# Properties of the Simulated Circumgalactic Medium

## TL;DR

This study uses high-resolution idealized simulations to analyze the properties of the circumgalactic medium in different galaxy-sized halos, revealing diverse behaviors and dependencies on galactic winds, which challenge the notion of a universal CGM model.

## Contribution

It provides a detailed characterization of the CGM in two halo mass regimes using idealized simulations, highlighting the variability and complexity of CGM properties.

## Key findings

- The $10^{12}M_\odot$ halo has a hot, hydrostatic CGM with cold gas condensing and falling inward.
- The $10^{11}M_\odot$ halo's CGM is not in hydrostatic equilibrium and exhibits more bulk motions.
- Pressure support in the $10^{11}M_\odot$ halo depends strongly on galactic wind parameters.

## Abstract

The circumgalactic medium (CGM) is closely linked to galaxy formation and evolution, but difficult to characterize observationally and typically poorly resolved in cosmological simulations. We use spherically-symmetric, idealized, high-resolution simulations of the CGM in $10^{12}M_\odot$ and $10^{11}M_\odot$ dark matter halos to characterize the gas pressure, turbulent and radial velocities, and degree of thermal and effective dynamic pressure support in the overall CGM as well as in its high- and low-temperature phases. We find that the $10^{12}M_\odot$ halo contains a CGM mostly formed of a hot gas halo in hydrostatic equilibrium out of which cold gas condenses and falls onto the central galaxy, while the $10^{11}M_\odot$ halo's CGM is not in hydrostatic equilibrium, has a wider spread of properties at a given galactocentric radius, does not have a clear separation of hot and cold phases, and is dominated by bulk motions. We also find that the degree of pressure support in the $10^{11}M_\odot$ halo is strongly dependent on the parameters of the galactic winds of the central galaxy. These results promote the idea that there is no "average" CGM and care must be taken when setting the initial conditions for a small-box simulation of a patch of the CGM.