The origin of the H αline profiles in simulated disc galaxies
Observations of ionized H αgas in high-redshift disc galaxies have ubiquitously found significant line broadening, σH α∼10 -100 km s-1 . To understand whether this broadening reflects gas turbulence within the interstellar medium (ISM) of galactic discs, or arises from out-of-plane emission in mass-loaded outflows, we perform radiation hydrodynamic simulations of isolated Milky Way-mass disc galax
