{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:1998:K6LHR5T6FX7I65TSFGVN3YWPQF","short_pith_number":"pith:K6LHR5T6","schema_version":"1.0","canonical_sha256":"579678f67e2dfe8f767229aadde2cf8163ba9383fdf6a6d01b30eafd473bafa1","source":{"kind":"arxiv","id":"astro-ph/9805201","version":1},"attestation_state":"computed","paper":{"title":"Observational Evidence from Supernovae for an Accelerating Universe and a Cosmological Constant","license":"","headline":"Distant Type Ia supernovae appear 10 to 15 percent farther than expected in a low-density universe without a cosmological constant.","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Adam G. Riess, Alan Diercks, Alejandro Clocchiattia, Alexei V. Filippenko, B. Leibundgut, Brian P. Schmidt, Christopher Stubbs, Craig J. Hogan, David Reiss, John Tonry, J. Spyromilio, M. M. Phillips, Nicholas B. Suntzeff, Peter Challis, Peter M. Garnavich, R. Chris Smith, Robert A. Schommer, Robert P. Kirshner, Ron L. Gilliland, Saurabh Jha","submitted_at":"1998-05-15T03:59:02Z","abstract_excerpt":"We present observations of 10 type Ia supernovae (SNe Ia) between 0.16 < z < 0.62. With previous data from our High-Z Supernova Search Team, this expanded set of 16 high-redshift supernovae and 34 nearby supernovae are used to place constraints on the Hubble constant (H_0), the mass density (Omega_M), the cosmological constant (Omega_Lambda), the deceleration parameter (q_0), and the dynamical age of the Universe (t_0). The distances of the high-redshift SNe Ia are, on average, 10% to 15% farther than expected in a low mass density (Omega_M=0.2) Universe without a cosmological constant. Differ"},"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":true,"formal_links_present":true},"canonical_record":{"source":{"id":"astro-ph/9805201","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"1998-05-15T03:59:02Z","cross_cats_sorted":[],"title_canon_sha256":"183a9a78dea911a90374b4eaa5918a0dc607792bc4615646708f77871a059ec9","abstract_canon_sha256":"9595602fc671b02f520e40a6a5eb2aa48c3d468c9714ab2e1a61d893e5d41b48"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:27:10.137429Z","signature_b64":"Y3CmzYd5hCUpnFSGx/OQp4k700P61o8Ra7GoE5xpDwAzcyYn5nwnupKUjqft8QWVJtGEf7nzgLy0xwXLDeysAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"579678f67e2dfe8f767229aadde2cf8163ba9383fdf6a6d01b30eafd473bafa1","last_reissued_at":"2026-07-04T15:27:10.136996Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:27:10.136996Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Observational Evidence from Supernovae for an Accelerating Universe and a Cosmological Constant","license":"","headline":"Distant Type Ia supernovae appear 10 to 15 percent farther than expected in a low-density universe without a cosmological constant.","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Adam G. Riess, Alan Diercks, Alejandro Clocchiattia, Alexei V. Filippenko, B. Leibundgut, Brian P. Schmidt, Christopher Stubbs, Craig J. Hogan, David Reiss, John Tonry, J. Spyromilio, M. M. Phillips, Nicholas B. Suntzeff, Peter Challis, Peter M. Garnavich, R. Chris Smith, Robert A. Schommer, Robert P. Kirshner, Ron L. Gilliland, Saurabh Jha","submitted_at":"1998-05-15T03:59:02Z","abstract_excerpt":"We present observations of 10 type Ia supernovae (SNe Ia) between 0.16 < z < 0.62. With previous data from our High-Z Supernova Search Team, this expanded set of 16 high-redshift supernovae and 34 nearby supernovae are used to place constraints on the Hubble constant (H_0), the mass density (Omega_M), the cosmological constant (Omega_Lambda), the deceleration parameter (q_0), and the dynamical age of the Universe (t_0). The distances of the high-redshift SNe Ia are, on average, 10% to 15% farther than expected in a low mass density (Omega_M=0.2) Universe without a cosmological constant. Differ"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"With no prior constraint on mass density other than Omega_M > 0, the spectroscopically confirmed SNe Ia are consistent with q_0 <0 at the 2.8 sigma and 3.9 sigma confidence levels, and with Omega_Lambda >0 at the 3.0 sigma and 4.0 sigma confidence levels, for two fitting methods respectively. For a flat-Universe prior the data require Omega_Lambda >0 at 7 sigma and 9 sigma.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"That Type Ia supernovae at z ~ 0.5 have the same peak luminosity and light-curve shape distribution as nearby ones, with no redshift-dependent evolution or selection effects large enough to produce the observed 10-15% distance excess.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"High-redshift Type Ia supernovae data indicate the universe is accelerating its expansion, requiring Omega_Lambda > 0 and q_0 < 0.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"Distant Type Ia supernovae appear 10 to 15 percent farther than expected in a low-density universe without a cosmological constant.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"1524b44e1e6edcf2614683c96d74c98d424b7a26332def9d0dfa4620fdbc5b4f"},"source":{"id":"astro-ph/9805201","kind":"arxiv","version":1},"verdict":{"id":"4c9a0206-1271-450d-8fd6-3d6f5834f1a7","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-10T21:15:27.199356Z","strongest_claim":"With no prior constraint on mass density other than Omega_M > 0, the spectroscopically confirmed SNe Ia are consistent with q_0 <0 at the 2.8 sigma and 3.9 sigma confidence levels, and with Omega_Lambda >0 at the 3.0 sigma and 4.0 sigma confidence levels, for two fitting methods respectively. For a flat-Universe prior the data require Omega_Lambda >0 at 7 sigma and 9 sigma.","one_line_summary":"High-redshift Type Ia supernovae data indicate the universe is accelerating its expansion, requiring Omega_Lambda > 0 and q_0 < 0.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"That Type Ia supernovae at z ~ 0.5 have the same peak luminosity and light-curve shape distribution as nearby ones, with no redshift-dependent evolution or selection effects large enough to produce the observed 10-15% distance excess.","pith_extraction_headline":"Distant Type Ia supernovae appear 10 to 15 percent farther than expected in a low-density universe without a cosmological constant."},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/astro-ph/9805201/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"references":{"count":4,"sample":[{"doi":"","year":1969,"title":"A New Method for Determining Cumulative Gravitational Lensing Effects in Inhomogeneous Universes","work_id":"6dd1662a-7374-4905-af31-a4eea278b9c6","ref_index":1,"cited_arxiv_id":"astro-ph/9708036","is_internal_anchor":false},{"doi":"","year":1998,"title":"Zehavi, I., Riess, A. G., Kirshner, R. P., & Dekel, A. 1998, Ap J, in press – 35 – Figure 1: Identification spectra (in f λ) of high-redshift SNe Ia. The spectra obtained for the 10 new SNe of the high","work_id":"4bd3aaf4-d86d-41e9-a93f-b646fe43fdc8","ref_index":2,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":1995,"title":"The open symbol is SN 1997ck (z = 0.97) which lacks spectroscopic classification and a color mea surement. The average difference between the data and the Ω M = 0.20, Ω Λ = 0 prediction is 0.25 mag. Fig","work_id":"e1b543a9-b899-432d-98f0-9be368a5889f","ref_index":3,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":null,"title":"G., et al., 1998, @doi [AJ] 10.1086/300499 , http://adsabs.harvard.edu/abs/1998AJ....116.1009R 116","work_id":"f4711f38-d7d5-454b-a88b-02642c09bbd4","ref_index":4,"cited_arxiv_id":"astro-ph/9805201","is_internal_anchor":true}],"resolved_work":4,"snapshot_sha256":"e4985563fc8efe1966d2d5815a3a51827105c5fcdc44ba19e36738b54da1fef8","internal_anchors":1},"formal_canon":{"evidence_count":2,"snapshot_sha256":"c536cd64216d060b40fbc2d0779f6c4edfd1ac61ec0ce004261309daccf92d63"},"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/9805201","created_at":"2026-07-04T15:27:10.137063+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/9805201v1","created_at":"2026-07-04T15:27:10.137063+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/9805201","created_at":"2026-07-04T15:27:10.137063+00:00"},{"alias_kind":"pith_short_12","alias_value":"K6LHR5T6FX7I","created_at":"2026-07-04T15:27:10.137063+00:00"},{"alias_kind":"pith_short_16","alias_value":"K6LHR5T6FX7I65TS","created_at":"2026-07-04T15:27:10.137063+00:00"},{"alias_kind":"pith_short_8","alias_value":"K6LHR5T6","created_at":"2026-07-04T15:27:10.137063+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":170,"internal_anchor_count":154,"sample":[{"citing_arxiv_id":"2607.06811","citing_title":"Particle Cosmology: 1980-2000","ref_index":36,"is_internal_anchor":true},{"citing_arxiv_id":"2607.08120","citing_title":"Phantom crossing from the Standard Model and General Relativity","ref_index":3,"is_internal_anchor":true},{"citing_arxiv_id":"2607.08544","citing_title":"How to measure tidal dissipation in long resonant chains","ref_index":6,"is_internal_anchor":true},{"citing_arxiv_id":"2607.06933","citing_title":"Constructing a Mock Galaxy Catalog for the All-sky SPECtroscopic Survey of Nearby Galaxies (A-SPEC) Using the Machine-assisted Semi-Simulation Model","ref_index":102,"is_internal_anchor":true},{"citing_arxiv_id":"2607.06338","citing_title":"SN 2022erq: A Superluminous Thermonuclear Supernova with Escalating Preexplosion Mass Loss","ref_index":67,"is_internal_anchor":true},{"citing_arxiv_id":"2606.25315","citing_title":"A hybrid method for reconstruction of the equation of state of dark energy and its application to Pantheon+SH0ES data","ref_index":22,"is_internal_anchor":true},{"citing_arxiv_id":"2606.26221","citing_title":"De Sitter Representations","ref_index":1,"is_internal_anchor":true},{"citing_arxiv_id":"2606.27290","citing_title":"A solid unification of the dark sector","ref_index":12,"is_internal_anchor":true},{"citing_arxiv_id":"2606.23624","citing_title":"Semiclassical decay of de Sitter space into black holes with vortex-deformed horizons","ref_index":2,"is_internal_anchor":true},{"citing_arxiv_id":"2606.20942","citing_title":"Dark bubbles, dark dimensions and fat gravitons","ref_index":9,"is_internal_anchor":true},{"citing_arxiv_id":"2607.01724","citing_title":"Classical and Loop Quantum Cosmology of Interacting Dark Energy: A Dynamical System Analysis with Superfluid Dark Matter and Dust Matter","ref_index":1,"is_internal_anchor":true},{"citing_arxiv_id":"2607.02017","citing_title":"Boson Stars in Teleparallel Gravity with a Nonminimally Coupled Field: The Violation of Energy Conditions and Gravitational Waveforms from EMRIs","ref_index":26,"is_internal_anchor":true},{"citing_arxiv_id":"2606.12464","citing_title":"Kinematic Probes of Type-II MMG: Pad\\'e Cosmographic Analysis of VCDM","ref_index":2,"is_internal_anchor":true},{"citing_arxiv_id":"2606.11368","citing_title":"Non-linear Structure Formation in Planck+DESI Favoured Interacting Dark Energy Cosmologies","ref_index":1,"is_internal_anchor":true},{"citing_arxiv_id":"2606.10597","citing_title":"Synergy between the gravitational potential decay rate and other structure growth probes in testing gravity","ref_index":3,"is_internal_anchor":true},{"citing_arxiv_id":"2606.08182","citing_title":"Higher-dimensional quantum-corrected Oppenheimer-Snyder model with a cosmological constant","ref_index":24,"is_internal_anchor":true},{"citing_arxiv_id":"2606.23522","citing_title":"Microscopic entropy of de Sitter spacetime and entropic solution to the old cosmological constant problem","ref_index":15,"is_internal_anchor":true},{"citing_arxiv_id":"2606.07854","citing_title":"Measurements of the Angular Homogeneity Scale from DESI DR1","ref_index":2,"is_internal_anchor":true},{"citing_arxiv_id":"2606.07391","citing_title":"Mass-Varying Neutrinos from an Inverse Symmetron","ref_index":26,"is_internal_anchor":true},{"citing_arxiv_id":"2607.00075","citing_title":"Decoding the Early-Time Light Curves of Type Ia Supernovae. I. A Hierarchical Bayesian Framework for Demographic Inference","ref_index":53,"is_internal_anchor":true},{"citing_arxiv_id":"2607.00081","citing_title":"Decoding the Early-Time Light Curves of Type Ia Supernovae. II. Population Parameters of One Thousand ZTF Supernovae","ref_index":83,"is_internal_anchor":true},{"citing_arxiv_id":"2607.00133","citing_title":"Modified Cosmology from Mass-to-Horizon Relation: Background Evolution","ref_index":5,"is_internal_anchor":true},{"citing_arxiv_id":"2606.05853","citing_title":"Reconstructing dark energy with fewer assumptions","ref_index":7,"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":2,"is_internal_anchor":true},{"citing_arxiv_id":"2606.05352","citing_title":"Running Vacuum in the expanding Universe: a unified QFT paradigm for Inflation and Dark Energy","ref_index":4,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":2,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/K6LHR5T6FX7I65TSFGVN3YWPQF","json":"https://pith.science/pith/K6LHR5T6FX7I65TSFGVN3YWPQF.json","graph_json":"https://pith.science/api/pith-number/K6LHR5T6FX7I65TSFGVN3YWPQF/graph.json","events_json":"https://pith.science/api/pith-number/K6LHR5T6FX7I65TSFGVN3YWPQF/events.json","paper":"https://pith.science/paper/K6LHR5T6"},"agent_actions":{"view_html":"https://pith.science/pith/K6LHR5T6FX7I65TSFGVN3YWPQF","download_json":"https://pith.science/pith/K6LHR5T6FX7I65TSFGVN3YWPQF.json","view_paper":"https://pith.science/paper/K6LHR5T6","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/9805201&json=true","fetch_graph":"https://pith.science/api/pith-number/K6LHR5T6FX7I65TSFGVN3YWPQF/graph.json","fetch_events":"https://pith.science/api/pith-number/K6LHR5T6FX7I65TSFGVN3YWPQF/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/K6LHR5T6FX7I65TSFGVN3YWPQF/action/timestamp_anchor","attest_storage":"https://pith.science/pith/K6LHR5T6FX7I65TSFGVN3YWPQF/action/storage_attestation","attest_author":"https://pith.science/pith/K6LHR5T6FX7I65TSFGVN3YWPQF/action/author_attestation","sign_citation":"https://pith.science/pith/K6LHR5T6FX7I65TSFGVN3YWPQF/action/citation_signature","submit_replication":"https://pith.science/pith/K6LHR5T6FX7I65TSFGVN3YWPQF/action/replication_record"}},"created_at":"2026-07-04T15:27:10.137063+00:00","updated_at":"2026-07-04T15:27:10.137063+00:00"}