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Context: Optical interferometry is a powerful tool for observing theintensity structure and angular diameter of stars. When combined withspectroscopy and/or spectrophotometry, interferometry provides a powerfulconstraint for model stellar atmospheres. Aims: The purpose of this work is totest the robustness of the spherically symmetric version of the Atlas stellaratmosphere program, SAtlas, using interferometric and spectrophotometricobservations. Methods: Cubes (three dimensional grids) of model stellaratmospheres, with dimensions of luminosity, mass, and radius, are computed tofit observations for three evolved giant stars, \psi Phoenicis, \gammaSagittae, and \alpha Ceti. The best-fit parameters are compared with previousresults. Results: The best-fit angular diameters and values of \chi^2 areconsistent with predictions using Phoenix and plane-parallel Atlas models. Thepredicted effective temperatures, using SAtlas, are about 100 to 200 K lower,and the predicted luminosities are also lower due to the differences ineffective temperatures. Conclusions: It is shown that the SAtlas program is arobust tool for computing models of extended stellar atmospheres that areconsistent with observations. The best-fit parameters are consistent withpredictions using Phoenix models, and the fit to the interferometric data for\psi Phe differs slightly, although both agree within the uncertainty of theinterferometric observations.

Determining Parameters of Cool Giant Stars by Modeling Spectrophotometric and Interferometric Observations Using the SAtlas Program