  Spitzer and Caltech Submillimeter Observatory (CSO) images and
spectrophotometry of epsilon Eridani at wavelengths from 3.5 to 350 um reveal
new details of its bright debris disk. The 350 um map confirms the presence of
a ring at r = 11-28 arcsec (35-90 AU) observed previously at longer sub-mm
wavelengths. The Spitzer mid- and far-IR images do not show the ring, but
rather a featureless disk extending from within a few arcsec of the star across
the ring to r ~ 34 arcsec (110 AU). The spectral energy distribution (SED) of
the debris system implies a complex structure. A model constrained by the
surface brightness profiles and the SED indicates that the sub-mm ring emission
is primarily from large (a ~ 135 um) grains, with smaller (a ~ 15 um) grains
also present in and beyond the ring. The Spitzer IRS and MIPS SED-mode
spectrophotometry data clearly show the presence of spatially compact excess
emission at lambda > 15 um that requires the presence of two additional narrow
belts of dust within the sub-mm ring's central void. The innermost belt at r ~
3 AU is composed of silicate dust. A simple dynamical model suggests that dust
produced collisionally by a population of about 11 M_Earth of planetesimals in
the sub-mm ring could be the source of the emission from both in and beyond the
sub-mm ring. Maintaining the inner belts and the inner edge to the sub-mm ring
may require the presence of three planets in this system including the
candidate radial velocity object.
