Diagnostic diagrams of the rotation signature detected in the core of the two clusters within 0.5′ from the center. This corresponds to the areas covered by the MUSE pointings. The left panels show the difference between the mean velocities ΔV_mean on each side of a line passing through the center with the given angle (PA) divided by the velocity dispersion in the core of each sample. The continuous line is the sine function that best fits the observed patterns. In these panels, labels identify the number of galaxies within 0.5′, the value of the PA that maximizes |ΔV_mean| (PA_r), the rotation velocity V (half of the amplitude) from the best-fit sine function, and the value of . The central panels show the position–velocity diagrams constructed by considering the line-of-sight velocities as a function of the projected distances from the rotation axis (XR) in arcminutes. The dashed lines are the least square linear fits to the data. The right panels show the cumulative line-of-sight velocity distributions for the galaxies with XR < 0 (solid line) and for those with XR > 0 (dotted line). The labels provide the Kolmogorov-Smirnov p-value indicating the probability that the two samples are extracted from the same parent distribution. The p-value should be close to zero if the clusters are characterized by the presence of mean rotation.