{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:1999:6VIVTDYXIKSEC3N4J72TG6EKWI","short_pith_number":"pith:6VIVTDYX","schema_version":"1.0","canonical_sha256":"f551598f1742a4416dbc4ff533788ab23a62c3797adcb13ec103d87491f2a48b","source":{"kind":"arxiv","id":"astro-ph/9904356","version":1},"attestation_state":"computed","paper":{"title":"Constraining the equation of state of the Universe from Distant Type Ia Supernovae and Cosmic Microwave Background Anisotropies","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"G. Efstathiou","submitted_at":"1999-04-26T13:38:53Z","abstract_excerpt":"We analyse the constraints that can be placed on a cosmological constant or quintessence-like component by combining observations of Type Ia supernovae with measurements of anisotropies in the cosmic microwave background. We use the recent supernovae sample of Perlmutter et al and observations of the CMB anisotropies to constraint the equation of state (w_Q = p/rho) in quintessence-like models via a likelihood analysis. The 2 sigma upper limits are w_Q < -0.6 if the Universe is assumed to be spatially flat, and w_Q < -0.4 for universes of arbitrary spatial curvature. The upper limit derived fo"},"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/9904356","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"1999-04-26T13:38:53Z","cross_cats_sorted":[],"title_canon_sha256":"c3f2e9cb35867908ab7712d775893a476399d1a21706f2b48509b302727d9491","abstract_canon_sha256":"dbd4462a56b0a40925df332c3f729e282f0c605024cb62af9317d7a3384155fb"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:10:55.631646Z","signature_b64":"VehevUV3NtaPAxGa5SWCS4twn5MLtj/X+KbqTPG/NIl8/pqESI6XxxYxc5nXuymciUDA6grrZXYlbspHC2WoBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"f551598f1742a4416dbc4ff533788ab23a62c3797adcb13ec103d87491f2a48b","last_reissued_at":"2026-07-04T16:10:55.631257Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:10:55.631257Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Constraining the equation of state of the Universe from Distant Type Ia Supernovae and Cosmic Microwave Background Anisotropies","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"G. Efstathiou","submitted_at":"1999-04-26T13:38:53Z","abstract_excerpt":"We analyse the constraints that can be placed on a cosmological constant or quintessence-like component by combining observations of Type Ia supernovae with measurements of anisotropies in the cosmic microwave background. We use the recent supernovae sample of Perlmutter et al and observations of the CMB anisotropies to constraint the equation of state (w_Q = p/rho) in quintessence-like models via a likelihood analysis. The 2 sigma upper limits are w_Q < -0.6 if the Universe is assumed to be spatially flat, and w_Q < -0.4 for universes of arbitrary spatial curvature. The upper limit derived fo"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/9904356","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/astro-ph/9904356/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/9904356","created_at":"2026-07-04T16:10:55.631323+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/9904356v1","created_at":"2026-07-04T16:10:55.631323+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/9904356","created_at":"2026-07-04T16:10:55.631323+00:00"},{"alias_kind":"pith_short_12","alias_value":"6VIVTDYXIKSE","created_at":"2026-07-04T16:10:55.631323+00:00"},{"alias_kind":"pith_short_16","alias_value":"6VIVTDYXIKSEC3N4","created_at":"2026-07-04T16:10:55.631323+00:00"},{"alias_kind":"pith_short_8","alias_value":"6VIVTDYX","created_at":"2026-07-04T16:10:55.631323+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":5,"sample":[{"citing_arxiv_id":"2606.17951","citing_title":"Data-Driven Discovery of a Simple Phantom-Crossing Dark Energy Parametrization","ref_index":53,"is_internal_anchor":true},{"citing_arxiv_id":"2606.05539","citing_title":"Dissipative Cosmology and the Nature of Dark Energy: Insights from Bulk Viscosity with DESI DR2 observations","ref_index":91,"is_internal_anchor":true},{"citing_arxiv_id":"2602.11936","citing_title":"Probing dynamical dark energy with late-time data: Evidence, tensions, and the limits of the $w_0w_a$CDM framework","ref_index":210,"is_internal_anchor":true},{"citing_arxiv_id":"2511.18657","citing_title":"How Complex is Dark Energy? A Bayesian Analysis of CPL Extensions with Recent DESI BAO Measurements","ref_index":43,"is_internal_anchor":true},{"citing_arxiv_id":"2103.01183","citing_title":"In the Realm of the Hubble tension $-$ a Review of Solutions","ref_index":162,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/6VIVTDYXIKSEC3N4J72TG6EKWI","json":"https://pith.science/pith/6VIVTDYXIKSEC3N4J72TG6EKWI.json","graph_json":"https://pith.science/api/pith-number/6VIVTDYXIKSEC3N4J72TG6EKWI/graph.json","events_json":"https://pith.science/api/pith-number/6VIVTDYXIKSEC3N4J72TG6EKWI/events.json","paper":"https://pith.science/paper/6VIVTDYX"},"agent_actions":{"view_html":"https://pith.science/pith/6VIVTDYXIKSEC3N4J72TG6EKWI","download_json":"https://pith.science/pith/6VIVTDYXIKSEC3N4J72TG6EKWI.json","view_paper":"https://pith.science/paper/6VIVTDYX","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/9904356&json=true","fetch_graph":"https://pith.science/api/pith-number/6VIVTDYXIKSEC3N4J72TG6EKWI/graph.json","fetch_events":"https://pith.science/api/pith-number/6VIVTDYXIKSEC3N4J72TG6EKWI/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/6VIVTDYXIKSEC3N4J72TG6EKWI/action/timestamp_anchor","attest_storage":"https://pith.science/pith/6VIVTDYXIKSEC3N4J72TG6EKWI/action/storage_attestation","attest_author":"https://pith.science/pith/6VIVTDYXIKSEC3N4J72TG6EKWI/action/author_attestation","sign_citation":"https://pith.science/pith/6VIVTDYXIKSEC3N4J72TG6EKWI/action/citation_signature","submit_replication":"https://pith.science/pith/6VIVTDYXIKSEC3N4J72TG6EKWI/action/replication_record"}},"created_at":"2026-07-04T16:10:55.631323+00:00","updated_at":"2026-07-04T16:10:55.631323+00:00"}