  We explore the signatures that a binary intermediate mass black hole (IMBH)
imprints on the velocity and on the angular momentum of globular cluster stars.
Simulating 3-body encounters between a star and a binary IMBH, we find that the
binary IMBH generates a family of few hundreds of stars (~100-300) which remain
bound to the globular cluster (GC) and have velocity significantly higher than
the dispersion velocity. For this reason we term them ''supra-thermal'' stars.
We also notice that, after the interaction, a considerable fraction (55-70%) of
stars tend to align their orbital angular momentum with the angular momentum of
the binary IMBH, introducing an anisotropy in the angular momentum distribution
of cluster stars. We simulate the dynamical evolution of these supra-thermal
stars before thermalization, and find that these stars tend to cluster at a
distance of few core radii from the GC center. We conclude that the
detectability of such signatures appears problematic with present telescopes.
