  The Next Generation Virgo Cluster Survey is a deep (with a $2\sigma$
detection limit $\mu_g$ = 29~mag~arcsec$^{-2}$ in the $g-$band) optical
panchromatic survey targeting the Virgo cluster from its core to virial radius,
for a total areal coverage of 104 square degrees. As such, the survey is well
suited for the study of galaxies' outskirts, haloes and low surface brightness
features that arise from dynamical interactions within the cluster environment.
We report the discovery of extremely faint ($\mu_g$ $>$ 25 mag arcsec$^{-2}$)
shells in three Virgo cluster early-type dwarf galaxies, VCC~1361, VCC~1447 and
VCC~1668. Among them, VCC~1447 has an absolute magnitude M$_{g}$ = -11.71 mag
and is {\it the least massive galaxy with a shell system discovered to date}.
We present a detailed study of these low surface brightness features. We detect
between three and four shells in each of our galaxies. Within the
uncertainties, we find no evidence of a color difference between the galaxy
main body and shell features. The observed arcs of the shells are located upto
several effective radii of the galaxies. We further explore the origin of these
low surface brightness features with the help of idealized numerical
simulations. We find that a near equal mass merger is best able to reproduce
the main properties of the shells, including their quite symmetric appearance
and their alignment along the major axis of the galaxy. The simulations provide
support for a formation scenario in which a recent merger, between two
near-equal mass, gas-free dwarf galaxies forms the observed shell systems.
