  We extend the grid of NLTE models presented in Paper II to explore variations
in abundance pattern in two ways: 1) The adoption of the Asplund et al. (2009)
(GASS10) abundances, 2) For stars of metallicity, [M/H], of -0.5, the adoption
of a non-solar enhancement of alpha-elements by +0.3 dex. Moreover, our grid of
synthetic spectral energy distributions (SEDs) is interpolated to a finer
numerical resolution in both T_eff (Delta T_eff = 25 K) and log g (Delta log g
= 0.25). We compare the values of T_eff and log g inferred from fitting LTE and
Non-LTE SEDs to observed SEDs throughout the entire visible band, and in an ad
hoc "blue" band. We compare our spectrophotometrically derived T_eff values to
a variety of T_eff calibrations, including more empirical ones, drawn from the
literature. For stars of solar metallicity, we find that the adoption of the
GASS10 abundances lowers the inferred T_eff value by 25 - 50 K for late-type
giants, and NLTE models computed with the GASS10 abundances give T_eff results
that are marginally in better agreement with other T_eff calibrations. For
stars of [M/H]=-0.5 there is marginal evidence that adoption of
alpha-enhancement further lowers the derived T_eff value by 50 K. Stellar
parameters inferred from fitting NLTE models to SEDs are more dependent than
LTE models on the wavelength region being fitted, and we find that the effect
depends on how heavily line blanketed the fitting region is, whether the
fitting region is to the blue of the Wien peak of the star's SED, or both.
