  The formation of "stellar halos" in dwarf galaxies have been discussed in
terms of early mergers or Galactic tides, although fluctuations in the
gravitational potential due to stellar feedback is also a possible candidate
mechanism. A Bayesian algorithm is used to find new candidate members in the
extreme outskirts of the Sculptor dwarf galaxy. Precise metallicities and
radial velocities for two distant stars are measured from their spectra taken
with the Gemini South GMOS spectrograph. The radial velocity, proper motion and
metallicity of these targets are consistent with Sculptor membership. As a
result, the known boundary of the Sculptor dwarf extends now out to an
elliptical distance of $\sim10$ half-light radii, which corresponds to a
projected physical distance of $\sim3$ kpc. As reported in earlier work, the
overall distribution of radial velocities and metallicities indicate the
presence of a more spatially and kinematically dispersed metal-poor population
that surrounds the more concentrated and colder metal-rich stars. Sculptor's
density profile shows a "kink" in its logarithmic slope at a projected distance
of $\sim25$ arcmin (620 pc), which we interpret as evidence that Galactic tides
have helped to populate the distant outskirts of the dwarf. We discuss further
ways to test and validate this tidal interpretation for the origin of these
distant stars.
