Cosmic Microwave Background anisotropies beyond the third peak

Abstract

Forthcoming CMB experiments will allow us to accurately investigate the power spectrum at very small scales ($\ell >1000$). We predict the level of the primary anisotropies, given the actual CMB measurements. The secondary anisotropies generated after matter-radiation decoupling contribute additional power in the tail of the CMB power spectrum. Together with the primary anisotropies, we compute the predicted power spectra for three dominant secondary effects induced by photon scattering. We predict these secondary contributions in flat cosmological models for parameters in agreement (to $2\sigma$) with the values allowed by current parameter estimates.

14 pages, 3 figures. Significantly modified version after referee's comments. Amplitude of the SZ contribution corrected for conversion factor, figure and results modified accordingly. One figure added to show ${\sigma }_8$ effect. Figure showing total contribution modified to add upper limits at small scales. Resubmitted to Astronomy and Astrophysics

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