{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2012:FWZZL3ZD5V7B5X3YHADLM6I3CM","short_pith_number":"pith:FWZZL3ZD","schema_version":"1.0","canonical_sha256":"2db395ef23ed7e1edf783806b6791b1310b72c3505a29c1a94b686ddcc3d96a7","source":{"kind":"arxiv","id":"1207.4759","version":2},"attestation_state":"computed","paper":{"title":"Testing general relativity with gravitational waves: a reality check","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Michele Vallisneri","submitted_at":"2012-07-19T19:00:14Z","abstract_excerpt":"The observations of gravitational-wave signals from astrophysical sources such as binary inspirals will be used to test General Relativity for self consistency and against alternative theories of gravity. I describe a simple formula that can be used to characterize the prospects of such tests, by estimating the matched-filtering signal-to-noise ratio required to detect non-General-Relativistic corrections of a given magnitude. The formula is valid for sufficiently strong signals; it requires the computation of a single number, the fitting factor between the General-Relativistic and corrected w"},"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":"1207.4759","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2012-07-19T19:00:14Z","cross_cats_sorted":[],"title_canon_sha256":"9ab1d9e7391adfcd872cb12503bff88cd2e4f11953fae3790b1b5623669c33ea","abstract_canon_sha256":"d9e6ea22813a43543aa6e7057e5684f133c5d88af5167ab1d077902eaa221efa"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T03:43:52.104413Z","signature_b64":"TImN0OiCpC5WRLd2T3VXvn36TTw1/B60yopOJmISlDi/o3L9kumW04J2JGQjYu8B1QS5afAIzPb9bSMgNIbqCQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"2db395ef23ed7e1edf783806b6791b1310b72c3505a29c1a94b686ddcc3d96a7","last_reissued_at":"2026-05-18T03:43:52.103924Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T03:43:52.103924Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Testing general relativity with gravitational waves: a reality check","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Michele Vallisneri","submitted_at":"2012-07-19T19:00:14Z","abstract_excerpt":"The observations of gravitational-wave signals from astrophysical sources such as binary inspirals will be used to test General Relativity for self consistency and against alternative theories of gravity. I describe a simple formula that can be used to characterize the prospects of such tests, by estimating the matched-filtering signal-to-noise ratio required to detect non-General-Relativistic corrections of a given magnitude. The formula is valid for sufficiently strong signals; it requires the computation of a single number, the fitting factor between the General-Relativistic and corrected w"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1207.4759","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":"1207.4759","created_at":"2026-05-18T03:43:52.103994+00:00"},{"alias_kind":"arxiv_version","alias_value":"1207.4759v2","created_at":"2026-05-18T03:43:52.103994+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1207.4759","created_at":"2026-05-18T03:43:52.103994+00:00"},{"alias_kind":"pith_short_12","alias_value":"FWZZL3ZD5V7B","created_at":"2026-05-18T12:27:06.952714+00:00"},{"alias_kind":"pith_short_16","alias_value":"FWZZL3ZD5V7B5X3Y","created_at":"2026-05-18T12:27:06.952714+00:00"},{"alias_kind":"pith_short_8","alias_value":"FWZZL3ZD","created_at":"2026-05-18T12:27:06.952714+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2509.08099","citing_title":"Black Hole Spectroscopy and Tests of General Relativity with GW250114","ref_index":176,"is_internal_anchor":true},{"citing_arxiv_id":"2605.04579","citing_title":"The Impact of Spin Priors on Parameterized Tests of General Relativity","ref_index":27,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/FWZZL3ZD5V7B5X3YHADLM6I3CM","json":"https://pith.science/pith/FWZZL3ZD5V7B5X3YHADLM6I3CM.json","graph_json":"https://pith.science/api/pith-number/FWZZL3ZD5V7B5X3YHADLM6I3CM/graph.json","events_json":"https://pith.science/api/pith-number/FWZZL3ZD5V7B5X3YHADLM6I3CM/events.json","paper":"https://pith.science/paper/FWZZL3ZD"},"agent_actions":{"view_html":"https://pith.science/pith/FWZZL3ZD5V7B5X3YHADLM6I3CM","download_json":"https://pith.science/pith/FWZZL3ZD5V7B5X3YHADLM6I3CM.json","view_paper":"https://pith.science/paper/FWZZL3ZD","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1207.4759&json=true","fetch_graph":"https://pith.science/api/pith-number/FWZZL3ZD5V7B5X3YHADLM6I3CM/graph.json","fetch_events":"https://pith.science/api/pith-number/FWZZL3ZD5V7B5X3YHADLM6I3CM/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/FWZZL3ZD5V7B5X3YHADLM6I3CM/action/timestamp_anchor","attest_storage":"https://pith.science/pith/FWZZL3ZD5V7B5X3YHADLM6I3CM/action/storage_attestation","attest_author":"https://pith.science/pith/FWZZL3ZD5V7B5X3YHADLM6I3CM/action/author_attestation","sign_citation":"https://pith.science/pith/FWZZL3ZD5V7B5X3YHADLM6I3CM/action/citation_signature","submit_replication":"https://pith.science/pith/FWZZL3ZD5V7B5X3YHADLM6I3CM/action/replication_record"}},"created_at":"2026-05-18T03:43:52.103994+00:00","updated_at":"2026-05-18T03:43:52.103994+00:00"}