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

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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 < T0/ < 2.5 and 1.3 < γ < 2.3, while the constraint obtained on f is 0.0202 < f < 0.0322. A reliable lower bound on J-12 can be used to put a lower bound on ΩBh2, which can be compared with similar constraints obtained from big bang nucleosynthesis (BBN) and cosmic microwave background radiation studies. We find that if J-12 > 1.2, the lower bound on ΩBh2 is in violation of the BBN value.