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Title: Measurements of the cosmological parameters {Omega} and {Lambda} from the first seven supernovae at z{ge}0.35

Abstract

We 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 more than 28 supernovae discovered to date in the high-redshift supernova search of the Supernova Cosmology Project. We find an observational dispersion in peak magnitudes of {sigma}{sub M{sub B}}=0.27; this dispersion narrows to {sigma}M{sub B},corr=0.19 after correcting the magnitudes using the light-curve width-luminosity relation found for nearby (z{le}0.1) Type Ia supernovae from the Calan/Tololo survey (Hamuy et al.). Comparing light-curve width-corrected magnitudes as a function of redshift of our distant (z=0.35{endash}0.46) supernovae to those of nearby Type Ia supernovae yields a global measurement of the mass density, {Omega}{sub M}=0.88{sub {minus}0.60}{sup +0.69} for a {Lambda}=0 cosmology. For a spatially flat universe (i.e., {Omega}{sub M}+{Omega}{sub {Lambda}}=1) we find {Omega}{sub M}=0.94{sub {minus}0.28}{sup +0.34} or, equivalently, a measurement of the cosmological constant, {Omega}{sub {Lambda}}=0.06{sub {minus}0.34}{sup +0.28} ({lt}0.51 at the 95{percent} confidence level). For the more general Friedmann-Lemaitre cosmologies with independent {Omega}{sub M} and {Omega}{sub {Lambda}}, the results are presented as a confidence region on the {Omega}{sub M}{endash}{Omega}{sub {Lambda}} plane. This region does not correspond to a unique value of the deceleration parameter q{submore » 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}{sub {Lambda}}-versus-{Omega}{sub 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. {copyright} {ital 1997} {ital The American Astronomical Society}« less

Authors:
 [1];  [2];  [1];  [3];  [1];  [4];  [5];
  1. Institute for Nuclear and Particle Astrophysics, E. O. Lawrence Berkeley National Laboratory, MS 50-232, University of California, 1 Cyclotron Road, Berkeley, California 94720 (United States)|[Center for Particle Astrophysics, University of California, Berkeley, California 94720 (United States)
  2. Institute for Nuclear and Particle Astrophysics, E. O. Lawrence Berkeley National Laboratory, MS 50-232, University of California, 1 Cyclotron Road, Berkeley, California 94720 (United States)|[Space Sciences Laboratory, U.C. Berkeley, California 94720 (United States)
  3. Institute for Nuclear and Particle Astrophysics, E. O. Lawrence Berkeley National Laboratory, MS 50-232, University of California, 1 Cyclotron Road, Berkeley, California 94720 (United States)|[Center for Particle Astrophysics, University of California, Berkeley, California 94720 (United States)|[University of Stockholm
  4. Center for Particle Astrophysics, University of California, Berkeley, California 94720 (United States)|[Department of Astronomy, University of California, Berkeley, California 94720-3411 (United States)
  5. Institute for Nuclear and Particle Astrophysics, E. O. Lawrence Berkeley National Laboratory, MS 50-232, University of California, 1 Cyclotron Road, Berkeley, California 94720 (United States)
Publication Date:
Research Org.:
Lawrence Berkeley National Laboratory
OSTI Identifier:
628701
DOE Contract Number:  
AC03-76SF00098
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 483; Journal Issue: 2; Other Information: PBD: Jul 1997
Country of Publication:
United States
Language:
English
Subject:
66 PHYSICS; COSMOLOGY; SUPERNOVAE; RED SHIFT; COSMOLOGICAL MODELS; LUMINOSITY; DISTANCE; DATA ANALYSIS; CALIBRATION; ERRORS

Citation Formats

Perlmutter, S., Gabi, S., Goldhaber, G., Goobar, A., Groom, D.E., Hook, I.M., Kim, A.G., and and others. Measurements of the cosmological parameters {Omega} and {Lambda} from the first seven supernovae at z{ge}0.35. United States: N. p., 1997. Web. doi:10.1086/304265.
Perlmutter, S., Gabi, S., Goldhaber, G., Goobar, A., Groom, D.E., Hook, I.M., Kim, A.G., & and others. Measurements of the cosmological parameters {Omega} and {Lambda} from the first seven supernovae at z{ge}0.35. United States. doi:10.1086/304265.
Perlmutter, S., Gabi, S., Goldhaber, G., Goobar, A., Groom, D.E., Hook, I.M., Kim, A.G., and and others. Tue . "Measurements of the cosmological parameters {Omega} and {Lambda} from the first seven supernovae at z{ge}0.35". United States. doi:10.1086/304265.
@article{osti_628701,
title = {Measurements of the cosmological parameters {Omega} and {Lambda} from the first seven supernovae at z{ge}0.35},
author = {Perlmutter, S. and Gabi, S. and Goldhaber, G. and Goobar, A. and Groom, D.E. and Hook, I.M. and Kim, A.G. and and others},
abstractNote = {We 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 more than 28 supernovae discovered to date in the high-redshift supernova search of the Supernova Cosmology Project. We find an observational dispersion in peak magnitudes of {sigma}{sub M{sub B}}=0.27; this dispersion narrows to {sigma}M{sub B},corr=0.19 after correcting the magnitudes using the light-curve width-luminosity relation found for nearby (z{le}0.1) Type Ia supernovae from the Calan/Tololo survey (Hamuy et al.). Comparing light-curve width-corrected magnitudes as a function of redshift of our distant (z=0.35{endash}0.46) supernovae to those of nearby Type Ia supernovae yields a global measurement of the mass density, {Omega}{sub M}=0.88{sub {minus}0.60}{sup +0.69} for a {Lambda}=0 cosmology. For a spatially flat universe (i.e., {Omega}{sub M}+{Omega}{sub {Lambda}}=1) we find {Omega}{sub M}=0.94{sub {minus}0.28}{sup +0.34} or, equivalently, a measurement of the cosmological constant, {Omega}{sub {Lambda}}=0.06{sub {minus}0.34}{sup +0.28} ({lt}0.51 at the 95{percent} confidence level). For the more general Friedmann-Lemaitre cosmologies with independent {Omega}{sub M} and {Omega}{sub {Lambda}}, the results are presented as a confidence region on the {Omega}{sub M}{endash}{Omega}{sub {Lambda}} plane. This region does not correspond to a unique value of the deceleration parameter q{sub 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}{sub {Lambda}}-versus-{Omega}{sub 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. {copyright} {ital 1997} {ital The American Astronomical Society}},
doi = {10.1086/304265},
journal = {Astrophysical Journal},
number = 2,
volume = 483,
place = {United States},
year = {1997},
month = {7}
}