{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2011:4AYFHCMLMCNAILAWJKY7UJRW4S","short_pith_number":"pith:4AYFHCML","schema_version":"1.0","canonical_sha256":"e03053898b609a042c164ab1fa2636e4ac18754b830870dc741db5c9038368f6","source":{"kind":"arxiv","id":"1107.5366","version":1},"attestation_state":"computed","paper":{"title":"Pulsar timing analysis in the presence of correlated noise","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.IM","authors_text":"D. J. Champion, G. Hobbs, J. P. W. Verbiest, R. N. Manchester, W. Coles","submitted_at":"2011-07-27T01:39:47Z","abstract_excerpt":"Pulsar timing observations are usually analysed with least-square-fitting procedures under the assumption that the timing residuals are uncorrelated (statistically \"white\"). Pulsar observers are well aware that this assumption often breaks down and causes severe errors in estimating the parameters of the timing model and their uncertainties. Ad hoc methods for minimizing these errors have been developed, but we show that they are far from optimal. Compensation for temporal correlation can be done optimally if the covariance matrix of the residuals is known using a linear transformation that wh"},"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":"1107.5366","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.IM","submitted_at":"2011-07-27T01:39:47Z","cross_cats_sorted":[],"title_canon_sha256":"9d66f1adb1f038afc147d7d6ef42dfefb855563ad5487c3da481888c6c40cf95","abstract_canon_sha256":"ec6e6760efae0b6cc908cdbb47aac2b03c86d72740c40bc014a4269261543b93"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:01:09.286824Z","signature_b64":"F1mOu/UuFIuOom5rcwVdPUA3mEwV1T47zuG75trJ1bwlC/3qK8LpQ54Yw6+GiU7AB3YfK1vpbS06sAf4ZpCnCQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"e03053898b609a042c164ab1fa2636e4ac18754b830870dc741db5c9038368f6","last_reissued_at":"2026-05-18T02:01:09.286266Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:01:09.286266Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Pulsar timing analysis in the presence of correlated noise","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.IM","authors_text":"D. J. Champion, G. Hobbs, J. P. W. Verbiest, R. N. Manchester, W. Coles","submitted_at":"2011-07-27T01:39:47Z","abstract_excerpt":"Pulsar timing observations are usually analysed with least-square-fitting procedures under the assumption that the timing residuals are uncorrelated (statistically \"white\"). Pulsar observers are well aware that this assumption often breaks down and causes severe errors in estimating the parameters of the timing model and their uncertainties. Ad hoc methods for minimizing these errors have been developed, but we show that they are far from optimal. Compensation for temporal correlation can be done optimally if the covariance matrix of the residuals is known using a linear transformation that wh"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1107.5366","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":"1107.5366","created_at":"2026-05-18T02:01:09.286363+00:00"},{"alias_kind":"arxiv_version","alias_value":"1107.5366v1","created_at":"2026-05-18T02:01:09.286363+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1107.5366","created_at":"2026-05-18T02:01:09.286363+00:00"},{"alias_kind":"pith_short_12","alias_value":"4AYFHCMLMCNA","created_at":"2026-05-18T12:26:20.644004+00:00"},{"alias_kind":"pith_short_16","alias_value":"4AYFHCMLMCNAILAW","created_at":"2026-05-18T12:26:20.644004+00:00"},{"alias_kind":"pith_short_8","alias_value":"4AYFHCML","created_at":"2026-05-18T12:26:20.644004+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2510.04537","citing_title":"Finding Supermassive Black Hole Binary Mergers in Pulsar Timing Array Data","ref_index":57,"is_internal_anchor":true},{"citing_arxiv_id":"2604.08506","citing_title":"The Heavy Tailed Non-Gaussianity of the Supermassive Black Hole Gravitational Wave Background","ref_index":44,"is_internal_anchor":false},{"citing_arxiv_id":"2604.08373","citing_title":"Stochastic problems in pulsar timing","ref_index":48,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/4AYFHCMLMCNAILAWJKY7UJRW4S","json":"https://pith.science/pith/4AYFHCMLMCNAILAWJKY7UJRW4S.json","graph_json":"https://pith.science/api/pith-number/4AYFHCMLMCNAILAWJKY7UJRW4S/graph.json","events_json":"https://pith.science/api/pith-number/4AYFHCMLMCNAILAWJKY7UJRW4S/events.json","paper":"https://pith.science/paper/4AYFHCML"},"agent_actions":{"view_html":"https://pith.science/pith/4AYFHCMLMCNAILAWJKY7UJRW4S","download_json":"https://pith.science/pith/4AYFHCMLMCNAILAWJKY7UJRW4S.json","view_paper":"https://pith.science/paper/4AYFHCML","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1107.5366&json=true","fetch_graph":"https://pith.science/api/pith-number/4AYFHCMLMCNAILAWJKY7UJRW4S/graph.json","fetch_events":"https://pith.science/api/pith-number/4AYFHCMLMCNAILAWJKY7UJRW4S/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/4AYFHCMLMCNAILAWJKY7UJRW4S/action/timestamp_anchor","attest_storage":"https://pith.science/pith/4AYFHCMLMCNAILAWJKY7UJRW4S/action/storage_attestation","attest_author":"https://pith.science/pith/4AYFHCMLMCNAILAWJKY7UJRW4S/action/author_attestation","sign_citation":"https://pith.science/pith/4AYFHCMLMCNAILAWJKY7UJRW4S/action/citation_signature","submit_replication":"https://pith.science/pith/4AYFHCMLMCNAILAWJKY7UJRW4S/action/replication_record"}},"created_at":"2026-05-18T02:01:09.286363+00:00","updated_at":"2026-05-18T02:01:09.286363+00:00"}