Abstract
We present an elemental abundance analysis of high-resolution spectra for five giant stars spatially located within the innermost regions of the bulge globular cluster NGC 6522 and derive Fe, Mg, Al, C, N, O, Si, and Ce abundances based on H-band spectra taken with the multi-object APOGEE-north spectrograph from the SDSS-IV Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey. Of the five cluster candidates, two previously unremarked stars are confirmed to have second-generation (SG) abundance patterns, with the basic pattern of depletion in C and Mg simultaneous with enrichment in N and Al as seen in other SG globular cluster populations at similar metallicity. In agreement with the most recent optical studies, the NGC 6522 stars analyzed exhibit (when available) only mild overabundances of the s-process element Ce, contradicting the idea that NGC 6522 stars are formed from gas enriched by spinstars and indicating that other stellar sources such as massive AGB stars could be the primary polluters of intra-cluster medium. The peculiar abundance signatures of SG stars have been observed in our data, confirming the presence of multiple generations of stars in NGC 6522.
| Original language | English (US) |
|---|---|
| Article number | A178 |
| Journal | Astronomy and Astrophysics |
| Volume | 627 |
| DOIs | |
| State | Published - Jul 1 2019 |
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science
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In: Astronomy and Astrophysics, Vol. 627, A178, 01.07.2019.
Research output: Contribution to journal › Article › peer-review
TY - JOUR
T1 - H-band discovery of additional second-generation stars in the Galactic bulge globular cluster NGC 6522 as observed by APOGEE and Gaia
AU - Fernández-Trincado, J. G.
AU - Zamora, O.
AU - Souto, Diogo
AU - Cohen, R. E.
AU - Dell'Agli, F.
AU - García-Hernández, D. A.
AU - Masseron, T.
AU - Schiavon, R. P.
AU - Mészáros, Sz
AU - Cunha, K.
AU - Hasselquist, S.
AU - Shetrone, M.
AU - Schiappacasse Ulloa, J.
AU - Tang, B.
AU - Geisler, D.
AU - Schleicher, D. R.G.
AU - Villanova, S.
AU - Mennickent, R. E.
AU - Minniti, D.
AU - Alonso-García, J.
AU - Manchado, A.
AU - Beers, T. C.
AU - Sobeck, J.
AU - Zasowski, G.
AU - Schultheis, M.
AU - Majewski, S. R.
AU - Rojas-Arriagada, A.
AU - Almeida, A.
AU - Santana, F.
AU - Oelkers, R. J.
AU - Longa-Peña, P.
AU - Carrera, R.
AU - Burgasser, A. J.
AU - Lane, R. R.
AU - Roman-Lopes, A.
AU - Ivans, I. I.
AU - Hearty, F. R.
N1 - Funding Information: Acknowledgements. We would like to thank the referee for insightful comments which helped to improve this work. J.G.F-T, P.L-P, and J.A-G were supported by MINEDUC-UA project, code ANT 1855. J.G.F-T also acknowledges financial support from the FONDECYT No. 3180210 and the ChETEC COST Action (CA16117), supported by COST (European Cooperation in Science and Technology). D.G. gratefully acknowledges support from the Chilean Centro de Excelencia en Astrofísica y Tecnologías Afines (CATA) BASAL grant AFB-170002. D.G. also acknowledges financial support from the Dirección de Investigación y Desarrollo de la Universidad de La Serena through the Pro-grama de Incentivo a la Investigación de Académicos (PIA-DIDULS). S.V gratefully acknowledges the support provided by Fondecyt reg. n. 1170518. Szabolcs Mészáros has been supported by the Premium Postdoctoral Research Program of the Hungarian Academy of Sciences, and by the Hungarian NKFI Grants K-119517 of the Hungarian National Research, Development and Innovation Office. R.E.M. acknowledges project fondecyt 1190621. D.M. and J.A-G. are supported also by FONDECYT No. 1170121 and 11150916 respectively, and by the Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC120009, awarded to the Millennium Institute of Astrophysics (MAS). DAGH, OZ, FDA, and TM 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. T.C.B. 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. BACCHUS have been executed on computers from the Institute of Astronomy and Planetary Sciences at Universidad de Atacama. This work has made use of results from the European Space Agency (ESA) space mission Gaia, the data from which were processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. The Gaia mission website is http://www.cosmos.esa.int/gaia. 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 Astrofìsica 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 Observatory of China, New Mexico State University, New York University, University of Dame, Observatório 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. Funding Information: We would like to thank the referee for insightful comments which helped to improve this work. J.G.F-T, P.L-P, and J.A-G were supported by MINEDUC-UA project, code ANT 1855. J.G.F-T also acknowledges financial support from the FONDECYT No. 3180210 and the ChETEC COST Action (CA16117), supported by COST (European Cooperation in Science and Technology). D.G. gratefully acknowledges support from the Chilean Centro de Excelencia en Astrof?sica y Tecnolog?as Afines (CATA) BASAL grant AFB-170002. D.G. also acknowledges financial support from the Direcci?n de Investigaci?n y Desarrollo de la Universidad de La Serena through the Programa de Incentivo a la Investigaci?n de Acad?micos (PIA-DIDULS). S.V gratefully acknowledges the support provided by Fondecyt reg. n. 1170518. Szabolcs M?sz?ros has been supported by the Premium Postdoctoral Research Program of the Hungarian Academy of Sciences, and by the Hungarian NKFI Grants K-119517 of the Hungarian National Research, Development and Innovation Office. R.E.M. acknowledges project fondecyt 1190621. D.M. and J.A-G. are supported also by FONDECYT No. 1170121 and 11150916 respectively, and by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to the Millennium Institute of Astrophysics (MAS). DAGH, OZ, FDA, and TM 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. T.C.B. 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. BACCHUS have been executed on computers from the Institute of Astronomy and Planetary Sciences at Universidad de Atacama. This work has made use of results from the European Space Agency (ESA) space mission Gaia, the data from which were processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. The Gaia mission website is http://www.cosmos.esa.int/gaia. 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 Astrof?sica 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 f?r Astrophysik Potsdam (AIP), Max-Planck-Institut f?r Astronomie (MPIA Heidelberg), Max-Planck-Institut f?r Astrophysik (MPA Garching), Max-Planck-Institut f?r Extraterrestrische Physik (MPE), National Astronomical Observatory of China, New Mexico State University, New York University, University of Dame, Observat?rio Nacional / MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Aut?noma de M?xico, 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: © J. G. Fernández-Trincado et al. 2019.
PY - 2019/7/1
Y1 - 2019/7/1
N2 - We present an elemental abundance analysis of high-resolution spectra for five giant stars spatially located within the innermost regions of the bulge globular cluster NGC 6522 and derive Fe, Mg, Al, C, N, O, Si, and Ce abundances based on H-band spectra taken with the multi-object APOGEE-north spectrograph from the SDSS-IV Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey. Of the five cluster candidates, two previously unremarked stars are confirmed to have second-generation (SG) abundance patterns, with the basic pattern of depletion in C and Mg simultaneous with enrichment in N and Al as seen in other SG globular cluster populations at similar metallicity. In agreement with the most recent optical studies, the NGC 6522 stars analyzed exhibit (when available) only mild overabundances of the s-process element Ce, contradicting the idea that NGC 6522 stars are formed from gas enriched by spinstars and indicating that other stellar sources such as massive AGB stars could be the primary polluters of intra-cluster medium. The peculiar abundance signatures of SG stars have been observed in our data, confirming the presence of multiple generations of stars in NGC 6522.
AB - We present an elemental abundance analysis of high-resolution spectra for five giant stars spatially located within the innermost regions of the bulge globular cluster NGC 6522 and derive Fe, Mg, Al, C, N, O, Si, and Ce abundances based on H-band spectra taken with the multi-object APOGEE-north spectrograph from the SDSS-IV Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey. Of the five cluster candidates, two previously unremarked stars are confirmed to have second-generation (SG) abundance patterns, with the basic pattern of depletion in C and Mg simultaneous with enrichment in N and Al as seen in other SG globular cluster populations at similar metallicity. In agreement with the most recent optical studies, the NGC 6522 stars analyzed exhibit (when available) only mild overabundances of the s-process element Ce, contradicting the idea that NGC 6522 stars are formed from gas enriched by spinstars and indicating that other stellar sources such as massive AGB stars could be the primary polluters of intra-cluster medium. The peculiar abundance signatures of SG stars have been observed in our data, confirming the presence of multiple generations of stars in NGC 6522.
UR - http://www.scopus.com/inward/record.url?scp=85070098334&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85070098334&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/201834391
DO - 10.1051/0004-6361/201834391
M3 - Article
AN - SCOPUS:85070098334
SN - 0004-6361
VL - 627
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A178
ER -