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Fig. 2.


Cluster member selection for NGC 5946. The upper panel shows in red the stars selected on the basis of radial velocity criteria, while black dots represent non-members. The mean radial velocity derived from the selected stars is shown as a red dashed line. This value is ∼15 km s−1 lower than the radial velocity in the Harris (1996) catalogue (black dashed line). Lower panel: selection based on the line strength of the Ca II triplet lines. For member selection we used isoabundance lines with a fixed slope as in Saviane et al. (2012; dotted lines). The green dots are stars accepted as cluster members on the basis of both criteria. Only one radial-velocity member was excluded from the sample because of its line strength (red dot).

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