WMAP 
First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations:

WMAP Firstyear Paper Figures, A. Kogut, et al.  
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Fig.1 Geometry for Stokes Q and U parameters. WMAP measures polarization by differencing two orthogonal polarization channels, then solving for Q and U as the spacecraft compound spin projects the OMT onto the sky at different angles γ relative to the Galactic meridians. All analysis uses coordinateindependent quantities Q' and U' defined with respect to the great circle connecting a pair of pixels (see text). 
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Fig.2 Temperaturepolarization correlation function for WMAP coadded QVW data. The gray band shows the 68% confidence interval for similar coadded data taken from Monte Carlo simulations without polarization. The inset shows data for θ < 10°. The data are inconsistent with no temperaturepolarization crosscorrelations at more than 10 σ. Note that the data are not independent between angular bins. 
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Fig.3 Angular templates for potential systematic errors caused by bandpass mismatch between the two radiometers in each DA. We fit this template to the correlation functions from each DA to detect or limit systematic errors related to bandpass mismatch in the main beam. The effect is significant only in the K and Ka bands, which have the brightest unpolarized foregrounds. 
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Fig.4 Fitted CMB(left) and foreground (right) components from a multifrequency decomposition of the measured twopoint correlation functions. Top: IQ (TE) correlation. Bottom: IU (TB) correlation. The CMB component is shown in units of thermodynamic temperature, while the foreground is shown in antenna temperature evaluated at 41 GHz. Different colors show the effect of using different temperature maps in the crosscorrelation or including different polarization frequency channels in the CMBforeground decomposition. ‘‘ Coadd ’’ refers to a noiseweighted linear combination of the correlation functions computed for individual frequency channels. ‘‘ Fit ’’ refers to a twocomponent fit (eq. [8]) using the specified polarization frequency channels. The gray band vshows the 68% confidence interval for the CMB component for the KKaQVW fit (which has the smallest statistical uncertainty) assuming CMB temperature anisotropy and instrument noise but no CMB polarization. ‘‘ Combination ’’ and ‘‘COBE DMR’’ replace the temperature map in eq. (6) with maps with reduced foreground emission: either the WMAP internal linear combination map or the COBE DMR map of the CMB temperature. ‘‘MEM Model ’’ and ‘‘ ILC Residual ’’ replace the temperature map in eq. (6) with maps dominated by foreground emission: either the WMAP maximumentropy foreground model or the residual map produced by subtracting the internal linear combination map from the individual temperature maps at each frequency. The fitted CMB component is stable as different frequency channels and data sets are analyzed. Foreground emission is faint compared to the cosmic signal. 
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Fig.5 Diagonal elements of the covariance matrix for the c _{l}^{TE} polarization crosspower spectrum. Points show the diagonal elements computed from 7500 Monte Carlo simulations. The solid line shows the analytical model (eq. [10]). Note we multiply M_{ll} by [(l+1)/2π]^{2} to match the units in Figs. 7 and 8. 
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Fig.6 Offdiagonal correlations r_{Δl} in the covariance matrix for the c _{l}^{TE} polarization crosspower spectrum, computed from simulations. All values are normalized to r_{Δl} = 1 at Δl = 0. The dotted line shows r_{Δl} = 0 for comparison. The anticorrelation at Δl = 2 results from the spatial symmetry of the sky cut and noise coverage. 
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Fig.7 Polarization crosspower spectra c _{l}^{TE} for the WMAP firstyear data. Note that we plot [(l + 1)/2π]c _{l}^{TE} and not [l(l + 1)/2π]c _{l}^{TE}. This choice emphasizes the oscillatory nature of c _{l}^{TE}. For clarity, the dotted line shows c_{l} = 0. The solid line shows the predicted signal based on the c _{l}^{TT}power spectrum of temperature anisotropy; there are no free parameters. The TE correlation on degree angular scales (l > 20) is in excellent agreement with the signal expected from adiabatic CMB perturbations. The excess power at low l indicates significant reionization at large angular scales. 
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Fig.8 WMAP polarization crosspower spectra c _{l}^{TE} (filled circles) compared with ΛCDM models with and without reionization. The rise in power for l < 10 is consistent with reionization optical depth τ = 0.17 ± 0.04. The error bars on WMAP data reflect measurement errors only; adjacent points are slightly anticorrelated. The gray band shows the 68% confidence interval from cosmic variance. The value at l = 7 is particularly sensitive to the foreground correction. 
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Fig.9 Likelihood function for optical depth τ for a ΛCDM cosmology, using all five WMAP frequency bands fitted to CMB plus foregrounds with foreground spectral index β =  3.7. After including systematic and foreground uncertainties, the optical depth is consistent with a value τ = 0.17 with a 95% confidence range 0.09 ≤ τ ≤ 0.28. 
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