In both panels the crosses mark velocity dispersions from Bedregal et al. (2006). The six open circles denote velocity dispersions of clusters fainter than R = 21.5 mag. Upper panel: some isotropic models. The lower short-dashed line is a model without dark matter and uses M/L_R = 3.5. The solid line is a log-halo with the parameters v₀ = 300 km s^-1 and r₀ = 0.5 kpc and uses M/L_R = 1.3. The upper short-dashed line is a NFW-type halo with M/L_R = 2.0. See the text for its parameters. The long-dashed line is a MONDian model with M/L_R = 2.5. Lower panel: models with the radial anisotropy of Hansen & Moore (2006). The solid line is a log-halo with the same parameters as above, but with M/L_R = 2.0. The short dashed line is the same NFW halo as above to show that M/L_R = 2.0 results in a central velocity dispersion that is too high, but a stellar M/L_R lower than 2.0 is difficult to justify.