{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:CDQEBTVN6MLA4W53LYQ3YC4LWU","short_pith_number":"pith:CDQEBTVN","schema_version":"1.0","canonical_sha256":"10e040ceadf3160e5bbb5e21bc0b8bb50b08e7581988338c64aa2d90ae907591","source":{"kind":"arxiv","id":"2101.11798","version":2},"attestation_state":"computed","paper":{"title":"Eccentric binary black hole surrogate models for the gravitational waveform and remnant properties: comparable mass, nonspinning case","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"gr-qc","authors_text":"Davide Gerosa, Gaurav Khanna, Harald P. Pfeiffer, Jackie Lodman, Lawrence E. Kidder, Mark A. Scheel, Scott E. Field, Tousif Islam, Vijay Varma","submitted_at":"2021-01-28T03:25:19Z","abstract_excerpt":"We develop new strategies to build numerical relativity surrogate models for eccentric binary black hole systems, which are expected to play an increasingly important role in current and future gravitational-wave detectors. We introduce a new surrogate waveform model, \\texttt{NRSur2dq1Ecc}, using 47 nonspinning, equal-mass waveforms with eccentricities up to $0.2$ when measured at a reference time of $5500M$ before merger. This is the first waveform model that is directly trained on eccentric numerical relativity simulations and does not require that the binary circularizes before merger. The "},"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":"2101.11798","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"gr-qc","submitted_at":"2021-01-28T03:25:19Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"9baf0d65b3ec2a44eae7bebe9784b5173ff65c240a1a2e95f4fb356bd9ca5318","abstract_canon_sha256":"6a265c3343956f64af2a36a22bb6cc5dec4a997a99e9cb7a9565de0298838eb1"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T02:26:17.545727Z","signature_b64":"nKiFcR/Hr9W49cWh1sDDMN0QAAcZhsaE08bvCbsZEygUGdMbBnk87Fh2L7CsIBPjszSZmoBRMQEV4qzibh/zDw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"10e040ceadf3160e5bbb5e21bc0b8bb50b08e7581988338c64aa2d90ae907591","last_reissued_at":"2026-07-05T02:26:17.545321Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T02:26:17.545321Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Eccentric binary black hole surrogate models for the gravitational waveform and remnant properties: comparable mass, nonspinning case","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"gr-qc","authors_text":"Davide Gerosa, Gaurav Khanna, Harald P. Pfeiffer, Jackie Lodman, Lawrence E. Kidder, Mark A. Scheel, Scott E. Field, Tousif Islam, Vijay Varma","submitted_at":"2021-01-28T03:25:19Z","abstract_excerpt":"We develop new strategies to build numerical relativity surrogate models for eccentric binary black hole systems, which are expected to play an increasingly important role in current and future gravitational-wave detectors. We introduce a new surrogate waveform model, \\texttt{NRSur2dq1Ecc}, using 47 nonspinning, equal-mass waveforms with eccentricities up to $0.2$ when measured at a reference time of $5500M$ before merger. This is the first waveform model that is directly trained on eccentric numerical relativity simulations and does not require that the binary circularizes before merger. The "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2101.11798","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/2101.11798/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":"2101.11798","created_at":"2026-07-05T02:26:17.545378+00:00"},{"alias_kind":"arxiv_version","alias_value":"2101.11798v2","created_at":"2026-07-05T02:26:17.545378+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2101.11798","created_at":"2026-07-05T02:26:17.545378+00:00"},{"alias_kind":"pith_short_12","alias_value":"CDQEBTVN6MLA","created_at":"2026-07-05T02:26:17.545378+00:00"},{"alias_kind":"pith_short_16","alias_value":"CDQEBTVN6MLA4W53","created_at":"2026-07-05T02:26:17.545378+00:00"},{"alias_kind":"pith_short_8","alias_value":"CDQEBTVN","created_at":"2026-07-05T02:26:17.545378+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":10,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2605.28715","citing_title":"Accurate waveforms for generic planar-orbit binary black holes: The multipolar effective-one-body model SEOBNRv6EHM","ref_index":141,"is_internal_anchor":false},{"citing_arxiv_id":"2404.14286","citing_title":"Evidence for eccentricity in the population of binary black holes observed by LIGO-Virgo-KAGRA","ref_index":172,"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":25,"is_internal_anchor":false},{"citing_arxiv_id":"2509.14924","citing_title":"Residual Test for the Third Gravitational-Wave Transient Catalog","ref_index":23,"is_internal_anchor":false},{"citing_arxiv_id":"2510.04332","citing_title":"Biased parameter inference of eccentric, spin-precessing binary black holes","ref_index":100,"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":25,"is_internal_anchor":false},{"citing_arxiv_id":"2604.14270","citing_title":"Fast neural network surrogate for multimodal effective-one-body gravitational waveforms from generically precessing compact binaries","ref_index":64,"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":23,"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":83,"is_internal_anchor":false},{"citing_arxiv_id":"2604.15431","citing_title":"Highly eccentric non-spinning binary black hole mergers: quadrupolar post-merger waveforms","ref_index":95,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/CDQEBTVN6MLA4W53LYQ3YC4LWU","json":"https://pith.science/pith/CDQEBTVN6MLA4W53LYQ3YC4LWU.json","graph_json":"https://pith.science/api/pith-number/CDQEBTVN6MLA4W53LYQ3YC4LWU/graph.json","events_json":"https://pith.science/api/pith-number/CDQEBTVN6MLA4W53LYQ3YC4LWU/events.json","paper":"https://pith.science/paper/CDQEBTVN"},"agent_actions":{"view_html":"https://pith.science/pith/CDQEBTVN6MLA4W53LYQ3YC4LWU","download_json":"https://pith.science/pith/CDQEBTVN6MLA4W53LYQ3YC4LWU.json","view_paper":"https://pith.science/paper/CDQEBTVN","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2101.11798&json=true","fetch_graph":"https://pith.science/api/pith-number/CDQEBTVN6MLA4W53LYQ3YC4LWU/graph.json","fetch_events":"https://pith.science/api/pith-number/CDQEBTVN6MLA4W53LYQ3YC4LWU/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/CDQEBTVN6MLA4W53LYQ3YC4LWU/action/timestamp_anchor","attest_storage":"https://pith.science/pith/CDQEBTVN6MLA4W53LYQ3YC4LWU/action/storage_attestation","attest_author":"https://pith.science/pith/CDQEBTVN6MLA4W53LYQ3YC4LWU/action/author_attestation","sign_citation":"https://pith.science/pith/CDQEBTVN6MLA4W53LYQ3YC4LWU/action/citation_signature","submit_replication":"https://pith.science/pith/CDQEBTVN6MLA4W53LYQ3YC4LWU/action/replication_record"}},"created_at":"2026-07-05T02:26:17.545378+00:00","updated_at":"2026-07-05T02:26:17.545378+00:00"}