New Constraints on ΩM, ΩΛ, and w from an Independent Set of 11 High-Redshift Supernovae Observed with the Hubble Space Telescope*

R. A. Knop; G. Aldering; R. Amanullah; P. Astier; G. Blanc; M. S. Burns; A. Conley; S. E. Deustua; M. Doi; R. Ellis; S. Fabbro; G. Folatelli; A. S. Fruchter; G. Garavini; S. Garmond; K. Garton; R. Gibbons; G. Goldhaber; A. Goobar; D. E. Groom; D. Hardin; I. Hook; D. A. Howell; A. G. Kim; B. C. Lee; C. Lidman; J. Mendez; S. Nobili; P. E. Nugent; R. Pain; N. Panagia; C. R. Pennypacker; S. Perlmutter; R. Quimby; J. Raux; N. Regnault; P. Ruiz-Lapuente; G. Sainton; B. Schaefer; K. Schahmaneche; E. Smith; A. L. Spadafora; V. Stanishev; M. Sullivan; N. A. Walton; L. Wang; W. M. Wood-Vasey; N. Yasuda; (The Supernova Cosmology Project)

doi:10.1086/378560

New Constraints on Ω_M, Ω_Λ, and w from an Independent Set of 11 High-Redshift Supernovae Observed with the Hubble Space Telescope^*

R. A. Knop^1,2,3, G. Aldering^3,4, R. Amanullah⁵, P. Astier⁶, G. Blanc^4,6, M. S. Burns⁷, A. Conley^4,8, S. E. Deustua^4,9, M. Doi¹⁰, R. Ellis¹¹, S. Fabbro^3,12, G. Folatelli⁵, A. S. Fruchter¹³, G. Garavini⁵, S. Garmond^4,8, K. Garton⁷, R. Gibbons⁴, G. Goldhaber^4,8, A. Goobar⁵, D. E. Groom^3,4, D. Hardin⁶, I. Hook¹⁴, D. A. Howell⁴, A. G. Kim^3,4, B. C. Lee⁴, C. Lidman¹⁵, J. Mendez^16,17, S. Nobili⁵, P. E. Nugent^3,4, R. Pain⁶, N. Panagia¹³, C. R. Pennypacker⁴, S. Perlmutter⁴, R. Quimby⁴, J. Raux⁶, N. Regnault^4,18, P. Ruiz-Lapuente¹⁷, G. Sainton⁶, B. Schaefer¹⁹, K. Schahmaneche⁶, E. Smith¹, A. L. Spadafora⁴, V. Stanishev⁵, M. Sullivan^11,20, N. A. Walton²¹, L. Wang⁴, W. M. Wood-Vasey^4,8, N. Yasuda²², and (The Supernova Cosmology Project)

© 2003. The American Astronomical Society. All rights reserved. Printed in U.S.A.
The Astrophysical Journal, Volume 598, Number 1 Citation R. A. Knop et al 2003 ApJ 598 102 DOI 10.1086/378560

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¹ Department of Physics and Astronomy, Vanderbilt University, P.O. Box 1803, Station B, Nashville, TN 37240

² Visiting Astronomer, Kitt Peak National Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under cooperative agreement with the National Science Foundation

³ Visiting Astronomer, Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under cooperative agreement with the National Science Foundation

⁴ E. O. Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720

⁵ Department of Physics, Stockholm University, SCFAB, S-106 91 Stockholm, Sweden

⁶ Laboratoire de Physique Nucléaire et de Haute Energies, CNRS-IN2P3, University of Paris VI and VII, Paris, France

⁷ Colorado College, 14 East Cache La Poudre Street, Colorado Springs, CO 80903

⁸ Department of Physics, University of California at Berkeley, 366 LeConte Hall, Berkeley, CA 94720-7300

⁹ American Astronomical Society, 2000 Florida Avenue, NW, Suite 400, Washington, DC 20009

¹⁰ Department of Astronomy, and Research Center for the Early Universe, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan

¹¹ California Institute of Technology, East California Boulevard, Pasadena, CA 91125

¹² Centro, Multidisiplinar de Astrofísica, Instituto Superior Técnico, P-1300 Lisbon, Portugal

¹³ Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218

¹⁴ Department of Physics, University of Oxford, Nuclear and Astrophysics Laboratory, Keble Road, Oxford OX1 3RH, UK

¹⁵ European Southern Observatory, St. Alonso de Córdova 3107, Vitacura, Casilla 19001, Santiago 19, Chile

¹⁶ Isaac Newton Group of Telescopes, Apartado de Correos 321, Santa Cruz de La Palma, E-38780 Canary Islands, Spain

¹⁷ Department of Astronomy, University of Barcelona, E-08028 Barcelona, Spain

¹⁸ Now at Laboratoire Leprince-Ringuet, CNRS-IN2P3, Ecole Polytechnique, Palaiseau, France

¹⁹ Department of Astronomy, University of Texas at Austin, RLM 15.308, Austin, TX 78712

²⁰ Department of Physics, University of Durham, South Road, Durham DH1 3LE, UK

²¹ Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK

²² National Astronomical Observatory of Japan, 2-21-1, Ohsawa, Mitaka, Tokyo 181-8588, Japan

Dates

Received 2003 May 24
Accepted 2003 July 16

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Abstract

We report measurements of Ω_M, Ω_Λ, and w from 11 supernovae (SNe) at z = 0.36-0.86 with high-quality light curves measured using WFPC2 on the Hubble Space Telescope (HST). This is an independent set of high-redshift SNe that confirms previous SN evidence for an accelerating universe. The high-quality light curves available from photometry on WFPC2 make it possible for these 11 SNe alone to provide measurements of the cosmological parameters comparable in statistical weight to the previous results. Combined with earlier Supernova Cosmology Project data, the new SNe yield a measurement of the mass density Ω_M = 0.25 (statistical) ± 0.04 (identified systematics), or equivalently, a cosmological constant of Ω_Λ = 0.75 (statistical) ± 0.04 (identified systematics), under the assumptions of a flat universe and that the dark energy equation-of-state parameter has a constant value w = -1. When the SN results are combined with independent flat-universe measurements of Ω_M from cosmic microwave background and galaxy redshift distortion data, they provide a measurement of w = -1.05 (statistical) ± 0.09 (identified systematic), if w is assumed to be constant in time. In addition to high-precision light-curve measurements, the new data offer greatly improved color measurements of the high-redshift SNe and hence improved host galaxy extinction estimates. These extinction measurements show no anomalous negative E(B-V) at high redshift. The precision of the measurements is such that it is possible to perform a host galaxy extinction correction directly for individual SNe without any assumptions or priors on the parent E(B-V) distribution. Our cosmological fits using full extinction corrections confirm that dark energy is required with P(Ω_Λ > 0) > 0.99, a result consistent with previous and current SN analyses that rely on the identification of a low-extinction subset or prior assumptions concerning the intrinsic extinction distribution.

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Footnotes

*
Based in part on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with programs GO-7336, GO-7590, and GO-8346. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. Based in part on observations obtained at the WIYN Observatory, which is a joint facility of the University of Wisconsin at Madison, Indiana University, Yale University, and the National Optical Astronomy Observatory. Based in part on observations made with the European Southern Observatory telescopes (ESO programs 60.A-0586 and 265.A-5721). Based in part on observations made with the Canada-France-Hawaii Telescope, operated by the National Research Council of Canada, le Centre National de la Recherche Scientifique de France, and the University of Hawaii.

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