  Comparisons of the kinematics of Mg II absorbing gas and the stellar rotation
curves in 0.5 < z < 1.0 spiral galaxies suggests that, at least in some cases,
the extended gaseous envelopes may be dynamically coupled to the stellar
matter. A strong correlation exists between the overall kinematic spread of Mg
II absorbing gas and C IV absorption strength, and therefore kinematics of the
higher-ionization gas. Taken together, the data may suggest a "halo/disk
connection" between z~1 galaxies and their extended gaseous envelopes. Though
the number of galaxies in our sample are few, there are no clear examples that
suggest the gas is accreting/infalling isotropically about the galaxies from
the intergalactic medium.
