/ITAJSISPNBW735SG4J7N5H62D2/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ITAJSISPNBW735SG4J7N5H62D2/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ITAJSISPNBW735SG4J7N5H62D2/action/storage_attestation","attest_author":"https://pith.science/pith/ITAJSISPNBW735SG4J7N5H62D2/action/author_attestation","sign_citation":"https://pith.science/pith/ITAJSISPNBW735SG4J7N5H62D2/action/citation_signature","submit_replication":"https://pith.science/pith/ITAJSISPNBW735SG4J7N5H62D2/action/replication_record"}},"created_at":"2026-07-05T04:22:17.610246+00:00","updated_at":"2026-07-05T04:22:17.610246+00:00"}