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New Constraints on $Omega_M$, $Omega_Lambda$, and w from an Independent Set of Eleven High-Redshift Supernovae Observed with HST | 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
; | Date: |
13 Sep 2003 | Journal: | Astrophys.J. 598 (2003) 102 | Subject: | astro-ph | Affiliation: | The Supernova Cosmology Project | Abstract: | We report measurements of $Omega_M$, $Omega_Lambda$, and w from eleven supernovae at z=0.36-0.86 with high-quality lightcurves measured using WFPC-2 on the HST. This is an independent set of high-redshift supernovae that confirms previous supernova evidence for an accelerating Universe. Combined with earlier Supernova Cosmology Project data, the new supernovae yield a flat-universe measurement of the mass density $Omega_M=0.25^{+0.07}_{-0.06}$ (statistical) $pm0.04$ (identified systematics), or equivalently, a cosmological constant of $Omega_Lambda=0.75^{+0.06}_{-0.07}$ (statistical) $pm0.04$ (identified systematics). When the supernova results are combined with independent flat-universe measurements of $Omega_M$ from CMB and galaxy redshift distortion data, they provide a measurement of $w=-1.05^{+0.15}_{-0.20}$ (statistical) $pm0.09$ (identified systematic), if w is assumed to be constant in time. The new data offer greatly improved color measurements of the high-redshift supernovae, 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 supernovae 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 $P(Omega_Lambda>0)>0.99$, a result consistent with previous and current supernova analyses which rely upon the identification of a low-extinction subset or prior assumptions concerning the intrinsic extinction distribution. | Source: | arXiv, astro-ph/0309368 | Services: | Forum | Review | PDF | Favorites |
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