Volume 518, July-August 2010Herschel: the first science highlights
|Number of page(s)||9|
|Section||Stellar structure and evolution|
|Published online||20 August 2010|
New Baade-Wesselink distances and radii for four metal-rich Galactic Cepheids*
European Southern Observatory (ESO), Karl-Schwarzschild-Strasse 2, 85748 Garching bei München, Germany e-mail: firstname.lastname@example.org
2 Università di Roma Tor Vergata, via della Ricerca Scientifica 1, 00133 Roma, Italy
3 Kapteyn Institute, University of Groningen, PO Box 800, 9700 AV Groningen, The Netherlands
4 Royal Observatory of Belgium, Ringlaan 3, 1180 Brussels, Belgium
5 INAF – Osservatorio Astronomico di Roma, via Frascati 33, Monte Porzio Catone, Italy
6 South African Astronomical Observatory, PO Box 9, 7935 Observatory, South Africa
7 Observatoire de Paris-Meudon, GEPI, 61 avenue de l'Observatoire, 75014 Paris, France
8 ASI–Science Data Center, ASDC c/o ESRIN, via G. Galilei, 00044 Frascati, Italy
9 Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
Accepted: 12 March 2010
Aims. We provide accurate estimates of distances, radii, and iron abundances of four metal-rich Cepheids, namely V340 Ara, UZ Sct, AV Sgr, and VY Sgr. The main aim of this investigation is to constrain their pulsation properties and their location across the Galactic inner disk.
Methods. We adopted new accurate NIR (J,H,K) light curves and new radial velocity measurements for the target Cepheids to determinate their distances and radii using the Baade-Wesselink technique. In particular, we adopted the most recent calibrations of both the IR surface brightness relation and the projection factor. We also provide accurate measurements of the iron abundance of the target Cepheids.
Results. Current distance estimates agree to within one σ with similar distances based on either empirical or theoretical NIR Period-Luminosity (P-L) relations. However, the uncertainties in the Baade-Wesselink distances are on average a factor of 3–4 smaller than errors affecting other distance determinations. Mean Baade-Wesselink radii also agree at the one σ level with Cepheid radii based either on empirical or theoretical Period-Radius relations. Iron abundances are, within one σ, similar to those determined by Andrievsky and collaborators, thus confirming that the target Cepheids are super metal-rich. We also found that the luminosity amplitudes of classical Cepheids, at odds with RR Lyrae stars, do not exhibit a clear correlation with their metal content. This circumstantial evidence appears to be caused by the Hertzsprung progression and the dependence of the topology of the instability strip on metallicity, evolutionary effects, and binaries.
Key words: stars: abundances / stars: distances / stars: variables: Cepheids / Galaxy: disk / stars: oscillations
© ESO, 2010
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