The current status and remaining questions of the geometry and physical extent of intermediate redshift galaxy halos are reviewed with an eye toward new results incorporating both the kinematics of the halo gas and the morphologies of the host galaxies. In the end, we find that our conventional wisdom requires significant revision. Using MgII absorption seen in background quasar spectra, earlier-epoch galaxy halos appear to be highly patchy with irregular geometries. We also refute the suggestions that so-called ``weak'' MgII absorbers arise in the intergalactic medium, in low surface brightness galaxies, or trace dwarf galaxies; these systems appear to be associated with normal galaxies over a wide range of impact parameters. We also show new results that connect the quantity of halo gas with the morphological perturbations of the galaxies. The implications for the formation and sustenance of extended galaxy halos will be discussed.