{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:DCFG4RV2EXBVN2Z6BXWKIHSGME","short_pith_number":"pith:DCFG4RV2","schema_version":"1.0","canonical_sha256":"188a6e46ba25c356eb3e0deca41e46613e0d9de66496b39a7b9182252289c427","source":{"kind":"arxiv","id":"1705.07089","version":3},"attestation_state":"computed","paper":{"title":"A Numerical Relativity Waveform Surrogate Model for Generically Precessing Binary Black Hole Mergers","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"B\\'ela Szil\\'agyi, Chad R. Galley, Christian D. Ott, Harald P. Pfeiffer, Jonathan Blackman, Lawrence E. Kidder, Mark A. Scheel, Michael Boyle, Scott E. Field","submitted_at":"2017-05-19T16:58:53Z","abstract_excerpt":"A generic, non-eccentric binary black hole (BBH) system emits gravitational waves (GWs) that are completely described by 7 intrinsic parameters: the black hole spin vectors and the ratio of their masses. Simulating a BBH coalescence by solving Einstein's equations numerically is computationally expensive, requiring days to months of computing resources for a single set of parameter values. Since theoretical predictions of the GWs are often needed for many different source parameters, a fast and accurate model is essential. We present the first surrogate model for GWs from the coalescence of BB"},"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":"1705.07089","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2017-05-19T16:58:53Z","cross_cats_sorted":[],"title_canon_sha256":"e7cfbf8a9a0d61ee1cfc2b7c16407f6e78b1789720a34d97c9e8aef350aeefcf","abstract_canon_sha256":"1627756ac7ca9f274f51a1f2b0f517943e274fd5b49d313267df4dde66c78dec"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:05:09.591740Z","signature_b64":"k9u3haOwYD6vQwPxzNwHrHRZnwCYN/NT3MeJmmipp715DJoVh+T65XVAUKdu/uP7aRTxO3L7HisllXJ2bHyGBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"188a6e46ba25c356eb3e0deca41e46613e0d9de66496b39a7b9182252289c427","last_reissued_at":"2026-05-18T00:05:09.591138Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:05:09.591138Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A Numerical Relativity Waveform Surrogate Model for Generically Precessing Binary Black Hole Mergers","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"B\\'ela Szil\\'agyi, Chad R. Galley, Christian D. Ott, Harald P. Pfeiffer, Jonathan Blackman, Lawrence E. Kidder, Mark A. Scheel, Michael Boyle, Scott E. Field","submitted_at":"2017-05-19T16:58:53Z","abstract_excerpt":"A generic, non-eccentric binary black hole (BBH) system emits gravitational waves (GWs) that are completely described by 7 intrinsic parameters: the black hole spin vectors and the ratio of their masses. Simulating a BBH coalescence by solving Einstein's equations numerically is computationally expensive, requiring days to months of computing resources for a single set of parameter values. Since theoretical predictions of the GWs are often needed for many different source parameters, a fast and accurate model is essential. We present the first surrogate model for GWs from the coalescence of BB"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1705.07089","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":"1705.07089","created_at":"2026-05-18T00:05:09.591227+00:00"},{"alias_kind":"arxiv_version","alias_value":"1705.07089v3","created_at":"2026-05-18T00:05:09.591227+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1705.07089","created_at":"2026-05-18T00:05:09.591227+00:00"},{"alias_kind":"pith_short_12","alias_value":"DCFG4RV2EXBV","created_at":"2026-05-18T12:31:10.602751+00:00"},{"alias_kind":"pith_short_16","alias_value":"DCFG4RV2EXBVN2Z6","created_at":"2026-05-18T12:31:10.602751+00:00"},{"alias_kind":"pith_short_8","alias_value":"DCFG4RV2","created_at":"2026-05-18T12:31:10.602751+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":9,"internal_anchor_count":6,"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":66,"is_internal_anchor":true},{"citing_arxiv_id":"2605.00124","citing_title":"Merger remnant and eccentricity dynamics surrogates for eccentric nonspinning black hole binaries","ref_index":23,"is_internal_anchor":true},{"citing_arxiv_id":"2511.10522","citing_title":"Learning Post-Newtonian Corrections from Numerical Relativity","ref_index":48,"is_internal_anchor":true},{"citing_arxiv_id":"1905.00869","citing_title":"Testing the no-hair theorem with GW150914","ref_index":51,"is_internal_anchor":true},{"citing_arxiv_id":"1905.09300","citing_title":"Surrogate models for precessing binary black hole simulations with unequal masses","ref_index":56,"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":72,"is_internal_anchor":true},{"citing_arxiv_id":"2605.00124","citing_title":"Merger remnant and eccentricity dynamics surrogates for eccentric nonspinning black hole binaries","ref_index":23,"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":26,"is_internal_anchor":false},{"citing_arxiv_id":"2604.17868","citing_title":"Including higher-order modes in a quadrupolar eccentric numerical relativity surrogate using universal eccentric modulation functions","ref_index":98,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/DCFG4RV2EXBVN2Z6BXWKIHSGME","json":"https://pith.science/pith/DCFG4RV2EXBVN2Z6BXWKIHSGME.json","graph_json":"https://pith.science/api/pith-number/DCFG4RV2EXBVN2Z6BXWKIHSGME/graph.json","events_json":"https://pith.science/api/pith-number/DCFG4RV2EXBVN2Z6BXWKIHSGME/events.json","paper":"https://pith.science/paper/DCFG4RV2"},"agent_actions":{"view_html":"https://pith.science/pith/DCFG4RV2EXBVN2Z6BXWKIHSGME","download_json":"https://pith.science/pith/DCFG4RV2EXBVN2Z6BXWKIHSGME.json","view_paper":"https://pith.science/paper/DCFG4RV2","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1705.07089&json=true","fetch_graph":"https://pith.science/api/pith-number/DCFG4RV2EXBVN2Z6BXWKIHSGME/graph.json","fetch_events":"https://pith.science/api/pith-number/DCFG4RV2EXBVN2Z6BXWKIHSGME/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/DCFG4RV2EXBVN2Z6BXWKIHSGME/action/timestamp_anchor","attest_storage":"https://pith.science/pith/DCFG4RV2EXBVN2Z6BXWKIHSGME/action/storage_attestation","attest_author":"https://pith.science/pith/DCFG4RV2EXBVN2Z6BXWKIHSGME/action/author_attestation","sign_citation":"https://pith.science/pith/DCFG4RV2EXBVN2Z6BXWKIHSGME/action/citation_signature","submit_replication":"https://pith.science/pith/DCFG4RV2EXBVN2Z6BXWKIHSGME/action/replication_record"}},"created_at":"2026-05-18T00:05:09.591227+00:00","updated_at":"2026-05-18T00:05:09.591227+00:00"}