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Traditional large-scale models of reionization usually employ simpledeterministic relations between halo mass and luminosity to predict howreionization proceeds. We here examine the impact on modelling reionization ofusing more detailed models for the ionizing sources as identified within the$100~{\rm Mpc/h}$ cosmological hydrodynamic simulation {\sc Simba}, coupledwith post-processed radiative transfer. Comparing with simple (one-to-one)models, the main difference of using {\sc Simba} sources is the scatter in therelation between dark matter halos and star formation, and hence ionizingemissivity. We find that, at the power spectrum level, the ionizationmorphology remains mostly unchanged, regardless of the variability in thenumber of sources or escape fraction. In particular, the power spectrum shaperemains unaffected and its amplitude changes slightly by less than 5-10\%,throughout reionization, depending on the scale and neutral fraction. Ourresults show that simplified models of ionizing sources remain viable toefficiently model the structure of reionization on cosmological scales,although the precise progress of reionization requires accounting for thescatter induced by astrophysical effects.

Reionization with Simba: How much does astrophysics matter in modeling cosmic reionization?