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\Planck\ 2015 temperature power spectrum. At multipoles $\ell\ge30$ we show the maximum likelihood frequency-averaged temperature spectrum computed from the \plik\ cross-half-mission likelihood, with foreground and other nuisance parameters determined from the MCMC analysis of the base \LCDM\ cosmology. In the multipole range $2 \le \ell \le 29$, we plot the power spectrum estimates from the {\tt Commander} component-separation algorithm, computed over 94\,\% of the sky. The best-fit base \LCDM\ theoretical spectrum fitted to the \planckTT\ likelihood is plotted in the upper panel. Residuals with respect to this model are shown in the lower panel. The error bars show $\pm 1\,\sigma$ uncertainties.

Residual plots illustrating the accuracy of the foreground modelling. The blue points in the upper panels show the \camspec\ 2015(CHM) spectra after subtraction of the best-fit \LCDM\ spectrum. The residuals in the upper panel should be accurately described by the foreground model. Major foreground components are shown by the solid lines, colour coded as follows: total foreground spectrum (red); Poisson point sources (orange); clustered CIB (blue); thermal SZ (green); and Galactic dust (purple). Minor foreground components are shown by the dotted lines, colour-coded as follows: kinetic SZ (green); and tSZ$\times$CIB cross-correlation (purple). The red points in the upper panels show the 545-GHz-cleaned spectra (minus the best-fit CMB as subtracted from the uncleaned spectra) that are fitted to a power-law residual foreground model, as discussed in the text. The lower panels show the spectra after subtraction of the best-fit foreground models. These agree to within a few $(\mu {\rm K})^2$. The $\chi^2$ values of the residuals of the blue points, and the number of bandpowers, are listed in the lower panels.

Residual plots illustrating the accuracy of the foreground modelling. The blue points in the upper panels show the \camspec\ 2015(CHM) spectra after subtraction of the best-fit \LCDM\ spectrum. The residuals in the upper panel should be accurately described by the foreground model. Major foreground components are shown by the solid lines, colour coded as follows: total foreground spectrum (red); Poisson point sources (orange); clustered CIB (blue); thermal SZ (green); and Galactic dust (purple). Minor foreground components are shown by the dotted lines, colour-coded as follows: kinetic SZ (green); and tSZ$\times$CIB cross-correlation (purple). The red points in the upper panels show the 545-GHz-cleaned spectra (minus the best-fit CMB as subtracted from the uncleaned spectra) that are fitted to a power-law residual foreground model, as discussed in the text. The lower panels show the spectra after subtraction of the best-fit foreground models. These agree to within a few $(\mu {\rm K})^2$. The $\chi^2$ values of the residuals of the blue points, and the number of bandpowers, are listed in the lower panels.

Residual plots illustrating the accuracy of the foreground modelling. The blue points in the upper panels show the \camspec\ 2015(CHM) spectra after subtraction of the best-fit \LCDM\ spectrum. The residuals in the upper panel should be accurately described by the foreground model. Major foreground components are shown by the solid lines, colour coded as follows: total foreground spectrum (red); Poisson point sources (orange); clustered CIB (blue); thermal SZ (green); and Galactic dust (purple). Minor foreground components are shown by the dotted lines, colour-coded as follows: kinetic SZ (green); and tSZ$\times$CIB cross-correlation (purple). The red points in the upper panels show the 545-GHz-cleaned spectra (minus the best-fit CMB as subtracted from the uncleaned spectra) that are fitted to a power-law residual foreground model, as discussed in the text. The lower panels show the spectra after subtraction of the best-fit foreground models. These agree to within a few $(\mu {\rm K})^2$. The $\chi^2$ values of the residuals of the blue points, and the number of bandpowers, are listed in the lower panels.

Frequency-averaged $TE$ and $EE$ spectra (without fitting for temperature-to-polarization leakage). The theoretical $TE$ and $EE$ spectra plotted in the upper panel of each plot are computed from the \planckTT\ best-fit model of Fig.~\ref{pgTT_final}. Residuals with respect to this theoretical model are shown in the lower panel in each plot. The error bars show $\pm 1\,\sigma$ errors. The green lines in the lower panels show the best-fit temperature-to-polarization leakage model of Eqs.~\eqref{PS0a} and \eqref{PS0b}, fitted separately to the $TE$ and $EE$ spectra.

Frequency-averaged $TE$ and $EE$ spectra (without fitting for temperature-to-polarization leakage). The theoretical $TE$ and $EE$ spectra plotted in the upper panel of each plot are computed from the \planckTT\ best-fit model of Fig.~\ref{pgTT_final}. Residuals with respect to this theoretical model are shown in the lower panel in each plot. The error bars show $\pm 1\,\sigma$ errors. The green lines in the lower panels show the best-fit temperature-to-polarization leakage model of Eqs.~\eqref{PS0a} and \eqref{PS0b}, fitted separately to the $TE$ and $EE$ spectra.

Conditionals for the \plik\ $TE$ and $EE$ spectra, given the $TT$ data computed from the \plik\ likelihood. The black lines show the expected $TE$ and $EE$ spectra {\it given the $TT$ data}. The shaded areas show the $\pm1$ and $\pm2\,\sigma$ ranges computed from Eq.~\eqref{CVEC3}. The blue points show the residuals for the measured $TE$ and $EE$ spectra.

Conditionals for the \plik\ $TE$ and $EE$ spectra, given the $TT$ data computed from the \plik\ likelihood. The black lines show the expected $TE$ and $EE$ spectra {\it given the $TT$ data}. The shaded areas show the $\pm1$ and $\pm2\,\sigma$ ranges computed from Eq.~\eqref{CVEC3}. The blue points show the residuals for the measured $TE$ and $EE$ spectra.

Conditionals for the \camspec\ $TE$ and $EE$ spectra, given the $TT$ data computed from the \camspec\ likelihood. As in Fig.~\ref{pgTE+EE_cond}, the shaded areas show $\pm1$ and $\pm2\,\sigma$ ranges, computed from Eq.~\eqref{CVEC3} and blue points show the residuals for the measured $TE$ and $EE$ spectra.

Conditionals for the \camspec\ $TE$ and $EE$ spectra, given the $TT$ data computed from the \camspec\ likelihood. As in Fig.~\ref{pgTE+EE_cond}, the shaded areas show $\pm1$ and $\pm2\,\sigma$ ranges, computed from Eq.~\eqref{CVEC3} and blue points show the residuals for the measured $TE$ and $EE$ spectra.

Comparison of the base \LCDM\ model parameter constraints from \planck\ temperature and polarization data.

Marginalized constraints on parameters of the base \LCDM\ model for various data combinations, excluding low-multipole polarization, compared to the \planckTT\ constraints.

Marginalized constraints on the reionization optical depth in the base \LCDM\ model for various data combinations. Solid lines do not include low-multipole polarization; in these cases the optical depth is constrained by \planck\ lensing. The dashed/dotted lines include LFI polarization (+\lowTEB), or the combination of LFI and WMAP polarization cleaned using 353\,GHz as a dust template (+\WMAPTEB).

Residual power with respect to the \planck\ TT+lowP $\Lambda$CDM best-fit model for the \planck\ (grey), ACT south (orange), ACT equatorial (red), and SPT (green) CMB bandpowers. The ACT and SPT bandpowers are scaled by the best-fit calibration factors.

\planck\ CMB power spectrum that is marginalized over foregrounds (red), including a prior on the thermal and kinetic SZ power. The inclusion of the full higher resolution ACT and SPT data (shown in blue) does not significantly decrease the errors.

68\,\% and 95\,\% confidence regions on 1-parameter extensions of the base \LCDM\ model for \planckTT\ (grey), \planckall\ (red), and \planckall+BAO (blue). Horizontal dashed lines correspond to the parameter values assumed in the base \LCDM\ cosmology, while vertical dashed lines show the mean posterior values in the base model for \planckall+BAO.