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An increasing number of non-terminal eruptions are being found in thenumerous surveys for optical transients. Very little is known about these gianteruptions, their progenitors and their evolutionary state. A greatly improvedcensus of the likely progenitor class, including the most luminous evolvedstars, the Luminous Blue Varaibles (LBVs), and the warm and cool hypergiants isnow needed for a complete picture of the final pre-SN stages of very massivestars. We have begun a survey of the evolved and un stable luminous starpopulations in several nearby resolved galaxies. In this second paper on M31and M33, we review the spectral characteristics, spectral energy distributions,circumstellar ejecta, and evidence for mass loss for 82 luminous and variablestars.We show that many of these stars have warm circumstellar dust includingseveral of the Fe II emission line stars, but conclude that the confirmed LBVsin M31 and M33 do not. The confirmed LBVs have relatively low wind speeds evenin their hot, quiescent or visual minimum state compared to the B-typesupergiants and Of/WN stars which they spectroscopically resemble. The natureof the Fe II emis sion line stars and their relation to the LBV state remainsuncertain, but some have properties in common with the warm hypergiants and thesgB[e] stars. Several individual stars are discussed in detail. We identifythree possible candidate LBVs and three additional post-red supergiantcandidates. We suggest that M33-013406.63 (UIT301,B416) is not an LBV/S Dorvariable, but is a very luminous late O-type supergiant and one of the mostluminous stars or pair of stars in M33.

Luminous and Variable Stars in M31 and M33. II. Luminous Blue Variables, Candidate LBVs, Fe II Emission Line Stars, and Other Supergiants