Source magnitudes in the faintest optical band against the brightest UV band. It is evident from this figure that the AGN in our sample are brighter in the optical when compared to the UV and even the faintest optical band is brighter than the brightest UV band. Therefore, based on the GALFIT simulations carried out in the UV band to obtain the correction factors for GALFIT-estimated PSF magnitudes and fluxes, only the faintest and farthest sources need to be corrected in the optical as well. The x = y line is shown in red.