  The progenitors of Type IIP supernovae have an apparent upper limit to their
initial masses of about 20 solar masses, suggesting that the most massive red
supergiants evolve to warmer temperatures before their terminal explosion. But
very few post-red supergiants are known. We have identified a small group of
luminous stars in M31 and M33 that are candidates for post-red supergiant
evolution. These stars have A -- F-type supergiant absorption line spectra and
strong hydrogen emission. Their spectra are also distinguished by the Ca II
triplet and [Ca II] doublet in emission formed in a low density circumstellar
environment. They all have significant near- and mid-infrared excess radiation
due to free-free emission and thermal emission from dust. We estimate the
amount of mass they have shed and discuss their wind parameters and mass loss
rates which range from a few times$ 10^-6 to 10^-4 solar masses/yr. On an HR
Diagram, these stars will overlap the region of the LBVs at maximum light,
however the warm hypergiants are not LBVs. Their non-spherical winds are not
optically thick and they have not exhibited any significant variability. We
suggest, however, that the warm hypergiants may be the progenitors of the "less
luminous" LBVs such as R71 and even SN1987A.
