  We study a compact nucleus embedded in an early-type dwarf galaxy,
MATLAS-167, which is in the process of disruption by the tidal force of the
neighboring giant S0 galaxy, NGC 936, in a group environment. Using the imaging
data of the MATLAS survey, we analyze the stellar tidal tail of MATLAS-167 and
its central compact nucleus, designated as NGC 936_UCD. We find that NGC
936_UCD has a luminosity of M$_{g}$ = $-$11.43$\pm$0.01 mag and a size of
66.5$\pm$17 pc, sharing the global properties of Ultra Compact Dwarf galaxies
(UCDs) but significantly larger and brighter compared to the typical UCD
populations observed in the Virgo cluster. By integrating the total luminosity
of both the tidal stream and MATLAS-167, we estimate that the disrupted dwarf
progenitor possesses a luminosity of M$_{g}$ = $-$15.92$\pm$0.06 mag, a typical
bright dE luminosity. With the help of the optical spectrum observed by the
SDSS survey, we derive the simple stellar population properties of NGC 936_UCD:
a light-weighted age of 5.6$\pm$0.7 Gyr and metallicity of [Z/H] =
$-$0.83$\pm$0.3 dex. Our findings suggest that tidal threshing is a possible
formation mechanism of bright UCD populations in close proximity to giant
galaxies.
