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Title:
First-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Determination of Cosmological Parameters
Authors:
Spergel, D. N.; Verde, L.; Peiris, H. V.; Komatsu, E.; Nolta, M. R.; Bennett, C. L.; Halpern, M.; Hinshaw, G.; Jarosik, N.; Kogut, A.; Limon, M.; Meyer, S. S.; Page, L.; Tucker, G. S.; Weiland, J. L.; Wollack, E.; Wright, E. L.
Affiliation:
AA(Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544.), AB(Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544; Chandra Postdoctral Fellow.), AC(Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544.), AD(Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544.), AE(Department of Physics, Jadwin Hall, Princeton, NJ 08544.), AF(NASA Goddard Space Flight Center, Code 685, Greenbelt, MD 20771.), AG(Department of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T 1Z1, Canada.), AH(NASA Goddard Space Flight Center, Code 685, Greenbelt, MD 20771.), AI(Department of Physics, Jadwin Hall, Princeton, NJ 08544.), AJ(NASA Goddard Space Flight Center, Code 685, Greenbelt, MD 20771.), AK(NASA Goddard Space Flight Center, Code 685, Greenbelt, MD 20771; National Research Council (NRC) Fellow.), AL(Departments of Astrophysics and Physics, EFI, and CfCP, University of Chicago, Chicago, IL 60637.), AM(Department of Physics, Jadwin Hall, Princeton, NJ 08544.), AN(NASA Goddard Space Flight Center, Code 685, Greenbelt, MD 20771; National Research Council (NRC) Fellow; Department of Physics, Brown University, Providence, RI 02912.), AO(Science Systems and Applications, Inc. (SSAI), 10210 Greenbelt Road, Suite 600, Lanham, MD 20706.), AP(NASA Goddard Space Flight Center, Code 685, Greenbelt, MD 20771.), AQ(Department of Astronomy, UCLA, P.O. Box 951562, Los Angeles, CA 90095-1562.)
Publication:
The Astrophysical Journal Supplement Series, Volume 148, Issue 1, pp. 175-194. (ApJS Homepage)
Publication Date:
09/2003
Origin:
UCP
Astronomy Keywords:
Cosmology: Cosmic Microwave Background, Cosmology: Cosmological Parameters- Cosmology: Observations, Cosmology: Early Universe
DOI:
10.1086/377226
Bibliographic Code:
2003ApJS..148..175S

Abstract

WMAP precision data enable accurate testing of cosmological models. We find that the emerging standard model of cosmology, a flat Lambda-dominated universe seeded by a nearly scale-invariant adiabatic Gaussian fluctuations, fits the WMAP data. For the WMAP data only, the best-fit parameters are h=0.72+/-0.05, Omegabh2=0.024+/-0.001, Omegamh2=0.14+/-0.02, tau=0.166+0.076-0.071, ns=0.99+/-0.04, and sigma8=0.9+/-0.1. With parameters fixed only by WMAP data, we can fit finer scale cosmic microwave background (CMB) measurements and measurements of large-scale structure (galaxy surveys and the Lyalpha forest). This simple model is also consistent with a host of other astronomical measurements: its inferred age of the universe is consistent with stellar ages, the baryon/photon ratio is consistent with measurements of the [D/H] ratio, and the inferred Hubble constant is consistent with local observations of the expansion rate. We then fit the model parameters to a combination of WMAP data with other finer scale CMB experiments (ACBAR and CBI), 2dFGRS measurements, and Lyalpha forest data to find the model's best-fit cosmological parameters: h=0.71+0.04-0.03, Omegabh2=0.0224+/-0.0009, Omegamh2=0.135+0.008-0.009, tau=0.17+/-0.06, ns(0.05 Mpc-1)=0.93+/-0.03, and sigma8=0.84+/-0.04. WMAP's best determination of tau=0.17+/-0.04 arises directly from the temperature-polarization (TE) data and not from this model fit, but they are consistent. These parameters imply that the age of the universe is 13.7+/-0.2 Gyr. With the Lyalpha forest data, the model favors but does not require a slowly varying spectral index. The significance of this running index is sensitive to the uncertainties in the Lyalpha forest.

By combining WMAP data with other astronomical data, we constrain the geometry of the universe, Omegatot=1.02+/-0.02, and the equation of state of the dark energy, w<-0.78 (95% confidence limit assuming w>=-1). The combination of WMAP and 2dFGRS data constrains the energy density in stable neutrinos: Omeganuh2<0.0072 (95% confidence limit). For three degenerate neutrino species, this limit implies that their mass is less than 0.23 eV (95% confidence limit). The WMAP detection of early reionization rules out warm dark matter.

WMAP is the result of a partnership between Princeton University and the NASA Goddard Space Flight Center. Scientific guidance is provided by the WMAP Science Team.

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