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Characterization of the morphology of strongly lensed galaxies is challengingbecause images of such galaxies are typically highly distorted. Lens modelingand source plane reconstruction is one approach that can provide reasonablyundistorted images from which morphological measurements can be made, althoughat the expense of a highly spatially variable telescope PSF when mapped back tothe source plane. Unfortunately, modeling the lensing mass is a time andresource intensive process, and in many cases there are too few constraints toprecisely model the lensing mass. If, however, useful morphologicalmeasurements could be made in the image plane rather than the source plane, itwould bypass this issue and obviate the need for a source reconstructionprocess for some applications. We examine the use of the Gini coefficient asone such measurement. Because it depends on the cumulative distribution of thelight of a galaxy, but not the relative spatial positions, the fact thatsurface brightness is conserved by lensing means that the Gini coefficient maybe well-preserved by strong gravitational lensing. Through simulations, we testthe extent to which the Gini coefficient is conserved, including by effects dueto PSF convolution and pixelization, to determine whether it is invariantenough under lensing to be used as a measurement of galaxy morphology that canbe made in the image plane.

The Gini Coefficient as a Morphological Measurement of Strongly Lensed Galaxies in the Image Plane