Astronomy & Astrophysics

Table of contents

A&A 453, 309-319 (2006)
DOI: 10.1051/0004-6361:20054333

High resolution spectroscopy for Cepheids distance determination

I. Line asymmetry

N. Nardetto¹, D. Mourard¹, P. Kervella², Ph. Mathias¹, A. Mérand² and D. Bersier^{3, 4}

¹ Observatoire de la Côte d'Azur, Dept. Gemini, UMR 6203, 06130 Grasse, France
e-mail: Nicolas.Nardetto@obs-azur.fr
² Observatoire de Paris-Meudon, LESIA, UMR 8109, 5 place Jules Janssen, 92195 Meudon Cedex, France
³ Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
⁴ Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead, CH41 1LD, UK

(Received 11 October 2005 / Accepted 11 March 2006)

Abstract
Context.The ratio of pulsation to radial velocity (the projection factor) is currently limiting the accuracy of the Baade-Wesselink method, and in particular of its interferometric version recently applied to several nearby Cepheids.
Aims.This work aims at establishing a link between the line asymmetry evolution over the Cepheids' pulsation cycles and their projection factor, with the final objective to improve the accuracy of the Baade-Wesselink method for distance determinations.
Methods.We present HARPS high spectral resolution observations ( $R=120\,000$ ) of nine galactic Cepheids: R Tra , S Cru , Y Sgr , $\beta$ Dor , $\zeta$ Gem , Y Oph , RZ Vel , $\ell$ Car and RS Pup , having a good period sampling (P=3.39d to P=41.52d). We fit spectral line profiles by an asymmetric bi-Gaussian to derive radial velocity, Full-Width at Half-Maximum in the line (FWHM) and line asymmetry for all stars. We then extract correlations curves between radial velocity and asymmetry. A geometric model providing synthetic spectral lines, including limb-darkening, a constant FWHM (hereafter $\sigma_{\rm C}$ ) and the rotation velocity is used to interpret these correlations curves.
Results.For all stars, comparison between observations and modelling is satisfactory, and we were able to determine the projected rotation velocities and $\sigma_{\rm C}$ for all stars. We also find a correlation between the rotation velocity ( $V_{\rm rot} \sin i$ ) and the period of the star: $V_{\rm rot} \sin i= (-11.5 \pm 0.9) \log\,(P) + (19.8 \pm 1.0)$ [ km s^-1] . Moreover, we observe a systematic shift in observational asymmetry curves (noted $\gamma_{\rm O}$ ), related to the period of the star, which is not explained by our static model: $\gamma_{\rm O}=(-10.7 \pm 0.1) \log\,(P) + (9.7 \pm 0.2) \mbox{ [in \%]}$ . For long-period Cepheids, in which velocity gradients, compression or shock waves seem to be large compared to short- or medium-period Cepheids we observe indeed a greater systematic shift in asymmetry curves.
Conclusions.This new way of studying line asymmetry seems to be very promising for a better understanding of Cepheids atmosphere and to determine, for each star, a dynamic projection factor.

Key words: techniques: spectroscopic -- stars: atmospheres -- stars: oscillations -- stars: variables: Cepheids -- stars: distances