TY - JOUR
T1 - Homogeneous analysis of globular clusters from the APOGEE survey with the BACCHUS code - II. The Southern clusters and overview
AU - Mészáros, Szabolcs
AU - Masseron, Thomas
AU - García-Hernández, D. A.
AU - Prieto, Carlos Allende
AU - Beers, Timothy C.
AU - Bizyaev, Dmitry
AU - Chojnowski, Drew
AU - Cohen, Roger E.
AU - Cunha, Katia
AU - Dell'Agli, Flavia
AU - Ebelke, Garrett
AU - Fernández-Trincado, José G.
AU - Frinchaboy, Peter
AU - Geisler, Doug
AU - Hasselquist, Sten
AU - Hearty, Fred
AU - Holtzman, Jon
AU - Johnson, Jennifer
AU - Lane, Richard R.
AU - Lacerna, Ivan
AU - Longa-Peña, Penelopé
AU - Majewski, Steven R.
AU - Martell, Sarah L.
AU - Minniti, Dante
AU - Nataf, David
AU - Nidever, David L.
AU - Pan, Kaike
AU - Schiavon, Ricardo P.
AU - Shetrone, Matthew
AU - Smith, Verne V.
AU - Sobeck, Jennifer S.
AU - Stringfellow, Guy S.
AU - Szigeti, László
AU - Tang, Baitian
AU - Wilson, John C.
AU - Zamora, Olga
N1 - Funding Information:
SzM has been supported by the Premium Postdoctoral Research Program and János Bolyai Research Scholarship of the Hungarian Academy of Sciences, by the Hungarian NKFI Grants K-119517 and GINOP-2.3.2-15-2016-00003 of the Hungarian National Research, Development and Innovation Office. DAGH, TM, OZ, and FDA acknowledge support from the State Research Agency (AEI) of the Spanish Ministry of Science, Innovation and Universities (MCIU) and the European Regional Development Fund (FEDER) under grant AYA2017-88254-P. JGF-T is supported by FONDECYT No. 3180210. DG gratefully acknowledges support from the Chilean Centro de Excelencia en Astrofísicay Tecnologías Afines (CATA) BASAL grant AFB-170002. DG also acknowledges financial support from the Direccin de Investigacin y Desarrollo de la Universidad de La Serena through the Programa de Incentivo a la Investigacin de Acadmicos (PIA-DIDULS). TCB acknowledges partial support from grant PHY 14-30152; Physics Frontier Center/JINA Center for the Evolution of the Elements (JINA-CEE), awarded by the US National Science Foundation, and from the Leverhulme Trust (UK), during his visiting professorship at the University of Hull. SLM acknowledges the support of the Australian Research Council through Discovery Project grant DP180101791. 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-IV 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-IV 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 (MPA Garching), Max-Planck-Institut für Extraterrestrische Physik (MPE), National Astronomical Observatories of China, New Mexico State University, New York University, University of Notre Dame, Observatário Nacional / MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autónoma 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:
© 2019 The Author(s)
PY - 2020/2/1
Y1 - 2020/2/1
N2 - We investigate the Fe, C, N, O, Mg, Al, Si, K, Ca, Ce, and Nd abundances of 2283 red giant stars in 31 globular clusters from high-resolution spectra observed in both the Northern and Southern hemisphere by the SDSS-IV APOGEE-2 survey. This unprecedented homogeneous data set, largest to date, allows us to discuss the intrinsic Fe spread, the shape, and statistics of Al-Mg and N-C anti-correlations as a function of cluster mass, luminosity, age, and metallicity for all 31 clusters. We find that the Fe spread does not depend on these parameters within our uncertainties including cluster metallicity, contradicting earlier observations. We do not confirm the metallicity variations previously observed in M22 and NGC 1851. Some clusters show a bimodal Al distribution, while others exhibit a continuous distribution as has been previously reported in the literature. We confirm more than two populations in ω Cen and NGC 6752, and find new ones in M79. We discuss the scatter of Al by implementing a correction to the standard chemical evolution of Al in the Milky Way. After correction, its dependence on cluster mass is increased suggesting that the extent of Al enrichment as a function of mass was suppressed before the correction. We observe a turnover in the Mg-Al anticorrelation at very low Mg in ω Cen, similar to the pattern previously reported in M15 and M92. ω Cen may also have a weak K-Mg anticorrelation, and if confirmed, it would be only the third cluster known to show such a pattern.
AB - We investigate the Fe, C, N, O, Mg, Al, Si, K, Ca, Ce, and Nd abundances of 2283 red giant stars in 31 globular clusters from high-resolution spectra observed in both the Northern and Southern hemisphere by the SDSS-IV APOGEE-2 survey. This unprecedented homogeneous data set, largest to date, allows us to discuss the intrinsic Fe spread, the shape, and statistics of Al-Mg and N-C anti-correlations as a function of cluster mass, luminosity, age, and metallicity for all 31 clusters. We find that the Fe spread does not depend on these parameters within our uncertainties including cluster metallicity, contradicting earlier observations. We do not confirm the metallicity variations previously observed in M22 and NGC 1851. Some clusters show a bimodal Al distribution, while others exhibit a continuous distribution as has been previously reported in the literature. We confirm more than two populations in ω Cen and NGC 6752, and find new ones in M79. We discuss the scatter of Al by implementing a correction to the standard chemical evolution of Al in the Milky Way. After correction, its dependence on cluster mass is increased suggesting that the extent of Al enrichment as a function of mass was suppressed before the correction. We observe a turnover in the Mg-Al anticorrelation at very low Mg in ω Cen, similar to the pattern previously reported in M15 and M92. ω Cen may also have a weak K-Mg anticorrelation, and if confirmed, it would be only the third cluster known to show such a pattern.
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U2 - 10.1093/mnras/stz3496
DO - 10.1093/mnras/stz3496
M3 - Article
AN - SCOPUS:85082715463
VL - 492
SP - 1641
EP - 1670
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 2
ER -