  We find that satellites of isolated disk galaxies at projected radii between
300 and 500 kpc are distributed asymmetrically about the parent galaxy and
aligned preferentially with the disk minor axis. The dynamical timescale at
these radii is sufficiently long that the shape of this distribution must
reflect the formation history of the outer halo rather than its internal
evolution. We also find that the orbital angular momenta of satellites at
projected major axis distances of $\ltsim$ 200 kpc tend to align with that of
the central disk. These results demonstrate that satellites are dynamically
related to their primary galaxy. Satellites drawn from current simulations of
hierarchical galaxy formation exhibit neither the systematic alignment nor the
net rotation with the central disk that we find in the data.
