Quantifying the magnitude of turbulence in protoplanetary discs is a long-standing problem. In the poster I will show our results regarding gauging turbulence in the discs observed by the DSHARP programme by indirectly measuring their vertical thickness. In order to do so we employ the differences in the gap contrasts observed along the major and the minor axes due to projection effects, and build a radiative transfer model to reproduce these features for different values of the dust scale heights. We find that (a) the scale heights that yield a better agreement with data are generally low (?4 AU at a radial distance of 100 AU), and in almost all cases we are only able to place upper limits on their exact values; these conclusions imply low turbulence levels of ?? ? 10<sup>-3</sup>-10<sup>-4</sup>; (b) for a large fraction of the DSHARP sample, our method yields no significant constraints on the disc vertical structure; we conclude that this is because these discs have either a low inclination or gaps that are not deep enough. Based on our analysis we provide an empirical criterion to assess whether a given disc is suitable to measure the vertical scale height.