2016MNRAS.457.4051K

Using our cosmological radiative transfer code, we study the implications of the updated quasi-stellar object (QSO) emissivity and star formation history for the escape fraction (f_esc) of hydrogen ionizing photons from galaxies. We estimate the f_esc that is required to reionize the Universe and to maintain the ionization state of the intergalactic medium in the post-reionization era. At z > 5.5, we show that a constant f_esc of 0.14-0.22 is sufficient to reionize the Universe. At zf_esc can have values from 0 to 0.05. However, a steep rise in f_esc, of at least a factor of ∼3, is required between z=3.5 and 5.5. It results from a rapidly decreasing QSO emissivity at z > 3 together with a nearly constant measured H i photoionization rates at 3 z f_esc over a very short time can be relaxed if we consider the contribution from a recently found large number density of faint QSOs at z >= 4. In addition, a simple extrapolation of the contribution of such QSOs to high-z suggests that QSOs alone can reionize the Universe. This implies, at z > 3.5, that either the properties of galaxies should evolve rapidly to increase the f_esc or most of the low-mass galaxies should host massive black holes and sustain accretion over a prolonged period. These results motivate a careful investigation of theoretical predictions of these alternate scenarios that can be distinguished using future observations. Moreover, it is also very important to revisit the measurements of H i photoionization rates that are crucial to the analysis presented here.