  Spectral energy distributions for models of arbitrarily rotating stars are
computed using two dimensional rotating stellar models, NLTE plane parallel
model atmospheres, and a code to integrate the appropriately weighted
intensities over the visible surface of the stellar disk. The spectral energy
distributions depend on the inclination angle between the observer and the
rotation axis of the model. We use these curves to deduce what one would infer
the model's luminosity and effective temperature to be assuming the object was
nonrotating.
