Fig. 2
Mass-metallicity relation from spectroscopy of individual stars (upper panel) and from gas-phase metallicities (lower panel) compared with the results from the LCID dwarfs. The gray line shows the fit obtained by Kirby et al. (2013; upper panel) and Berg et al. (2012; lower panel) in each case. For the LCID dwarfs, the [Fe/H] values have been converted into log (O/H) + 12 using a solar scale.
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