On the physical size of the Milky Way globular cluster NGC 7089 (M2)

We study the outer regions of the Milky Way globular cluster NGC 7089 based on new Dark Energy Camera observations. The resulting background-cleaned stellar density profile reveals the existence of an extended envelope. We confirm previous results that cluster stars are found out up to similar to 1 degrees from the cluster's centre, which is nearly three times the value of the most robust tidal radii estimations. We also used results from direct N-body simulations in order to compare with the observations. We found a fairly good agreement between the observed and numerically generated stellar density profiles. Because of the existence of gaps and substructures along globular cluster tidal tails, we closely examined the structure of the outer cluster region beyond the Jacobi radius. We extended the analysis to a sample of 35 globular clusters, 20 of them with observed tidal tails. We found that if the stellar density profile follows a power law proportional to r(-alpha), the alpha slope correlates with the globular cluster present mass, in the sense that, the more massive the globular cluster, the smaller the alpha value. This trend is not found in globular clusters without observed tidal tails. The origin of such a phenomenon could be related, among other reasons, to the proposed so-called potential escapers or to the formation of globular clusters within dark matter minihaloes.

Automated summary

This study investigates the outer regions of the Milky Way globular cluster NGC 7089 using new Dark Energy Camera observations. The analysis reveals the presence of an extended envelope and confirms previous findings regarding the distribution of cluster stars. The results also show a correlation between the slope of the stellar density profile and the mass of the globular cluster.