Luminous and Variable Stars in M31 and M33 V. The Upper HR Diagram

TL;DR

This study presents Hertzsprung-Russell diagrams for massive stars in M31 and M33, analyzing various evolved star types to understand their properties, relationships, and evolutionary stages.

Contribution

It provides detailed HR diagrams and analysis of emission-line stars, clarifying their classifications and evolutionary relationships in M31 and M33.

Findings

LBV candidates near the instability strip support their classification.

Most B[e] supergiants are less luminous and dustier than LBVs.

B[e] supergiants and LBVs are not sequential evolutionary stages.

Abstract

We present HR Diagrams for the massive star populations in M31 and M33 including several different types of emission-line stars: the confirmed Luminous Blue Variables (LBVs), candidate LBVs, B[e] supergiants and the warm hypergiants. We estimate their apparent temperatures and luminosities for comparison with their respective massive star populations and to evaluate the possible relationships of these different classes of evolved, massive stars, and their evolutionary state. Several of the LBV candidates lie near the LBV/S Dor instability strip which supports their classification. Most of the B[e] supergiants, however, are less luminous than the LBVs. Many are very dusty with the infrared flux contributing one-third or more to their total flux. They are also relatively isolated from other luminous OB stars. Overall, their spatial distribution suggests a more evolved state. Some may be post-RSGs like the warm hypergiants, and there may be more than one path to becoming a B[e] star. There are sufficient differences in the spectra, luminosities, spatial distribution, and the presence or lack of dust between the LBVs and B[e] supergiants to conclude that one group does not evolve into the other.