Understanding the outskirts of galaxy clusters at the virial radius (R200) and beyond is critical for an accurate determination of cluster masses and to ensure unbiased cosmological parameter estimates from cluster surveys. This problem has drawn ren
ewed interest due to recent determinations of gas mass fractions beyond R200, which appear to be considerably larger than the cosmic mean, and because the clusters total Sunyaev-Zeldovich flux receives a significant contribution from these regions. Here, we use a large suite of cosmological hydrodynamical simulations to study the clumpiness of density and pressure and employ different variants of simulated physics, including radiative gas physics and thermal feedback by active galactic nuclei. We find that density and pressure clumping closely trace each other as a function of radius, but the bias on density remains on average < 20% within the virial radius R200. At larger radius, clumping increases steeply due to the continuous infall of coherent structures that have not yet passed the accretion shock. Density and pressure clumping increase with cluster mass and redshift, which probes on average dynamically younger objects that are still in the process of assembling. The angular power spectra of gas density and pressure show that the clumping signal is dominated by comparably large substructures with scales >R200/5, signaling the presence of gravitationally-driven super-clumping. In contrast, the angular power spectrum of the dark matter (DM) shows an almost uniform size distribution due to unimpeded subhalos. The quadrupolar anisotropy dominates the signal and correlates well across different radii as a result of the prolateness of the DM potential. We provide a synopsis of the radial dependence of the clusters non-equilibrium measures (kinetic pressure support, ellipticity, and clumping) that all increase sharply beyond R200.
