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J/MNRAS/478/3138  Luminous cool supergiants in Magellanic Clouds (Davies+, 2018)

The luminosities of cool supergiants in the Magellanic Clouds. Davies B., Crowther P.A., Beasor E.R. <Mon. Not. R. Astron. Soc. 478, 3138 (2018)> =2018MNRAS.478.3138D (SIMBAD/NED BibCode)
ADC_Keywords: Magellanic Clouds ; Stars, supergiant; Stars, late-type; Stars, luminous; Photometry, UBVRI Keywords: stars: massive - stars: evolution - supergiants Abstract: The empirical upper luminosity boundary Lmax of cool supergiants, 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 Lmax by studying the luminosity distributions of cool supergiants (SGs) in the Large and Small Magellanic Clouds (LMC/SMC). We assemble highly-complete samples of cool SGs in each galaxy, and determine their spectral energy distributions from the optical to the mid-infrared using modern multi-wavelength survey data. We show that in both cases Lmax appears to be lower than previously quoted, and is in the region of logL/L=5.5. There is no evidence for Lmax 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 Lmax 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 over-predict 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 supergiants. Description: Name, position, luminosity and extinction for luminous cool SGs in each of the Magellanic Clouds, sorted by luminosity (logL/L≥4.5). We provide for each star the SIMBAD designation, as well as those from Massey (2002ApJS..141...81M) and Gonzalez-Fernandez et al. (2015A&A...578A...3G, Cat. J/A+A/578/A3) where available, together with photometry from the U-band to 22 microns, plus 70 micron for two LMC supergiants. Where stars are known to be variable we list the minimum and maximum spectral types and luminosity classes. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file lmc.dat 323 297 Properties of LMC cool supergiants smc.dat 323 245 Properties of SMC cool supergiants
See also: J/A+A/578/A3 : New survey of supergiants in the MCs (Gonzalez-Fernandez+, 2015) Byte-by-byte Description of file: lmc.dat smc.dat
Bytes Format Units Label Explanations
1- 23 A23 --- SIMBAD SIMBAD designation 24- 33 A10 --- Massey Massey (2002ApJS..141...81M) catalogue number, LMC NNNNNN or SMC NNNNNN 35- 40 A6 --- GF Gonzalez-Fernandez (2015, Cat. J/A+A/578/A3) catalogue number, LMCNNN or SMCNNN 42- 51 F10.6 deg RAdeg Right ascension (J2000.0) 53- 62 F10.6 deg DEdeg Declination (J2000.0) 64- 78 A15 --- SpType Literature MK spectral type 80- 83 F4.2 Lsun logL Luminosity 85- 88 F4.2 Lsun e_logL Uncertainty in logL 90- 94 F5.2 mag AV Visual extinction AV 96- 99 F4.2 mag e_AV Uncertainty in visual extinction AV 101-106 F6.3 mag Umag ? U band magnitude 108-113 F6.3 mag e_Umag ? Uncertainty in U band magnitude 115-120 F6.3 mag Bmag ? B band magnitude 122-127 F6.3 mag e_Bmag ? Uncertainty in B band magnitude 129-134 F6.3 mag Vmag ? V band magnitude 136-141 F6.3 mag e_Vmag ? Uncertainty in V band magnitude 143-148 F6.3 mag Imag ? I band magnitude 150-155 F6.3 mag e_Imag ? Uncertainty in I band magnitude 157-162 F6.3 mag Jmag J band magnitude 164-169 F6.3 mag e_Jmag Uncertainty in J band magnitude 171-176 F6.3 mag Hmag ? H band magnitude 178-183 F6.3 mag e_Hmag ? Uncertainty in H band magnitude 185-190 F6.3 mag Kmag K band magnitude 192-197 F6.3 mag e_Kmag Uncertainty in K band magnitude 199-204 F6.3 mag I1mag ? Spitzer IRAC I1 band magnitude 206-211 F6.3 mag e_I1mag ? Uncertainty in IRAC I1 band magnitude 213-218 F6.3 mag I2mag ? Spitzer IRAC I2 band magnitude 220-225 F6.3 mag e_I2mag ? Uncertainty in IRAC I2 band magnitude 227-232 F6.3 mag I3mag ? Spitzer IRAC I3 band magnitude 234-239 F6.3 mag e_I3mag ? Uncertainty in IRAC I3 band magnitude 241-246 F6.3 mag I4mag ? Spitzer IRAC I4 band magnitude 248-253 F6.3 mag e_I4mag ? Uncertainty in IRAC I4 magnitude 255-260 F6.3 mag W1mag ? WISE W1 band magnitude 262-267 F6.3 mag e_W1mag ? Uncertainty in WISE W1 magnitude 269-274 F6.3 mag W2mag ? WISE W2 band magnitude 276-281 F6.3 mag e_W2mag ? Uncertainty in WISE W2 magnitude 283-288 F6.3 mag W3mag ? WISE W3 band magnitude 290-295 F6.3 mag e_W3mag ? Uncertainty in WISE W3 magnitude 297-302 F6.3 mag W4mag ? WISE W4 band magnitude 304-309 F6.3 mag e_W4mag ? Uncertainty in WISE W4 magnitude 311-316 F6.3 mag M2mag ? Spitzer MIPS M2 band magnitude 318-323 F6.3 mag e_M2mag ? Uncertainty in MIPS M2 band magnitude
Acknowledgements: Paul Crowther, Paul.Crowther(at)sheffield.ac.uk
(End) Paul Crowther [Sheffield], Patricia Vannier [CDS] 14-May-2018
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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