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Three‐Year<i>Wilkinson Microwave Anisotropy Probe</i>(<i>WMAP</i>) Observations: Implications for Cosmology
The Astrophysical Journal Supplement Series · 2007 · Vol. 170(2) · pp. 377–408
David N. Spergel✉(Cerro Tololo Inter-American Observatory)Rachel Bean(Princeton University)Olivier Doré(Canadian Institute for Theoretical Astrophysics)M. R. Nolta(Canadian Institute for Theoretical Astrophysics)C. L. Bennett(Johns Hopkins University)J. Dunkley(Princeton University)G. Hinshaw(Goddard Space Flight Center)N. Jarosik(Princeton University)Eiichiro Komatsu(Princeton University)Lyman A. Page(Princeton University)Hiranya V. Peiris(Princeton University)Licia Verde(University of Pennsylvania)M. Halpern(University of British Columbia)Ryley Hill(Science Systems and Applications (United States))A. Kogut(Goddard Space Flight Center)M. Limon(Goddard Space Flight Center)S. S. Meyer(University of Chicago)N. Odegard(Goddard Space Flight Center)Gregory S. Tucker(Brown University)J. L. Weiland(Goddard Space Flight Center)Edward J. Wollack(Goddard Space Flight Center)E. L. Wright
Abstract
A simple cosmological model with only six parameters (matter density,mh 2, baryon density,bh 2, Hubble con-stant, H0, amplitude of fluctuations, 8, optical depth, , and a slope for the scalar perturbation spectrum, ns) fits not only the 3 yearWMAP temperature and polarization data, but also small-scale CMB data, light element abundances, large-scale structure observations, and the supernova luminosity/distance relationship.UsingWMAP data only, the best-fit values for cosmological parameters for the power-law flat cold dark matter (CDM) model are (mh
Cosmology and Gravitation TheoriesGalaxies: Formation, Evolution, PhenomenaDark Matter and Cosmic PhenomenaCMB cold spotPhysicsCosmic microwave backgroundAstrophysicsSpectral indexCosmologyHubble's lawSpectral densityDark energyCosmic background radiation
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