Stellar accretion rate Ṁ_acc vs. gas disc mass M_disc, analogous to Fig. 5, but for populations with a strong FUV field distribution (see Table 1). A snapshot for the individual systems is shown at 4 Myr (orange circles) in comparison with observational data from σ Orionis. Observational dust disc masses are taken from Ansdell et al. (2017) and converted to gas masses by assuming the standard dust-to-gas ratio of 0.01. Stellar accretion rates are taken from Rigliaco et al. (2011).