Semianalytic Approach to Understanding the Distribution of Neutral Hydrogen in the Universe: Comparison of Simulations with Observations

Abstract

Following Bi & Davidsen, we perform one-dimensional semianalytic simulations along the lines of sight to model the intergalactic medium (IGM). Since this procedure is computationally efficient in probing the parameter space—and reasonably accurate—we use it to recover the values of various parameters related to the IGM (for a fixed background cosmology) by comparing the model predictions with different observations. For the currently favored low-density cold dark matter model (Ωm = 0.4, ΩΛ = 0.6, and h = 0.65), we obtain, using statistics obtained from the transmitted flux, constraints on (1) the combination f = (ΩBh2)2/J-12, where ΩB is the baryonic density parameter and J-12 is the total photoionization rate in units of 10-12 s-1, (2) temperature T0 corresponding to the mean density, and (3) the slope γ of the effective equation of state of the IGM at a mean redshift z 2.5. We find that 0.8 1.2, the lower bound on ΩBh2 is in violation of the BBN value.