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Fig. 5

image

Average abundance trends from Fig. 4 given by the (green) bullets with the abundances of the coadded group-spectra overplotted. In both panels, predictions from stellar structure models including atomic diffusion with additional mixing with different efficiencies are overplotted. The dashed horizontal lines represent the initial abundances of the models, which have been adjusted so that predictions match the observed abundance level at the cool end of the Teff scale.

This figure is made of several images, please see below:

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