Schematic of the structure of a starburst-driven outflow embedded in a galactic halo, propelled by thermal gas pressure and/or non-thermal CR pressure. The scale height of the warm ISM is indicated. All galaxies are embedded in a gravitational potential, g, which opposes the outflow. Superscripts + and − on quantities indicate whether each term contributes to or opposes the outflow, respectively. Left: In the absence of a substantial gas halo, outflowing gas is unconfined, allowing it to escape beyond the galaxy ecosystem against the galaxy’s gravitational potential. Center: As the galaxy builds up its stellar mass, feedback processes form a hot gas halo that suppresses the outflow, promoting baryonic recycling and enriching the CGM (see Ferrara et al. 2005; Shin et al. 2021). Right: When CRs are supplied to the halo, they accumulate over time, introducing a non-thermal halo component. Since non-thermal CR pressure gradients operate over larger length scales than thermal pressure gradients, an outflow erupting into the galaxy halo encounters distinct layers where thermally dominated and CR-dominated pressure gradients hinder its development.