  The metal line profiles of different ions observed in high HI column density
systems [N(HI) > 10^{16} cm^{-2}] in quasar spectra can be used to constrain
the ionization structure and kinematic characteristics of the absorbers. For
these purposes, a modified Monte Carlo Inversion (MCI) procedure was applied to
the study of three absorption systems in the spectrum of the HDF-South quasar
J2233-606 obtained with the UVES spectrograph at the VLT/Kueyen telescope. The
MCI does not confirm variations of metal abundances within separate systems
which were discussed in the literature. Instead, we found that an assumption of
a homogeneous metal content and a unique photoionizing background is sufficient
to describe the observed complex metal profiles. It was also found that the
linear size L and the line-of-sight velocity dispersion sigma_v measured within
the absorbers obey a scaling relation, namely, sigma_v increases with
increasing L, and that metal abundance is inversely proportional to the linear
size of the system: the highest metallicity was measured in the system with the
smallest L.
