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Fig. 4.

image

Panels a–c: posterior probability distributions for the normalization of the σap − L scaling relation, that is aperture projected velocity dispersion , and truncation radius (), obtained with different lens models for clusters under study. The green contours and distributions refer to our best models which include the kinematic prior based on measured velocity dispersions of member galaxies (Fig. 2). For visualization clarity, in panel c we omit the C16 results because they are outside the chosen range of velocity dispersion, as visible in the bottom panel of Fig. 2. The reference magnitudes for each cluster are in Table 2. Panel d: posterior distribution of the reference central velocity () and reference truncation radius () in each cluster, normalized to an absolute mag , close to L* of the early-type galaxy population. The different colors correspond to the models with kinematic priors and contours refer to 1, 2, 3-σ confidence levels. Once normalized to the same luminosity, the three scaling relations for σ and rcut are consistent.

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