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We have developed a technique to systematically discover and studyhigh-redshift supernovae that can be used to measure the cosmologicalparameters. We report here results based on the initial seven of >28 supernovaediscovered to date in the high-redshift supernova search of the SupernovaCosmology 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" themagnitudes 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 ofour distant (z = 0.35-0.46) supernovae to those of nearby type Ia supernovaeyields 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, ameasurement of the cosmological constant, Omega_Lambda = 0.06 ^{+0.28}_{-0.34}(<0.51 at the 95% confidence level). For the more general Friedmann-Lemaitrecosmologies with independent Omega_M and Omega_Lambda, the results arepresented as a confidence region on the Omega_M-Omega_Lambda plane. This regiondoes not correspond to a unique value of the deceleration parameter q_0. Wepresent analyses and checks for statistical and systematic errors, and alsoshow that our results do not depend on the specifics of the width-luminositycorrection. The results for Omega_Lambda-versus-Omega_M are inconsistent withLambda-dominated, low density, flat cosmologies that have been proposed toreconcile the ages of globular cluster stars with higher Hubble constantvalues.

Measurements of the Cosmological Parameters Ω and Λ from the First Seven Supernovae atz≥ 0.35