  Aims: To determine the metallicities of 113 Southern Hemisphere Vega-like
candidate stars in relation to the Exoplanet host group and field stars.
  Methods: We applied two spectroscopic methods of abundance determinations:
equivalent width measurements together with the ATLAS9 (Kurucz 1993) model
atmospheres and the WIDTH9 program, and a comparison of observed spectra with
the grid of synthetic spectra of Munari et al. (2005).
  Results: For the Vega-like group, the metallicities are indistinguishable
from those of field stars not known to be associated with planets or disks.
This result is quite different from the metallicities of Exoplanet host stars
which are metal-rich in comparison to field stars.
