The impact of star formation feedback on the circumgalactic medium

We use idealized 3D hydrodynamic simulations to study the dynamics and thermal structure of the circumgalactic medium (CGM). Our simulations quantify the role of cooling, stellar feedback driven galactic winds and cosmological gas accretion in setting the properties of the CGM in dark matter haloes ranging from 10¹¹ to 10¹² M☉. Our simulations support a conceptual picture in which the properties of the CGM, and the key physics governing it, change markedly near a critical halo mass of M_crit ≈ 10^11.5 M☉. As in calculations without stellar feedback, above M_crit halo gas is supported by thermal pressure created in the virial shock. The thermal properties at small radii are regulated by feedback triggered when t_cool/t_ff ≲ 10 in the hot gas. Below M_crit, however, there is no thermally supported halo and self-regulation at t_cool/t_ff ∼ 10 does not apply. Instead, the gas is out of hydrostatic equilibrium and largely supported against gravity by bulk flows (turbulence and coherent inflow/outflow) arising from the interaction between cosmological gas inflow and outflowing galactic winds. In these lower mass haloes, the phase structure depends sensitively on the outflows' energy per unit mass and mass-loading, which may allow measurements of the CGM thermal state to constrain the nature of galactic winds. Our simulations account for some of the properties of the multiphase halo gas inferred from quasar absorption line observations, including the presence of significant mass at a wide range of temperatures, and the characteristic O VI and C IV column densities and kinematics. However, we underpredict the neutral hydrogen content of the z ∼ 0 CGM.