Noise-variance maps (shown as noise rms in μK-arcmin) that we use to filter the SMICA CMB maps that are fed into the quadratic estimators when performing inhomogeneous filtering. The upper panel shows the temperature noise map, with median over our unmasked sky area of 27 μK-arcmin. We use a common noise map for Q and U polarization, also neglecting Q and U noise correlations, shown in the lower panel, which spans an entire order of magnitude, with median 52 μK-arcmin (larger than times the temperature noise because not all the Planck detectors are polarized). In temperature, the variance map has a homogeneous (approximately 5 μK-arcmin) contribution from the isotropic additional Gaussian power that we add to the simulations to account for residual foreground contamination.
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