{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:4RQXP2EQDZ45M74VELURMDBMPL","short_pith_number":"pith:4RQXP2EQ","schema_version":"1.0","canonical_sha256":"e46177e8901e79d67f9522e9160c2c7acad6ef6672ecc41e02dade49ad26f151","source":{"kind":"arxiv","id":"2102.08614","version":1},"attestation_state":"computed","paper":{"title":"A higher-multipole gravitational waveform model for an eccentric binary black holes based on the effective-one-body-numerical-relativity formalism","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Xiaolin Liu, Zhoujian Cao, Zong-Hong Zhu","submitted_at":"2021-02-17T07:34:48Z","abstract_excerpt":"We construct a new factorized waveform including $(l,|m|)=(2,2),(2,1),(3,3),(4,4)$ modes based on effective-one-body (EOB) formalism, which is valid for spinning binary black holes (BBH) in general equatorial orbit. When combined with the dynamics of $\\texttt{SEOBNRv4}$, the $(l,|m|)=(2,2)$ mode waveform generated by this new waveform can fit the original $\\texttt{SEOBNRv4}$ waveform very well in the case of a quasi-circular orbit. We have calibrated our new waveform model to the Simulating eXtreme Spacetimes (SXS) catalog. The comparison is done for BBH with total mass in $(20,200)M_\\odot$ us"},"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":"2102.08614","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2021-02-17T07:34:48Z","cross_cats_sorted":[],"title_canon_sha256":"2a7b8b516e343dc15460a66bc065157277633d2b57edd17a82f82eff9359f625","abstract_canon_sha256":"0a5fdacdbcf4307fc2d18d1cecf7cda31f712da3fba615a88392d1758c23e1fe"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T03:52:56.003200Z","signature_b64":"zdxI1dkfKvnaRDvubg9HhdLaAcsgjLr/aY3r5bPtyxlUWKnlv2SoQOgmYPSmOA5hVR6jy2nolAC9z0lyLWgfAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"e46177e8901e79d67f9522e9160c2c7acad6ef6672ecc41e02dade49ad26f151","last_reissued_at":"2026-07-05T03:52:56.002795Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T03:52:56.002795Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A higher-multipole gravitational waveform model for an eccentric binary black holes based on the effective-one-body-numerical-relativity formalism","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Xiaolin Liu, Zhoujian Cao, Zong-Hong Zhu","submitted_at":"2021-02-17T07:34:48Z","abstract_excerpt":"We construct a new factorized waveform including $(l,|m|)=(2,2),(2,1),(3,3),(4,4)$ modes based on effective-one-body (EOB) formalism, which is valid for spinning binary black holes (BBH) in general equatorial orbit. When combined with the dynamics of $\\texttt{SEOBNRv4}$, the $(l,|m|)=(2,2)$ mode waveform generated by this new waveform can fit the original $\\texttt{SEOBNRv4}$ waveform very well in the case of a quasi-circular orbit. We have calibrated our new waveform model to the Simulating eXtreme Spacetimes (SXS) catalog. The comparison is done for BBH with total mass in $(20,200)M_\\odot$ us"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2102.08614","kind":"arxiv","version":1},"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/2102.08614/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":"2102.08614","created_at":"2026-07-05T03:52:56.002853+00:00"},{"alias_kind":"arxiv_version","alias_value":"2102.08614v1","created_at":"2026-07-05T03:52:56.002853+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2102.08614","created_at":"2026-07-05T03:52:56.002853+00:00"},{"alias_kind":"pith_short_12","alias_value":"4RQXP2EQDZ45","created_at":"2026-07-05T03:52:56.002853+00:00"},{"alias_kind":"pith_short_16","alias_value":"4RQXP2EQDZ45M74V","created_at":"2026-07-05T03:52:56.002853+00:00"},{"alias_kind":"pith_short_8","alias_value":"4RQXP2EQ","created_at":"2026-07-05T03:52:56.002853+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.30594","citing_title":"Efficient Eccentric Effective-One-Body Dynamics via Near-Identity Averaging Transformations","ref_index":101,"is_internal_anchor":false},{"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":269,"is_internal_anchor":false},{"citing_arxiv_id":"2509.14924","citing_title":"Residual Test for the Third Gravitational-Wave Transient Catalog","ref_index":20,"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":144,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/4RQXP2EQDZ45M74VELURMDBMPL","json":"https://pith.science/pith/4RQXP2EQDZ45M74VELURMDBMPL.json","graph_json":"https://pith.science/api/pith-number/4RQXP2EQDZ45M74VELURMDBMPL/graph.json","events_json":"https://pith.science/api/pith-number/4RQXP2EQDZ45M74VELURMDBMPL/events.json","paper":"https://pith.science/paper/4RQXP2EQ"},"agent_actions":{"view_html":"https://pith.science/pith/4RQXP2EQDZ45M74VELURMDBMPL","download_json":"https://pith.science/pith/4RQXP2EQDZ45M74VELURMDBMPL.json","view_paper":"https://pith.science/paper/4RQXP2EQ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2102.08614&json=true","fetch_graph":"https://pith.science/api/pith-number/4RQXP2EQDZ45M74VELURMDBMPL/graph.json","fetch_events":"https://pith.science/api/pith-number/4RQXP2EQDZ45M74VELURMDBMPL/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/4RQXP2EQDZ45M74VELURMDBMPL/action/timestamp_anchor","attest_storage":"https://pith.science/pith/4RQXP2EQDZ45M74VELURMDBMPL/action/storage_attestation","attest_author":"https://pith.science/pith/4RQXP2EQDZ45M74VELURMDBMPL/action/author_attestation","sign_citation":"https://pith.science/pith/4RQXP2EQDZ45M74VELURMDBMPL/action/citation_signature","submit_replication":"https://pith.science/pith/4RQXP2EQDZ45M74VELURMDBMPL/action/replication_record"}},"created_at":"2026-07-05T03:52:56.002853+00:00","updated_at":"2026-07-05T03:52:56.002853+00:00"}