Fully Coupled Simulation Of Cosmic Reionization. II. Recombinations, Clumping Factors, And The Photon Budget For Reionization

Journal Article · Tue Jun 24 00:00:00 EDT 2014 · The Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637x/789/2/149· OSTI ID:1565189

So, Geoffrey C. ^[1]; Norman, Michael L. ^[1]; Reynolds, Daniel R. ^[2]; Wise, John H. ^[3]

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1. Univ. of California, San Diego, CA (United States)
2. Southern Methodist Univ., Dallas, TX (United States)
3. Georgia Inst. of Technology, Atlanta, GA (United States). Center for Relativistic Astrophysics

We use a fully coupled cosmological simulation including dark matter dynamics, multispecies hydrodynamics, nonequilibrium chemical ionization, flux-limited diffusion radiation transport, and a parameterized model of star formation and feedback (thermal and radiative) to investigate the epoch of hydrogen reionization in detail. In this paper, the first of several application papers, we investigate the mechanics of reionization from stellar sources forming in high-z galaxies, the utility of various formulations for the gas clumping factor on accurately estimating the effective recombination time in the intergalactic medium (IGM), and the photon budget required to achieve reionization. We also test the accuracy of the static and time-dependent models of Madau et al. as predictors of reionization completion/maintenance. We simulate a WMAP7 ΛCDM cosmological model in a 20 comoving Mpc cube, resolved with 8003 uniform fluid cells and dark matter particles. By tuning our star formation recipe to approximately match the observed high-redshift star formation rate density and galaxy luminosity function, we have created a fully coupled radiation hydrodynamical realization of hydrogen reionization, which begins to ionize at z ≈ 10 and is completed at z ≈ 5.8 without further tuning. We find that roughly two ionizing photons per H atom are required to convert the neutral IGM to a highly ionized state. After reionization concludes, we find that the quantity $$\dot{n}_{{\rm ion}}\times (1\ {\rm Gyr})/n_{{\rm H}}$$ is ~9 at z = 5, in rough agreement with measurements of the ionizing emissivity by Becker & Bolton. The complicated events during reionization that lead to this number can be generally described as inside-out, but in reality, the narrative depends on the level of ionization of the gas one attributes as being ionized. We find that the formula for the ionizing photon production rate needed to maintain the IGM in an ionized state derived by Madau et al. should not be used to predict the epoch of reionization completion because it ignores history-dependent terms in the global ionization balance which are not ignorable. We find that the time-dependent model for the ionized volume fraction Q H II is more predictive, but overestimates the redshift of reionization completion z reion by Δz ≈ 1. We propose a revised formulation of the time-dependent model that agrees with our simulation to a few percent accuracy. Finally, we use our simulation data to measure the absorption of ionizing radiation due to circumgalactic gas resolved on our mesh and find $$\bar{f}_{{\rm esc}}({\rm CGM}) \approx 0.7$$.

• Research Organization: Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States). Oak Ridge Leadership Computing Facility (OLCF)
• Sponsoring Organization: USDOE Office of Science (SC)
• OSTI ID: 1565189
• Journal Information: The Astrophysical Journal, Vol. 789, Issue 2; ISSN 0004-637X
• Publisher: Institute of Physics (IOP)
• Country of Publication: United States
• Language: English

Related Subjects

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Astronomy & Astrophysics