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We use a numerical simulation of a loose group containing a Milky Way halo toprobe that in the hierarchical universe the Magellanic Clouds and some dSphshave been accreted into the Milky Way halo from a late infalling group ofdwarfs. Our simulations show that the tidal breakup of the Magellanic groupoccurs before it enters the Milky Way halo. Only half of the satellitescontributed from the group are predicted to be inside the Milky Way virialradius. Half of its subhalos survive outside the current virial radius in theform of satellites, whereas the remaining material contributes to the diffuseMilky Way halo. At z~0 the disrupted group contributes less than 10% to theMilky Way halo mass but 20% of the brightest dwarf galaxies of the Milky Wayhave been part of this group. This scenario points out that some dSphs mighthave been form away from giant spirals and been accreted already as spheroids,by a late infall group in contrast with the classical picture of tidalstripping of dSph formation models. This would naturally explain severalpeculiarities of the local dSph: why Draco and the other luminous dSphs existcompared to other ultra-faint satellite galaxies, the location of Tucana andCetus in the outskirts of the Local Group and the mismatch in metallicitybetween the stellar halo of the Milky Way and the dwarf galaxies that many havesuspected dissolved to build it.

Breaking up the Magellanic Group into the Milky Way Halo: Understanding the Local Dwarf Galaxy Properties