We present self-consistent radiation hydrodynamic simulations of hydrogen reionization performed with arepo-rt complemented by a state-of-the-art galaxy formation model .
We examine how photoheating feedback , due to reionization , shapes the galaxies properties .
Our fiducial model completes reionization by z \approx 6 and matches observations of the Ly \alpha forest , the CMB electron scattering optical depth , the high-redshift UV luminosity function , and stellar mass function .
Contrary to previous works , photoheating suppresses star formation rates by more than 50 \% only in halos less massive than \sim 10 ^ { 8.4 } M _ { \odot } ( \sim 10 ^ { 8.8 } M _ { \odot } ) at z = 6 ( z = 5 ) , suggesting inefficient photoheating feedback from photons within galaxies .
The use of a uniform UV background that heats up the gas at z \approx 10.7 generates an earlier onset of suppression of star formation compared to our fiducial model .
This discrepancy can be mitigated by adopting a UV background model with a more realistic reionization history .
In the absence of stellar feedback , photoheating alone is only able to quench halos less massive than \sim 10 ^ { 9 } M _ { \odot } at z \gtrsim 5 , implying that photoheating feedback is sub-dominant in regulating star formation .
In addition , stellar feedback , implemented as a non-local galactic wind scheme in the simulations , weakens the strength of photoheating feedback by reducing the amount of stellar sources .
Most importantly , photoheating does not leave observable imprints in the UV luminosity function , stellar mass function , or the cosmic star formation rate density .
The feasibility of using these observables to detect imprints of reionization therefore requires further investigation .