  Absorption line spectroscopy offers one of the best opportunities to
constrain the properties of galactic outflows and the environment of the
circumgalactic medium. Extracting physical information from line profiles is
difficult, however, for the physics governing the underlying radiation transfer
is complicated and depends on many different parameters. Idealized analytical
models are necessary to constrain the large parameter spaces efficiently, but
are typically plagued by model degeneracy and systematic errors. Comparison
tests with idealized numerical radiation transfer codes offer an excellent
opportunity to confront both of these issues. In this paper, we present a
detailed comparison between SALT, an analytical radiation transfer model for
predicting UV spectra of galactic outflows, with the numerical radiation
transfer software, RASCAS. Our analysis has lead to upgrades to both models
including an improved derivation of SALT and a customizable adaptive mesh
refinement routine for RASCAS. We explore how well SALT, when paired with a
Monte Carlo fitting procedure, can recover flow parameters from non-turbulent
and turbulent flows. When the velocity and density gradients are excluded, we
find that flow parameters are well recovered from high resolution (20 $\rm{km}$
$\rm{s}^{-1}$) data and moderately well from medium resolution (100 $\rm{km}$
$\rm{s}^{-1}$) data without turbulence at a S/N = 10, while derived quantities
(e.g., mass outflow rates, column density, etc.) are well recovered at all
resolutions. In the turbulent case, biased errors emerge in the recovery of
individual parameters, but derived quantities are still well recovered.
