Effect of non-equilibrium ionization on derived physical conditions of the high-z intergalactic medium

 Non-equilibrium ionization effects are important in cosmological hydrodynamical simulations but are computationally expensive. We study the effect of non-equilibrium ionization evolution and UV ionizing background (UVB) generated with different quasar spectral energy distribution (SED) on the derived physical conditions of the intergalactic medium at 2 ≤ z ≤ 6 using our post-processing tool ‘Code for Ionization and Temperature Evolution’ (cite). cite produces results matching well with self-consistent simulations more efficiently. The  He ii reionization progresses more rapidly in non-equilibrium model compared to equilibrium models. The redshift of  He ii reionization strongly depends on the quasar SED and occurs earlier for UVB models with flatter quasar SEDs. During this epoch, the normalization of temperature–density relation, T0(z), has a maximum while the slope, γ(z), has a minimum, but occurring at different redshifts. The T0 is higher in non-equilibrium models using UVB obtained with flatter quasar SEDs. While our models produce the observed median  He ii effective optical depth evolution and its scatter for equilibrium and non-equilibrium considerations, to explain the observed cumulative distributions we may need to consider fluctuating UVB. For a given UVB model, the redshift dependence of the  H i photoionization rate derived from the observed  H i effective optical depth (τeff, H i) for the equilibrium model is different from that for the non-equilibrium model. This may lead to different requirements on the evolution of ionizing emissivities of sources. We show that, in the absence of strong differential pressure smoothing effects, it is possible to recover the T0 and γ realized in non-equilibrium model from the equilibrium models generated by rescaling photoheating rates while producing the same τeff, H i.