The LMC's Galactic Wind through the Eyes of ULLYSES

Outflows from galaxies are known to have a significant impact on the physical processes driving star formation and the evolution of galaxies. These winds are complex, so outflows must be observed at sub-kpc scales to tie wind properties with local driving sources. The Large Magellanic Cloud offers an opportunity to resolve star-formation-driven outflows at the right scales: it is face on, lacks an AGN, and individual sources are resolved in stars, gas, and dust. We propose an Archival Legacy program to map the LMC's galactic wind (and any inflows) using high-quality STIS and COS absorption-line observations along 140 sightlines to O, B, and WR stars together with a wealth of ancillary HI, H-alpha, and O VI observations. Using the detailed profiles of absorption in multiphase diagnostic UV ions, we will (1) characterize the ionization state and kinematics of the wind, (2) measure its covering fraction, mass distribution, and outflow rate, and (3) assess the impact of the 30 Doradus starburst on the flow. We will compare the observed LMC winds with new constrained-realization simulations of the Milky Way/Magellanic system to disentangle these outflows from surrounding coronal gas. We will release high-level data products, including science-ready databases of line measurements, customized packages of ancillary data, simulated maps and spectra, and visualization tools. This large-scale, resolved census of the LMC's outflow will fill a critical gap in our knowledge of how winds work with an unprecedentedly large sample of measurements right at the scale of the driving forces, in a galaxy where all the major influences can be resolved.