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We examine the properties of the circumgalactic medium (CGM) at low redshiftin a range of simulated Milky Way mass halos. The sample is comprised of sevenidealized simulations, an adaptive mesh refinement cosmological zoom-insimulation, and two groups of 50 halos with star forming or quiescent galaxiestaken from the IllustrisTNG100 simulation. The simulations have very differentsetups, resolution, and feedback models, but are analyzed in a uniform manner.By comparing median radial profiles and mass distributions of CGM properties,we isolate key similarities and differences. In doing so, we advance theefforts of the SMAUG (Simulating Multiscale Astrophysics to UnderstandGalaxies) project that aims to understand the inherently multiscale galaxyformation process. In the cosmological simulations, the CGM exhibits nearlyflat temperature distributions, and broad pressure and radial velocitydistributions. In the idealized simulations, similar distributions are found inthe inner CGM ($\lesssim 0.5 \, r_{\rm 200c}$) when strong galactic feedbackmodels are employed, but the outer CGM ($\gtrsim 0.5 \, r_{\rm 200c}$) has amuch less prominent cold phase, and narrower pressure and velocitydistributions even in models with strong feedback. This comparative analysisdemonstrates the dominant role feedback plays in shaping the inner CGM and theincreased importance of cosmological effects, such as nonspherical accretionand satellite galaxies, in the outer CGM. Furthermore, our findings highlightthat while cosmological simulations are required to capture the multiphasestructure of the CGM at large radii, idealized simulations provide a robustframework to study how galactic feedback interacts with the inner CGM andthereby provide a reliable avenue to constrain feedback prescriptions.

astrophysical journal/the astrophysical journal

First results from SMAUG: Uncovering the Origin of the Multiphase  Circumgalactic Medium with a Comparative Analysis of Idealized and  Cosmological Simulations