J/A+A/625/A68 Radii and masses of the CARMENES targets (Schweitzer+, 2019)
The CARMENES search for exoplanets around M dwarfs:
Different roads to radii and masses of the target stars.
Schweitzer A., Passegger V.M., Cifuentes C., Bejar V.J.S.,
Cortes-Contreras M., A. Caballero J., del Burgo C., Czesla S.,
Kuerster M., Montes D., Zapatero Osorio M.R., Ribas I., Reiners A.,
Quirrenbach A., Amado P.J., Aceituno J., Anglada-Escude G., Bauer F.F.,
Dreizler S., Jeffers S.V., Guenther E.W., Henning T., Kaminski A.,
Lafarga M., Marfil E., Morales J.C., Schmitt J.H.M.M., Seifert W.,
Solano E., Tabernero H.M., Zechmeister M.
<Astron. Astrophys. 625, A68 (2019)>
=2019A&A...625A..68S 2019A&A...625A..68S (SIMBAD/NED BibCode)
ADC_Keywords: Stars, M-type ; Stars, masses ; Stars, diameters ;
Abundances, [Fe/H] ; Effective temperatures
Keywords: stars: fundamental parameters - stars: low mass - stars: late type -
stars: general
Abstract:
We determine the radii and masses of 293 nearby, bright M dwarfs of
the CARMENES survey. This is the first time that such a large and
homogeneous high-resolution (R>80000) spectroscopic survey has been
used to derive these fundamental stellar parameters.
We derived the radii using Stefan-Boltzmann's law. We obtained the
required effective temperatures Teff from a spectral analysis and we
obtained the required luminosities L from integrated broadband
photometry together with the Gaia DR2 parallaxes. The mass was then
determined using a mass-radius relation that we derived from eclipsing
binaries known in the literature. We compared this method with three
other methods: (1) We calculated the mass from the radius and the
surface gravity logg, which was obtained from the same spectral
analysis as Teff. (2) We used a widely used infrared mass-magnitude
relation. (3) We used a Bayesian approach to infer stellar parameters
from the comparison of the absolute magnitudes and colors of our
targets with evolutionary models.
Between spectral types M0V and M7V our radii cover the range
0.1R☉<R<0.6R☉ with an error of 2-3% and our masses cover
0.09M☉<M<0.6M☉ with an error of 3-5%. We find good
agreement between the masses determined with these different methods
for most of our targets. Only the masses of very young objects show
discrepancies. This can be well explained with the assumptions that we
used for our methods.
Description:
Table B1 contains the stellar parameters of our sample. The sample
consists of 293 nearby, bright M dwarfs with no known close
companions. Their metallicities spread around solar metallicity. Most
stars are inactive or mildly active and older than a few hundred
million years. However, known active or young stars are also included
although most of the analyses assume inactive main sequence stars. All
parameters are determined by us except where noted otherwise.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tableb1.dat 238 293 Stellar parameters of all stars of our sample
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See also:
J/A+A/577/A128 : CARMENES input catalog of M dwarfs I (Alonso-Floriano+, 2015)
J/A+A/612/A49 : 324 CARMENES M dwarfs velocities (Reiners+, 2018)
J/A+A/615/A6 : Photospheric parameters of CARMENES stars (Passegger+, 2018)
J/A+A/621/A126 : CARMENES input catalogue of M dwarfs. IV. (Diez Alonso+ 2019)
J/A+A/623/A44 : CARMENES M-dwarfs activity indicators (Schoefer+, 2019)
Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Karmn CARMENES identifier (JHHMMm+DDdA)
13- 35 A23 --- Name Gliese name, Gliese Jahreiss name or
discovery name
37- 40 I4 K Teff Effective temperature
42- 43 I2 K e_Teff Error of effective temperature
45- 50 A6 --- SpType Luminosity class V spectral type (1)
52- 55 F4.2 [cm/s2] logg Spectroscopic surface gravity
57- 60 F4.2 [cm/s2] e_logg Error of spectroscopic surface gravity
62- 66 F5.3 [cm/s2] loggc Calculated surface gravity
68- 72 F5.3 [cm/s2] e_loggc Error of calculated surface gravity
74- 78 F5.2 [-] [Fe/H] Metallicity
80- 83 F4.2 [-] e_[Fe/H] Error of metallicity
85- 93 E9.4 Lsun Lum Luminosity
95-101 E7.3 Lsun e_Lum Error of luminosity
103-112 E10.4 pc d Distance
114-120 E7.2 pc e_d Error of distance
122-126 A5 --- r_d Reference for distance (2)
128-136 E9.4 Rsun Rad Radius based on Stefan-Boltzmann's law
138-144 E7.2 Rsun e_Rad Error of radius based on
Stefan-Boltzmann's law
146-154 E9.4 Rsun RadP ? PARSEC based radius
156-162 E7.2 Rsun e_RadP ? Error of PARSEC based radius
164-172 E9.4 Msun MassMR Mass based on mass-radius relation
174-180 E7.2 Msun e_MassMR Error of mass based on mass-radius relation
182-190 E9.4 Msun MassMMKs Photometric mass
192-198 E7.2 Msun e_MassMMKs Error of photometric mass
200-208 E9.4 Msun MassLogg Spectroscopic mass
210-216 E7.2 Msun e_MassLogg Error of Spectroscopic mass
218-226 E9.4 Msun MassP ? PARSEC based mass
228-234 E7.2 Msun e_MassP ? Error of PARSEC based mass
236-238 A3 --- Com Comment (3)
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Note (1): The spectral types are taken from Alonso-Floriano et al.
(2015A&A...577A.128A 2015A&A...577A.128A, Cat. J/A+A/577/A128) and references therein.
Note (2): Sources used for the distances as follows:
GAIA2 = Gaia DR2 parallaxes, Gaia collaboration,
2018A&A...616A...1G 2018A&A...616A...1G, Cat. I/345
HIP = Hipparcos parallaxes, van Leuwen, 2007A&A...474..653V 2007A&A...474..653V, Cat. I/311
URAT = Parallaxes obtained by the United States Naval Observatory Robotic
Astrometric Telescope, Finch & Zacharias,
2016AJ....151..160F 2016AJ....151..160F, Cat. J/AJ/151/160
Yale = Yale catalog of parallaxes, van Altena et al.,
1995gcts.book.....V 1995gcts.book.....V, Cat. I/238A
CC17 = Spectro-photometric distances using the M_J-SpType relation of
Cortes-Contreras et al., 2017A&A...597A..47C 2017A&A...597A..47C, Cat. J/A+A/597/A47
Note (3): Comments as follows:
Out = Listed as outlier in the paper. Use with care.
New = Not tabulated by Reiners et al. 2018A&A...612A..49R 2018A&A...612A..49R, Cat. J/A+A/612/A49
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Acknowledgements:
Andreas Schweitzer, aschweitzer(at)hs.uni-hamburg.de
(End) Patricia Vannier [CDS] 04-Apr-2019