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We improve the algorithm of Kosowsky, Milosavljevic, and Jimenez for computing power spectra of the cosmic microwave background. The present algorithm computes not only the temperature power spectrum but also the E- and B-mode polarization and the temperature-polarization cross power spectra, providing the accuracy required for current cosmological parameter estimation. Both unlensed and lensed (with non-linear evolution) power spectra are provided up to l=3000 for temperature and polarization signals. We refine the optimum set of cosmological parameters for computing the power spectra as perturbations around a fiducial model, leading to an accuracy better than 0. 5% for the temperature power spectrum throughout the region of parameter space within the Wilkinson Microwave Anisotropic Probe's first-year 3 confidence region. This accuracy is comparable to the difference between the widely used CMBFAST code of Seljak and Zaldarriaga and Boltzmann codes. Our algorithm (CMBWARP) makes possible a full exploration of the likelihood region for eight cosmological parameters in about one hour on a laptop computer. We provide the code to compute power spectra as well as the Markov chain Monte Carlo algorithm for cosmological parameters estimation at http: //www. physics. upenn. edu//CMBwarp.
Jiménez et al. (2004) studied this question.