2021MNRAS.507.1127K

The peripheral regions of globular clusters (GCs) are extremely challenging to study due to their low surface brightness nature and the dominance of Milky Way contaminant populations along their sightlines. We have developed a probabilistic approach to this problem through utilizing a mixture model in spatial and proper motion space that separately models the cluster, extra-tidal, and contaminant stellar populations. We demonstrate the efficacy of our method through application to Gaia third early data release photometry and astrometry in the direction of NGC 5139 (ω Centauri, hereafter ω Cen), a highly challenging target on account of its Galactic latitude (b ≃ 15^*) and low proper motion contrast with the surrounding field. We recover the spectacular tidal extensions, spanning the 10^* on the sky explored here, seen in earlier work and quantify the star count profile and ellipticity of the system out to a cluster-centric radius of 4^*. We show that both RR Lyrae and blue horizontal branch stars consistent with belonging to ω Cen are found in the tidal tails, and calculate that these extensions contain at least ≃0.1 per cent of the total stellar mass in the system. Our high-probability members provide prime targets for future spectroscopic studies of ω Cen out to unprecedented radii.