Bibliographic Details
| Title: |
Stellar Characterization of M Dwarfs from the APOGEE Survey: A Calibrator Sample for M-dwarf Metallicities. |
| Authors: |
Diogo Souto1,2 souto@on.br, Katia Cunha2,3, Verne V. Smith4, C. Allende Prieto5,6, Adam Burgasser7, Kevin Covey8, D. A. García-Hernández5,6, Jon A. Holtzman9, Jennifer A. Johnson10, Henrik Jönsson11,12, Suvrath Mahadevan13, Steven R. Majewski14, Thomas Masseron5,6, Matthew Shetrone15, Bárbara Rojas-Ayala16, Jennifer Sobeck14, Keivan G. Stassun17, Ryan Terrien18, Johanna Teske19,20, Fábio Wanderley2 |
| Source: |
Astrophysical Journal. 2/20/2020, Vol. 890 Issue 2, p1-1. 1p. |
| Subject Terms: |
*DWARF stars, *GALACTIC evolution, *MAIN sequence (Astronomy), *ECLIPSING binaries, *ASTRONOMICAL surveys, *BINARY stars |
| Company/Entity: |
SLOAN Digital Sky Survey |
| 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 Teff 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 –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⊙. 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. [ABSTRACT FROM AUTHOR] |
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