The role of the accretion disk, dust, and jets in the IR emission of
  low-luminosity AGN
  We use recent high-resolution infrared (IR; 1 - 20 micron) photometry to
examine the origin of the IR emission in low-luminosity active galactic nuclei
(LLAGN). The data are compared with published model fits that describe the
spectral energy distribution of LLAGN in terms of an advection-dominated
accretion flow (ADAF), truncated thin accretion disk, and jet. The truncated
disk in these models is usually not luminous enough to explain the observed IR
emission, and in all cases its spectral shape is much narrower than the broad
IR peaks in the data. Synchrotron radiation from the jet appears to be
important in very radio-loud nuclei, but the detection of strong silicate
emission features in many objects indicates that dust must also contribute. We
investigate this point by fitting the IR SED of NGC 3998 using dusty torus and
optically thin (tau_MIR ~ 1) dust shell models. While more detailed modeling is
necessary, these initial results suggest that dust may account for the nuclear
mid-IR emission of many LLAGN.
