Abstract and slides by speaker > Finley Hayley

In recent years, evidence has been growing that diffuse emission from non-resonant FeII* transitions traces galactic outflows. The diffuse FeII* emission varies with the galaxy ISM, dust content, and outflow geometry, thereby connecting CGM observations with galaxy properties. To constrain the properties that lead to galactic outflows and FeII* emission, we approach the question with both observations and radiative transfer simulations. From observations, we characterize the emission strength and kinematics for a sample of 270 galaxies at z ~ 1 detected in the MUSE Hubble Ultra Deep Field to interpret trends along the galaxy main sequence. From simulations, we test models with a variety of outflow geometries, velocities, dust contents and gas densities to reproduce the spectra of representative galaxies from the MUSE sample. By combining observations and models of FeII* emission, we strive to determine characteristic values of galactic outflows and provide informed constraints for simulations of galaxy formation and evolution.