  There is strong evidence that the mass in the Universe is dominated by dark
matter, which exerts gravitational attraction but whose exact nature is
unknown. In particular, all galaxies are believed to be embedded in massive
haloes of dark matter. This view has recently been challenged by surprisingly
low random stellar velocities in the outskirts of ordinary elliptical galaxies,
which were interpreted as indicating a lack of dark matter (Mendez et al. 2001;
Romanowsky et al. 2003). Here we show that the low velocities are in fact
compatible with galaxy formation in dark-matter haloes. Using numerical
simulations of disc-galaxy mergers, we find that the stellar orbits in the
outer regions of the resulting ellipticals are very elongated. These stars were
torn by tidal forces from their original galaxies during the first close
passage and put on outgoing trajectories. The elongated orbits, combined with
the steeply falling density profile of the observed tracers, explain the
observed low velocities even in the presence of large amounts of dark matter.
Projection effects when viewing a triaxial elliptical can lead to even lower
observed velocities along certain lines of sight.
