Fourier method of determining the rotational velocities in OB stars ^*,**

¹ Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain e-mail: sergio.simon-diaz@obspm.fr
² LUTh, Observatoire de Meudon, 92195 Meudon Cedex, France
³ Departamento de Astrofísica, Universidad de La Laguna, 38071 La Laguna, Spain

Received: 18 July 2006
Accepted: 6 March 2007

Abstract

Aims.We present a comprehensive study that applies the Fourier transform to a sample of O and early B-type stars (either dwarfs, giants, or supergiants) to determine their projected rotational velocities. We then compare them with previous values obtained with other methods and seek evidence of extra broadening in the spectral lines

Methods.The Fourier technique, extensively used in the study of cooler stars, has only been marginally applied to early-type stars. The comparison of  values obtained through the ft and FWHM  methods shows that the FWHM technique must be used with care in the analysis of OB giants and supergiants and when it is applied to lines. In contrast, the ft method appears to be a powerful tool for deriving reliable projected rotational velocities and separating the effect of rotation from other broadening mechanisms present in these stars.

Results.The analysis of the sample of OB stars shows that while dwarfs and giants display a broad range of projected rotational velocities, from less than 30 up to 450 km s^-1, supergiants have in general values close to or below 100 km s^-1. The analysis has also definitely shown that, while the effect of extra broadening is negligible in OB dwarfs, it is clearly present in supergiants. When examining the behavior of the projected rotational velocities with the stellar parameters and across the HR diagram, we conclude, in agreement with previous researchers, that the rotational velocity should decrease when the stars evolve. On the contrary, macroturbulence may be constant, therefore resulting in an increasing importance as compared to rotation when the stars evolve.