TY - JOUR
T1 - 12C/13C isotopic ratios in red-giant stars of the open cluster NGC 6791
AU - Szigeti, László
AU - Mészáros, Szabolcs
AU - Smith, Verne V.
AU - Cunha, Katia
AU - Lagarde, Nadège
AU - Charbonnel, Corinne
AU - García-Hernández, D. A.
AU - Shetrone, Matthew
AU - Pinsonneault, Marc
AU - Prieto, Carlos Allende
AU - Fernández-Trincado, J. G.
AU - Kovács, József
AU - Villanova, Sandro
N1 - Funding Information:
L Sz and SzM have been supported by the Hungarian NKFI Grants K-119517 of the Hungarian National Research, Development and Innovation Office. SzM has been supported by the Premium Postdoctoral Research Program of the Hungarian Academy of Sciences. JGF-T gratefully acknowledges support from the Chilean BASAL Centro de Excelencia an Astrofísica Technologías Afines (CATA) grant PFB-06/2007. SV gratefully acknowledges the support provided by Fondecyt reg. n. 1170518. DAGH was funded by the Ramon y Cajal fellowship number RYC-2013-14182 and he acknowledges support provided by the Spanish Ministry of Economy and Competitiveness (MINECO) under grant AYA-2014-58082-P. 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 acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS web site is www.sdss.org. SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, Harvard-Smithsonian Center for Astrophysics, Instituto de Astrofísica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU) / University of Tokyo, Lawrence Berkeley National Laboratory, Leibniz Institut für Astrophysik Potsdam (AIP), Max-Planck-Institut für Astronomie (MPIA Heidelberg), Max-Planck-Institut für Astrophysik (MPAGarching), Max-Planck-Institut für Extraterrestrische Physik (MPE), National Astronomical Observatories of China, New Mexico State University, New York University, University of Notre Dame, Observatorio Nacional / MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autonoma de México, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University
Publisher Copyright:
© 2017 The Author(s).
PY - 2018/3/1
Y1 - 2018/3/1
N2 - Carbon isotope ratios, along with carbon and nitrogen abundances, are derived in a sample of 11 red-giant members of one of the most metal-rich clusters in the Milky Way, NGC 6791. The selected red-giants have a mean metallicity and standard deviation of [Fe/H] = +0.39 ± 0.06 (Cunha et al. 2015). We used high-resolution H-band spectra obtained by the SDSS-IV Apache Point Observatory Galactic Evolution Experiment. The advantage of using high-resolution spectra in the H band is that lines of CO are well represented and their line profiles are sensitive to the variation of 12C/13C. Values of the 12C/13C ratio were obtained from a spectrum synthesis analysis. The derived 12C/13C ratios varied between 6.3 and 10.6 in NGC 6791, in agreement with the final isotopic ratios from thermohaline-induced mixing models. The ratios derived here are combined with those obtained for more metal poor red-giants from the literature to examine the correlation between 12C/13C, mass, metallicity, and evolutionary status.
AB - Carbon isotope ratios, along with carbon and nitrogen abundances, are derived in a sample of 11 red-giant members of one of the most metal-rich clusters in the Milky Way, NGC 6791. The selected red-giants have a mean metallicity and standard deviation of [Fe/H] = +0.39 ± 0.06 (Cunha et al. 2015). We used high-resolution H-band spectra obtained by the SDSS-IV Apache Point Observatory Galactic Evolution Experiment. The advantage of using high-resolution spectra in the H band is that lines of CO are well represented and their line profiles are sensitive to the variation of 12C/13C. Values of the 12C/13C ratio were obtained from a spectrum synthesis analysis. The derived 12C/13C ratios varied between 6.3 and 10.6 in NGC 6791, in agreement with the final isotopic ratios from thermohaline-induced mixing models. The ratios derived here are combined with those obtained for more metal poor red-giants from the literature to examine the correlation between 12C/13C, mass, metallicity, and evolutionary status.
KW - Stars: abundances
KW - Stars: evolution
KW - Stars: late-type
KW - Stars: low-mass
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U2 - 10.1093/mnras/stx3027
DO - 10.1093/mnras/stx3027
M3 - Article
AN - SCOPUS:85049190789
VL - 474
SP - 4810
EP - 4817
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 4
ER -