Measurements of Ω and Λ from 42 High-Redshift Supernovae

S. Perlmutter; G. Aldering; G. Goldhaber; R. A. Knop; P. Nugent; P. G. Castro; S. Deustua; S. Fabbro; A. Goobar; D. E. Groom; I. M. Hook; A. G. Kim; M. Y. Kim; J. C. Lee; N. J. Nunes; R. Pain; C. R. Pennypacker; R. Quimby; C. Lidman; R. S. Ellis; M. Irwin; R. G. McMahon; P. Ruiz-Lapuente; N. Walton; B. Schaefer; B. J. Boyle; A. V. Filippenko; T. Matheson; A. S. Fruchter; N. Panagia; H. J. M. Newberg; W. J. Couch; The Supernova Cosmology Project

doi:10.1086/307221

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S. Perlmutter et al. 1999 ApJ 517 565 doi:10.1086/307221

Measurements of Ω and Λ from 42 High-Redshift Supernovae

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S. Perlmutter^1,12, G. Aldering¹, G. Goldhaber^1,12, R. A. Knop¹, P. Nugent¹, P. G. Castro^1,13, S. Deustua¹, S. Fabbro^1,14, A. Goobar^1,15, D. E. Groom¹, I. M. Hook^1,16, A. G. Kim^1,12,17, M. Y. Kim¹, J. C. Lee^1,18, N. J. Nunes^1,13, R. Pain^1,14, C. R. Pennypacker^1,19, R. Quimby¹, C. Lidman², R. S. Ellis³, M. Irwin³, R. G. McMahon³, P. Ruiz-Lapuente⁴, N. Walton⁵, B. Schaefer⁶, B. J. Boyle⁷, A. V. Filippenko⁸, T. Matheson⁸, A. S. Fruchter⁹, N. Panagia^9,20, H. J. M. Newberg¹⁰, W. J. Couch¹¹, and The Supernova Cosmology Project

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¹ Institute for Nuclear and Particle Astrophysics, E. O. Lawrence Berkeley National Laboratory, Berkeley, CA 94720
² European Southern Observatory, La Silla, Chile
³ Institute of Astronomy, Cambridge, England, UK
⁴ Department of Astronomy, University of Barcelona, Barcelona, Spain
⁵ Isaac Newton Group, La Palma, Spain
⁶ Department of Astronomy, Yale University, New Haven, CT
⁷ Anglo-Australian Observatory, Sydney, Australia
⁸ Department of Astronomy, University of California, Berkeley, CA
⁹ Space Telescope Science Institute, Baltimore, MD
¹⁰ Fermi National Laboratory, Batavia, IL
¹¹ University of New South Wales, Sydney, Australia
¹² Center for Particle Astrophysics, University of California, Berkeley, California
¹³ Instituto Superior Técnico, Lisbon, Portugal
¹⁴ LPNHE, CNRS-IN2P3, and University of Paris VI and VII, Paris, France
¹⁵ Department of Physics, University of Stockholm, Stockholm, Sweden
¹⁶ European Southern Observatory, Munich, Germany
¹⁷ PCC, CNRS-IN2P3, and Collège de France, Paris, France
¹⁸ Institute of Astronomy, Cambridge, England, UK
¹⁹ Space Sciences Laboratory, University of California, Berkeley, California
²⁰ Space Sciences Department, European Space Agency

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Abstract References Cited By

We report measurements of the mass density, Ω_M, and cosmological-constant energy density, Ω_Λ, of the universe based on the analysis of 42 type Ia supernovae discovered by the Supernova Cosmology Project. The magnitude-redshift data for these supernovae, at redshifts between 0.18 and 0.83, are fitted jointly with a set of supernovae from the Calán/Tololo Supernova Survey, at redshifts below 0.1, to yield values for the cosmological parameters. All supernova peak magnitudes are standardized using a SN Ia light-curve width-luminosity relation. The measurement yields a joint probability distribution of the cosmological parameters that is approximated by the relation 0.8Ω_M-0.6Ω_Λ≈-0.2±0.1 in the region of interest (Ω_M lesssim 1.5). For a flat (Ω_M+Ω_Λ=1) cosmology we find Ω_M^flat=0.28^+0.09_-0.08 (1 σ statistical) ^+0.05_-0.04 (identified systematics). The data are strongly inconsistent with a Λ=0 flat cosmology, the simplest inflationary universe model. An open, Λ=0 cosmology also does not fit the data well: the data indicate that the cosmological constant is nonzero and positive, with a confidence of P(Λ>0)=99%, including the identified systematic uncertainties. The best-fit age of the universe relative to the Hubble time is t₀^flat=14.9^+1.4_-1.1(0.63/h) Gyr for a flat cosmology. The size of our sample allows us to perform a variety of statistical tests to check for possible systematic errors and biases. We find no significant differences in either the host reddening distribution or Malmquist bias between the low-redshift Calán/Tololo sample and our high-redshift sample. Excluding those few supernovae that are outliers in color excess or fit residual does not significantly change the results. The conclusions are also robust whether or not a width-luminosity relation is used to standardize the supernova peak magnitudes. We discuss and constrain, where possible, hypothetical alternatives to a cosmological constant.

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