{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:1997:AK2LQIOZAV7KBFFRCUZAHUZYZC","short_pith_number":"pith:AK2LQIOZ","schema_version":"1.0","canonical_sha256":"02b4b821d9057ea094b1153203d338c8b3fab81124ce360c3ad072a602f672f0","source":{"kind":"arxiv","id":"gr-qc/9701039","version":2},"attestation_state":"computed","paper":{"title":"Measuring gravitational waves from binary black hole coalescences: I. Signal to noise for inspiral, merger, and ringdown","license":"","headline":"","cross_cats":["astro-ph"],"primary_cat":"gr-qc","authors_text":"Eanna E. Flanagan, Scott A. Hughes","submitted_at":"1997-01-16T23:31:49Z","abstract_excerpt":"We estimate the expected signal-to-noise ratios (SNRs) from the three phases (inspiral,merger,ringdown) of coalescing binary black holes (BBHs) for initial and advanced ground-based interferometers (LIGO/VIRGO) and for space-based interferometers (LISA). LIGO/VIRGO can do moderate SNR (a few tens), moderate accuracy studies of BBH coalescences in the mass range of a few to about 2000 solar masses; LISA can do high SNR (of order 10^4) high accuracy studies in the mass range of about 10^5 to 10^8 solar masses. BBHs might well be the first sources detected by LIGO/VIRGO: they are visible to much "},"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/9701039","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"gr-qc","submitted_at":"1997-01-16T23:31:49Z","cross_cats_sorted":["astro-ph"],"title_canon_sha256":"29e8ab86f414cc5092cd9aae8bf4752fb22908a4b6e0092c428d41d916a6d498","abstract_canon_sha256":"1e2627badd023fed8968710711eb1d86efbf26a80106f2b968d9f3284092c996"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T17:18:23.059306Z","signature_b64":"bWxnkn8tXNusvVqvgSAHKNn71+0B8cCSUPc96W5zwxN93+P3t0HQI7yVa8qiOg3ZTDAn1obcMmSwnKhgbj3UAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"02b4b821d9057ea094b1153203d338c8b3fab81124ce360c3ad072a602f672f0","last_reissued_at":"2026-07-04T17:18:23.058969Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T17:18:23.058969Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Measuring gravitational waves from binary black hole coalescences: I. Signal to noise for inspiral, merger, and ringdown","license":"","headline":"","cross_cats":["astro-ph"],"primary_cat":"gr-qc","authors_text":"Eanna E. Flanagan, Scott A. Hughes","submitted_at":"1997-01-16T23:31:49Z","abstract_excerpt":"We estimate the expected signal-to-noise ratios (SNRs) from the three phases (inspiral,merger,ringdown) of coalescing binary black holes (BBHs) for initial and advanced ground-based interferometers (LIGO/VIRGO) and for space-based interferometers (LISA). LIGO/VIRGO can do moderate SNR (a few tens), moderate accuracy studies of BBH coalescences in the mass range of a few to about 2000 solar masses; LISA can do high SNR (of order 10^4) high accuracy studies in the mass range of about 10^5 to 10^8 solar masses. BBHs might well be the first sources detected by LIGO/VIRGO: they are visible to much "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"gr-qc/9701039","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/gr-qc/9701039/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":"gr-qc/9701039","created_at":"2026-07-04T17:18:23.059028+00:00"},{"alias_kind":"arxiv_version","alias_value":"gr-qc/9701039v2","created_at":"2026-07-04T17:18:23.059028+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.gr-qc/9701039","created_at":"2026-07-04T17:18:23.059028+00:00"},{"alias_kind":"pith_short_12","alias_value":"AK2LQIOZAV7K","created_at":"2026-07-04T17:18:23.059028+00:00"},{"alias_kind":"pith_short_16","alias_value":"AK2LQIOZAV7KBFFR","created_at":"2026-07-04T17:18:23.059028+00:00"},{"alias_kind":"pith_short_8","alias_value":"AK2LQIOZ","created_at":"2026-07-04T17:18:23.059028+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":7,"internal_anchor_count":4,"sample":[{"citing_arxiv_id":"2606.21549","citing_title":"Binary Black Hole Coalescence and the Dynamics of Scalar Hair in Einstein-Maxwell-Scalar Theory","ref_index":8,"is_internal_anchor":true},{"citing_arxiv_id":"2606.19446","citing_title":"Dynamical Tidal Response of Neutron Stars: from Effective Field Theory to Gravitational Waveforms","ref_index":105,"is_internal_anchor":true},{"citing_arxiv_id":"2606.03346","citing_title":"Model-Independent Search Discards Faint Lensed-Pairs of Gravitational Wave Events in the Sub-Threshold Candidates of GWTC-4","ref_index":90,"is_internal_anchor":true},{"citing_arxiv_id":"2603.23634","citing_title":"Testing Dark Energy with Black Hole Ringdown","ref_index":86,"is_internal_anchor":true},{"citing_arxiv_id":"gr-qc/9909058","citing_title":"Quasi-Normal Modes of Stars and Black Holes","ref_index":90,"is_internal_anchor":false},{"citing_arxiv_id":"0905.2975","citing_title":"Quasinormal modes of black holes and black branes","ref_index":90,"is_internal_anchor":false},{"citing_arxiv_id":"2604.22731","citing_title":"Precision Analysis for $\\boldsymbol{H_0}$ Using Upcoming Multi-band Gravitational Wave Observations","ref_index":42,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/AK2LQIOZAV7KBFFRCUZAHUZYZC","json":"https://pith.science/pith/AK2LQIOZAV7KBFFRCUZAHUZYZC.json","graph_json":"https://pith.science/api/pith-number/AK2LQIOZAV7KBFFRCUZAHUZYZC/graph.json","events_json":"https://pith.science/api/pith-number/AK2LQIOZAV7KBFFRCUZAHUZYZC/events.json","paper":"https://pith.science/paper/AK2LQIOZ"},"agent_actions":{"view_html":"https://pith.science/pith/AK2LQIOZAV7KBFFRCUZAHUZYZC","download_json":"https://pith.science/pith/AK2LQIOZAV7KBFFRCUZAHUZYZC.json","view_paper":"https://pith.science/paper/AK2LQIOZ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=gr-qc/9701039&json=true","fetch_graph":"https://pith.science/api/pith-number/AK2LQIOZAV7KBFFRCUZAHUZYZC/graph.json","fetch_events":"https://pith.science/api/pith-number/AK2LQIOZAV7KBFFRCUZAHUZYZC/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/AK2LQIOZAV7KBFFRCUZAHUZYZC/action/timestamp_anchor","attest_storage":"https://pith.science/pith/AK2LQIOZAV7KBFFRCUZAHUZYZC/action/storage_attestation","attest_author":"https://pith.science/pith/AK2LQIOZAV7KBFFRCUZAHUZYZC/action/author_attestation","sign_citation":"https://pith.science/pith/AK2LQIOZAV7KBFFRCUZAHUZYZC/action/citation_signature","submit_replication":"https://pith.science/pith/AK2LQIOZAV7KBFFRCUZAHUZYZC/action/replication_record"}},"created_at":"2026-07-04T17:18:23.059028+00:00","updated_at":"2026-07-04T17:18:23.059028+00:00"}