REIONIZATION ON LARGE SCALES. III. PREDICTIONS FOR LOW-l COSMIC MICROWAVE BACKGROUND POLARIZATION AND HIGH-l KINETIC SUNYAEV-ZEL'DOVICH OBSERVABLES

We present new predictions for cosmic microwave background (CMB) temperature (on small angular scales) and polarization (on large angular scales) anisotropies induced during the epoch of reionization (EoR). Using a novel method calibrated from radiation-hydrodynamic simulations, we model the EoR in large volumes (L ∼> 2 Gpc h –1). We find that the EoR contribution to the kinetic Sunyaev-Zel'dovich power spectrum (patchy kSZ) ranges between ∼0.6-2.8 μK2 at l = 3000 for the explored parameter space. For each model, the patchy kSZ power spectrum is calculated from three large 15° × 15° maps for better numerical convergence. Decreasing the size of these maps biases the overall patchy kSZ power to higher values. We find that the amplitude of the patchy kSZ power spectrum at l = 3000 follows simple scalings of Dl=3000kSZ∝ z-bar and Dl=3000kSZ∝Δz0.51 for the mean redshift ( z-bar ) and duration (Δz) of reionization. Using the constraints on z-bar from the Wilkinson Microwave Anisotropy Probe seven year results and the lower limit on Δz from EDGES, we find a lower limit of ∼0.4 μK2 at l = 3000. Planck will infer the mean redshift from the Thomson optical depth imprinted in the low-l polarization power spectrum. Future measurements of the high-l CMB power spectrum from the Atacama Cosmology Telescope and South Pole Telescope should detect the patchy kSZ signal if the cross correlation between the thermal SZ effect and the cosmic infrared background is constrained. We show that the combination of temperature and polarization measurements constrains both z-bar and Δz. The patchy kSZ maps, power spectra templates, and the polarization power spectra will be publicly available