Notes. The second references in the Ref column contain the values of the X-ray properties ( and kT) we adopt in this paper, because these are updated and/or consistent with our cosmology. The parameters and are the velocity dispersion and the number of members used to compute it, respectively, quoted from the literature. They generally differ from the and values we obtained with the 3σ clipping procedure described in Sect. 3.3. For those clusters without a public redshift dataset the latter values are not computable (“n.a.”) and the ones quoted in the literature are used in our study. Systems defined by the authors as experiencing major merger events are indicated in the last column with a check mark and marked with red squares in Figs. 3, 4, 6, and 7.

Reference. Do99: Donahue et al. (1999); Et04: Ettori et al. (2004); Gi99: Gioia et al. (1999); Tr99: Tran et al. (1999); Gi04: Gioia et al. (2004); Re11: Reichert et al. (2011); Me12: cluster “El Gordo”, Menanteau et al. (2012); Lu04: Lubin et al. (2004); Sa09: Santos et al. (2009); Fa11: Fassbender et al. (2011b); Br10: Brodwin et al. (2010); Fo11: Foley et al. (2011); Ro04: Rosati et al. (2004); Wi09: Wilson et al. (2009); Mu05: Mullis et al. (2005); Br11: Brodwin et al. (2011); An11: Andreon et al. (2011); Hi10: Hilton et al. (2010).