Potential omega Cen associate EW

Stars that originated from the second generation of dissolved or dissolving clusters can be readily identified via distinct light-element signatures such as enhanced N and Na and simultaneously depleted C and O abundances. In this paper we present an extensive chemical abundance analysis of the halo star J110842, which was previously kinematically associated with the massive MW GC {omega} Centauri ({omega} Cen), and we discuss viable scenarios from escape to encounter.

Based on a high-resolution, high signal-to-noise spectrum of this star using the UVES spectrograph, we were able to measure 33 species of 31 elements across all nucleosynthetic channels. The star's low metallicity of [FeII/H]=2.10+/-0.02(stat.)+/-0.07(sys.) dex places it in the lower sixth percentile of {omega} Cen's metallicity distribution. We find that all of the heavier-element abundances, from - and Fepeak elements to neutron-capture elements are closely compatible with {omega} Cen's broad abundance distribution.