  Recently Vernstrom et al. (2021) claimed the first definitive detection of
the synchrotron cosmic web, obtained by `stacking' hundreds of thousands of
pairs of close-proximity clusters in low-frequency radio observations and
looking for a residual excess signal spanning the intracluster bridge. A
reproduction study by Hodgson et al. (2022), using both the original radio data
as well as new observations with the Murchison Widefield Array, failed to
confirm these findings. Whilst the detection remains unsure, we here turn to
stacking a simulated radio sky to understand what kind of excess radio signal
is predicted by our current best cosmological models of the synchrotron cosmic
web. We use the FIlaments & GAlactic RadiO (Hodgson et al., 2021a) simulation,
which models both the synchrotron cosmic web as well as various subtypes of
active galactic nucleii and star forming galaxies. Being a simulation, we have
perfect knowledge of the location of clusters and galaxy groups which we use in
our own stacking experiment. Whilst we do find an excess radio signature in our
stacks that is attributable to the synchrotron cosmic web, its distribution is
very different to that found by Vernstrom et al. (2021). Instead, we observe
the appearance of excess emission on the immediate interiors of cluster pairs
as a result of asymmetric, `radio relic'-like shocks surrounding cluster cores,
whilst the excess emission spanning the intracluster region -- attributable to
filaments proper -- is two orders of magnitude lower and undetectable in our
experiment even under ideal conditions.
