  During the last $\sim$ 30 Myr the nuclear stellar disk in the Galactic center
has been the most prolific star forming region of the Milky Way when averaged
by volume. Remarkably, the combined mass of the only three clusters present
today in the nuclear stellar disk adds up to only $\sim$10\% of the total
expected mass of young stars formed in this period. Several causes could
explain this apparent absence of clusters and stellar associations. The stellar
density in the area is so high that only the most massive clusters would be
detectable against the dense background of stars. The extreme tidal forces
reigning in the Galactic center could dissolve even the most massive of the
clusters in just a few Myr. Close encounters with one of the massive molecular
clouds, that are abundant in the nuclear stellar disk, can also rapidly make
any massive cluster or stellar association dissolve beyond recognition.
However, traces of some dissolving young clusters/associations could still be
detectable as co-moving groups. It is our aim to identify so far unknown
clusters or groups of young stars in the Galactic Center. We focus our search
on known, spectroscopically identified massive young stars to see whether they
can pinpoint such structures. We created an algorithm to detect over-densities
in the five-dimensional space spanned by proper-motion, position on the plane
of the sky and line-of-sight distances, using reddening as a proxy for the
latter. Since co-moving groups must be young in this environment, proper
motions provide a good means to search for young stars in the Galactic center.
We found four co-moving groups around massive stars, two of which are very
close in position and velocity to the Arches' most likely orbit
