Planck 2018 results
Open Access

Fig. 33.


Best-fit foreground and nuisance models for all of the cross-spectra used in the TT high- likelihood. The data, with the best-fit theoretical CMB C spectrum subtracted, are shown in black with a binning of Δ = 50. The TT CMB spectra divided by 20 are shown in the top parts of each panel. The bottom parts of each panel show the residual after foreground and nuisance correction. Grey shaded areas indicate regions of multipole space not used for cosmology. Nuisance contributions (i.e., beam leakage and sub-pixel effects) are always much smaller than astrophysical foregrounds in the ranges we keep.

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