  We present a study of the structural properties and metallicity distribution
of the nearby peculiar galaxy NGC3077. Using data from our survey of the M81
Group with the Hyper Suprime-Cam on the Subaru Telescope, we construct deep
color-magnitude diagrams that are used to probe the old red giant branch
population of NGC3077. We map these stars out to and beyond the nominal tidal
radius, which allows us to derive the structural properties and stellar content
of the peripheral regions. We show that NGC3077 has an extended stellar halo
and pronounced ``S-shaped" tidal tails that diverge from the radial profile of
the inner region. The average metallicity of the old population in NGC3077 is
estimated from individual RGBs to be $\rm{[M/H]}=-0.98 \pm 0.26$, which
decreases with the distance from the galaxy center as $\rm{[M/H]}=-0.17$ dex
$\rm{R_{h}}^{-1}$. The metallicity of the S-shaped structure is similar to that
of the regions lying at $r\sim4\times\rm{R_{h}} (\sim 30$~kpc), indicating that
the stellar constituents of the tidal tails have come from the outer envelope
of NGC3077. These results suggest that this peculiar galaxy was probably a
rather normal dwarf elliptical galaxy before the tidal interaction with M81 and
M82. We also examine the evidence in our dataset for the six recently-reported
ultra-faint dwarf candidates around NGC3077. We recover a spatial overdensity
of sources coinciding with only one of these.
