Статья

First‐Year<i>Wilkinson Microwave Anisotropy Probe</i>(<i>WMAP</i>) Observations: Parameter Estimation Methodology

Licia VerdeChandra FellowHiranya V. PeirisDepartment of Astrophysical Sciences, Princeton University, Peyton Hall, Princeton, NJ 08544David N. SpergelDepartment of Astrophysical Sciences, Princeton University, Peyton Hall, Princeton, NJ 08544M. R. NoltaDepartment of Physics, Princeton University, Jadwin Hall, P.O. Box 708, Princeton, NJ 08544C. L. BennettNASA Goddard Space Flight Center, Code 685, Greenbelt, MD 20771M. HalpernDepartment of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, CanadaG. HinshawNASA Goddard Space Flight Center, Code 685, Greenbelt, MD 20771N. JarosikDepartment of Physics, Princeton University, Jadwin Hall, P.O. Box 708, Princeton, NJ 08544A. KogutNASA Goddard Space Flight Center, Code 685, Greenbelt, MD 20771M. LimonNASA Goddard Space Flight Center, Code 685, Greenbelt, MD 20771S. S. MeyerDepartments of Astrophysics and Physics, EFI, and CfCP, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637Lyman A. PageDepartment of Physics, Princeton University, Jadwin Hall, P.O. Box 708, Princeton, NJ 08544Gregory S. TuckerDepartment of Physics, Brown University, Providence, RI 02912Edward J. WollackNASA Goddard Space Flight Center, Code 685, Greenbelt, MD 20771E. L. Wright

2003en

ABI

Аннотация

We describe our methodology for comparing the WMAP measurements of the cosmic microwave background (CMB) and other complementary data sets to theoretical models. The unprecedented quality of the WMAP data, and the tight constraints on cosmological parameters that are derived, require a rigorous analysis so that the approximations made in the modeling do not lead to significant biases. We describe our use of the likelihood function to characterize the statistical properties of the microwave background sky. We outline the use of the Monte Carlo Markov Chains to explore the likelihood of the data given a model to determine the best fit cosmological parameters and their uncertainties. We add to the WMAP data the l>~700 CBI and ACBAR measurements of the CMB, the galaxy power spectrum at z~0 obtained from the 2dF galaxy redshift survey (2dFGRS), and the matter power spectrum at z~3 as measured with the Ly alpha forest. These last two data sets complement the CMB measurements by probing the matter power spectrum of the nearby universe. Combining CMB and 2dFGRS requires that we include in our analysis a model for galaxy bias, redshift distortions, and the non-linear growth of structure. We show how the statistical and systematic uncertainties in the model and the data are propagated through the full analysis.

Перевод пока недоступен

Идентификаторы

DOI: 10.1086/377335

Цитирования и источники

Цитирований: 2Использованных источников: 0

Показатели — AkademScholar