Three‐Year<i>Wilkinson Microwave Anisotropy Probe</i>(<i>WMAP</i>) Observations: Implications for Cosmology
David N. SpergelDepartment of Astrophysical Sciences, Princeton University, Princeton, NJ 08544-1001Rachel BeanCornell University, Ithaca, NY 14853Olivier DoréCanadian Institute for Theoretical Astrophysics, University of Toronto, ON M5S 3H8, CanadaM. R. NoltaCanadian Institute for Theoretical Astrophysics, University of Toronto, ON M5S 3H8, CanadaC. L. BennettDepartment of Physics and Astronomy, The Johns Hopkins University, Baltimore, MD 21218-2686J. DunkleyDepartment of Astrophysical Sciences, Princeton University, Princeton, NJ 08544-1001G. HinshawNASA Goddard Space Flight Center, Greenbelt, MD 20771N. JarosikDepartment of Physics, Jadwin Hall, Princeton University, Princeton, NJ 08544-0708Eiichiro KomatsuDepartment of Astronomy, University of Texas, Austin, TXLyman A. PageDepartment of Physics, Jadwin Hall, Princeton University, Princeton, NJ 08544-0708Hiranya V. PeirisDepartment of Astrophysical Sciences, Princeton University, Princeton, NJ 08544-1001Licia VerdeDepartment of Astrophysical Sciences, Princeton University, Princeton, NJ 08544-1001M. HalpernDepartment of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T 1Z1, CanadaRyley HillNASA Goddard Space Flight Center, Greenbelt, MD 20771A. KogutNASA Goddard Space Flight Center, Greenbelt, MD 20771M. LimonNASA Goddard Space Flight Center, Greenbelt, MD 20771S. S. MeyerDeptartments of Astrophysics and Physics, KICP and EFI, University of Chicago, Chicago, IL 60637N. OdegardNASA Goddard Space Flight Center, Greenbelt, MD 20771Gregory S. TuckerDepartment of Physics, Brown University, Providence, RI 02912-1843J. L. WeilandNASA Goddard Space Flight Center, Greenbelt, MD 20771Edward J. WollackNASA Goddard Space Flight Center, Greenbelt, MD 20771E. L. Wright
2007en
ABI
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
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