A simple cosmological model with only six parameters (matter density, Ωmh2, baryon density, Ωbh 2, Hubble constant, H0, amplitude of fluctuations, σ8, optical depth, τ, and a slope for the scalar perturbation spectrum, ns) fits not only the 3 year WMAP temperature and polarization data, but also small-scale CMB data, light element abundances, large-scale structure observations, and the supernova luminosity/distance relationship. Using WMAP data only, the bestfit values for cosmological parameters for the power-law flat A cold dark matter (ACDM) model are (Ωmh2, Ωbh2, h, n s, τ, σ8) = (0.1277-0.0079 +0.0080,0.02229 ± 0.00073, 0.732-0.032 +0.031,0.958 ± 0.016, 0.089 ± 0.030, 0.761 -0.048+0.049). The 3 year data dramatically shrink the allowed volume in this six-dimensional parameter space. Assuming that the primordial fluctuations are adiabatic with a power-law spectrum, the WMAP data alone require dark matter and favor a spectral index that is significantly less than the Harrison-Zel'dovich-Peebles scale-invariant spectrum (ns = 1, r = 0). Adding additional data sets improves the constraints on these components and the spectral slope. For power-law models, WMAP data alone puts an improved upper limit on the tensor-to-scalar ratio, r0.002 < 0.65 (95% CL) and the combination of WMAP and the lensing-normalized SDSS galaxy survey implies r0.002 < 0.30 (95% CL). Models that suppress large-scale power through a running spectral index or a large-scale cutoff in the power spectrum are a better fit to the WMAP and small-scale CMB data than the power-law ACDM model; however, the improvement in the fit to the WMAP data is only Δχ2 = 3 for 1 extra degree of freedom. Models with a running-spectral index are consistent with a higher amplitude of gravity waves. In a flat universe, the combination of WMAP and the Supernova Legacy Survey (SNLS) data yields a significant constraint on the equation of state of the dark energy, w = -0.967-0.072+0.073. If we assume w = -1, then the deviations from the critical density, ΩK, are small: the combination of WMAP and the SNLS data implies Ωk = -0.011 ± 0.012. The combination of WMAP 3 year data plus the HST Key Project constraint on H0 implies ±k = -0.014 ± 0.017 and ΩA = 0.716 ± 0.055. Even if we do not include the prior that the universe is flat, by combining WMAP, large-scale structure, and supernova data, we can still put a strong constraint on the dark energy equation of state, w = -1.08 ± 0.12. For a flat universe, the combination of WMAP and other astronomical data yield a constraint on the sum of the neutrino masses, Σmv < 0.66 eV (95%CL). Consistent with the predictions of simple inflationary theories, we detect no significant deviations from Gaussianity in the CMB maps using Minkowski functional, the bispectrum, trispectrum, and a new statistic designed to detect large-scale anisotropies in the fluctuations.
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science
- Cosmic microwave background
- Cosmology: observations