High-resolution (R ~ 38 000) UVES spectra of solar metallicity Galactic Cepheid RY Sco ([Fe/H] = 0.01 ± 0.06). From top to bottom the spectra were plotted for increasing pulsational phase (see the corresponding Teff curve in Fig. 3). The S/N of this sample is around 100 in the spectral range λ ~ 5650–7500 Å. The vertical dashed lines display selected Fe I (λλ5930.17, 5934.66, 5952.73, 5956.7, 5975.35, 5976.78, 5983.69, 5984.79, 5987.05, 5997.78 Å) and Fe II (λλ5932.06, 5991.37 Å) lines included in our abundance analysis (see Table 1 and Romaniello et al. 2008).
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