Strong gravitational lensing produces dramatic arcs, Einstein rings, and multiple images of background galaxies when their light passes close to massive foreground structures like galaxy clusters. However, observations reveal several puzzles: the abundance of giant arcs (with length-to-width ratios exceeding 10:1) is higher than predicted by Lambda-CDM simulations, the arc radii and positions sometimes disagree with mass models derived from weak lensing or X-ray observations, and some arcs exhibit asymmetries or distortions that are difficult to explain with smooth dark matter halos alone (Bartelmann et al. 1998; Meneghetti et al. 2013). Additionally, the detailed morphology of arc systems—particularly the presence of radial arcs, tangential arcs at unexpected radii, and multiply-imaged systems with anomalous flux ratios—suggests that the mass distribution in lensing clusters is more complex, clumpy, or extended than the standard NFW dark matter halo profiles predict. Lambda-CDM struggles because it relies on smooth, spherically symmetric (or mildly elliptical) dark matter halos to model lensing, and reproducing the observed arc statistics and morphologies often requires fine-tuning the halo concentration, substructure abundance, or invoking line-of-sight projections that seem statistically unlikely.