The ESO-NTT set-up as described in Gelbmann et al. (1997) was used for the observations and all subsequent reductions, merging of echelle orders to one continuous spectrum and normalization to the continuum were done with IRAF and are referred to as "low resolution spectra" in this paper. The Abundance Analysis Procedure software package AAP (Gelbmann 1995) was used to derive the basic stellar parameters and abundance pattern. If not mentioned otherwise, all procedures were the same as described in our series of Paper I to Paper IV.
An additional high resolution spectrum (ESO CAT-CES instrument, R = 122000) ranging from 6123 to 6178 Å which shows resolved Zeeman components was available. This spectrum is an average of six individual spectra which were observed almost at the same phase and close to magnetic maximum and they are described in Mathys et al. (1997).
© European Southern Observatory (ESO) 2000
Online publication: March 28, 2000