Dynamical environment classification of giant radio galaxies (left), radio galaxies in general (centre), and the Local Universe in its entirety (right; from Table 3 of Leclercq et al. 2015). We define clusters, filaments, sheets, and voids in the T-web sense. These distributions depend on the scale to which the Cosmic Web density field is smoothed; in this case, the smoothing scale is 2.9 Mpc h⁻¹. If giants and RGs were scattered uniformly throughout the Cosmic Web, their distributions would be similar to that of the volume-filling fractions (VFFs). Instead, observed RGs – and observed giants in particular – favour cluster and filament environments.