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The six parameters of the standard $\Lambda$CDM model have best-fit valuesderived from the Planck temperature power spectrum that are shifted somewhatfrom the best-fit values derived from WMAP data. These shifts are driven byfeatures in the Planck temperature power spectrum at angular scales that hadnever before been measured to cosmic-variance level precision. We investigatethese shifts to determine whether they are within the range of expectation andto understand their origin in the data. Taking our parameter set to be theoptical depth of the reionized intergalactic medium $\tau$, the baryon density$\omega_{\rm b}$, the matter density $\omega_{\rm m}$, the angular size of thesound horizon $\theta_*$, the spectral index of the primordial power spectrum,$n_{\rm s}$, and $A_{\rm s}e^{-2\tau}$ (where $A_{\rm s}$ is the amplitude ofthe primordial power spectrum), we examine the change in best-fit valuesbetween a WMAP-like large angular-scale data set (with multipole moment$\ell<800$ in the Planck temperature power spectrum) and an all angular-scaledata set ($\ell<2500$ Planck temperature power spectrum), each with a prior on$\tau$ of $0.07\pm0.02$. We find that the shifts, in units of the 1$\sigma$expected dispersion for each parameter, are $\{\Delta \tau, \Delta A_{\rm s}e^{-2\tau}, \Delta n_{\rm s}, \Delta \omega_{\rm m}, \Delta \omega_{\rm b},\Delta \theta_*\} = \{-1.7, -2.2, 1.2, -2.0, 1.1, 0.9\}$, with a $\chi^2$ valueof 8.0. We find that this $\chi^2$ value is exceeded in 15% of our simulateddata sets, and that a parameter deviates by more than 2.2$\sigma$ in 9% ofsimulated data sets, meaning that the shifts are not unusually large. Comparing$\ell<800$ instead to $\ell>800$, or splitting at a different multipole, yieldssimilar results. We examine the $\ell<800$ model residuals in the $\ell>800$power spectrum data and find that the features there... [abridged]

Planck intermediate results. LI. Features in the cosmic microwave background temperature power spectrum and shifts in cosmological parameters