Measurements of the Cosmological Parameters Omega and Lambda from the First 7 Supernovae at z >= 0.35

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dc.creatorPerlmutter, S.
dc.creatorGabi, S.
dc.creatorGoldhaber, G.
dc.creatorGroom, D. E.
dc.creatorHook, I. M.
dc.creatorKim, A. G.
dc.creatorKim, M. Y.
dc.creatorLee, J. C.
dc.creatorPennypacker, C. R.
dc.creatorSmall, I. A.
dc.creatorGoobar, A.
dc.creatorPain, R.
dc.creatorEllis, R. S.
dc.creatorMcMahon, R. G.
dc.creatorBoyle, B. J.
dc.creatorBunclark, P. S.
dc.creatorCarter, D.
dc.creatorIrwin, M. J.
dc.creatorGlazebrook, K.
dc.creatorNewberg, H. J. M.
dc.creatorFilippenko, A. V.
dc.creatorMatheson, T.
dc.creatorDopita, M.
dc.creatorCouch, W. J.
dc.date1996-08-28
dc.date1997-01-25
dc.date.accessioned2026-07-07T10:31:43Z
dc.date.available2026-07-07T10:31:43Z
dc.descriptionWe have developed a technique to systematically discover and study high-redshift supernovae that can be used to measure the cosmological parameters. We report here results based on the initial seven of >28 supernovae discovered to date in the high-redshift supernova search of the Supernova Cosmology Project. We find a dispersion in peak magnitudes of sigma_{M_B} = 0.27 this dispersion narrows to sigma_{M_B,corr} = 0.19 after "correcting" the magnitudes using the light-curve "width-luminosity" relation found for nearby (z <= 0.1) type Ia supernovae from the Calan/Tololo survey (Hamuy et al. 1996). Comparing lightcurve-width-corrected magnitudes as a function of redshift of our distant (z = 0.35-0.46) supernovae to those of nearby type Ia supernovae yields a global measurement of the mass density, Omega_M = 0.88^{+0.69}_{-0.60} for a Lambda = 0 cosmology. For a spatially flat universe (i.e., Omega_M +Omega_Lambda = 1), we find Omega_M = 0.94 ^{+0.34}_{-0.28} or, equivalently, a measurement of the cosmological constant, Omega_Lambda = 0.06 ^{+0.28}_{-0.34} (<0.51 at the 95% confidence level). For the more general Friedmann-Lemaitre cosmologies with independent Omega_M and Omega_Lambda, the results are presented as a confidence region on the Omega_M-Omega_Lambda plane. This region does not correspond to a unique value of the deceleration parameter q_0. We present analyses and checks for statistical and systematic errors, and also show that our results do not depend on the specifics of the width-luminosity correction. The results for Omega_Lambda-versus-Omega_M are inconsistent with Lambda-dominated, low density, flat cosmologies that have been proposed to reconcile the ages of globular cluster stars with higher Hubble constant values.
dc.descriptionVery minor revisions. Paper is 36 pages long, with 6 postscript figures. Also available on http://www-supernova.lbl.gov . Paper has been accepted by ApJ
dc.identifierhttps://arxiv.org/abs/astro-ph/9608192
dc.identifierhttp://arxiv.org/abs/astro-ph/9608192
dc.identifierAstrophys.J.483:565,1997
dc.identifierdoi:10.1086/304265
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/178512
dc.subjectAstrophysics
dc.titleMeasurements of the Cosmological Parameters Omega and Lambda from the First 7 Supernovae at z >= 0.35
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