Direct imaging of outflows and the interface to the CGM

Galactic winds are among the most important mechanisms in galaxy evolution. Simulations require aalactic outflows to regulate star formation in galaxies and thus reproduce the stellar masses, morphology and sizes of galaxies that we observe. We know they are needed, however significant gaps in our knowledge as to the physical model of outflows remain. For example, cosmological simulations require very high mass-loss rates from the halo, which are not observed in galaxies. The era of image slicers, like MUSE, is a critical step forward. Deep observations reveal the physical properties in winds, including not just kinematics but also structure of electron density, the presence of shock heating, and the metal content of the wind. I will review recent results in this area, and discuss prospects of future work with new instruments like MAVIS.