  Observations of infrared emission from AGN show that grains exist over a
broad range of distances from the central object, extending to the point where
they are destroyed by sublimation. These ~1000 K grains produce much of the 1
micron continuum. In this region closest to the central object there must be a
gaseous component associated with the hot grains. This paper employs a state of
the art grain model and shows that the gas must be very hot, with temperatures
in the neighborhood of 10^6 K. The dusty component has a covering factor of
roughly 50% and so this region also reprocesses much of the total x-ray
emission. Our explicit models of the IR through x-ray spectral energy
distributions allow the x-ray component to be predicted from IR observations.
We are creating a grid of such predictions and will make them available as an
XSPEC add-in, allowing this spectral component to be included in quantitative
modeling of AGN spectra.
