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dc.contributor.authorSzigeti, László
dc.contributor.authorMészáros, Szabolcs
dc.contributor.authorSmith, Verne V
dc.contributor.authorCunha, Katia
dc.contributor.authorLagarde, Nadège
dc.contributor.authorCharbonnel, Corinne
dc.contributor.authorGarcía-Hernández, D A
dc.contributor.authorShetrone, Matthew
dc.contributor.authorPinsonneault, Marc
dc.contributor.authorAllende Prieto, Carlos
dc.contributor.authorFernández-Trincado, J G
dc.contributor.authorKovács, József
dc.contributor.authorVillanova, Sandro
dc.date.accessioned2018-03-27T23:13:24Z
dc.date.available2018-03-27T23:13:24Z
dc.date.issued2018-03
dc.identifier.citation12C/13C isotopic ratios in red-giant stars of the open cluster NGC 6791 2018, 474 (4):4810 Monthly Notices of the Royal Astronomical Societyen
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.doi10.1093/mnras/stx3027
dc.identifier.urihttp://hdl.handle.net/10150/627135
dc.description.abstractCarbon 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 C-12/C-13. Values of the C-12/C-13 ratio were obtained from a spectrum synthesis analysis. The derived C-12/C-13 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 C-12/C-13, mass, metallicity, and evolutionary status.
dc.description.sponsorshipHungarian NKFI of the Hungarian National Research, Development and Innovation Office [K-119517]; Hungarian Academy of Sciences; Chilean BASAL Centro de Excelencia an Astrofisica Technologias Afines (CATA) [PFB-06/2007]; Fondecyt [1170518]; Ramon y Cajal fellowship [RYC-2013-14182]; Spanish Ministry of Economy and Competitiveness (MINECO) [AYA-2014-58082-P]; Alfred P. Sloan Foundation; U.S. Department of Energy Office of Science; Center for High-Performance Computing at the University of Utah; Brazilian Participation Group; Carnegie Institution for Science, Carnegie Mellon University; Chilean Participation Group; French Participation Group; Harvard-Smithsonian Center for Astrophysics; Instituto de Astrofisica de Canarias; Johns Hopkins University; Kavli Institute for the Physics and Mathematics of the Universe (IPMU) / University of Tokyo; Lawrence Berkeley National Laboratory; Leibniz Institut fur Astrophysik Potsdam (AIP); Max-Planck- Institut fur Astronomie (MPIA Heidelberg); Max-Planck- Institut fur Astrophysik (MPA Garching); Max-Planck-Institut fur Extraterrestrische Physik (MPE); National Astronomical Observatories of China; New Mexico State University; New York University; University of Notre Dame; Observatorio Nacional / MCTI; Ohio State University; Pennsylvania State University; Shanghai Astronomical Observatory; United Kingdom Participation Group; Universidad Nacional Autonoma de Mexico; 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; Yale Universityen
dc.language.isoenen
dc.publisherOXFORD UNIV PRESSen
dc.relation.urlhttp://academic.oup.com/mnras/article/474/4/4810/4655200en
dc.rights© 2017 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Societyen
dc.subjectstars: abundancesen
dc.subjectstars: evolutionen
dc.subjectstars: late-typeen
dc.subjectstars: low-massen
dc.title12C/13C isotopic ratios in red-giant stars of the open cluster NGC 6791en
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Steward Observen
dc.identifier.journalMonthly Notices of the Royal Astronomical Societyen
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en
dc.eprint.versionFinal published versionen
refterms.dateFOA2018-09-12T07:05:31Z
html.description.abstractCarbon 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 C-12/C-13. Values of the C-12/C-13 ratio were obtained from a spectrum synthesis analysis. The derived C-12/C-13 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 C-12/C-13, mass, metallicity, and evolutionary status.


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