17093

In the current cosmological framework comma galactic superwinds play a pivotal role in regulating star formation and producing the observed stellar mass function. Theory suggests that galactic winds impede the flow of cool gas from the circumgalactic medium (CGM) onto the disk of galaxies however comma the microphysics of how galactic winds do so is still a mystery. The goal of this program is to unveil this elusive process. We propose to observe the CGM of a complete sample of 42 galaxies via QSO-absorption spectroscopy in three coronal lines - CIV comma NV comma and OVI - that match the predicted energetics of the wind-CGM interactions. Theoretical models advocate that the differences in the strengths and kinematics of the coronal lines are necessary and sufficient indicators to identify the complex processes involved in the multiphase wind-CGM fluid interactions. Currently comma we have only 4 galaxies with archival data on all three lines. Thus comma the proposed dataset will be essential for constraining models of galactic feedback. Our program will - (1) detect evidence for wind-CGM interactions in star-forming galaxies (2) determine how the strength of the wind-CGM interactions vary with galaxy properties and (3) compare coronal lines between observations and those predicted by idealized and cosmological simulations. Our idealized simulations incorporate non-equilibrium physics in the presence of a weak magnetic field - conditions similar to the real CGM. We will release our data products to the community via the Hubble Legacy Archive within six months of the last observations. It will be a comprehensive dataset suitable for direct comparison with a host of ongoing simulation efforts.