A Formation Scenario for the Disk of Satellites: Accretion of Satellites
  during Mergers
  The Disk of Satellites (DoS) observed in the Andromeda galaxy is a thin and
extended group of satellites, nearly perpendicular to the disk plane, that
share a common direction of rotation about the centre of Andromeda. Although a
DoS is also observed in the Milky Way galaxy, the prevalance of such structures
in more distant galaxies remains controversial. Explanations for the formation
of such DoSs vary widely from filamentary infall, or flattening due to the
potential field from large scale structure, to galaxy interactions in a Mondian
paradigm. Here we present an alternative scenario -- during a merger, a galaxy
may bring its own satellite population when merging with another galaxy. We
demonstrate how, under the correct circumstances, during the coalescence of the
two galaxies, the satellite population can be spread into an extended,
flattened structure, with a common direction of rotation about the merger
remnant. We investigate the key parameters of the interaction, and the
satellite population, that are required to form a DoS in this scenario.
