The luminosities of cool supergiants in the Magellanic Clouds, and the Humphreys–Davidson limit revisited. Issue 3 (18th May 2018)

• Record Type: Journal Article
• Authors: Davies, Ben; Crowther, Paul A; Beasor, Emma R
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 478:Issue 3(2018)
• Page Start: 3138
• Page End: 3148
• Publication Date: 2018-05-18
• Subjects: stars: massive -- stars: evolution -- supergiants; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/sty1302
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: The empirical upper luminosity boundary L max of cool supergiants (SGs), often referred to as the Humphreys-Davidson limit, is thought to encode information on the general mass-loss behaviour of massive stars. Further, it delineates the boundary at which single stars will end their lives stripped of their hydrogen-rich envelope, which in turn is a key factor in the relative rates of Type-II to Type-Ibc supernovae from single star channels. In this paper we have revisited the issue of L max by studying the luminosity distributions of cool SGs in the Large and Small Magellanic Clouds (LMC/SMC). We assemble samples of cool SGs in each galaxy which are highly complete above log L /L⊙ = 5.0, and determine their spectral energy distributions from the optical to the mid-infrared using modern multiwavelength survey data. We show that in both cases L max appears to be lower than previously quoted, and is in the region of log L /L⊙ = 5.5. There is no evidence for L max being higher in the SMC than in the LMC, as would be expected if metallicity-dependent winds were the dominant factor in the stripping of stellar envelopes. We also show that L max aligns with the lowest luminosity of single nitrogen-rich Wolf-Rayet stars, indicating of a change in evolutionary sequence for stars above a critical mass. From population synthesis analysis we show that the Geneva evolutionary models greatly overpredict the numbers of cool SGs in the SMC. We also argue that the trend of earlier average spectral types of cool SGs in lower metallicity environments represents a genuine shift to hotter temperatures. Finally, we use our new bolometric luminosity measurements to provide updated bolometric corrections for cool SGs.