Fig. E.3.

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Angular power spectra of B-mode residuals in the CMB solutions when using the FGBuster (left) and NILC (right) component separation methods for the different considered foreground models. Systematic residuals are shown with solid lines, while statistical ones with dashed lines. All angular power spectra are computed excluding the Galactic plane with the Planck HFI GAL70 mask which retains 70% of the sky.
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