{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:OIL73YWV3CS2UD3YQKO37MPEE3","short_pith_number":"pith:OIL73YWV","schema_version":"1.0","canonical_sha256":"7217fde2d5d8a5aa0f78829dbfb1e426ec1d276ef14a6933a063de94b588e56f","source":{"kind":"arxiv","id":"2203.10109","version":2},"attestation_state":"computed","paper":{"title":"Targeted large mass ratio numerical relativity surrogate waveform model for GW190814","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"gr-qc","authors_text":"Carl-Johan Haster, Harald P. Pfeiffer, Jooheon Yoo, Lawrence E. Kidder, Mark A. Scheel, Matthew Giesler, Michael Boyle, Vijay Varma","submitted_at":"2022-03-18T18:08:05Z","abstract_excerpt":"Gravitational wave observations of large mass ratio compact binary mergers like GW190814 highlight the need for reliable, high-accuracy waveform templates for such systems. We present NRHybSur2dq15, a new surrogate model trained on hybridized numerical relativity (NR) waveforms with mass ratios $q\\leq15$, and aligned spins $|\\chi_{1z}|\\leq0.5$ and $\\chi_{2z}=0$. We target the parameter space of GW190814-like events as large mass ratio NR simulations are very expensive. The model includes the (2,2), (2,1), (3,3), (4,4), and (5,5) spin-weighted spherical harmonic modes, and spans the entire LIGO"},"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":"2203.10109","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"gr-qc","submitted_at":"2022-03-18T18:08:05Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"8e34fb31f25369e4d3b4089399887e3beb4c2cc68d868d3c51afd69f5ea6593b","abstract_canon_sha256":"db7fe8b85206a11506ef1045686a16036decb42936b6e4d9f93140d2e19ec44b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T04:48:44.980574Z","signature_b64":"L4khsaRlfbJcHVL/Qpgxhu6feYA87cpdN5s1dkaOWMHBCcLam5VfWTOzbBCLfjU9Dr4PtiR4Hnn6d1+ie+GeBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"7217fde2d5d8a5aa0f78829dbfb1e426ec1d276ef14a6933a063de94b588e56f","last_reissued_at":"2026-07-05T04:48:44.980138Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T04:48:44.980138Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Targeted large mass ratio numerical relativity surrogate waveform model for GW190814","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"gr-qc","authors_text":"Carl-Johan Haster, Harald P. Pfeiffer, Jooheon Yoo, Lawrence E. Kidder, Mark A. Scheel, Matthew Giesler, Michael Boyle, Vijay Varma","submitted_at":"2022-03-18T18:08:05Z","abstract_excerpt":"Gravitational wave observations of large mass ratio compact binary mergers like GW190814 highlight the need for reliable, high-accuracy waveform templates for such systems. We present NRHybSur2dq15, a new surrogate model trained on hybridized numerical relativity (NR) waveforms with mass ratios $q\\leq15$, and aligned spins $|\\chi_{1z}|\\leq0.5$ and $\\chi_{2z}=0$. We target the parameter space of GW190814-like events as large mass ratio NR simulations are very expensive. The model includes the (2,2), (2,1), (3,3), (4,4), and (5,5) spin-weighted spherical harmonic modes, and spans the entire LIGO"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2203.10109","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/2203.10109/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":"2203.10109","created_at":"2026-07-05T04:48:44.980194+00:00"},{"alias_kind":"arxiv_version","alias_value":"2203.10109v2","created_at":"2026-07-05T04:48:44.980194+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2203.10109","created_at":"2026-07-05T04:48:44.980194+00:00"},{"alias_kind":"pith_short_12","alias_value":"OIL73YWV3CS2","created_at":"2026-07-05T04:48:44.980194+00:00"},{"alias_kind":"pith_short_16","alias_value":"OIL73YWV3CS2UD3Y","created_at":"2026-07-05T04:48:44.980194+00:00"},{"alias_kind":"pith_short_8","alias_value":"OIL73YWV","created_at":"2026-07-05T04:48:44.980194+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2407.18319","citing_title":"Gravitational wave surrogate model for spinning, intermediate mass ratio binaries based on perturbation theory and numerical relativity","ref_index":24,"is_internal_anchor":false},{"citing_arxiv_id":"2605.00124","citing_title":"Merger remnant and eccentricity dynamics surrogates for eccentric nonspinning black hole binaries","ref_index":26,"is_internal_anchor":false},{"citing_arxiv_id":"2511.10522","citing_title":"Learning Post-Newtonian Corrections from Numerical Relativity","ref_index":69,"is_internal_anchor":false},{"citing_arxiv_id":"2605.00124","citing_title":"Merger remnant and eccentricity dynamics surrogates for eccentric nonspinning black hole binaries","ref_index":26,"is_internal_anchor":false},{"citing_arxiv_id":"2604.07388","citing_title":"GW190711_030756 and GW200114_020818: astrophysical interpretation of two asymmetric binary black hole mergers in the IAS catalog","ref_index":28,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/OIL73YWV3CS2UD3YQKO37MPEE3","json":"https://pith.science/pith/OIL73YWV3CS2UD3YQKO37MPEE3.json","graph_json":"https://pith.science/api/pith-number/OIL73YWV3CS2UD3YQKO37MPEE3/graph.json","events_json":"https://pith.science/api/pith-number/OIL73YWV3CS2UD3YQKO37MPEE3/events.json","paper":"https://pith.science/paper/OIL73YWV"},"agent_actions":{"view_html":"https://pith.science/pith/OIL73YWV3CS2UD3YQKO37MPEE3","download_json":"https://pith.science/pith/OIL73YWV3CS2UD3YQKO37MPEE3.json","view_paper":"https://pith.science/paper/OIL73YWV","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2203.10109&json=true","fetch_graph":"https://pith.science/api/pith-number/OIL73YWV3CS2UD3YQKO37MPEE3/graph.json","fetch_events":"https://pith.science/api/pith-number/OIL73YWV3CS2UD3YQKO37MPEE3/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/OIL73YWV3CS2UD3YQKO37MPEE3/action/timestamp_anchor","attest_storage":"https://pith.science/pith/OIL73YWV3CS2UD3YQKO37MPEE3/action/storage_attestation","attest_author":"https://pith.science/pith/OIL73YWV3CS2UD3YQKO37MPEE3/action/author_attestation","sign_citation":"https://pith.science/pith/OIL73YWV3CS2UD3YQKO37MPEE3/action/citation_signature","submit_replication":"https://pith.science/pith/OIL73YWV3CS2UD3YQKO37MPEE3/action/replication_record"}},"created_at":"2026-07-05T04:48:44.980194+00:00","updated_at":"2026-07-05T04:48:44.980194+00:00"}