Fig. 15.

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Comparison between Li observations and theoretical Li isochrones as a function of Teff in different [Fe/H] bins. Blue and red isochrone lines and data points correspond to two age ranges, 10 ± 1 and 12 ± 1 Gyr respectively. Circles and arrows correspond to Li abundance determinations and upper limits respectively. Error bars show mean Teff and A(Li) uncertainty of stars in a given bin. Top and bottom: N23 and GALAH sample stars respectively. In the upper left panel, we show the position of the star most Fe-poor dwarf of our sample, J0023+037, with the Li and Teff values from N23 (red five-pointed star) and from Aguado et al. (2019, green five-pointed star), with the theoretical Li-isochrones for the corresponding [Fe/H] = −5 to 8 dex models.
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