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We use a set of 3D radiative transfer simulations to study the effect that alarge fraction of binary stars in galaxies during the epoch of reionization hason the physical properties of the intergalactic medium (i.e. the gastemperature and the ionization state of hydrogen and helium), on the topologyof the ionized bubbles and on the 21 cm power spectra. Consistently to previousliterature, we find that the inclusion of binary stars can speed up thereionization process of HI and HeI, while HeII reionization is still dominatedby more energetic sources, especially accreting black holes. The earlierionization attained with binary stars allows for more time for cooling andrecombination, so that gas fully ionized by binary stars is typically colderthan that ionized by single stars at any given redshift. With the same volumeaveraged ionization fraction, the inclusion of binary stars results in fewersmall ionized bubbles and more large ones, with visible effects also on thelarge scales of the 21 cm power spectrum.

A CRASH simulation of the contribution of binary stars to the epoch of reionization