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We propose that the Ultra-Diffuse Galaxy (UDG) population represents a set ofsatellite galaxies born in $\sim10^{10}-10^{11}$ M$_\odot$ halos, similar tofield dwarfs, which suffer a dramatic reduction in surface brightness due totidal stripping and heating. This scenario is observationally motivated by theradial alignment of UDGs in Coma as well as the significant dependence of UDGabundance on cluster mass. As a test of this formation scenario, we apply asemi-analytic model describing the change in stellar mass and half-light radiusof dwarf satellites, occupying either cored or cuspy halos, to cluster subhalosin the Illustris-dark simulation. Key to this model are results fromsimulations which indicate that galaxies in cored dark-matter halos expandsignificantly in response to tidal stripping and heating, whereas galaxies incuspy halos experience limited size evolution. Our analysis indicates that apopulation of tidally-stripped dwarf galaxies, residing in cored halos (likethose hosting low-surface brightness field dwarfs), is able to reproduce theobserved sizes and stellar masses of UDGs in clusters remarkably well.

The Formation of Ultra Diffuse Galaxies in Cored Dark Matter Halos Through Tidal Stripping and Heating