  We follow up on the surprising recent announcement by Vernstrom et al. (2021)
of the detection of the synchrotron cosmic web. We attempt to reproduce their
detection with new observations with the Phase II, extended configuration of
the Murchison Widefield Array at \SI{118.5}{\mega \hertz}. We reproduce their
detection methodology by stacking pairs of nearby luminous red galaxies (LRGs)
-- used as tracers for clusters and galaxy groups -- contained in our low
frequency radio observations. We show that our observations are significantly
more sensitive than those used in Vernstrom et al., and that our angular
sensitivity is sufficient. And yet, we make no statistically significant
detection of excess radio emission along the bridge spanning the LRG pairs.
This non-detection is true both for the original LRG pair catalogue as used in
Vernstrom et al., as well as for other larger catalogues with modified
selection criteria. Finally, we return to the original data sets used in
Vernstrom et al., and find that whilst we clearly reproduce the excess X-ray
emission from ROSAT, we are not able to reproduce any kind of broad and
extended excess intercluster filamentary emission using the original 118.5 MHz
MWA survey data. In the interests of understanding this result, as part of this
paper we release images of the 14 fields used in this study, the final stacked
images, as well as key components of our stacking and modelling code.
