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 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 2002ApJS..141...81M)
and Gonzalez-Fernandez et al. (2015A&A...578A...3G 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:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
lmc.dat 323 297 Properties of LMC cool supergiants
smc.dat 309 245 Properties of SMC cool supergiants
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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
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Bytes Format Units Label Explanations
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1- 23 A23 --- SIMBAD SIMBAD designation, when the table was build
24- 33 A10 --- Massey Massey (2002ApJS..141...81M 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
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Acknowledgements:
Paul Crowther, Paul.Crowther(at)sheffield.ac.uk
(End) Paul Crowther [Sheffield], Patricia Vannier [CDS] 14-May-2018