  We consider the possibility that the Magellanic Clouds were the largest
members of a group of dwarf galaxies that entered the Milky Way (MW) halo at
late times. Seven of the eleven brightest satellites of the MW may have been
part of this system. The proximity of some dwarfs to the plane of the orbit of
the Large Magellanic Cloud (LMC) has been used to argue that they formed from
tidal debris from the LMC and Small Magellanic Cloud (SMC). Instead, they may
owe to the tidal breakup of the Magellanic Group. This can explain the
association of many of the dwarf galaxies in the Local Group with the LMC
system. It provides a mechanism for lighting up dwarf galaxies and reproduces
the bright end of the cumulative circular velocity distribution of the
satellites in the MW without invoking a stripping scenario for the subhalos to
match the satellite distribution expected according to CDM theory. Finally, our
model predicts that other isolated dwarfs will be found to have companions.
Evidence for this prediction is provided by nearby, recently discovered dwarf
associations.
