This candidate binary cluster is located at the northwestern rim of the LMC bar. We use the CaII triplet in the spectra of individual red giants to derive radial velocities. In this sense the cluster pair may constitute a true binary cluster. We furthermore investigate the stellar densities in and around the star clusters and compare them with isopleths created from artificial, interacting as well as non-interacting star clusters.
Gravitational interaction leads to a distortion which can also be found in the observed pair.