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First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Preliminary Maps and Basic Results | C. L. Bennett
; M. Halpern
; G. Hinshaw
; N. Jarosik
; A. Kogut
; M. Limon
; S. S. Meyer
; L. Page
; D. N. Spergel
; G. S. Tucker
; E. Wollack
; E. L. Wright
; C. Barnes
; M. R. Greason
; R. S. Hill
; E. Komatsu
; M. R. Nolta
; N. Odegard
; H. V. Peirs
; L. Verde
; J. L. Weiland
; | Date: |
11 Feb 2003 | Journal: | Astrophys.J.Suppl. 148 (2003) 1 | Subject: | astro-ph | Affiliation: | 1,4), S. S. Meyer , L. Page , D. N. Spergel , G. S. Tucker , E. Wollack , E. L. Wright , C. Barnes , M. R. Greason , R. S. Hill , E. Komatsu , M. R. Nolta , N. Odegard , H. V. Peirs , L. Verde , J. L. Weiland ( NASA’s GSFC, UBC, Princeton, N | Abstract: | We present full sky microwave maps in five bands (23 to 94 GHz) from the WMAP first year sky survey. Calibration errors are <0.5% and the low systematic error level is well specified. The 21 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 0.17 +/- 0.04, which implies a reionization epoch of 180+220-80 Myr (95% CL) after the Big Bang at a redshift of 20+10-9 (95% CL) for a range of ionization scenarios. This early reionization is incompatible with the presence of a significant warm dark matter density. The age of the best-fit universe is 13.7 +/- 0.2 Gyr old. Decoupling was 379+8-7 kyr after the Big Bang at a redshift of 1089 +/- 1. The thickness of the decoupling surface was dz=195 +/- 2. The matter density is Omega_m h^2 = 0.135 +0.008 -0.009, the baryon density is Omega_b h^2 = 0.0224 +/- 0.0009, and the total mass-energy of the universe is Omega_tot = 1.02 +/- 0.02. The spectral index of scalar fluctuations is fit as n_s = 0.93 +/- 0.03 at wavenumber k_0 = 0.05 Mpc^-1, with a running index slope of dn_s/d ln k = -0.031 +0.016 -0.018 in the best-fit model. This flat universe model is composed of 4.4% baryons, 22% dark matter and 73% dark energy. The dark energy equation of state is limited to w<-0.78 (95% CL). Inflation theory is supported with n_s~1, Omega_tot~1, Gaussian random phases of the CMB anisotropy, and superhorizon fluctuations. An admixture of isocurvature modes does not improve the fit. The tensor-to-scalar ratio is r(k_0=0.002 Mpc^-1)<0.90 (95% CL). | Source: | arXiv, astro-ph/0302207 | Services: | Forum | Review | PDF | Favorites |
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