  Numerous studies have established the theoretical potential of the 21cm
bispectrum to boost our understanding of the Epoch of Reionization (EoR), and
therefore early generation of stars and galaxies. In this paper we look at the
impact of foregrounds and instrumental effects on the 21cm bispectrum and our
ability to measure it. Unlike the power spectrum for which (in the absence of
instrumental effects) there is a window clear of smooth-spectrum foregrounds in
which the 21cm power spectrum may be detectable, there is no such "EoR window"
for the bispectrum. Instead, on smaller scales EoR structure modulates that of
the foregrounds (FG) to alter the EoR+FG bispectrum from that of the
foregrounds in a complex manner. On larger scales the EoR structures are
completely swamped by those of the foregrounds, and the EoR+FG bispectrum is
entirely dominated by that of the foregrounds. It is therefore unlikely that
the bispectrum will be useful in cases where we are observationally restricted
to using foreground avoidance techniques. We also find that there is potential
for instrumental effects to seriously corrupt the bispectrum, possibly even
rendering the bispectrum useless for parameter estimation. On larger scales,
foreground removal using GMCA is found to recover the EoR bispectrum to a
reasonable level of accuracy (even better than the power spectrum for certain
configurations). Further studies are necessary to understand the error and/or
bias associated with foreground removal before the 21cm bispectrum can be
practically applied in analysis of future data.
