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Stellar Characterization of M Dwarfs from the APOGEE Survey : A Calibrator Sample for M-dwarf Metallicities

Souto, Diogo ; Cunha, Katia ; Smith, Verne V. ; Allende Prieto, C. ; Burgasser, Adam ; Covey, Kevin ; García-Hernández, D. A. ; Holtzman, Jon A. LU ; Johnson, Jennifer A. LU and Jönsson, Henrik LU , et al. (2020) In Astrophysical Journal 890(2).
Abstract

We present spectroscopic determinations of the effective temperatures, surface gravities, and metallicities for 21 M dwarfs observed at high resolution (R ∼ 22,500) in the H band as part of the Sloan Digital Sky Survey (SDSS)-IV Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey. The atmospheric parameters and metallicities are derived from spectral syntheses with 1D LTE plane-parallel MARCS models and the APOGEE atomic/molecular line list, together with up-to-date H2O and FeH molecular line lists. Our sample range in T eff from ∼3200 to 3800 K, where 11 stars are in binary systems with a warmer (FGK) primary, while the other 10 M dwarfs have interferometric radii in the literature. We define an... (More)

We present spectroscopic determinations of the effective temperatures, surface gravities, and metallicities for 21 M dwarfs observed at high resolution (R ∼ 22,500) in the H band as part of the Sloan Digital Sky Survey (SDSS)-IV Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey. The atmospheric parameters and metallicities are derived from spectral syntheses with 1D LTE plane-parallel MARCS models and the APOGEE atomic/molecular line list, together with up-to-date H2O and FeH molecular line lists. Our sample range in T eff from ∼3200 to 3800 K, where 11 stars are in binary systems with a warmer (FGK) primary, while the other 10 M dwarfs have interferometric radii in the literature. We define an MKS-radius calibration based on our M-dwarf radii derived from the detailed analysis of APOGEE spectra and Gaia DR2 distances, as well as a mass-radius relation using the spectroscopically derived surface gravities. A comparison of the derived radii with interferometric values from the literature finds that the spectroscopic radii are slightly offset toward smaller values, with Δ = -0.01 ± 0.02 R∗/R o-. In addition, the derived M-dwarf masses based upon the radii and surface gravities tend to be slightly smaller (by ∼5%-10%) than masses derived for M-dwarf members of eclipsing binary systems for a given stellar radius. The metallicities derived for the 11 M dwarfs in binary systems, compared to metallicities obtained for their hotter FGK main-sequence primary stars from the literature, show excellent agreement, with a mean difference of [Fe/H](M dwarf - FGK primary) = +0.04 ± 0.18 dex, confirming the APOGEE metallicity scale derived here for M dwarfs.

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Astrophysical Journal
volume
890
issue
2
article number
133
publisher
American Astronomical Society
external identifiers
  • scopus:85081699936
ISSN
0004-637X
DOI
10.3847/1538-4357/ab6d07
language
English
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yes
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2bfa3f6b-e70f-42c6-91fa-a3f2b5e49dd8
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2020-04-03 14:12:49
date last changed
2020-04-04 01:58:02
@article{2bfa3f6b-e70f-42c6-91fa-a3f2b5e49dd8,
  abstract     = {<p>We present spectroscopic determinations of the effective temperatures, surface gravities, and metallicities for 21 M dwarfs observed at high resolution (R ∼ 22,500) in the H band as part of the Sloan Digital Sky Survey (SDSS)-IV Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey. The atmospheric parameters and metallicities are derived from spectral syntheses with 1D LTE plane-parallel MARCS models and the APOGEE atomic/molecular line list, together with up-to-date H<sub>2</sub>O and FeH molecular line lists. Our sample range in T <sub>eff</sub> from ∼3200 to 3800 K, where 11 stars are in binary systems with a warmer (FGK) primary, while the other 10 M dwarfs have interferometric radii in the literature. We define an M<sub>KS</sub>-radius calibration based on our M-dwarf radii derived from the detailed analysis of APOGEE spectra and Gaia DR2 distances, as well as a mass-radius relation using the spectroscopically derived surface gravities. A comparison of the derived radii with interferometric values from the literature finds that the spectroscopic radii are slightly offset toward smaller values, with Δ = -0.01 ± 0.02 R∗/R <sub>o-</sub>. In addition, the derived M-dwarf masses based upon the radii and surface gravities tend to be slightly smaller (by ∼5%-10%) than masses derived for M-dwarf members of eclipsing binary systems for a given stellar radius. The metallicities derived for the 11 M dwarfs in binary systems, compared to metallicities obtained for their hotter FGK main-sequence primary stars from the literature, show excellent agreement, with a mean difference of [Fe/H](M dwarf - FGK primary) = +0.04 ± 0.18 dex, confirming the APOGEE metallicity scale derived here for M dwarfs.</p>},
  author       = {Souto, Diogo and Cunha, Katia and Smith, Verne V. and Allende Prieto, C. and Burgasser, Adam and Covey, Kevin and García-Hernández, D. A. and Holtzman, Jon A. and Johnson, Jennifer A. and Jönsson, Henrik and Mahadevan, Suvrath and Majewski, Steven R. and Masseron, Thomas and Shetrone, Matthew and Rojas-Ayala, Bárbara and Sobeck, Jennifer and Stassun, Keivan G. and Terrien, Ryan and Teske, Johanna and Wanderley, Fábio and Zamora, Olga},
  issn         = {0004-637X},
  language     = {eng},
  month        = {02},
  number       = {2},
  publisher    = {American Astronomical Society},
  series       = {Astrophysical Journal},
  title        = {Stellar Characterization of M Dwarfs from the APOGEE Survey : A Calibrator Sample for M-dwarf Metallicities},
  url          = {http://dx.doi.org/10.3847/1538-4357/ab6d07},
  doi          = {10.3847/1538-4357/ab6d07},
  volume       = {890},
  year         = {2020},
}