a) Radial density profiles of the gas (solid lines) and DM (dashed lines) of the galaxy cluster models used in this study. The profiles are shown at the beginning of the galaxy interaction, after the cluster models were allowed to relax for ~1 Gyr. Vertical dotted lines indicate the virial radius r₂₀₀ for clusters A, B, and C, from right to left. b) Corresponding temperature profiles of the ICM.