Multiphase gas in Circumgalactic cloud complexes: Insights from kiloparsec-scale Magnetohydrodynamic Turbulence Simulations

The circumgalactic medium (CGM) is the diffuse gas surrounding a galaxy’s halo, and it plays a vital role in the galactic baryon cycle. However, its mass distribution across the virial phase and the cooler, denser atomic phase, remains uncertain. To investigate this, we perform high-resolution magnetohydrodynamic simulations of 0.125–8 kpc-scale representative patches of the CGM, with parameters informed by quasar absorption line observations. Our simulations are in global thermal balance and resolve the cooling length (the minimum across all temperatures of , where c s is the sound speed and is the cooling time in isobaric conditions), allowing us to track the evolution of cold gas more accurately. We find that low-density CGM gas ( 3 × 10 − 4 cm) cannot sustain cold gas below 10 4 K for long, due to a large value of the ratio between the cooling to mixing time (). In contrast, higher-density environments () reach a turbulent multiphase steady state, with up to 50 % of the mass in the cold phase, occupying only about 1 % of the volume. To connect with large-volume cosmological simulations and small -scale idealized simulations, we explore different box sizes (0.125–8 kpc) and identify a key scaling relation: simulations with similar exhibit comparable cold gas mass fractions and lifetimes. Importantly, we find that simply sub-sampling (reducing box-size) a small region from a large-volume simulation while maintaining a constant turbulent energy density injection rate from larger to smaller scales artificially shortens t m i x , leading to inaccurate predictions for cold gas survival. This means that cold gas at small ≲ 10 kpc scales arises in relatively dense, quiescent regions of the CGM rather than the turbulent ones undergoing cascade from large scales.