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 Ly \alpha systems found at z = 1.920 and z = 2.076 .
For the z = 1.920 system , we measure accurate abundances ( relative to solar ) for Fe , Cr Si , Ni , Ti , and Zn : [ Fe/H ] = -0.705 \pm 0.097 , [ Cr/H ] = -0.580 \pm 0.100 , [ Si/H ] = -0.402 \pm 0.098 , [ Ni/H ] = -1.012 \pm 0.095 , [ Ti/H ] = -0.776 \pm 0.081 , and [ Zn/H ] = -0.379 \pm 0.097 .
This system exhibits the highest metallicity we have measured for a damped Ly \alpha system .
By contrast the z = 2.076 system is the most metal poor ( [ Zn/H ] < -1.745 ) we have analyzed , showing absorption features for only the strongest transitions .
We determine accurate abundances for Fe , Si and Al : [ Fe/H ] = -2.621 \pm 0.071 , [ Si/H ] = -2.225 \pm 0.075 , and [ Al/H ] = -2.727 \pm 0.070 .

Analyses of the abundance variations of Fe , Ni , Cr , and Si relative to Zn and the abundance trends versus condensation temperature do not offer positive evidence for the presence of dust in the damped system at z = 1.920 .
In addition , the relative abundance ratio [ Ti/Fe ] \approx 0 further suggests the absence of ISM-like dust .
Unfortunately , the lack of measurable Zn absorption in the z = 2.076 system does not allow a similar investigation for the presence of dust .

In addition to the significant difference in metallicity , the two damped systems have vastly different kinematic characteristics .
The z = 1.920 system spans \approx 150 km s ^ { -1 } in velocity space ( measured from the low-ion transitions ) while the z = 2.076 system spans a mere 30 km s ^ { -1 } .
Furthermore , the z = 1.920 profiles are significantly asymmetric while the z = 2.076 profiles are highly symmetric .
Even with these differences , we contend the two systems are consistent with one physical description , that of a thick , rotating disk .

In addition to the two previously identified damped Ly \alpha systems , we investigate a very strong Mg II system at z = 0.752 which is very likely yet a third damped Ly \alpha system along the line of sight .
The very weak Mn II 2606 , 2594 , 2576 and Ti II 3073 , 3342 , and 3384 transitions have been positively measured and suggest a very conservative lower limit H I abundance of \log { N ( { HI } ) } > 19.0 assuming metallicity relative to solar equal to 0 and no depletion .
Together with the damped system at z = 1.920 , this marks the first confident ( > 5 \sigma ) detection of Ti in QSO absorption line systems .
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 ( [ 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 km s ^ { -1 } and 8.9 km s ^ { -1 } for Si IV and C IV respectively ) for this component suggest a temperature of 4.7 { \times 10 ^ { 4 } } K .
Because collisional ionization can explain the observed abundances only for T > 8 { \times 10 ^ { 4 } } K , we contend these ions must have formed through a different physical process ( e.g .
photoionization ) .