Gas-phase metallicity derived from absorption profiles may hold a unique key into the origins of the CGM. To determine the origins of the CGM requires a substantial dataset, which includes a combination of quasar spectra from HST/COS, from Keck/HIRES and VLT/UVES, HST galaxy imaging and galaxy spectra. Using these data, we modelled the metallicity of 50 absorption systems associated with isolated galaxies that have quantified morphologies. We will present our results showing the spatial distribution of metals around galaxies at z~0.3 and address if the combination of spatial location and metallicity can be used to distinguish between gas accretion and outflows.