Detailed Chemical Abundances for a Benchmark Sample of M Dwarfs from the APOGEE Survey

Souto, Diogo; Cunha, Katia; Smith, Verne V.; Prieto, C. Allende; Covey, Kevin; García-Hernández, D. A.; Holtzman, Jon A.; Jönsson, Henrik; Mahadevan, Suvrath; Majewski, Steven R.; Masseron, Thomas; Pinsonneault, Marc; Schneider, Donald P.; Shetrone, Matthew; Stassun, Keivan G.; Terrien, Ryan; Zamora, Olga; Stringfellow, Guy S.; Lane, Richard R.; Nitschelm, Christian; Rojas-Ayala, Bárbara
Referencia bibliográfica

The Astrophysical Journal

Fecha de publicación:
3
2022
Número de autores
21
Número de autores del IAC
4
Número de citas
18
Número de citas referidas
15
Descripción
Individual chemical abundances for 14 elements (C, O, Na, Mg, Al, Si, K, Ca, Ti, V, Cr, Mn, Fe, and Ni) are derived for a sample of M dwarfs using high-resolution, near-infrared H-band spectra from the Sloan Digital Sky Survey-IV/Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey. The quantitative analysis included synthetic spectra computed with 1D LTE plane-parallel MARCS models using the APOGEE Data Release 17 line list to determine chemical abundances. The sample consists of 11 M dwarfs in binary systems with warmer FGK dwarf primaries and 10 measured interferometric angular diameters. To minimize atomic diffusion effects, [X/Fe] ratios are used to compare M dwarfs in binary systems and literature results for their warmer primary stars, indicating good agreement (<0.08 dex) for all studied elements. The mean abundance difference in primaries minus this work's M dwarfs is -0.05 ± 0.03 dex. It indicates that M dwarfs in binary systems are a reliable way to calibrate empirical relationships. A comparison with abundance, effective temperature, and surface gravity results from the APOGEE Stellar Parameter and Chemical Abundances Pipeline (ASPCAP) Data Release 16 finds a systematic offset of [M/H], T eff, log g = +0.21 dex, -50 K, and 0.30 dex, respectively, although ASPCAP [X/Fe] ratios are generally consistent with this study. The metallicities of the M dwarfs cover the range of [Fe/H] = -0.9 to +0.4 and are used to investigate Galactic chemical evolution via trends of [X/Fe] as a function of [Fe/H]. The behavior of the various elemental abundances [X/Fe] versus [Fe/H] agrees well with the corresponding trends derived from warmer FGK dwarfs, demonstrating that the APOGEE spectra can be used to examine Galactic chemical evolution using large samples of selected M dwarfs.
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