{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2002:3J76YNUSXL4NSRUJWC725ER5IX","short_pith_number":"pith:3J76YNUS","schema_version":"1.0","canonical_sha256":"da7fec3692baf8d94689b0bfae923d45eae0e3e9f968d0e04c37112439eb1176","source":{"kind":"arxiv","id":"astro-ph/0201547","version":1},"attestation_state":"computed","paper":{"title":"Statistics: Handle with Care, Detecting Multiple Model Components with the Likelihood Ratio Test","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Alanna Connors (Eureka Scientific), Aneta Siemiginowska (Harvard-Smithsonian Center for Astrophysics), David A. van Dyk (Harvard University, Department of Statistics), Rostislav Protassov (Harvard University, Vinay L. Kashyap (Harvard-Smithsonian Center for Astrophysics)","submitted_at":"2002-01-31T20:32:23Z","abstract_excerpt":"The likelihood ratio test (LRT) and the related $F$ test, do not (even asymptotically) adhere to their nominal $\\chi^2$ and $F$ distributions in many statistical tests common in astrophysics, thereby casting many marginal line or source detections and non-detections into doubt. Although there are many legitimate uses of these statistics, in some important cases it can be impossible to compute the correct false positive rate. For example, it has become common practice to use the LRT or the $F$ test for detecting a line in a spectral model or a source above background despite the lack of certain"},"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":"astro-ph/0201547","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2002-01-31T20:32:23Z","cross_cats_sorted":[],"title_canon_sha256":"a4e356fa9576af17d142a5f8757a03e058813543c474474ce844ae11ee7372cb","abstract_canon_sha256":"905973746f0b7b17882499e66414adcf6f7c4cda0def732c8d2a48d8202b555b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:20:22.805918Z","signature_b64":"uLXnkxPxJAETm+nqZ7NUuDFjXHaimcJczrOb0wU7+hPx36mnjntq1qYwkskA7wPsYI41AEdFlrNMI0Jmmwj2CQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"da7fec3692baf8d94689b0bfae923d45eae0e3e9f968d0e04c37112439eb1176","last_reissued_at":"2026-05-18T01:20:22.805230Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:20:22.805230Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Statistics: Handle with Care, Detecting Multiple Model Components with the Likelihood Ratio Test","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Alanna Connors (Eureka Scientific), Aneta Siemiginowska (Harvard-Smithsonian Center for Astrophysics), David A. van Dyk (Harvard University, Department of Statistics), Rostislav Protassov (Harvard University, Vinay L. Kashyap (Harvard-Smithsonian Center for Astrophysics)","submitted_at":"2002-01-31T20:32:23Z","abstract_excerpt":"The likelihood ratio test (LRT) and the related $F$ test, do not (even asymptotically) adhere to their nominal $\\chi^2$ and $F$ distributions in many statistical tests common in astrophysics, thereby casting many marginal line or source detections and non-detections into doubt. Although there are many legitimate uses of these statistics, in some important cases it can be impossible to compute the correct false positive rate. For example, it has become common practice to use the LRT or the $F$ test for detecting a line in a spectral model or a source above background despite the lack of certain"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0201547","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":""},"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":"astro-ph/0201547","created_at":"2026-05-18T01:20:22.805354+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0201547v1","created_at":"2026-05-18T01:20:22.805354+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0201547","created_at":"2026-05-18T01:20:22.805354+00:00"},{"alias_kind":"pith_short_12","alias_value":"3J76YNUSXL4N","created_at":"2026-05-18T12:25:50.845339+00:00"},{"alias_kind":"pith_short_16","alias_value":"3J76YNUSXL4NSRUJ","created_at":"2026-05-18T12:25:50.845339+00:00"},{"alias_kind":"pith_short_8","alias_value":"3J76YNUS","created_at":"2026-05-18T12:25:50.845339+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.18427","citing_title":"Iron line diagnostics of the stellar wind in X1908+075","ref_index":80,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/3J76YNUSXL4NSRUJWC725ER5IX","json":"https://pith.science/pith/3J76YNUSXL4NSRUJWC725ER5IX.json","graph_json":"https://pith.science/api/pith-number/3J76YNUSXL4NSRUJWC725ER5IX/graph.json","events_json":"https://pith.science/api/pith-number/3J76YNUSXL4NSRUJWC725ER5IX/events.json","paper":"https://pith.science/paper/3J76YNUS"},"agent_actions":{"view_html":"https://pith.science/pith/3J76YNUSXL4NSRUJWC725ER5IX","download_json":"https://pith.science/pith/3J76YNUSXL4NSRUJWC725ER5IX.json","view_paper":"https://pith.science/paper/3J76YNUS","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0201547&json=true","fetch_graph":"https://pith.science/api/pith-number/3J76YNUSXL4NSRUJWC725ER5IX/graph.json","fetch_events":"https://pith.science/api/pith-number/3J76YNUSXL4NSRUJWC725ER5IX/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/3J76YNUSXL4NSRUJWC725ER5IX/action/timestamp_anchor","attest_storage":"https://pith.science/pith/3J76YNUSXL4NSRUJWC725ER5IX/action/storage_attestation","attest_author":"https://pith.science/pith/3J76YNUSXL4NSRUJWC725ER5IX/action/author_attestation","sign_citation":"https://pith.science/pith/3J76YNUSXL4NSRUJWC725ER5IX/action/citation_signature","submit_replication":"https://pith.science/pith/3J76YNUSXL4NSRUJWC725ER5IX/action/replication_record"}},"created_at":"2026-05-18T01:20:22.805354+00:00","updated_at":"2026-05-18T01:20:22.805354+00:00"}