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Cosmological hydrodynamical simulations of galaxy evolution are increasinglyable to produce realistic galaxies, but the largest hurdle remaining is inconstructing subgrid models that accurately describe the behavior of stellarfeedback. As an alternate way to test and calibrate such models, we propose tofocus on the circumgalactic medium. To do so, we generate a suite ofadaptive-mesh refinement (AMR) simulations for a Milky-Way-massed galaxy run toz=0, systematically varying the feedback implementation. We then post-processthe simulation data to compute the absorbing column density for a wide range ofcommon atomic absorbers throughout the galactic halo, including H I, Mg II, SiII, Si III, Si IV, C IV, N V, O VI, and O VII. The radial profiles of theseatomic column densities are compared against several quasar absorption linestudies, to determine if one feedback prescription is favored. We find thatalthough our models match some of the observations (specifically those ionswith lower ionization strengths), it is particularly difficult to match O VIobservations. There is some indication that the models with increased feedbackintensity are better matches. We demonstrate that sufficient metals exist inthese halos to reproduce the observed column density distribution in principle,but the simulated circumgalactic medium lacks significant multiphasesubstructure and is generally too hot. Furthermore, we demonstrate the failingsof inflow-only models (without energetic feedback) at populating the CGM withadequate metals to match observations even in the presence of multiphasestructure. Additionally, we briefly investigate the evolution of the CGM fromz=3 to present. Overall, we find that quasar absorption line observations ofthe gas around galaxies provide a new and important constraint on feedbackmodels.

Constraints on Hydrodynamical Subgrid Models from Quasar Absorption Line Studies of the Simulated Circumgalactic Medium