TY - JOUR
T1 - Detailed Chemical Abundances for a Benchmark Sample of M Dwarfs from the APOGEE Survey
AU - Souto, Diogo
AU - Cunha, Katia
AU - Smith, Verne V.
AU - Prieto, C. Allende
AU - Covey, Kevin
AU - García-Hernández, D. A.
AU - Holtzman, Jon A.
AU - Jönsson, Henrik
AU - Mahadevan, Suvrath
AU - Majewski, Steven R.
AU - Masseron, Thomas
AU - Pinsonneault, Marc
AU - Schneider, Donald P.
AU - Shetrone, Matthew
AU - Stassun, Keivan G.
AU - Terrien, Ryan
AU - Zamora, Olga
AU - Stringfellow, Guy S.
AU - Lane, Richard R.
AU - Nitschelm, Christian
AU - Rojas-Ayala, Bárbara
N1 - Funding Information:
Funding for the Sloan Digital Sky Survey-IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS website is www.sdss.org .
Funding Information:
K.C. and V.S. acknowledge that their work here is supported, in part, by the National Science Foundation through NSF grant No. AST-2009507, as well as by the National Aeronautics and Space Administration under grant No. 16-XRP16_2-0004, issued through the Astrophysics Division of the Science Mission Directorate. D.A.G.H., O.Z., and T.M. acknowledge support from the State Research Agency (AEI) of the Ministry of Science, Innovation and Universities (MCIU) and the European Regional Development Fund (FEDER) under grant No. AYA2017-88254-P. S.M. acknowledges the Penn State’s Center for Exoplanets and Habitable worlds. B.R.-A. acknowledges funding support from FONDECYT through grant No. 11181295.
Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.
PY - 2022/3/1
Y1 - 2022/3/1
N2 - 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], Teff, 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.
AB - 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], Teff, 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.
UR - http://www.scopus.com/inward/record.url?scp=85126628850&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85126628850&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/ac4891
DO - 10.3847/1538-4357/ac4891
M3 - Article
AN - SCOPUS:85126628850
SN - 0004-637X
VL - 927
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 123
ER -