Radio relics and halos are large, diffuse synchrotron sources in galaxy clusters: relics sit in the outskirts tracing merger shocks, while halos fill cluster cores with turbulent radio emission and are observed only in a subset of dynamically disturbed systems (Feretti et al. 2012; van Weeren et al. 2019). Within ΛCDM, simulations can link relics and halos to merger-driven shocks and turbulence, but matching their occurrence rates, morphologies, sizes, and spectral properties across redshift requires uncertain assumptions about particle acceleration efficiency, seed electron populations, and intracluster magnetic fields, limiting their use as robust cosmological probes (Brunetti & Jones 2014; Nuza et al. 2017).