  We use a numerical simulation of a loose group containing a Milky Way halo to
probe that in the hierarchical universe the Magellanic Clouds and some dSphs
have been accreted into the Milky Way halo from a late infalling group of
dwarfs. Our simulations show that the tidal breakup of the Magellanic group
occurs before it enters the Milky Way halo. Only half of the satellites
contributed from the group are predicted to be inside the Milky Way virial
radius. Half of its subhalos survive outside the current virial radius in the
form of satellites, whereas the remaining material contributes to the diffuse
Milky Way halo. At z~0 the disrupted group contributes less than 10% to the
Milky Way halo mass but 20% of the brightest dwarf galaxies of the Milky Way
have been part of this group. This scenario points out that some dSphs might
have been form away from giant spirals and been accreted already as spheroids,
by a late infall group in contrast with the classical picture of tidal
stripping of dSph formation models. This would naturally explain several
peculiarities of the local dSph: why Draco and the other luminous dSphs exist
compared to other ultra-faint satellite galaxies, the location of Tucana and
Cetus in the outskirts of the Local Group and the mismatch in metallicity
between the stellar halo of the Milky Way and the dwarf galaxies that many have
suspected dissolved to build it.
