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We model the interstellar dust content of the reionization era with a suiteof cosmological, fluid-dynamical simulations of galaxies with stellar massesranging from $\sim 10^5 - 10^9 M_{\odot}$ in the first $1.2$ billion years ofthe universe. We use a post-processing method that accounts for dust creationand destruction processes, allowing us to systematically vary the parameters ofthese processes to test whether dust-dependent observable quantities ofgalaxies at these epochs could be useful for placing constraints on dustphysics. We then forward model observable properties of these galaxies tocompare to existing data. We find that we are unable to simultaneously matchexisting observational constraints with any one set of model parameters.Specifically, the models which predict the largest dust masses $D/Z \gtrsim0.1$ at $z = 5$ -- because of high assumed production yields and/or efficientgrowth via accretion in the interstellar medium -- are preferred by constraintson total dust mass and infrared luminosities, but these models produce far toomuch extinction in the ultraviolet, preventing them from matching observationsof $\beta_{\rm UV}$. To investigate this discrepancy, we analyze the relativespatial distribution of stars and dust as probed by infrared (IR) andultraviolet (UV) emission, which appear to exhibit overly symmetricmorphologies compared to existing data, likely due to the limitations of thestellar feedback model used in the simulations. Our results indicate that theobservable properties of the dust distribution in high redshift galaxies are aparticularly strong test of stellar feedback.

Modeling Dust Production, Growth, and Destruction in Reionization-Era  Galaxies with the CROC Simulations II: Predicting the Dust Content of  High-Redshift Galaxies