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Chemical abundances of the young inner-disc open cluster NGC 6705 observed by APOGEE: sodium-rich and not α-enhanced

Journal Article · · Monthly Notices of the Royal Astronomical Society
 [1];  [2];  [3];  [4];  [1];  [5];  [1];  [6];  [7];  [8];  [9];  [1];  [10];  [11];  [12];  [13];  [14];  [15];  [16];  [17] more »;  [18];  [19] « less
  1. Observatório Nacional, Rio de Janeiro (Brazil)
  2. Observatório Nacional, Rio de Janeiro (Brazil); University of Arizona, Tucson, AZ (United States); Sorbonne Université, Paris (France)
  3. Universidade Federal de Sergipe (Brazil)
  4. Sorbonne Université, Paris (France); NSF’s NOIRLab, Tucson, AZ (United States)
  5. Leibniz-Institut für Astrophysik Potsdam (AIP), Potsdam (Germany)
  6. Flatiron Institute, New York, NY (United States)
  7. Universidad de La Laguna, Tenerife (Spain)
  8. The Observatories of the Carnegie Institution for Science, Pasadena, CA (United States)
  9. Apache Point Observatory and New Mexico State University, Sunspot, NM (United States); Moscow State University (Russia)
  10. Texas Christian University, Fort Worth, TX (United States)
  11. Space Telescope Science Institute, Baltimore, MD (United States)
  12. NRC Herzberg Astronomy and Astrophysics Research Centre, Victoria, BC (Canada)
  13. New Mexico State University, Las Cruces, NM (United States)
  14. Malmö University (Sweden)
  15. University of Virginia, Charlottesville, VA (United States)
  16. ELTE Eötvös Loránd University (Hungary); MTA-ELTE Lendület ‘Momentum’ Milky Way Research Group (Hungary)
  17. Montana State University, Bozeman, MT (United States)
  18. The Ohio State University, Columbus, OH (United States)
  19. University of Utah, Salt Lake City, UT (United States)
+ Show Author Affiliations
Previous results in the literature have found the young inner-disc open cluster NGC 6705 to be mildly α-enhanced. We examined this possibility via an independent chemical abundance analysis for 11 red-giant members of NGC 6705. The analysis is based on near-infrared APOGEE spectra and relies on LTE calculations using spherical model atmospheres and radiative transfer. We find a mean cluster metallicity of $$\rm [Fe/H] = +0.13 \pm 0.04$$, indicating that NGC 6705 is metal-rich, as may be expected for a young inner-disc cluster. The mean α-element abundance relative to iron is $$\rm \langle [\alpha /Fe]\rangle =-0.03 \pm 0.05$$, which is not at odds with expectations from general Galactic abundance trends. NGC 6705 also provides important probes for studying stellar mixing, given its turn-off mass of M ∼ 3.3 M⊙. Its red giants have low 12C abundances ([12C/Fe] = −0.16) and enhanced 14N abundances ([14N/Fe] = +0.51), which are key signatures of the first dredge-up on the red giant branch. An additional signature of dredge-up was found in the Na abundances, which are enhanced by [Na/Fe] = +0.29, with a very small non-LTE correction. The 16O and Al abundances are found to be near-solar. All of the derived mixing-sensitive abundances are in agreement with stellar models of approximately 3.3 M⊙ evolving along the red giant branch and onto the red clump. As found in young open clusters with similar metallicities, NGC 6705 exhibits a mild excess in the s-process element cerium with $$\rm [Ce/Fe] = +0.13\pm 0.07$$.
Research Organization:
US Department of Energy (USDOE), Washington, DC (United States). Office of Science, Sloan Digital Sky Survey (SDSS)
Sponsoring Organization:
National Science Foundation (NSF); USDOE; USDOE Office of Science (SC)
OSTI ID:
2007558
Alternate ID(s):
OSTI ID: 2425121
Journal Information:
Monthly Notices of the Royal Astronomical Society, Journal Name: Monthly Notices of the Royal Astronomical Society Journal Issue: 2 Vol. 526; ISSN 0035-8711
Publisher:
Oxford University PressCopyright Statement
Country of Publication:
United States
Language:
English

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Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
Astronomy & Astrophysics
Galaxy: inner disc
infrared: stars
stars: abundances
stars: giants
stars: open cluster