  We present high-resolution Keck LWS SiC filter (10.5-12.9 micron) mid-IR
(MIR) images and photometry of a sample of nearby LLAGN. All MIR images show
extended emission on small scales (e.g. 90% maximum widths 18 - 106 pc) deep
within the nucleus. Because the profile of this small-scale emission is
inconsistent with the near-IR stellar emission profile, we conclude the MIR
emission is not from the stellar population. Because strong starburst emission
is not reported for our objects, we eliminate this origin as well, and conclude
that the extended component of the MIR emission is most likely due to a warm
dust structure deep in the nucleus, consistent with the gross details of a
Unified Model Torus.
  Because MIR and X-ray flux measurements are very insensitive to the effects
of pure dust extinction, the ratio of MIR and X emission can be used as a
discriminator of emission processes that is insensitive to dust extinction. X
and MIR emission are known to be correlated in quasars and Seyfert galaxies.
Our LLAGN objects follow this correlation with small scatter down to extremely
low luminosity, suggesting that the same continuum emission mechanisms are
present in LLAGN as in Seyferts and quasars. This result suggests that weak UV
emission (relative to other bands) in LLAGN compared to Seyferts and quasars
could be due to dust extinction; it then follows that modifications to standard
AGN continuum emission models for LLAGN (e.g. ADAF accretion) are not required.
