MARINO, AnnaAnnaMARINOMilone, A. P.A. P.MiloneRenzini, A.A.RenziniYong, D.D.YongAsplund, M.M.AsplundDa Costa, G. S.G. S.Da CostaJerjen, H.H.JerjenCordoni, G.G.CordoniCarlos,M.CarlosDondoglio, E.E.DondoglioLagioia, E. P.E. P.LagioiaJang, S.S.JangTailo, M.M.Tailo2023-09-132023-09-1320210004-637Xhttp://hdl.handle.net/20.500.12386/34390Recent work has revealed two classes of Globular Clusters (GCs), dubbed Type-I and Type-II. Type-II GCs are characterized by a blue- and a red- red giant branch composed of stars with different metallicities, often coupled with distinct abundances in the slow-neutron capture elements (s-elements). Here we continue the chemical tagging of Type-II GCs by adding the two least-massive clusters of this class, NGC1261 and NGC6934. Based on both spectroscopy and photometry, we find that red stars in NGC1261 are slightly enhanced in [Fe/H] by ~0.1 dex and confirm that red stars of NGC 6934 are enhanced in iron by ~0.2 dex. Neither NGC1261 nor NGC6934 show internal variations in the s-elements, which suggests a GC mass threshold for the occurrence of s-process enrichment. We found a significant correlation between the additional Fe locked in the red stars of Type-II GCs and the present-day mass of the cluster. Nevertheless, most Type II GCs retained a small fraction of Fe produced by SNe II, lower than the 2%; NGC6273, M54 and omega Centauri are remarkable exceptions. In the appendix, we infer for the first time chemical abundances of Lanthanum, assumed as representative of the s-elements, in M54, the GC located in the nucleus of the Sagittarius dwarf galaxy. Red-sequence stars are marginally enhanced in [La/Fe] by 0.10\pm0.06 dex, in contrast with the large [La/Fe] spread of most Type II GCs. We suggest that different processes are responsible for the enrichment in iron and s-elements in Type-II GCs.STAMPAenArticle10.3847/1538-4357/ac282c2-s2.0-85121785832https://iopscience.iop.org/article/10.3847/1538-4357/ac282chttp://arxiv.org/abs/2106.15978v1FIS/05 - ASTRONOMIA E ASTROFISICA