  We show that dissipative dark matter can potentially explain the large
observed mass to light ratio of the dwarf satellite galaxies that have been
observed in the recently identified planar structure around Andromeda, which
are thought to result from tidal forces during a galaxy merger. Whereas dwarf
galaxies created from ordinary disks would be dark matter poor, dark matter
inside the galactic plane not only provides a source of dark matter, but one
that is more readily bound due to the dark matter's lower velocity. This
initial N-body study shows that with a thin disk of dark matter inside the
baryonic disk, mass-to-light ratios as high as O(30) can be generated when
tidal forces pull out patches of sizes similar to the scales of Toomre
instabilities of the dark disk. A full simulation will be needed to confirm
this result.
