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First‐Year <i>Wilkinson Microwave Anisotropy Probe</i> ( <i>WMAP</i> ) Observations: Preliminary Maps and Basic Results

C. L. BennettNASA/Goddard Space Flight Center, Code 685, Greenbelt, MD 20771M. HalpernDepartment of Physics and Astronomy, University of British Columbia, Vancouver, BC, V6T 1Z1, CanadaG. HinshawNASA/Goddard Space Flight Center, Code 685, Greenbelt, MD 20771N. JarosikDepartment of Physics, Jadwin Hall, Princeton, NJ 08544A. KogutNASA/Goddard Space Flight Center, Code 685, Greenbelt, MD 20771M. LimonNational Research Council FellowS. S. MeyerDepartments of Astrophysics and Physics, EFI, and CFCP, University of Chicago, Chicago, IL 60637Lyman A. PageDepartment of Physics, Jadwin Hall, Princeton, NJ 08544David N. SpergelDepartment of Astrophysical Sciences,Princeton University,Princeton,NJ 08544Gregory S. TuckerDepartment of Physics, Brown University, Providence, RI 02912Edward J. WollackNASA/Goddard Space Flight Center, Code 685, Greenbelt, MD 20771E. L. WrightC. BarnesDepartment of Physics, Jadwin Hall, Princeton, NJ 08544M. R. GreasonScience Systems and Applications, Inc. (SSAI), 10210 Greenbelt Road, Suite 600, Lanham, MD 20706Robert HillScience Systems and Applications, Inc. (SSAI), 10210 Greenbelt Road, Suite 600, Lanham, MD 20706Eiichiro KomatsuDepartment of Astrophysical Sciences,Princeton University,Princeton,NJ 08544Michael R. NoltaDepartment of Physics, Jadwin Hall, Princeton, NJ 08544N. OdegardScience Systems and Applications, Inc. (SSAI), 10210 Greenbelt Road, Suite 600, Lanham, MD 20706Hiranya V. PeirisDepartment of Astrophysical Sciences,Princeton University,Princeton,NJ 08544Licia VerdeDepartment of Astrophysical Sciences,Princeton University,Princeton,NJ 08544J. L. WeilandScience Systems and Applications, Inc. (SSAI), 10210 Greenbelt Road, Suite 600, Lanham, MD 20706

2003en

ABI

Annotatsiya

We present full sky microwave maps in five frequency bands (23 to 94 GHz) from the WMAP first year sky survey. Calibration errors are less than 0.5% and the low systematic error level is well specified. The cosmic microwave background (CMB) is separated from the foregrounds using multifrequency data. The sky maps are consistent with the 7 in. full-width at half-maximum (FWHM) Cosmic Background Explorer (COBE) maps. We report more precise, but consistent, dipole and quadrupole values. The CMB anisotropy obeys Gaussian statistics with -58 less than f(sub NL) less than 134 (95% CL). The 2 less than or = l less than or = 900 anisotropy power spectrum is cosmic variance limited for l less than 354 with a signal-to-noise ratio greater than 1 per mode to l = 658. The temperature-polarization cross-power spectrum reveals both acoustic features and a large angle correlation from reionization. The optical depth of reionization is tau = 0.17 +/- 0.04, which implies a reionization epoch of t(sub r) = 180(sup +220, sub -80) Myr (95% CL) after the Big Bang at a redshift of z(sub r) = 20(sup +10, sub -9) (95% CL) for a range of ionization scenarios. This early reionization is incompatible with the presence of a significant warm dark matter density. A best-fit cosmological model to the CMB and other measures of large scale structure works remarkably well with only a few parameters. The age of the best-fit universe is t(sub 0) = 13.7 +/- 0.2 Gyr old. Decoupling was t(sub dec) = 379(sup +8, sub -7)kyr after the Big Bang at a redshift of z(sub dec) = 1089 +/- 1. The thickness of the decoupling surface was Delta(sub z(sub dec)) = 195 +/- 2. The matter density of the universe is Omega(sub m)h(sup 2) = 0.135(sup +0.008, sub -0.009) the baryon density is Omega(sub b)h(sup 2) = 0.0224 +/- 0.0009, and the total mass-energy of the universe is Omega(sub tot) = 1.02 +/- 0.02. There is progressively less fluctuation power on smaller scales, from WMAP to fine scale CMB measurements to galaxies and finally to the Ly-alpha forest. This is accounted for with a running spectral index, significant at the approx. 2(sigma) level. The spectral index of scalar fluctuations is fit as n(sub s) = 0.93 +/-0.03 at wavenumber k(sub o) = 0.05/Mpc ((sub eff) approx. = 700), with a slope of dn(sub s)/d I(sub nk) = -0.031(sup + 0.016, sub -0.018) in the best-fit model.

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DOI: 10.1086/377253

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