{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2004:I23TZQS2C6LC2CIGD4HP5QMJIY","short_pith_number":"pith:I23TZQS2","schema_version":"1.0","canonical_sha256":"46b73cc25a17962d09061f0efec189461f7e2b8a122ffc769cb4444c3cd24d17","source":{"kind":"arxiv","id":"gr-qc/0411146","version":4},"attestation_state":"computed","paper":{"title":"Parameter estimation of inspiralling compact binaries using 3.5 post-Newtonian gravitational wave phasing: The non-spinning case","license":"","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Bala R Iyer, B. S. Sathyaprakash, K. G. Arun, Pranesh A. Sundararajan","submitted_at":"2004-11-30T11:25:13Z","abstract_excerpt":"(Abridged) We revisit the problem of parameter estimation of gravitational-wave chirp signals from inspiralling non-spinning compact binaries in the light of the recent extension of the post-Newtonian (PN) phasing formula to order $(v/c)^7$ beyond the leading Newtonian order. We study in detail the implications of higher post-Newtonian orders from 1PN up to 3.5PN in steps of 0.5PN ($\\sim v/c$), and examine their convergence. In both initial and advanced detectors the estimation of the chirp mass (${\\cal M}$) and symmetric mass ratio ($\\eta$) improve at higher PN orders but oscillate with every"},"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":"gr-qc/0411146","kind":"arxiv","version":4},"metadata":{"license":"","primary_cat":"gr-qc","submitted_at":"2004-11-30T11:25:13Z","cross_cats_sorted":[],"title_canon_sha256":"6d5a37ed9b598fda098106d8553c0d7d2372295eba4ef34681016b6e81246872","abstract_canon_sha256":"095d54f35948f358b28c0a18ba429b5438f6ebf3c78fa06a7fd4ac830c1ca8bd"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:37:27.762263Z","signature_b64":"Z7rnydJl3z/Om/fTGVfopo4gb69IVab4Yt5wLb87IsRp6IOJDOquQjMGhcF8FVVLlUiUdEBCmcQYiurCdDRaCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"46b73cc25a17962d09061f0efec189461f7e2b8a122ffc769cb4444c3cd24d17","last_reissued_at":"2026-05-18T02:37:27.761612Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:37:27.761612Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Parameter estimation of inspiralling compact binaries using 3.5 post-Newtonian gravitational wave phasing: The non-spinning case","license":"","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Bala R Iyer, B. S. Sathyaprakash, K. G. Arun, Pranesh A. Sundararajan","submitted_at":"2004-11-30T11:25:13Z","abstract_excerpt":"(Abridged) We revisit the problem of parameter estimation of gravitational-wave chirp signals from inspiralling non-spinning compact binaries in the light of the recent extension of the post-Newtonian (PN) phasing formula to order $(v/c)^7$ beyond the leading Newtonian order. We study in detail the implications of higher post-Newtonian orders from 1PN up to 3.5PN in steps of 0.5PN ($\\sim v/c$), and examine their convergence. In both initial and advanced detectors the estimation of the chirp mass (${\\cal M}$) and symmetric mass ratio ($\\eta$) improve at higher PN orders but oscillate with every"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"gr-qc/0411146","kind":"arxiv","version":4},"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":"gr-qc/0411146","created_at":"2026-05-18T02:37:27.761698+00:00"},{"alias_kind":"arxiv_version","alias_value":"gr-qc/0411146v4","created_at":"2026-05-18T02:37:27.761698+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.gr-qc/0411146","created_at":"2026-05-18T02:37:27.761698+00:00"},{"alias_kind":"pith_short_12","alias_value":"I23TZQS2C6LC","created_at":"2026-05-18T12:25:52.687210+00:00"},{"alias_kind":"pith_short_16","alias_value":"I23TZQS2C6LC2CIG","created_at":"2026-05-18T12:25:52.687210+00:00"},{"alias_kind":"pith_short_8","alias_value":"I23TZQS2","created_at":"2026-05-18T12:25:52.687210+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2305.15473","citing_title":"Worldline effective field theory of inspiralling black hole binaries in presence of dark photon and axionic dark matter","ref_index":26,"is_internal_anchor":true},{"citing_arxiv_id":"1310.1528","citing_title":"Post-Newtonian Theory for Gravitational Waves","ref_index":13,"is_internal_anchor":false},{"citing_arxiv_id":"2605.04579","citing_title":"The Impact of Spin Priors on Parameterized Tests of General Relativity","ref_index":15,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/I23TZQS2C6LC2CIGD4HP5QMJIY","json":"https://pith.science/pith/I23TZQS2C6LC2CIGD4HP5QMJIY.json","graph_json":"https://pith.science/api/pith-number/I23TZQS2C6LC2CIGD4HP5QMJIY/graph.json","events_json":"https://pith.science/api/pith-number/I23TZQS2C6LC2CIGD4HP5QMJIY/events.json","paper":"https://pith.science/paper/I23TZQS2"},"agent_actions":{"view_html":"https://pith.science/pith/I23TZQS2C6LC2CIGD4HP5QMJIY","download_json":"https://pith.science/pith/I23TZQS2C6LC2CIGD4HP5QMJIY.json","view_paper":"https://pith.science/paper/I23TZQS2","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=gr-qc/0411146&json=true","fetch_graph":"https://pith.science/api/pith-number/I23TZQS2C6LC2CIGD4HP5QMJIY/graph.json","fetch_events":"https://pith.science/api/pith-number/I23TZQS2C6LC2CIGD4HP5QMJIY/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/I23TZQS2C6LC2CIGD4HP5QMJIY/action/timestamp_anchor","attest_storage":"https://pith.science/pith/I23TZQS2C6LC2CIGD4HP5QMJIY/action/storage_attestation","attest_author":"https://pith.science/pith/I23TZQS2C6LC2CIGD4HP5QMJIY/action/author_attestation","sign_citation":"https://pith.science/pith/I23TZQS2C6LC2CIGD4HP5QMJIY/action/citation_signature","submit_replication":"https://pith.science/pith/I23TZQS2C6LC2CIGD4HP5QMJIY/action/replication_record"}},"created_at":"2026-05-18T02:37:27.761698+00:00","updated_at":"2026-05-18T02:37:27.761698+00:00"}