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  The CARMENES search for exoplanets around M dwarfs: Stellar atmospheric parameters of target stars with STEPARSYN

Marfil, E., Tabernero, H. M., Montes, D., Caballero, J. A., Lázaro, F. J., González Hernández, J. I., et al. (2021). The CARMENES search for exoplanets around M dwarfs: Stellar atmospheric parameters of target stars with STEPARSYN. Astronomy and Astrophysics, 656: A162. doi:10.1051/0004-6361/202141980.

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Marfil, E., Author
Tabernero, H. M., Author
Montes, D., Author
Caballero, J. A., Author
Lázaro, F. J., Author
González Hernández, J. I. , Author
Nagel, E., Author
Passegger, V. M., Author
Schweitzer, A., Author
Ribas, I., Author
Reiners, A., Author
Quirrenbach, A., Author
Amado, P. J., Author
Cifuentes, C., Author
Cortés-Contreras, M., Author
Dreizler, S., Author
Duque-Arribas, C., Author
Galadí-Enríquez, D., Author
Henning, Th., Author
Jeffers, Sandra V.1, Author           
Kaminski, A., AuthorKürster, M., AuthorLafarga, M., AuthorLópez-Gallifa, Á., AuthorMorales, J. C., AuthorShan, Y., AuthorZechmeister, M., Author more..
1Department Solar and Stellar Interiors, Max Planck Institute for Solar System Research, Max Planck Society, ou_1832287              


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 Abstract: We determined effective temperatures, surface gravities, and metallicities for a sample of 343 M dwarfs observed with CARMENES, the double-channel, high-resolution spectrograph installed at the 3.5 m telescope at Calar Alto Observatory. We employed STEPARSYN, a Bayesian spectral synthesis implementation particularly designed to infer the stellar atmospheric parameters of late-type stars following a Markov chain Monte Carlo approach. We made use of the BT-Settl model atmospheres and the radiative transfer code turbospectrum to compute a grid of synthetic spectra around 75 magnetically insensitive Fe I and Ti I lines plus the TiO γ and ϵ bands. To avoid any potential degeneracy in the parameter space, we imposed Bayesian priors on Teff and logg based on the comprehensive, multi-band photometric data available for the sample. We find that this methodology is suitable down to M7.0 V, where refractory metals such as Ti are expected to condense in the stellar photospheres. The derived Teff, logg, and [Fe/H] range from 3000 to 4200 K, 4.5 to 5.3 dex, and −0.7 to 0.2 dex, respectively. Although our Teff scale is in good agreement with the literature, we report large discrepancies in the [Fe/H] scales, which might arise from the different methodologies and sets of lines considered. However, our [Fe/H] is in agreement with the metallicity distribution of FGK-type stars in the solar neighbourhood and correlates well with the kinematic membership of the targets in the Galactic populations. Lastly, excellent agreement in Teff is found for M dwarfs with interferometric angular diameter measurements, as well as in the [Fe/H] between the components in the wide physical FGK+M and M+M systems included in our sample.


Language(s): eng - English
 Dates: 2021
 Publication Status: Published online
 Pages: -
 Publishing info: -
 Table of Contents: -
 Rev. Type: Peer
 Identifiers: DOI: 10.1051/0004-6361/202141980
 Degree: -



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Title: Astronomy and Astrophysics
  Other : Astron. Astrophys.
Source Genre: Journal
Publ. Info: Les Ulis Cedex A France : EDP Sciences
Pages: - Volume / Issue: 656 Sequence Number: A162 Start / End Page: - Identifier: ISSN: 1432-0746
ISSN: 0004-6361
CoNE: https://pure.mpg.de/cone/journals/resource/954922828219_1