  With a Jupiter-like exoplanet and a debris disk with both asteroid and Kuiper
belt analogs, $\epsilon$ Eridani has a fascinating resemblance to our
expectations for a young Solar System. We present a deep HST/STIS coronographic
dataset using eight orbit visits and the PSF calibrator $\delta$ Eridani. While
we were unable to detect the debris disk, we place stringent constraints on the
scattered light surface brightness of $\sim 4 \, \mu Jy/arcsec^{2}$. We combine
this scattered light detection limit with a reanalysis of archival near and
mid-infrared observations and a dynamical model of the full planetary system to
refine our model of the $\epsilon$ Eridani debris disk components. Radiative
transfer modeling suggests an asteroid belt analog inside of 3 au, an
intermediate disk component in the 6 - 37 au region and a Kuiper belt analog
co-located with the narrow belt observed in the millimeter (69 au). Modeling
also suggests a large minimum grain size requiring either very porous grains or
a suppression of small grain production, and a radially stratified particle
size distribution. The inner disk regions require a steep power law slope
($s^{-3.8}$ where $s$ is the grain size) weighted towards smaller grains and
the outer disk prefers a shallower slope ($s^{-3.4}$) with a minimum particle
size of $> 2 \, \mu m$. These conclusions will be enhanced by upcoming
coronographic observations of the system with the James Webb Space Telescope,
which will pinpoint the radial location of the dust belts and further diagnose
the dust particle properties.
