  There are a growing number of nearby SNe for which the progenitor star is
detected in archival pre-explosion imaging. From these images it is possible to
measure the progenitor's brightness a few years before explosion, and
ultimately estimate its initial mass. Previous work has shown that II-P and
II-L supernovae (SNe) have Red Supergiant (RSG) progenitors, and that the range
of initial masses for these progenitors seems to be limited to $<$17M$_\odot$.
This is in contrast with the cutoff of 25-30M$_\odot$ predicted by evolutionary
models, a result which is termed the 'Red Supergiant Problem'. Here we
investigate one particular source of systematic error present in converting
pre-explosion photometry into an initial mass, that of the bolometric
correction (BC) used to convert a single-band flux into a bolometric
luminosity. We show, using star clusters, that RSGs evolve to later spectral
types as they approach SN, which in turn causes the BC to become larger.
Failure to account for this results in a systematic underestimate of a star's
luminosity, and hence its initial mass. Using our empirically motivated BCs we
reappraise the II-P and II-L SNe that have their progenitors detected in
pre-explosion imaging. Fitting an initial mass function to these updated masses
results in an increased upper mass cutoff of $M_{\rm
hi}$=$19.0^{+2.5}_{-1.3}$M$_\odot$, with a 95% upper confidence limit of
$<$27M$_\odot$. Accounting for finite sample size effects and systematic
uncertainties in the mass-luminosity relationship raises the cutoff to $M_{\rm
hi}$=25M$_\odot$ ($<$33M$_\odot$, 95% confidence). We therefore conclude that
there is currently no strong evidence for `missing' high mass progenitors to
core-collapse SNe.
