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We explore how the assumption of ionization equilibrium modulates the modeledintergalactic medium (IGM) at the end of the hydrogen Epoch of Reionizationusing the cosmological radiation hydrodynamic \textsc{Technicolor Dawn}simulation. In neutral and partially-ionized regions where the metagalacticultraviolet background (UVB) is weak, the ionization timescale$t_\mathrm{ion}\equiv \Gamma^{-1}$ exceeds the Hubble time. Assumingphotoionization equilibrium in such regions artificially boosts the ionizationrate, accelerating reionization. By contrast, the recombination time$t_\mathrm{rec} < t_\mathrm{ion}$ in photoionized regions, with the result thatassuming photoionization equilibrium artificially increases the neutralhydrogen fraction. Using snapshots between $8 \geq z \geq 5$, we compare thepredicted Lyman-$\alpha$ forest flux power spectrum with and without theassumption of ionization equilibrium. Small scales ($k > 0.1$ rad s km$^{-1}$)exhibit reduced power from $7 \leq z \leq 5.5$ in the ionization equilibriumcase while larger scales are unaffected. This occurs for the same reasons:ionization equilibrium artificially suppresses the neutral fraction inself-shielded gas and boosts ionizations in voids, suppressing small-scalefluctuations in the ionization field. When the volume-averaged neutral fractiondrops below $10^{-4}$, the signature of non-equilibrium ionizations on theLyman-$\alpha$ forest (LAF) disappears. Comparing with recent observationsindicates that these non-equilibrium effects are not yet observable in the LAFflux power spectrum.

astrophysical journal/the astrophysical journal

Assuming Ionization Equilibrium and the Impact on the  Lyman-$\mathrm{\alpha}$ Forest Power Spectrum during the End of Reionization  at $8 \geq z \geq 5$