{"paper":{"title":"Measurements of Omega and Lambda from 42 High-Redshift Supernovae","license":"","headline":"The analysis of 42 high-redshift Type Ia supernovae indicates that the cosmological constant is non-zero and positive.","cross_cats":["hep-ex","hep-ph"],"primary_cat":"astro-ph","authors_text":"A.G. Kim, A. Goobar, A.S. Fruchter, A.V. Filippenko, B.J. Boyle, B. Schaefer, C. Lidman, C.R. Pennypacker, D.E. Groom, G. Aldering, G. Goldhaber, H.J.M. Newberg, I. M. Hook, J.C. Lee, M. Irwin, M.Y. Kim, N.J. Nunes, N. Panagia, N. Walton, P.G. Castro, P. Nugent, P. Ruiz-Lapuente, R.A. Knop, R.G. McMahon, R. Pain, R. Quimby, R.S. Ellis, S. Deustua, S. Fabbro, S. Perlmutter, T. Matheson, W.J. Couch (The Supernova Cosmology Project)","submitted_at":"1998-12-08T03:27:34Z","abstract_excerpt":"We report measurements of the mass density, Omega_M, and cosmological-constant energy density, Omega_Lambda, of the universe based on the analysis of 42 Type Ia supernovae discovered by the Supernova Cosmology Project. The magnitude-redshift data for these SNe, at redshifts between 0.18 and 0.83, are fit jointly with a set of SNe from the Calan/Tololo Supernova Survey, at redshifts below 0.1, to yield values for the cosmological parameters. All SN peak magnitudes are standardized using a SN Ia lightcurve width-luminosity relation. The measurement yields a joint probability distribution of the "},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"The data indicate that the cosmological constant is non-zero and positive, with a confidence of P(Lambda > 0) = 99%, including the identified systematic uncertainties. The data are strongly inconsistent with a Lambda = 0 flat cosmology.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"That Type Ia supernovae at high redshift can be standardized to the same intrinsic luminosity as local ones using the lightcurve width-luminosity relation, with no significant evolutionary changes or unrecognized systematics between the samples.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"42 high-redshift Type Ia supernovae yield Omega_M = 0.28 for a flat universe and show the cosmological constant is positive at 99% confidence.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"The analysis of 42 high-redshift Type Ia supernovae indicates that the cosmological constant is non-zero and positive.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"a771449453f865cd130eb64663db08465d4b5e6528931fa53282207b33c86826"},"source":{"id":"astro-ph/9812133","kind":"arxiv","version":1},"verdict":{"id":"ba1a0092-952c-43d2-bc58-1e0d2ee99ee6","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-10T19:59:03.841360Z","strongest_claim":"The data indicate that the cosmological constant is non-zero and positive, with a confidence of P(Lambda > 0) = 99%, including the identified systematic uncertainties. The data are strongly inconsistent with a Lambda = 0 flat cosmology.","one_line_summary":"42 high-redshift Type Ia supernovae yield Omega_M = 0.28 for a flat universe and show the cosmological constant is positive at 99% confidence.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"That Type Ia supernovae at high redshift can be standardized to the same intrinsic luminosity as local ones using the lightcurve width-luminosity relation, with no significant evolutionary changes or unrecognized systematics between the samples.","pith_extraction_headline":"The analysis of 42 high-redshift Type Ia supernovae indicates that the cosmological constant is non-zero and positive."},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/astro-ph/9812133/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"references":{"count":13,"sample":[{"doi":"","year":1938,"title":"A., & Fan, X","work_id":"e79c466d-ed2d-4ad1-a2e8-ba5d49fb0037","ref_index":1,"cited_arxiv_id":"astro-ph/9803277","is_internal_anchor":false},{"doi":"","year":1989,"title":"IUE - ULDA Access Guide No. 6: Supernovae, The Netherlands: ESA Cardelli, J. A., Clayton, G. C., & Mathis, J. S. 1989, ApJ, 345, 245 Carlberg, R. G. 1997, astro-ph/9708054 Carlberg, R. G., et al. 1998","work_id":"1b7ceccb-8f53-46a2-b237-5cefcbac74e1","ref_index":2,"cited_arxiv_id":"astro-ph/9708054","is_internal_anchor":true},{"doi":"","year":1997,"title":"In Presentations at the NATO ASI i n Aiguablava, Spain, LBL-38400, page III.1; also published in Thermonuclear Supernova, P. Ruiz-Lapuente, R. Canal, and J.Isern, editors, Dordrecht: Kluwer, page 777 ","work_id":"38e1f70f-157f-496a-949d-758be6619035","ref_index":3,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":1996,"title":"Kayser, R., Helbig, P., & Schramm T. 1996, A&A, 318,","work_id":"b80ad076-82dd-464e-af48-adde95bc4844","ref_index":4,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":1998,"title":"1998, ApJ, in preparation Kim, A., Goobar, A., & Perlmutter, S","work_id":"308d7a2c-d3bf-4489-bfd7-cfcfa4dc8f28","ref_index":5,"cited_arxiv_id":"","is_internal_anchor":false}],"resolved_work":13,"snapshot_sha256":"7807d4d082182d20d1d6a2ee24eff591bd6709c0f8a38b32bea179f6ce828716","internal_anchors":2},"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"}