Fig. 10
υsini as a function of temperature for our solar metallicity slow rotating models with masses from 3 to 5 M⊙ and for a fast rotator of 3.5 M⊙. The colour of the data points refers to each individual wGb star in our sample as specified in Table 1. The colour of the tracks indicates the evolutionary phase: green for subgaint and RGB phases, blue for clump.
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