We present new results on the connections between MgII absorption selected galaxies and their halo gas. We also analyze mock quasar absorption line observations of galaxies and their gaseous halos in Lambda-CDM cosmological simulations in order constrain the dynamic interaction of the galaxy/halo/cosmic web environment and the distribution of gas within halos. We find previous results suggesting spherical halos with a uniform distribution of gas are not consistent with our data nor with the simulations. Statistically, gaseous halos have sizes of 43-88 kpc with a gas covering fraction of around 60%. Previous observational results from six edge-on galaxies suggest that halo gas velocities are consistent with extended disk-like rotation at galactocentric distances of 25-72 kpc. We demonstrate that the gas velocities are by and large not consistent with being kinematically coupled to the galaxy over galactocentric distances of 25-105 kpc. The simulations and our new observations support the picture in which gaseous halos are chemically enriched by outflowing shock-heated supernovae winds while low metallicity gas inflowing along filaments produces an inhomogeneous temperature, velocity and metallicity distributions with a non-unity gas covering fraction.