  Next-generation wide-field spectroscopic surveys will observe the infall
regions around large numbers of galaxy clusters with high sampling rates for
the first time. Here we assess the feasibility of extracting the large-scale
cosmic web around clusters using forthcoming observations, given realistic
observational constraints. We use a sample of 324 hydrodynamic zoom-in
simulations of massive galaxy clusters from TheThreeHundred project to create a
mock-observational catalogue spanning $5R_{200}$ around 160 analogue clusters.
These analogues are matched in mass to the 16 clusters targetted by the
forthcoming WEAVE Wide-Field Cluster Survey (WWFCS). We consider the effects of
the fibre allocation algorithm on our sampling completeness and find that we
successfully allocate targets to 81.7 $\% \pm$ 1.3 of the members in the
cluster outskirts. We next test the robustness of the filament extraction
algorithm by using a metric, $D_{\text{skel}}$, which quantifies the distance
to the filament spine. We find that the median positional offset between
reference and recovered filament networks is $D_{\text{skel}} = 0.13 \pm 0.02$
Mpc, much smaller than the typical filament radius of $\sim$ 1 Mpc. Cluster
connectivity of the recovered network is not substantially affected. Our
findings give confidence that the WWFCS will be able to reliably trace cosmic
web filaments in the vicinity around massive clusters, forming the basis of
environmental studies into the effects of pre-processing on galaxy evolution.

Astrophysics of Galaxies;Cosmology and Nongalactic Astrophysics