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We extend the grid of NLTE models presented in Paper II to explore variationsin 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 adoptionof a non-solar enhancement of alpha-elements by +0.3 dex. Moreover, our grid ofsynthetic spectral energy distributions (SEDs) is interpolated to a finernumerical 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 andNon-LTE SEDs to observed SEDs throughout the entire visible band, and in an adhoc "blue" band. We compare our spectrophotometrically derived T_eff values toa variety of T_eff calibrations, including more empirical ones, drawn from theliterature. For stars of solar metallicity, we find that the adoption of theGASS10 abundances lowers the inferred T_eff value by 25 - 50 K for late-typegiants, and NLTE models computed with the GASS10 abundances give T_eff resultsthat are marginally in better agreement with other T_eff calibrations. Forstars of [M/H]=-0.5 there is marginal evidence that adoption ofalpha-enhancement further lowers the derived T_eff value by 50 K. Stellarparameters inferred from fitting NLTE models to SEDs are more dependent thanLTE models on the wavelength region being fitted, and we find that the effectdepends on how heavily line blanketed the fitting region is, whether thefitting region is to the blue of the Wien peak of the star's SED, or both.

Modeling the near-UV band of GK stars, Paper III: Dependence on abundance pattern