A MUSE view of the multiple populations’ chemistry in Galactic Globular Clusters

Stars in Galactic globular clusters are known to exhibit abundance variations in specific elements such as He, C, N, O, Na, and Al. These variations can be observed via spectroscopy but also photometrically by using CMD constructed with various filter combinations. Although these multiple populations have been, and still are, the subject of many investigations, the origin of their elemental abundance variations remain rather mysterious.
I will present some of our recent results on that topic based on the spectroscopic survey of 26 globular clusters that is currently carried out as part of the MUSE GTO time. With the MUSE survey covering the central regions of the clusters for which HST photometry is available, we can use these photometric catalogs to separate the RGB stars into two or more populations based on their position in the pseudo-two-color diagrams. Although the MUSE spectra are of relatively low-resolution (R ~ 2500), by combining the spectra of the stars within a distinct populations, we are able to study their abundance variations and relate them directly with the populations distinguished on the pseudo-two-color diagrams.