  Wide or fragile pairs are sensitive probes of the galactic potential, and
they have been used to provide information about the galactic tidal field, the
density of GMC and the masses of dark matter perturbers present in both the
disk and the halo. Halo wide binaries and moving clusters, since they are
likely to be the remains of past mergers or of dissolved clusters, can provide
information on the dynamical and merger history of our Galaxy. Such remnants
should continue to show similar motions over times of the order of their ages.
We have looked for phase space groupings among the low-metallicity stars of
Schuster et al. (2006) and have identified a number of candidate moving
clusters. In several of the moving clusters we found a wide CPM binary already
identified in our catalogue of wide binaries among high-velocity and metal-poor
stars (Allen et al 2000a). Spectroscopic follow-up studies of these stars would
confirm the physical reality of the groups, as well as allow us to distinguish
whether their progenitors are dissolved clusters or accreted extragalactic
systems
