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We estimate CMB polarization and temperature power spectra using WMAP 5-yearforeground contaminated maps. The power spectrum is estimated by using a modelindependent method, which does not utilize directly the diffuse foregroundtemplates nor the detector noise model. The method essentially consists of twosteps, (i) removal of diffuse foregrounds contamination by making linearcombination of individual maps in harmonic space and (ii) cross-correlation offoreground cleaned maps to minimize detector noise bias. For temperature powerspectrum we also estimate and subtract residual unresolved point sourcecontamination in the cross-power spectrum using the point source model providedby the WMAP science team. Our $TT$, $TE$ and $EE$ power spectra are in goodagreement with the published results of the WMAP science team. The error barson the polarization power spectra, however, turn out to be smaller incomparison to what is obtained by the WMAP science team. We perform detailednumerical simulations to test for bias in our procedure. We find that the biasis small in all cases. A negative bias at low $l$ in $TT$ power spectrum hasbeen pointed in an earlier publication. We find that the bias correctedquadrupole power ($l(l+1)C_l/2\pi)$ is 532 $\mu K^2$, approximately 2.5 timesthe estimate (213.4 $\mu K^2$) made by the WMAP team.

CMB Polarization and Temperature Power Spectra Estimation using Linear Combination of WMAP 5-year Maps