Notes. Debris-disc masses greater than 1000 M_⊕ are potentially unfeasible, given the quantity of solids that would have been available at the protoplanetary disc stage (Krivov & Wyatt 2021); this could imply that other stirring mechanisms operate in the systems listed. Also shown are the minimum planet masses required to stir the discs, M_p,stir, from Sect. 4.2; all stirring planets are consistent with being below our L′-band detection limits at their predicted locations, implying that all of these discs can be planet-stirred, but not all can be self-stirred. Only systems with resolved discs are shown, where the ‘Disc data’ column lists the observational data source for the disc edge locations. For axisymmetric discs, the ‘Disc location and extent’ column lists the disc inner edge, a_i, and outer edge, a_o, as ‘a_i → a_o'. For asymmetric discs, this column shows the inner edge pericentre, q_i, inner edge apocentre, Q_i, outer edge pericentre, q_o, and outer edge apocentre, Q_o, as ‘q_i, Q_i → q_o, Q_o'. Uncertainties are 1σ.