{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2003:V6WEZ4DACIY42OG2ZDUQH4MS2S","short_pith_number":"pith:V6WEZ4DA","schema_version":"1.0","canonical_sha256":"afac4cf0601231cd38dac8e903f192d4a39d8aaa207a01b04c206c5abf30e6ec","source":{"kind":"arxiv","id":"astro-ph/0302209","version":3},"attestation_state":"computed","paper":{"title":"First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Determination of Cosmological Parameters","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"(3) NASA's GSFC, (4) UBC, (5) U. Chicaco, (6) Brown, (7) SSAI, (8) UCLA), A. Kogut (2), C. L. Bennett (2), D. N. Spergel (1), E. Komatsu (1), E. L. Wright (8) ((1) Princeton, E. Wollack (2), G. Hinshaw (2), G. S. Tucker (2), H. V. Peiris (1), J. L. Weiland (7), L. Page (1), L. Verde (1), M. Halpern (4), M. Limon (2), M. R. Nolta (1), N. Jarosik (1), S. S. Meyer (5)","submitted_at":"2003-02-11T20:59:59Z","abstract_excerpt":"WMAP precision data enables accurate testing of cosmological models. We find that the emerging standard model of cosmology, a flat Lambda-dominated universe seeded by nearly scale-invariant adiabatic Gaussian fluctuations, fits the WMAP data. With parameters fixed only by WMAP data, we can fit finer scale CMB measurements and measurements of large scle structure (galaxy surveys and the Lyman alpha forest). This simple model is also consistent with a host of other astronomical measurements. We then fit the model parameters to a combination of WMAP data with other finer scale CMB experiments (AC"},"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/0302209","kind":"arxiv","version":3},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2003-02-11T20:59:59Z","cross_cats_sorted":[],"title_canon_sha256":"b2eb2f1756f5be0a3757e4d0e5157aafb5f52773bcda1d171a3a5439ec5e2289","abstract_canon_sha256":"bbbbdac4bd2f4d0e6009be6e83c1b462ac67d745414b60c8093b44c077275838"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:42:18.822770Z","signature_b64":"cqW2SFujYI01MUnNyeXh8udX9Oqj7UvUA33zZUQecNlAmWNvGFyCzu+5QeL9NVNvsX4VCtE74TwrOmR1nx3LCQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"afac4cf0601231cd38dac8e903f192d4a39d8aaa207a01b04c206c5abf30e6ec","last_reissued_at":"2026-07-04T15:42:18.822370Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:42:18.822370Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Determination of Cosmological Parameters","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"(3) NASA's GSFC, (4) UBC, (5) U. Chicaco, (6) Brown, (7) SSAI, (8) UCLA), A. Kogut (2), C. L. Bennett (2), D. N. Spergel (1), E. Komatsu (1), E. L. Wright (8) ((1) Princeton, E. Wollack (2), G. Hinshaw (2), G. S. Tucker (2), H. V. Peiris (1), J. L. Weiland (7), L. Page (1), L. Verde (1), M. Halpern (4), M. Limon (2), M. R. Nolta (1), N. Jarosik (1), S. S. Meyer (5)","submitted_at":"2003-02-11T20:59:59Z","abstract_excerpt":"WMAP precision data enables accurate testing of cosmological models. We find that the emerging standard model of cosmology, a flat Lambda-dominated universe seeded by nearly scale-invariant adiabatic Gaussian fluctuations, fits the WMAP data. With parameters fixed only by WMAP data, we can fit finer scale CMB measurements and measurements of large scle structure (galaxy surveys and the Lyman alpha forest). This simple model is also consistent with a host of other astronomical measurements. We then fit the model parameters to a combination of WMAP data with other finer scale CMB experiments (AC"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0302209","kind":"arxiv","version":3},"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/0302209/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/0302209","created_at":"2026-07-04T15:42:18.822425+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0302209v3","created_at":"2026-07-04T15:42:18.822425+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0302209","created_at":"2026-07-04T15:42:18.822425+00:00"},{"alias_kind":"pith_short_12","alias_value":"V6WEZ4DACIY4","created_at":"2026-07-04T15:42:18.822425+00:00"},{"alias_kind":"pith_short_16","alias_value":"V6WEZ4DACIY42OG2","created_at":"2026-07-04T15:42:18.822425+00:00"},{"alias_kind":"pith_short_8","alias_value":"V6WEZ4DA","created_at":"2026-07-04T15:42:18.822425+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":19,"internal_anchor_count":18,"sample":[{"citing_arxiv_id":"2606.18987","citing_title":"From Evidence to Evident: Decisive Cosmological Evidence for the Normal Neutrino Mass Hierarchy","ref_index":34,"is_internal_anchor":true},{"citing_arxiv_id":"2606.19110","citing_title":"Kiselev black hole and the ultra-slow evaporating behavior","ref_index":3,"is_internal_anchor":true},{"citing_arxiv_id":"2606.18491","citing_title":"The Coherence Principle: A Falsifiable Prior for Model Selection from the Grammar of Theories","ref_index":71,"is_internal_anchor":true},{"citing_arxiv_id":"2607.00610","citing_title":"Correcting the hydrostatic mass for non-thermal gas motions: a comparison of two approaches","ref_index":297,"is_internal_anchor":true},{"citing_arxiv_id":"2607.00764","citing_title":"The age of the Universe from a large sample of the oldest Galactic stars","ref_index":178,"is_internal_anchor":true},{"citing_arxiv_id":"2606.31978","citing_title":"COSMOS-Web: does halo mass alone shape the clustering of star-forming and quiescent galaxies?","ref_index":287,"is_internal_anchor":true},{"citing_arxiv_id":"2606.02712","citing_title":"Constraints on the gravitational potential from DESI DR2 BAO and its implications for the local void scenario","ref_index":178,"is_internal_anchor":true},{"citing_arxiv_id":"2606.21826","citing_title":"Dark Energy in the DESI Era: A Brief Review of Evidence, Beyond-$\\Lambda$CDM Interpretations, and Tensions","ref_index":3,"is_internal_anchor":true},{"citing_arxiv_id":"2606.23651","citing_title":"Revisiting the 'Lensing is Low' Problem with UNIONS","ref_index":55,"is_internal_anchor":true},{"citing_arxiv_id":"1907.04473","citing_title":"CMB-S4 Science Case, Reference Design, and Project Plan","ref_index":34,"is_internal_anchor":true},{"citing_arxiv_id":"2402.01270","citing_title":"Dynamical system analysis in descending dark energy model","ref_index":4,"is_internal_anchor":true},{"citing_arxiv_id":"2503.16355","citing_title":"DEMNUni: the Sunyaev-Zel'dovich effect in the presence of massive neutrinos and dynamical dark energy","ref_index":1,"is_internal_anchor":true},{"citing_arxiv_id":"2605.18939","citing_title":"The Lumina Project: CMB Optical Depth Fluctuations from Patchy Reionization","ref_index":85,"is_internal_anchor":true},{"citing_arxiv_id":"2505.24732","citing_title":"The Quintom theory of dark energy after DESI DR2","ref_index":67,"is_internal_anchor":true},{"citing_arxiv_id":"2507.05207","citing_title":"Interacting Scalar Fields as Dark Energy and Dark Matter in Einstein scalar Gauss Bonnet Gravity","ref_index":4,"is_internal_anchor":true},{"citing_arxiv_id":"2509.09202","citing_title":"Interacting $k$-essence field with non-pressureless Dark Matter: Cosmological Dynamics and Observational Constraints","ref_index":4,"is_internal_anchor":true},{"citing_arxiv_id":"2605.15078","citing_title":"KiDS+VIKING-450 cosmology with Bayesian hierarchical model redshift distributions","ref_index":168,"is_internal_anchor":true},{"citing_arxiv_id":"2604.02433","citing_title":"Cosmology-Independent Constraints on the Etherington Relation and SNeIa Absolute Magnitude Evolution from DESI-DR2","ref_index":11,"is_internal_anchor":true},{"citing_arxiv_id":"2604.23793","citing_title":"From Big Bang Nucleosynthesis to Late-Time Acceleration in $f(Q,L_m)$ Gravity","ref_index":4,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/V6WEZ4DACIY42OG2ZDUQH4MS2S","json":"https://pith.science/pith/V6WEZ4DACIY42OG2ZDUQH4MS2S.json","graph_json":"https://pith.science/api/pith-number/V6WEZ4DACIY42OG2ZDUQH4MS2S/graph.json","events_json":"https://pith.science/api/pith-number/V6WEZ4DACIY42OG2ZDUQH4MS2S/events.json","paper":"https://pith.science/paper/V6WEZ4DA"},"agent_actions":{"view_html":"https://pith.science/pith/V6WEZ4DACIY42OG2ZDUQH4MS2S","download_json":"https://pith.science/pith/V6WEZ4DACIY42OG2ZDUQH4MS2S.json","view_paper":"https://pith.science/paper/V6WEZ4DA","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0302209&json=true","fetch_graph":"https://pith.science/api/pith-number/V6WEZ4DACIY42OG2ZDUQH4MS2S/graph.json","fetch_events":"https://pith.science/api/pith-number/V6WEZ4DACIY42OG2ZDUQH4MS2S/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/V6WEZ4DACIY42OG2ZDUQH4MS2S/action/timestamp_anchor","attest_storage":"https://pith.science/pith/V6WEZ4DACIY42OG2ZDUQH4MS2S/action/storage_attestation","attest_author":"https://pith.science/pith/V6WEZ4DACIY42OG2ZDUQH4MS2S/action/author_attestation","sign_citation":"https://pith.science/pith/V6WEZ4DACIY42OG2ZDUQH4MS2S/action/citation_signature","submit_replication":"https://pith.science/pith/V6WEZ4DACIY42OG2ZDUQH4MS2S/action/replication_record"}},"created_at":"2026-07-04T15:42:18.822425+00:00","updated_at":"2026-07-04T15:42:18.822425+00:00"}