  We present early-time Keck spectroscopic observations and late-time Hubble
Space Telescope (HST) imaging of GRB 000926. The HST images show a small offset
between the optical transient and the compact host galaxy. Combined with the
large equivalent widths measured for metallic absorption lines by the Keck
Echellette Spectrograph and Imager (ESI) and the Low-Resolution Imaging
Spectrometer (LRIS), this indicates that the GRB exploded near the center of
its host. The ESI spectroscopy reveals two absorption systems centered at z =
2.0379 \pm 0.0008 with a velocity separation of 168 km s^{-1}, which we
interpret as being due to individual clouds in the host galaxy. The ratios of
chromium to zinc equivalent widths indicates the host is depleted in dust
relative to local values to a similar degree as damped Lyman alpha systems at
the same redshift. Further, the two clouds appear to have similar relative
metal abundance and dust to gas ratio. If one cloud is associated with the GRB
site, this implies the explosion did not significantly alter the surrounding
environment.
