GaLight (Galaxy shapes of Light) performs two-dimensional model fitting of optical and near-infrared images to characterize the light distribution of galaxies with components including a disk, bulge, bar and quasar. Light is decomposes into PSF and Sersic, and the fitting is based on lenstronomy (ascl:1804.01). GaLight's automated features including searching PSF stars in the FOV, automatically estimating the background noise level, and cutting out the target object galaxies (QSOs) and preparing the materials to model the data. It can also detect objects in the cutout stamp and quickly create Sersic keywords to model them, and model QSOs and galaxies using 2D Sersic profile and scaled point source.

PSFr empirically reconstructs an oversampled version of the point spread function (PSF) from astronomical imaging observations. The code provides a light-weighted API of a refined version of an algorithm originally implemented in lenstronomy (ascl:1804.012). It provides user support with different artifacts in the data and supports the masking of pixels, or the treatment of saturation levels. PSFr has been used to reconstruct the PSF from multiply imaged lensed quasar images observed by the Hubble Space Telescope in a crowded lensing environment and more recently with James Webb Space Telescope (JWST) imaging data for a wide dynamical flux range.