The projection factor of Cepheids

Details The projection factor of Cepheids The projection factor of Cepheids

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005sf2a.conf..307n&link_type=abstract

SF2A-2005: Semaine de l'Astrophysique Francaise, meeting held in Strasbourg, France, June 27 - July 1, 2005, Edited by F. Casoli

Astronomy and Astrophysics

Astrophysics

Scientific paper

The distance of galactic Cepheids can be derived through the interferometric Baade-Wesselink method. In this method, the projection factor which is the ratio of the pulsation velocity (Vpuls) to the radial velocity deduced from line profile position (Vrad) is of crucial importance. Using a geometric model, we compare different definitions of the radial velocity. The so-called barycentric velocity, which is independent of the FWHM of the line and the rotation, is certainly the most adapted for Cepheids distance determination. However, the projection factor remains sensible to velocity gradient effects. In Nardetto et al. (2004), we showed that the impact of velocity gradient on the average projection factor, and consequently on the final distance, is of the order of 6%. Here we find that spectro-interferometry can provide a new way to constrain directly the projection factor by observations.

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