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Simulating dwarf galaxy halos in a reionizing Universe puts severeconstraints on the sub-grid model employed in the simulations. Using the samesub-grid model that works for simulations without a UV-background (UVB) resultsin gas poor galaxies that stop forming stars very early on, except for haloswith high masses. This is in strong disagreement with observed galaxies, whichare gas rich and star forming down to a much lower mass range. To resolve thisdiscrepancy, we ran a large suite of isolated dwarf galaxy simulations toexplore a wide variety of sub-grid models and parameters, including timing andstrength of the UVB, strength of the stellar feedback, and metallicitydependent Pop III feedback. We compared these simulations to observed dwarfgalaxies by means of the baryonic Tully-Fisher relation (BTFR), which links thebaryonic content of a galaxy to the observationally determined strength of itsgravitational potential. We found that the results are robust to changes in theUVB. The strength of the stellar feedback shifts the results on the BTFR, butdoes not help to form gas rich galaxies at late redshifts. Only by includingPop III feedback are we able to produce galaxies that lie on the observationalBTFR and that have neutral gas and ongoing star formation at redshift zero.

Constraining the subgrid physics in simulations of isolated dwarf galaxies