  Recently it has been shown that a large fraction of the dwarf satellite
galaxies orbiting the Andromeda galaxy are surprisingly aligned in a thin,
extended and kinematically coherent planar structure. The presence of such a
structure seems to challenge the current Cold Dark Matter paradigm of structure
formation, which predicts a more uniform distribution of satellites around
central objects. We show that it is possible to obtain a thin, extended,
rotating plane of satellites resembling the one in Andromeda in cosmological
collisionless simulations based on the Cold Dark Matter model. Our new high
resolution simulations show a correlation between the formation time of the
dark matter halo and the thickness of the plane of satellites. Our simulations
have a high incidence of satellite planes as thin, extended, and as rich as the
one in Andromeda and with a very coherent kinematic structure when we select
high concentration/early forming halos. By tracking the formation of the
satellites in the plane we show that they have been mainly accreted onto the
main object along thin dark matter filaments at high redshift. Our results show
that the presence of a thin, extended, rotating plane of satellites is not a
challenge for the Cold Dark Matter paradigm, but actually supports one of the
predictions of this paradigm related to the presence of filaments of dark
matter around galaxies at high redshift.
