Automated spectroscopic abundances of A and F-type stars using echelle spectrographs

Using the method presented in Erspamer & North (2002, hereafter Paper I), detailed abundances of 140 stars are presented. The uncertainties characteristic of this method are presented and discussed. In particular, we show that for a ratio higher than 200, the method is applicable to stars with a rotational velocity as high as 200 . There is no correlation between abundances and , except a spurious one for Sr, Sc and Na which we explain by the small number of lines of these elements combined with a locally biased continuum. Metallic giants (Hauck 1986) show larger abundances than normal giants for at least 8 elements: Al, Ca, Ti, Cr, Mn, Fe, Ni and Ba. The anticorrelation for Na, Mg, Si, Ca, Fe and Ni with suggested by Varenne & Monier (1999) is not confirmed. The predictions of the Montréal models (e.g. Richard et al. 2001) are not fulfilled in general. However, a correlation between and is found for stars of 1.8 to 2.0 . Various possible causes are discussed, but the physical reality of this correlation seems inescapable.