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During the last $\sim$ 30 Myr the nuclear stellar disk in the Galactic centerhas been the most prolific star forming region of the Milky Way when averagedby volume. Remarkably, the combined mass of the only three clusters presenttoday in the nuclear stellar disk adds up to only $\sim$10\% of the totalexpected mass of young stars formed in this period. Several causes couldexplain this apparent absence of clusters and stellar associations. The stellardensity in the area is so high that only the most massive clusters would bedetectable against the dense background of stars. The extreme tidal forcesreigning in the Galactic center could dissolve even the most massive of theclusters in just a few Myr. Close encounters with one of the massive molecularclouds, that are abundant in the nuclear stellar disk, can also rapidly makeany massive cluster or stellar association dissolve beyond recognition.However, traces of some dissolving young clusters/associations could still bedetectable as co-moving groups. It is our aim to identify so far unknownclusters or groups of young stars in the Galactic Center. We focus our searchon known, spectroscopically identified massive young stars to see whether theycan pinpoint such structures. We created an algorithm to detect over-densitiesin the five-dimensional space spanned by proper-motion, position on the planeof the sky and line-of-sight distances, using reddening as a proxy for thelatter. Since co-moving groups must be young in this environment, propermotions 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 veryclose in position and velocity to the Arches' most likely orbit

Co-moving groups around massive stars in the Nuclear Stellar Disk