{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:1999:VGKKCGDPYSFNV2I63PX6Q34XZB","short_pith_number":"pith:VGKKCGDP","schema_version":"1.0","canonical_sha256":"a994a1186fc48adae91edbefe86f97c8433e38628298233795ab7b4638280d89","source":{"kind":"arxiv","id":"astro-ph/9908056","version":2},"attestation_state":"computed","paper":{"title":"The Correlation Function in Redshift Space: General Formula with Wide-angle Effects and Cosmological Distortions","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Takahiko Matsubara","submitted_at":"1999-08-06T04:33:27Z","abstract_excerpt":"A general formula for the correlation function in redshift space is derived in linear theory. The formula simultaneously includes wide-angle effects and cosmological distortions. The formula is applicable to any pair with arbitrary angle $\\theta$ between lines of sight, and arbitrary redshifts, $z_1$, $z_2$, which are not necessarily small. The effects of the spatial curvature both on geometry and on fluctuation spectrum are properly taken into account, and thus our formula holds in a Friedman-Lema\\^{\\i}tre universe with arbitrary cosmological parameters $\\Omega_0$ and $\\lambda_0$. We illustra"},"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/9908056","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"1999-08-06T04:33:27Z","cross_cats_sorted":[],"title_canon_sha256":"46d268dece0dd8c2c9c002a27b03942569f3288c97e6355e3b1151625d7fc58e","abstract_canon_sha256":"fdd98746fa82c75ca1884706cd69ea9ab340bc4b2984b03f8a11121e89b9c391"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:11:30.028829Z","signature_b64":"AmgbY4lcC2bxypEx33uyXH0D7E7xJzY+8/9F3OQx6MKWp9nvYMGsKCDUC436dtaBjducUn9GwmTa9LYH1VmIAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"a994a1186fc48adae91edbefe86f97c8433e38628298233795ab7b4638280d89","last_reissued_at":"2026-07-04T16:11:30.028454Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:11:30.028454Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Correlation Function in Redshift Space: General Formula with Wide-angle Effects and Cosmological Distortions","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Takahiko Matsubara","submitted_at":"1999-08-06T04:33:27Z","abstract_excerpt":"A general formula for the correlation function in redshift space is derived in linear theory. The formula simultaneously includes wide-angle effects and cosmological distortions. The formula is applicable to any pair with arbitrary angle $\\theta$ between lines of sight, and arbitrary redshifts, $z_1$, $z_2$, which are not necessarily small. The effects of the spatial curvature both on geometry and on fluctuation spectrum are properly taken into account, and thus our formula holds in a Friedman-Lema\\^{\\i}tre universe with arbitrary cosmological parameters $\\Omega_0$ and $\\lambda_0$. We illustra"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/9908056","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/astro-ph/9908056/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":"astro-ph/9908056","created_at":"2026-07-04T16:11:30.028504+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/9908056v2","created_at":"2026-07-04T16:11:30.028504+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/9908056","created_at":"2026-07-04T16:11:30.028504+00:00"},{"alias_kind":"pith_short_12","alias_value":"VGKKCGDPYSFN","created_at":"2026-07-04T16:11:30.028504+00:00"},{"alias_kind":"pith_short_16","alias_value":"VGKKCGDPYSFNV2I6","created_at":"2026-07-04T16:11:30.028504+00:00"},{"alias_kind":"pith_short_8","alias_value":"VGKKCGDP","created_at":"2026-07-04T16:11:30.028504+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2605.29806","citing_title":"The observer power spectrum for lightcone statistics, integrated relativistic observables and wide angle effects","ref_index":16,"is_internal_anchor":true},{"citing_arxiv_id":"2606.27927","citing_title":"Large-scale structures of the Universe: physics, phenomenology, statistics","ref_index":74,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/VGKKCGDPYSFNV2I63PX6Q34XZB","json":"https://pith.science/pith/VGKKCGDPYSFNV2I63PX6Q34XZB.json","graph_json":"https://pith.science/api/pith-number/VGKKCGDPYSFNV2I63PX6Q34XZB/graph.json","events_json":"https://pith.science/api/pith-number/VGKKCGDPYSFNV2I63PX6Q34XZB/events.json","paper":"https://pith.science/paper/VGKKCGDP"},"agent_actions":{"view_html":"https://pith.science/pith/VGKKCGDPYSFNV2I63PX6Q34XZB","download_json":"https://pith.science/pith/VGKKCGDPYSFNV2I63PX6Q34XZB.json","view_paper":"https://pith.science/paper/VGKKCGDP","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/9908056&json=true","fetch_graph":"https://pith.science/api/pith-number/VGKKCGDPYSFNV2I63PX6Q34XZB/graph.json","fetch_events":"https://pith.science/api/pith-number/VGKKCGDPYSFNV2I63PX6Q34XZB/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/VGKKCGDPYSFNV2I63PX6Q34XZB/action/timestamp_anchor","attest_storage":"https://pith.science/pith/VGKKCGDPYSFNV2I63PX6Q34XZB/action/storage_attestation","attest_author":"https://pith.science/pith/VGKKCGDPYSFNV2I63PX6Q34XZB/action/author_attestation","sign_citation":"https://pith.science/pith/VGKKCGDPYSFNV2I63PX6Q34XZB/action/citation_signature","submit_replication":"https://pith.science/pith/VGKKCGDPYSFNV2I63PX6Q34XZB/action/replication_record"}},"created_at":"2026-07-04T16:11:30.028504+00:00","updated_at":"2026-07-04T16:11:30.028504+00:00"}