Cosmic microwave background anisotropies resulting from feedback-regulated inhomogeneous reionization

We calculate the secondary anisotropies in the cosmic microwave background (CMB) produced by inhomogeneous reionization from simulations in which the effects of radiative and stellar feedback effects on galaxy formation have been included. This allows us to determine self-consistently the beginning (z(i)approximate to 30), the duration (deltaz approximate to 20) and the (non-linear) evolution of the reionization process for a critical density cold dark matter (CDM) model. In addition, from the simulated spatial distribution of ionized regions, we are able to calculate the evolution of the two-point ionization correlation function, C-chi, and obtain the power spectrum of the anisotropies, C-l, in the range 5000 <l < 10(6). The power spectrum has a broad maximum around l approximate to 30 000, where it reaches the value 2x10(-12). We also show that the ionization correlation function C-chi is not Gaussian, but at separation angles theta less than or similar to 10(-4) rad it can be approximated by a modified Lorentzian shape; at larger separations an anticorrelation signal is predicted for both C-chi and C(theta). Detection of signals as above will be possible with future millimetre-wavelength interferometers like the Atacama Large Millimeter Array (ALMA), which appears as an optimum instrument to search for signatures of inhomogeneous reionization.