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tokens: the surface brightness of the SZE signature is independent of the cluster redshift, which together with the expected temperature and density evolution of the cluster ICM at fixed virial mass and the changing solid angle of clusters with redshift lead an SZE signal-to noise-selected sample to be approximately mass-limited (Haiman, Mohr Holder 2001 ; Holder, Haiman Mohr 2001 ). Because we plan to carry out a dynamical analysis, the cluster sample we analyse includes only those SPT systems with spectroscopic follow-up. This spectroscopic subsample is not a signal-to-noise-selected sample, but rather is the largest sample of SPT-selected clusters we could assemble for the analysis. We plot the sample of 110 clusters in the space of redshift versus mass in Fig. 1 , together with the full distribution of the SPT–SZ sample with the latest available redshifts (Bayliss et al. 2016 ; Khullar et al. 2018 ; Strazzullo et al. 2018 , Bocquet et al., in preparation) . Note that in comparison to the SPT–SZ cosmology sample (de Haan et al. 2016 ), the median redshift and mass for our sample is 0.56 and 7.26 × 10 14 M ⊙ as compared to 0.55 and 6.08 × 10 14 M ⊙ . Approximately 6 per cent of the sample lies at > 1 as compared to ∼9 per cent of the full SPT–SZ ξ > 5 sample (with updated redshifts from Bocquet et al., in preparation). Thus, in comparison to the complete SPT–SZ sample, the subset of those clusters we study here have somewhat higher masses and are somewhat under-represented at high redshift. Full information on the cluster sample is provided in Table 1 . From left to right, the columns correspond to the SPT cluster designation, the total number of passive galaxy redshifts available, the number of passive galaxy member redshifts, the cluster redshift, the SZE-based mass , and the corresponding virial radius (described in Section 3.3.1 ). Figure 1. Masses versus redshifts of the cluster sample. The coloured dots are coded according to the number of member galaxies in each cluster (see colour bar on right). Overplotted in grey is the full distribution of the SPT–SZ sample. Table 1. Cluster spectroscopic sample: we present the cluster name, total number of passive galaxies in the spectroscopic sample N tot , members used in our analysis after interloper rejection N mem , cluster redshift clus , and cluster mass and corresponding virial radius from Bocquet et al. ( 2015 ). 3.2 Spectroscopic sample We use spectroscopic follow-up including data taken using the Gemini Multi Object Spectrograph (Hook et al. 2004 ) on Gemini South, the Focal Reducer and low dispersion Spectrograph (Appenzeller et al. 1998 ) on VLT Antu, the Inamori Magellan Areal Camera and Spectrograph (Dressler et al. 2006 ) on Magellan Baade, and the Low Dispersion Survey Spectrograph (Allington-Smith et al. 1994 ) on Magellan Clay. We combine the data sets presented in Ruel et al. ( 2014 ) and Bayliss et al. ( 2016 ) with the one described in Sifón et al. ( 2013 ), obtaining a sample of