  The combination of STIS and optical spectroscopy with STIS imaging of the
field surrounding J2233-606 afford a unique opportunity to study the physical
nature of the Quasar Absorption Line systems. We present an analysis of the
ionization state, chemical abundances, and kinematic characteristics of two
metal-line systems at z=1.92 and z=1.94 toward J2233-606. We focus on these two
systems because (i) the observations provide full coverage of the Lyman series,
hence an accurate determination of their HI column densities and (ii) the
metal-line transitions allow a measurement of their ionization state.
  Line-profile fits of the Lyman series for the two systems indicate log N(HI)
= 17.15 \pm 0.02 cm^-2 evenly distributed between two components for the z=1.92
system and log N(HI) = 16.33 \pm 0.04 cm^-2 for the z=1.94 system. By comparing
observed ionic ratios of C and Si against calculations performed with the
CLOUDY software package, we find the ionization state is high and well
constrained in both systems. Applying ionization corrections to the measured
ionic column densities, we determine that the systems exhibit significantly
different metallicities: ~ 1/50 solar and < 1/200 solar for the two components
of z=1.92 and ~40% solar at z=1.94. The properties of the z=1.92 system are
consistent with a low metallicity galaxy (e.g. a dwarf galaxy) as well as
absorption by large scale structure of the IGM. On the other hand, the high
metallicity of the z=1.94 system suggests significant star formation and is
therefore most likely associated with a galactic system. Furthermore, we
predict it is the most likely to be observed with the STIS imaging and
follow-up observations. If a galaxy is identified, our results provide direct
measurements on the properties of the ISM for a z~2 galaxy.
