  Supernova-driven galactic winds are multiphase streams of gas that are often
observed flowing at a range of velocities out of star-forming regions in
galaxies. In this study, we use high resolution 3D simulations of multiphase
galactic winds modeled with the hydrodynamics code Cholla to investigate the
connection between numerical studies and observations. Using a simulated
interaction between a hot $T\sim 10^{7}\,\rm K$ supernova-driven wind and a
cool $T\sim 10^{4}\,\rm K$ cloud of interstellar material, we create mock
observables, including the optical depth and covering fraction of six commonly
observed ions (Si II, C II, Si IV, C IV, N V, and O VI) as a function of gas
velocity. We compare our mock observables to surveys of galactic winds in the
literature, finding good agreement with velocities and profiles of the low
ions. We then compute "empirical" values for the optical depth and covering
fraction following observational techniques, and compare them to the values
calculated directly from the simulation data. We find that the empirically
computed values tend to underestimate the "true" value of $\tau$ for ions with
high optical depth, and overestimate the "true" value of $\tau$ for ions with
low optical depth, relative to the simulated data.
