Bergamini, P.P.BergaminiRosati, P.P.RosatiMERCURIO, AMATAAMATAMERCURIOGrillo, C.C.GrilloCaminha, G. B.G. B.CaminhaMENEGHETTI, MASSIMOMASSIMOMENEGHETTIAgnello, A.A.AgnelloBIVIANO, ANDREAANDREABIVIANOCalura, F.F.CaluraGIOCOLI, CarloCarloGIOCOLILombardi, M.M.LombardiRodighiero, G.G.RodighieroVanzella, E.E.Vanzella2021-02-112021-02-1120190004-6361http://hdl.handle.net/20.500.12386/30328We present an improved determination of the total mass distribution of three massive clusters from the Cluster Lensing and Supernova Survey with Hubble and Hubble Frontier Fields, MACS J1206.2-0847 (z = 0.44), MACS J0416.1-2403 (z = 0.40), Abell S1063 (z = 0.35). We specifically reconstructed the sub-halo mass component with robust stellar kinematics information of cluster galaxies, in combination with precise strong lensing models based on large samples of spectroscopically identified multiple images. We used integral-field spectroscopy in the cluster cores, from the Multi Unit Spectroscopic Explorer on the Very Large Telescope, to measure the stellar velocity dispersion, σ, of 40-60 member galaxies per cluster, covering four to five magnitudes to m<SUB>F160W</SUB> ≃ 21.5. We verified the robustness and quantified the accuracy of the velocity dispersion measurements with extensive spectral simulations. With these data, we determined the normalization and slope of the galaxy L-σ Faber-Jackson relation in each cluster and used these parameters as a prior for the scaling relations of the sub-halo population in the mass distribution modeling. When compared to our previous lens models, the inclusion of member galaxies' kinematics provides a similar precision in reproducing the positions of the multiple images. However, the inherent degeneracy between the central effective velocity dispersion, σ<SUB>0</SUB>, and truncation radius, r<SUB>cut</SUB>, of sub-halos is strongly reduced, thus significantly alleviating possible systematics in the measurements of sub-halo masses. The three independent determinations of the σ<SUB>0</SUB> - r<SUB>cut</SUB> scaling relation in each cluster are found to be fully consistent, enabling a statistical determination of sub-halo sizes as a function of σ<SUB>0</SUB>, or halo masses. Finally, we derived the galaxy central velocity dispersion functions of the three clusters projected within 16% of their virial radius, finding that they are well in agreement with each other. We argue that such a methodology, when applied to high-quality kinematics and strong lensing data, allows the sub-halo mass functions to be determined and compared with those obtained from cosmological simulations.STAMPAenArticle10.1051/0004-6361/2019359742-s2.0-85076194779000515098500001https://www.aanda.org/articles/aa/full_html/2019/11/aa35974-19/aa35974-19.html2019A&A...631A.130BFIS/05 - ASTRONOMIA E ASTROFISICAPE9