We have explored the galaxy disk/extended halo gas kinematic relationship using rotation curves ( Keck/ESI ) of ten intermediate redshift galaxies which were selected by Mg ii halo gas absorption observed in quasar spectra .
Previous results of six edge–on galaxies , probed along their major axis , suggest that observed halo gas velocities are consistent with extended disk–like halo rotation at galactocentric distances of 25–72 kpc .
Using our new sample , we demonstrate that the gas velocities are by and large not consistent with being directly coupled to the galaxy kinematics .
Thus , mechanisms other than co–rotation dynamics ( i.e. , gas inflow , feedback , galaxy–galaxy interactions , etc . )
must be invoked to account for the overall observed kinematics of the halo gas .

In order to better understand the dynamic interaction of the galaxy/halo/cosmic web environment , we performed similar mock observations of galaxies and gaseous halos in \Lambda –CDM cosmological simulations .
We discuss an example case of a z = 0.92 galaxy with various orientations probing halo gas at a range of positions .
The gas dynamics inferred using simulated quasar absorption lines are consistent with observational data .