  We present nuclear spectral energy distributions (SEDs) in the range
0.4-16micron for an expanded CfA sample of Seyfert galaxies. The spectral
indices from 1-16micron range from alpha_IR 0.9 to 3.8. The shapes of the
spectra are correlated with Seyfert type in the sense that steeper nuclear SEDs
(nu*f_nu increasing with increasing wavelength) tend to be found in Seyfert 2s
and flatter SEDs (nu *f_nu constant) in Seyfert 1-1.5s. The galaxies optically
classified as Seyferts 1.8s and 1.9s display values of alpha_IR as in type 1
objects, or values intermediate between those of Seyfert 1s and Seyfert 2s. The
intermediate SEDs of many Seyfert 1.8-1.9s may be consistent with the presence
of a pure Seyfert 1 viewed through a moderate amount (A_V <5mag) of foreground
galaxy extinction. We find, however, that between 10 and 20% of galaxies with
broad optical line components have steep infrared SEDs.
  Torus models usually adopt high equatorial opacities to reproduce the
infrared properties of Seyfert 1s and 2s, resulting in a dichotomy of infrared
SEDs (flat for type 1s, and steep for type 2s). Such a dichotomy, however, is
not observed in our sample. The wide range of spectral indices observed in the
type 2 objects, the lack of extremely steep SEDs, and the large numbers of
objects with intermediate spectral indices cannot be reconciled with
predictions from existing optically thick torus models. We discuss possible
modifications to improve torus models, including low optical depth tori, clumpy
dusty tori, and high-optical-depth tori with an extended optically thin
component.
