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Fig. 16

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Upper panel: [Y/Ba] vs. [Fe/H] for the four sample stars (blue filled squares) compared with literature abundances from Yong et al. (2014) for M 62 (magenta filled pentagons) and Bensby et al. (2013) for their stars older than 11 Gyr (green filled trianges). We also show chemical evolution model predictions for the bulge (see density scale in the colour bar at the bottom of the figure), where the contribution of both spinstars and magneto-rotationally driven (MRD) supernovae are taken into account (see Chiappini et al. 2014; Cescutti & Chiappini 2014; Cescutti et al. 2013). Lower panel: same as the upper panel, but now also showing the old abundance values (open blue squares) for the stars for which we have re-obtained better chemical abundances (filled blue squares). The dashed line in both panels corresponds to the r-process fractions, which were adopted from Sneden et al. (2008) for metal-poor r-element-rich stars. Note that in all panels we have excluded star B-108.

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