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We present high-precision multi-band photometry for the globular cluster (GC)M2. We combine the analysis of the photometric data obtained from the HubbleSpace Telescope UV Legacy Survey of Galactic GCs GO-13297, with chemicalabundances by Yong et al.(2014), and compare the photometry with models inorder to analyze the multiple stellar sequences we identified in thecolor-magnitude diagram (CMD). We find three main stellar components, composedof metal-poor, metal-intermediate, and metal-rich stars (hereafter referred toas population A, B, and C, respectively). The components A and B include starswith different $s$-process element abundances. They host six sub-populationswith different light-element abundances, and exhibit an internal variation inhelium up to Delta Y~0.07 dex. In contrast with M22, another clustercharacterized by the presence of populations with different metallicities, M2contains a third stellar component, C, which shows neither evidence forsub-populations nor an internal spread in light-elements. Population C does notexhibit the typical photometric signatures that are associated with abundancevariations of light elements produced by hydrogen burning at hot temperatures.We compare M2 with other GCs with intrinsic heavy-element variations andconclude that M2 resembles M22, but it includes an additional stellar componentthat makes it more similar to the central region of the Sagittarius galaxy,which hosts a GC (M54) and the nucleus of the Sagittarius galaxy itself.

The Hubble Space Telescope UV Legacy Survey of Galactic Globular Clusters. II. The seven stellar populations of NGC7089 (M2)