“Void edge sharpness” refers to the observation that many cosmic voids exhibit relatively steep density transitions at their boundaries, with galaxy counts and matter density rising quickly over a small radial range as one moves from the void interior into surrounding filaments and walls (Colberg et al. 2005; Hamaus et al. 2014). In ΛCDM, voids form from the gradual evacuation of underdense regions in a nearly Gaussian initial field, so simulations often predict smoother, more gradual density profiles, and reproducing the sharp, quasi-compensated edges and steep gradients seen in some surveys can require fine-tuned galaxy bias, complex feedback, or special selection, highlighting a mild but persistent mismatch between idealized void models and observed void profiles (Ceccarelli et al. 2013; Nadathur & Hotchkiss 2015).