Planck 2018 temperature power spectrum. At multipoles ℓ ≥ 30 we show the frequency-coadded temperature spectrum computed from the Plik cross-half-mission likelihood, with foreground and other nuisance parameters fixed to a best fit assuming the base-ΛCDM cosmology. In the multipole range 2 ≤ ℓ ≤ 29, we plot the power-spectrum estimates from the Commander component-separation algorithm, computed over 86% of the sky (see Sect. 2.1.1). The base-ΛCDM theoretical spectrum best fit to the likelihoods is plotted in light blue in the upper panel. Residuals with respect to this model are shown in the middle panel. The vertical scale changes at ℓ = 30, where the horizontal axis switches from logarithmic to linear. The error bars show ±1 σ diagonal uncertainties, including cosmic variance (approximated as Gaussian) and not including uncertainties in the foreground model at ℓ ≥ 30. The 1 σ region in the middle panel corresponds to the errors of the unbinned data points (which are in grey). Bottom panel: difference between the 2015 and 2018 coadded high-multipole spectra (green points). The 1 σ region corresponds to the binned data errors. The vertical scale differs from the one of the middle panel. The trend seen for ℓ < 300 corresponds to the change in the dust correction model described in Sect. 3.3.2.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.