4.7 Article

A Metallicity Study of F, G, K, and M Dwarfs in the Coma Berenices Open Cluster from the APOGEE Survey

期刊

ASTROPHYSICAL JOURNAL
卷 917, 期 1, 页码 -

出版社

IOP Publishing Ltd
DOI: 10.3847/1538-4357/abfdb5

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资金

  1. National Aeronautics and Space Administration [16-XRP16_2-0004, 18-2ADAP18-0113]
  2. Alfred P. Sloan Foundation
  3. U.S. Department of Energy Office of Science
  4. Brazilian Participation Group
  5. Carnegie Institution for Science
  6. Carnegie Mellon University
  7. Chilean Participation Group
  8. French Participation Group
  9. Harvard-Smithsonian Center for Astrophysics
  10. Instituto de Astrofisica de Canarias
  11. Johns Hopkins University
  12. Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo
  13. Lawrence Berkeley National Laboratory
  14. Leibniz Institut fur Astrophysik Potsdam (AIP)
  15. Max-Planck-Institut fur Astronomie (MPIA Heidelberg)
  16. Max-Planck-Institut fur Astrophysik (MPA Garching)
  17. Max-Planck-Institut fur Extraterrestrische Physik (MPE)
  18. National Astronomical Observatory of China
  19. New Mexico State University
  20. New York University
  21. University of Notre Dame
  22. Observatorio Nacional/MCTI
  23. Ohio State University
  24. Pennsylvania State University
  25. Shanghai Astronomical Observatory
  26. United Kingdom Participation Group
  27. Universidad Nacional Autonoma de Mexico
  28. University of Arizona
  29. University of Colorado Boulder
  30. University of Oxford
  31. University of Portsmouth
  32. University of Utah
  33. University of Virginia
  34. University of Washington
  35. University of Wisconsin
  36. Vanderbilt University
  37. Yale University
  38. Center for High Performance Computing at the University of Utah

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The study investigated metallicities in main-sequence stars of the young open cluster Coma Berenices using high-resolution NIR spectra, finding that metallicities are near-solar and homogeneous within the same stellar class. F-type stars showed slightly lower metallicities compared to cooler members, with atomic diffusion potentially playing a role. This dip in [Fe/H] occurred in a similar effective temperature range as seen in previous lithium and beryllium abundance analyses in the cluster.
We present a study of metallicities in a sample of main-sequence stars with spectral types M, K, G, and F (T (eff) similar to 3200-6500K and log g similar to 4.3-5.0 dex) belonging to the solar neighborhood young open cluster Coma Berenices. Metallicities were determined using the high-resolution (R = lambda/Delta lambda similar to 22,500) NIR spectra (lambda 1.51-lambda 1.69 mu m) of the Sloan Digital Sky Survey IV APOGEE survey. Membership to the cluster was confirmed using previous studies in the literature along with APOGEE radial velocities and Gaia DR2. An LTE analysis using plane-parallel MARCS model atmospheres and the APOGEE DR16 line list was adopted to compute synthetic spectra and derive atmospheric parameters (T (eff) and log g) for the M dwarfs and metallicities for the sample. The derived metallicities are near-solar and are homogeneous at the level of the expected uncertainties, in particular when considering stars from a given stellar class. The mean metallicity computed for the sample of G, K, and M dwarfs is [Fe/H] = +0.04 +/- 0.02 dex; however, the metallicities of the F-type stars are slightly lower, by about 0.04 dex, when compared to cooler and less massive members. Models of atomic diffusion can explain this modest abundance dip for the F dwarfs, indicating that atomic diffusion operates in Coma Berenices stars. The [Fe/H] dip occurs in nearly the same effective temperature range as that found in previous analyses of the lithium and beryllium abundances in Coma Berenices.

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