Spin parameter λ_re as a function of projected ellipticity ϵ for the distant quiescent galaxies in our sample (squares). We also show four previously identified quiescent rotating discs at z = 1.95 − 3.06 from Newman et al. (2018) (diamonds) and D’Eugenio et al. (2024) (triangle). The data points are coloured by stellar mass. We show the distribution of low-z early-type galaxies from the SAMI (van de Sande et al. 2017), ATLAS3d (Emsellem et al. 2011), and MASSIVE surveys (Veale et al. 2017) in two mass ranges as contours. The dotted line shows the separation between fast and slow rotators defined by Cappellari (2016); all ten galaxies in our sample for which we can constrain rotational support are classified as fast rotators. The five galaxies for which we could only obtain lower limits for the spin parameter are shown in grey.