Velocity anisotropy profiles β(r), of different cluster galaxy populations as obtained from the inversion of the Jeans equation adopting the best-fit MAMPOSSt solution for the mass profile. Top panel: all cluster members. The β(r) is represented by the solid (black) curve and the hatched gray region represents 68% confidence levels on the solution. The best-fit MAMPOSSt β(r) model is represented by the dot-dashed (brown) curve. In both panels, the vertical dashed and dash-dotted (magenta) lines indicate the location of r_-2 and r₂₀₀, respectively, and the horizontal dotted line indicates β = 0. Below (resp. above) this line, galaxy orbits are more tangentially (resp. radially) elongated. Bottom panel: passive and SF cluster members, separately. Their β(r) are represented by red solid and blue dashed curves, resp. for passive and SF galaxies, within their 68% confidence levels (orange and cyan hatched regions, for passive and SF, resp.; green in the overlap region).