{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:WJWHKYMA2KVM6P227GAALPTJIA","short_pith_number":"pith:WJWHKYMA","schema_version":"1.0","canonical_sha256":"b26c756180d2aacf3f5af98005be69402b0c1cff7932bd932bc055fc6790d62f","source":{"kind":"arxiv","id":"1602.03081","version":2},"attestation_state":"computed","paper":{"title":"Frequency and time domain inspiral templates for comparable mass compact binaries in eccentric orbits","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Achamveedu Gopakumar, Maria Haney, Sashwat Tanay","submitted_at":"2016-02-09T17:19:06Z","abstract_excerpt":"Inspiraling compact binaries with non-negligible orbital eccentricities are plausible gravitational wave (GW) sources for the upcoming network of GW observatories. In this paper, we present two prescriptions to compute post-Newtonian (PN) accurate inspiral templates for such binaries. First, we adapt and extend the post-circular scheme of Yunes {\\it et al.} [Phys. Rev. D 80, 084001 (2009)] to obtain a Fourier-domain inspiral approximant that incorporates the effects of PN-accurate orbital eccentricity evolution. This results in a fully analytic frequency-domain inspiral waveform with Newtonian"},"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":"1602.03081","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2016-02-09T17:19:06Z","cross_cats_sorted":[],"title_canon_sha256":"b15925c53d920a7f6bdaa5d754ca9f4f089f51421998332a60a7770a0d677b65","abstract_canon_sha256":"e559a0e8d416b6bf9193c4d039b6020627dc1e6d912b30b0c8ef6f81684088f3"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:14:52.488151Z","signature_b64":"abN/IYWyJuYsQ/mqgBAfyVxYK11zsrp/ZnqsPnFy7GV/luc59ytHHqaLItY56XDCqzDnskCW7qWHK/+FmKi2Bw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"b26c756180d2aacf3f5af98005be69402b0c1cff7932bd932bc055fc6790d62f","last_reissued_at":"2026-05-18T01:14:52.487667Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:14:52.487667Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Frequency and time domain inspiral templates for comparable mass compact binaries in eccentric orbits","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Achamveedu Gopakumar, Maria Haney, Sashwat Tanay","submitted_at":"2016-02-09T17:19:06Z","abstract_excerpt":"Inspiraling compact binaries with non-negligible orbital eccentricities are plausible gravitational wave (GW) sources for the upcoming network of GW observatories. In this paper, we present two prescriptions to compute post-Newtonian (PN) accurate inspiral templates for such binaries. First, we adapt and extend the post-circular scheme of Yunes {\\it et al.} [Phys. Rev. D 80, 084001 (2009)] to obtain a Fourier-domain inspiral approximant that incorporates the effects of PN-accurate orbital eccentricity evolution. This results in a fully analytic frequency-domain inspiral waveform with Newtonian"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1602.03081","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":""},"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":"1602.03081","created_at":"2026-05-18T01:14:52.487747+00:00"},{"alias_kind":"arxiv_version","alias_value":"1602.03081v2","created_at":"2026-05-18T01:14:52.487747+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1602.03081","created_at":"2026-05-18T01:14:52.487747+00:00"},{"alias_kind":"pith_short_12","alias_value":"WJWHKYMA2KVM","created_at":"2026-05-18T12:30:48.956258+00:00"},{"alias_kind":"pith_short_16","alias_value":"WJWHKYMA2KVM6P22","created_at":"2026-05-18T12:30:48.956258+00:00"},{"alias_kind":"pith_short_8","alias_value":"WJWHKYMA","created_at":"2026-05-18T12:30:48.956258+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2412.20664","citing_title":"Enhancing Early Detection and Localization of Gravitational Waves via Eccentricity-Induced Higher Harmonic Modes with 2G Detector Networks","ref_index":29,"is_internal_anchor":true},{"citing_arxiv_id":"2510.04332","citing_title":"Biased parameter inference of eccentric, spin-precessing binary black holes","ref_index":104,"is_internal_anchor":true},{"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":64,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/WJWHKYMA2KVM6P227GAALPTJIA","json":"https://pith.science/pith/WJWHKYMA2KVM6P227GAALPTJIA.json","graph_json":"https://pith.science/api/pith-number/WJWHKYMA2KVM6P227GAALPTJIA/graph.json","events_json":"https://pith.science/api/pith-number/WJWHKYMA2KVM6P227GAALPTJIA/events.json","paper":"https://pith.science/paper/WJWHKYMA"},"agent_actions":{"view_html":"https://pith.science/pith/WJWHKYMA2KVM6P227GAALPTJIA","download_json":"https://pith.science/pith/WJWHKYMA2KVM6P227GAALPTJIA.json","view_paper":"https://pith.science/paper/WJWHKYMA","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1602.03081&json=true","fetch_graph":"https://pith.science/api/pith-number/WJWHKYMA2KVM6P227GAALPTJIA/graph.json","fetch_events":"https://pith.science/api/pith-number/WJWHKYMA2KVM6P227GAALPTJIA/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/WJWHKYMA2KVM6P227GAALPTJIA/action/timestamp_anchor","attest_storage":"https://pith.science/pith/WJWHKYMA2KVM6P227GAALPTJIA/action/storage_attestation","attest_author":"https://pith.science/pith/WJWHKYMA2KVM6P227GAALPTJIA/action/author_attestation","sign_citation":"https://pith.science/pith/WJWHKYMA2KVM6P227GAALPTJIA/action/citation_signature","submit_replication":"https://pith.science/pith/WJWHKYMA2KVM6P227GAALPTJIA/action/replication_record"}},"created_at":"2026-05-18T01:14:52.487747+00:00","updated_at":"2026-05-18T01:14:52.487747+00:00"}