EDP Sciences
Free access
Volume 566, June 2014
Article Number A37
Number of page(s) 30
Section Galactic structure, stellar clusters and populations
DOI http://dx.doi.org/10.1051/0004-6361/201323198
Published online 04 June 2014

Online material

thumbnail Fig. 1

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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Table 1

Intrinsic parameters and abundances for the current sample of classical Cepheids based on individual spectra.

Table 3

Mean NIR magnitudes, mean distances and mean iron abundances for the current sample of classical Cepheids.

Table 4

Galactic Cepheids for which the iron abundance was available in the literature.

Table 5

Individual ages, distances, and metallicities for the current sample of open clusters.

Table 6

Structural parameters and metallicities of the candidate Cepheid groups.

Table 7

Intrinsic parameters for field and cluster (NGC 1850, NGC 1866) Magellanic Cepheids with accurate iron abundances.

© ESO, 2014