  In the z=1.94 CIV absorption line system in the spectrum of quasar Q1222+228
(z_em=2.04), we find two clouds which have contrasting physical conditions,
although they are only at a 17 km/s velocity separation. In the first cloud
SiII, SiIV, and CII are detected, and AlII and AlIII column density limits in
conjunction with photoionization models allow us to infer that this cloud has a
large Si abundance and a small Al abundance relative to a solar abundance
pattern. This pattern resembles that of Galactic metal-poor halo stars, which
must have formed from such high redshift gas. The second cloud, in contrast,
has detected AlII and AlIII (also SiIV and CII), but no detected SiII. We
demonstrate, using photoionization models, that Al/Si must be greater than
(Al/Si)_Sun in this unusual cloud. Such a ratio is not found in absorption
profiles looking through Milky Way gas. It cannot be explained by dust
depletion since Al depletes more severely than Si. Comparing to other Al-rich
environments, we speculate about the processes and conditions that could give
rise to this abundance pattern.
