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

Journal Article · · The Astrophysical Journal
ORCiD logo [1]; ORCiD logo [2]; ORCiD logo [3]; ORCiD logo [4]; ORCiD logo [5]; ORCiD logo [4]; ORCiD logo [6]; ORCiD logo [7]; ORCiD logo [8]; ORCiD logo [9]; ORCiD logo [4]; ORCiD logo [10]; ORCiD logo [8];  [11]; ORCiD logo [12]; ORCiD logo [13]; ORCiD logo [4]; ORCiD logo [14]; ORCiD logo [15]; ORCiD logo [16] more »; ORCiD logo [17] « less
  1. Universidade Federal de Sergipe, São Cristóvão, SE (Brazil)
  2. Univ. of Arizona, Tucson, AZ (United States); National Observatory, Rio de Janeiro (Brazil)
  3. NOIRLab, Tucson, AZ (United States)
  4. Univ. of La Laguna, San Cristobal de La Laguna, Tenerife (Spain); Instituto de Astrofísica de Canarias, Tenerife (Spain)
  5. Western Washington University, Bellingham, WA (United States)
  6. New Mexico State Univ., Las Cruces, NM (United States)
  7. Malmo University (Sweden)
  8. Pennsylvania State Univ., University Park, PA (United States)
  9. Univ. of Virginia, Charlottesville, VA (United States)
  10. The Ohio State Univ., Columbus, OH (United States)
  11. Univ. of Texas, Austin, TX (United States). McDonald Observatory
  12. Vanderbilt Univ., Nashville, TN (United States)
  13. Carleton College, Northfield, MN (United States)
  14. Univ. of Colorado, Boulder, CO (United States)
  15. Universidad Bernardo O'Higgins, Santiago (Chile)
  16. Universidad de Antofagasta (Chile)
  17. Universidad de Tarapaca, Arica (Chile)

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.

Research Organization:
US Department of Energy (USDOE), Washington, DC (United States). Office of Science, Sloan Digital Sky Survey (SDSS)
Sponsoring Organization:
USDOE Office of Science (SC); National Science Foundation (NSF); National Aeronautics and Space Administration (NASA); State Research Agency (AEI); European Regional Development Fund (ERDF); National Fund for Scientific and Technological Development (FONDECYT)
Grant/Contract Number:
AST-2009507; 16-XRP16_2-0004; AYA2017-88254-P; 11181295
OSTI ID:
1983227
Journal Information:
The Astrophysical Journal, Vol. 927, Issue 1; ISSN 0004-637X
Publisher:
IOP PublishingCopyright Statement
Country of Publication:
United States
Language:
English

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