X-ray and Sunyaev-Zel'dovich (SZ) observations reveal that the pressure profiles of galaxy clusters are not perfectly self-similar, especially in the outskirts where the "universal" profile often overpredicts the observed thermal pressure. This deficit is attributed to a significant contribution from non-thermal pressure (turbulence, bulk flows) which increases with radius, potentially reaching 20-40% at the virial boundary. However, the exact radial scaling and magnitude of this turbulent component are difficult to reproduce consistently in simulations without fine-tuning viscosity or accretion physics, leading to tensions in derived hydrostatic masses (Planck Collaboration 2013; Eckert et al. 2019).