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We use a cosmological hydrodynamic simulation calculated with Enzo and thesemi-analytic galaxy formation model (SAM) GAMMA to address the chemicalevolution of dwarf galaxies in the early universe. The long-term goal of theproject is to better understand the origin of metal-poor stars and theformation of dwarf galaxies and the Milky Way halo by cross-validating thesetheoretical approaches. We combine GAMMA with the merger tree of the mostmassive galaxy found in the hydrodynamic simulation and compare the starformation rate, the metallicity distribution function (MDF), and theage-metallicity relationship predicted by the two approaches. We found that theSAM can reproduce the global trends of the hydrodynamic simulation. However,there are degeneracies between the model parameters and more constraints (e.g.,star formation efficiency, gas flows) need to be extracted from the simulationto isolate the correct semi-analytic solution. Stochastic processes such asbursty star formation histories and star formation triggered by supernovaexplosions cannot be reproduced by the current version of GAMMA. Non-uniformmixing in the galaxy's interstellar medium, coming primarily fromself-enrichment by local supernovae, causes a broadening in the MDF that can beemulated in the SAM by convolving its predicted MDF with a Gaussian functionhaving a standard deviation of ~0.2 dex. We found that the most massive galaxyin the simulation retains nearby 100% of its baryonic mass within its virialradius, which is in agreement with what is needed in GAMMA to reproduce theglobal trends of the simulation.

Validating Semi-Analytic Models of High-Redshift Galaxy Formation using Radiation Hydrodynamical Simulations