Best-fit double Schechter function parameters of the cGSMFs shown in Fig. 8 using the same colour-coding by filament radius. The differences between filaments and voids found for M^⋆, α₁, and α₂ when using the entire galaxy sample in panel (a) vanish after removing all grouped galaxies from the filament samples in panel (b). We note the different scaling of the y-axes in (a) and (b).