A Spectroscopic Survey for Omega Centauri Members at and beyond the Cluster Tidal Radius

TL;DR

This spectroscopic survey of omega Centauri aimed to detect extra-tidal members and assess the extent of tidal debris, finding minimal evidence for significant extra-tidal populations and constraining the cluster's tidal disruption history.

Contribution

The study provides the first large-scale spectroscopic analysis of omega Centauri's outer regions, setting limits on the amount of mass beyond the tidal radius and informing models of its origin.

Findings

Less than 0.7% of cluster mass is beyond the tidal radius.

No significant extra-tidal population detected.

Results support early tidal stripping in omega Centauri's history.

Abstract

We have used the two-degree field (2dF) multi-fibre spectrograph of the Anglo-Australian Telescope to search for candidate members of the unusual globular cluster omega Centauri at and beyond the cluster tidal radius. Velocities with an accuracy of ~10 kms-1 were obtained for 4105 stars selected to lie in the vicinity of the lower giant branch in the cluster colour-magnitude diagram and which cover an area on the sky of ~2.4x3.9 deg2 centered on the cluster. Within the velocity interval 190-270 kms-1, the cluster member candidates have a steeply declining surface density distribution consistent with the adopted tidal radius of 57`. For stars in the sample beyond the tidal radius, an analysis of line-strengths from the spectra, as well as radial velocities, identifies only six stars as possible candidates for extra-tidal association with the cluster. If all six of these stars are indeed related to the cluster, then a maximum of 0.7 +/- 0.2 per cent of the total cluster mass is contained in the region between one and two tidal radii. Given this limit, we conclude that there is no compelling evidence for any significant extra-tidal population in omega Cen. The effects of tidal shocks on the outer parts of the cluster are consistent with this limit. Theories for the origin of omega Cen frequently suggest that the cluster is the former nucleus of a tidally stripped dwarf galaxy. Our results require that the stripping process must have been largely complete at early epochs, consistent with dynamical models of the process. The stripped former dwarf galaxy stars are therefore now widely distributed around the Galaxy.