Fig. 10
a) Comparison of spectroscopic metallicities obtained in the infrared (this work) versus in the optical (Marino et al. 2009) for s-poor (open circles) and s-rich (filled circles) stars. Typical uncertainties are shown.b) [Fe/H] residuals (ours minus optical values), where the dashed lines represent 1σ scatter over the mean value found (full line).
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