The influence of chemical composition on the properties of Cepheid stars

Free access article

Issue		A&A Volume 429, Number 2, January II 2005


Page(s)		L37 - L40
Section		Letters
DOI		http://dx.doi.org/10.1051/0004-6361:200400110

A&A 429, L37-L40 (2005)
DOI: 10.1051/0004-6361:200400110

Letter

I. Period-Luminosity relation vs. iron abundance

M. Romaniello¹, F. Primas¹, M. Mottini¹, M. Groenewegen², G. Bono³ and P. François⁴

¹ European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching bei München, Germany
e-mail: mromanie@eso.org
² Instituut voor Sterrenkunde, PACS - ICC, Celestijnenlaan 200B, 3001 Leuven, Belgium
³ INAF - Osservatorio Astronomico di Roma, via di Frascati 33, 00040 Monte Porzio Catone, Italy
⁴ Observatoire de Paris-Meudon, GEPI, 61 avenue de l'Observatoire, 75014 Paris, France

(Received 11 October 2004 / Accepted 20 November 2004)

Abstract
We have assessed the influence of the stellar iron content on the Cepheid Period-Luminosity ( PL) relation by relating the V band residuals from the Freedman et al. (2001) PL relation to [Fe/H] for 37 Galactic and Magellanic Clouds Cepheids. The iron abundances were measured from FEROS and UVES high-resolution and high-signal to noise optical spectra. Our data indicate that the stars become fainter as metallicity increases, until a plateau or turnover point is reached at about solar metallicity. Our data are incompatible with both no dependence of the PL relation on iron abundance, and with the linearly decreasing behavior often found in the literature (e.g. Kennicutt et al. 1998; Sakai et al. 2004). On the other hand, non-linear theoretical models of Fiorentino et al. (2002) provide a fairly good description of the data.

Key words: stars: abundances -- stars: distances -- Cepheids

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