Tidal tails in open clusters

We used N-body simulations to visualize and compare the observables with real data. Further analysis was done on the detected cluster and tail stars to study their internal dynamics and populations, including binary fraction. We also applied the residual velocity method to detect rotational patterns in the clusters and their tails.

We identified tidal tails in all five clusters, with detected tails extending farther in some clusters and containing significantly more stars than previously reported (tails ranging from 40 to 100pc, one to four times the Jacobi radius, with 100-200 tail stars). The luminosity functions of the tails and their parent clusters were generally consistent, and tails lacked massive stars. In general, the binary fraction was found to be higher in the tidal tails.

Significant rotation was detected in M67 and NGC 2281 for the first time.