Galaxy bias is the relation between the visible distribution of galaxies and their invisible dark matter-dominated environment. Studying galaxy bias leads not only to improved cosmological constraints using galaxy observations, but invariably also to new insights about the galaxy-environment connection. This talk will describe a number of recent numerical advances that led to the first predictions for galaxy bias using hydrodynamical simulations. By comparing to the bias of dark matter halos, I will discuss what these results can tell us about the environmental dependence of the galaxy-halo connection. I will also discuss how robust priors on galaxy bias from hydrodynamical simulations are imperative to the goal of many future galaxy surveys to constrain inflation models through searches for local-type primordial non-Gaussianity.