Standard $\Lambda$CDM simulations predict a monotonic, inverse relationship between a dark matter halo's mass and its concentration (the $c-M$ relation), where less massive halos are more concentrated because they formed in a denser early universe. However, observational data from galaxy clusters often show a flatter relation or significant outliers, with massive clusters exhibiting higher-than-expected concentrations that are difficult to reconcile with the standard hierarchical growth model. This discrepancy suggests either a misunderstanding of halo assembly or the influence of non-gravitational physics on the core structure of massive halos (Dutton & Macciò 2014; Meneghetti et al. 2014).