Stellar Characterization of M Dwarfs from the APOGEE Survey : A Calibrator Sample for M-dwarf Metallicities
(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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- author
- organization
- publishing date
- 2020-02-20
- type
- Contribution to journal
- publication status
- published
- subject
- in
- 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
- LU publication?
- yes
- id
- 2bfa3f6b-e70f-42c6-91fa-a3f2b5e49dd8
- date added to LUP
- 2020-04-03 14:12:49
- date last changed
- 2024-04-17 06:18:30
@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}}, }