PR3 Cosmology Products

Cosmological Parameters Full Grid: The 2018 cosmological parameter results explore a variety of cosmological models with combinations of Planck and other data. We provide results from MCMC exploration chains, as well as best fits, and sets of parameter tables. Definitions, conventions, and references are contained in Planck 2013 results XVI, Planck 2015 results XIII, and the 2018 parameters paper Planck 2018 results VI. Angular Power Spectrum:* TT: The Planck bestfit CMB temperature power spectrum, shown in the figure below, covers the wide range of multipoles ℓ 22508. Over the multipole range ℓ 229, the power spectrum is derived from the Commander componentseparation algorithm applied to the combination of Planck 2018 temperature data between 30 and 857 GHz, including 86% of the sky (Planck2018 results VI). The asymmetric error bars associated with this spectrum are the 68% confidence limits and include the uncertainties due to foreground subtraction. For multipoles equal or greater than ℓ 30, instead, the spectrum is derived from the Plik crosshalfmission likelihood Planck2018l05[2], with foreground and other nuisance parameters fixed to a best fit assuming the baseΛCDM cosmology. Associated 1σ errors include beam uncertainties. Commander is described in more detail in Planck2018 results IV, and Plik is described in more detail in Planck 2018 results V. * TE, EE, and EB, BB: The Planck bestfit CMB polarization and temperaturepolarization crosscorrelation power spectra, shown in the figure below, cover the multipole range ℓ 21996. In the multipole range 2 ≤ l ≤ 29, we plot the power spectra estimates from the SimAll likelihood (though only the EE spectrum is used in the baseline parameter analysis at l ≤ 29), see Planck 2018 results VI. The spectra are obtained using a cross quasi maximum likelihood algorithm (QML) on the 100 and 143 GHz maps and validated against high fidelity endto[truncated, see actual data for full text]