  We present high resolution, high SNR spectra of the QSO Q2206-199 obtained
with HIRES on the 10m W.M. Keck Telescope. Our analysis focuses on the two
previously identified damped \lya systems found at $z=1.920$ and $z=2.076$. For
each system, we measure accurate abundances. The $z=1.920$ system exhibits the
highest metallicity we have measured for a damped \lya system. We report the
first confident ($>5 \sigma$) detection of Ti in a QSO absorption line system.
By contrast the $z=2.076$ system is the most metal poor we have analyzed,
showing absorption features for only the strongest transitions. We find no
positive evidence for the presence of dust in either system. The two damped
systems exhibit significantly different kinematic characteristics, yet we
contend the two systems are consistent with one physical description: that of a
thick, rotating disk.
  We investigate a very strong Mg II system at $z=0.752$ which is very likely
yet a third damped \lya system. The very weak Mn II and Ti II transitions have
been positively measured and imply $\log \N{HI} > 19.0$. We analyze the
abundance ratios [Mn/Fe] and [Ti/Fe] and their values are inconsistent with
dust depletion, yet consistent with the abundance pattern detected for halo
stars in the Galaxy (see Lu et al. 1996a).
  Finally, we identify a C IV system at $z=2.014$ that shows a very narrow
feature in Si IV and C IV absorption. The corresponding $b$ values (5.5 \kms
and 8.9 \kms for Si IV and C IV) for this component suggest a temperature of
$4.7 \sci{4} \rm K$. Because collisional ionization can explain the observed
abundances only for $T > 8 \sci{4} \rm K$, we contend these ions must have
formed through a different physical process (e.g. photoionization).
