Fig. 5
Examples of spectral synthesis applied to different types of stars. Left panel: a cold giant star (Teff = 4815 K), with [Fe/H] and [C/Fe] close to the solar values; middle panel: a hot dwarf star (Teff = 6215 K), also with solar values for Fe and C abundance; and right panel: a Fe-poor ([Fe/H] = −0.31) dwarf star, for which both temperature and C abundance are close to solar. Other parameters are listed in Tables 4 and 6.
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