  The spectral energy distribution as a function of inclination is computed
using 2D rotating stellar models and NLTE plane parallel stellar atmospheres.
These models cover the range from $1.875M_{\odot}$ to $3.0M_{\odot}$. The
deduced effective temperature is determined by B-V computed from the spectral
energy distribution, and the deduced luminosity is computed as the integral of
the spectral energy distribution over all frequencies, assuming the distance
and reddening are known. These deduced quantities are obtained from the
observed spectral energy distribution assuming the objects are spherically
symmetric, and thus the results are dependent on the inclination. Previous work
has shown that the surface properties between two rotating stellar models with
the same surface shape scale, and this is also true for the deduced effective
temperature and luminosity over this limited mass range.
