The Chemical Composition of Cepheids in the Milky Way and the Magellanic Clouds

Details The Chemical Composition of Cepheids in the Milky Way and the Magellanic Clouds The Chemical Composition of Cepheids in the Milky Way and the Magellanic Clouds

2005-10-18

arxiv.org/abs/astro-ph/0510514v1

Mem.Soc.Ast.It.77:156-159,2006

Astronomy and Astrophysics

Astrophysics

4 pages, 1 figure, to appear in the proceedings of the conference "Stellar Pulsation and Evolution", 2005. Monte Porzio Catone

Scientific paper

We have measured the elemental abundances of 68 Galactic and Magellanic Cepheids from FEROS and UVES high-resolution and high signal-to-noise spectra in order to establish the influence of the chemical composition on the properties of these stars (see Romaniello et al. 2005). Here we describe the robust analytical procedure we have developed to accurately determine them. The resulting iron abundances span a range between ~ -0.80 dex for stars in the Small Magellanic Cloud and ~ +0.20 dex for the most metal-rich ones in the Galaxy. While the average values for each galaxy are in good agreement with non-pulsating stars of similar age, Cepheids display a significant spread. Thus it is fundamental to measure the metallicity of individual stars.

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