Abstract
Context. Bulge globular clusters (BGCs) are exceptional tracers of the formation and chemodynamical evolution of this oldest Galactic component. However, until now, observational difficulties have prevented us from taking full advantage of these powerful Galactic archeological tools. Aims. CAPOS, the bulge Cluster APOgee Survey, addresses this key topic by observing a large number of BGCs, most of which have only been poorly studied previously. Even their most basic parameters, such as metallicity, [α/Fe], and radial velocity, are generally very uncertain. We aim to obtain accurate mean values for these parameters, as well as abundances for a number of other elements, and explore multiple populations. In this first paper, we describe the CAPOS project and present initial results for seven BGCs. Methods. CAPOS uses the APOGEE-2S spectrograph observing in the H band to penetrate obscuring dust toward the bulge. For this initial paper, we use abundances derived from ASPCAP, the APOGEE pipeline. Results. We derive mean [Fe/H] values of -0.85 ± 0.04 (Terzan 2), -1.40 ± 0.05 (Terzan 4), -1.20 ± 0.10 (HP 1), -1.40 ± 0.07 (Terzan 9), -1.07 ± 0.09 (Djorg 2), -1.06 ± 0.06 (NGC 6540), and -1.11 ± 0.04 (NGC 6642) from three to ten stars per cluster. We determine mean abundances for eleven other elements plus the mean [α/Fe] and radial velocity. CAPOS clusters significantly increase the sample of well-studied Main Bulge globular clusters (GCs) and also extend them to lower metallicity. We reinforce the finding that Main Bulge and Main Disk GCs, formed in situ, have [Si/Fe] abundances slightly higher than their accreted counterparts at the same metallicity. We investigate multiple populations and find our clusters generally follow the light-element (anti)correlation trends of previous studies of GCs of similar metallicity. We finally explore the abundances of the iron-peak elements Mn and Ni and compare their trends with field populations. Conclusions. CAPOS is proving to be an unprecedented resource for greatly improving our knowledge of the formation and evolution of BGCs and the bulge itself.
| Original language | English (US) |
|---|---|
| Article number | A157 |
| Journal | Astronomy and astrophysics |
| Volume | 652 |
| DOIs | |
| State | Published - Aug 1 2021 |
Keywords
- Galaxy: bulge
- Globular clusters: general
- Stars: abundances
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science
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CAPOS : The bulge Cluster APOgee Survey: I. Overview and initial ASPCAP results. / Geisler, D.; Villanova, S.; O'Connell, J. E. et al.
In: Astronomy and astrophysics, Vol. 652, A157, 01.08.2021.Research output: Contribution to journal › Article › peer-review
}
TY - JOUR
T1 - CAPOS
T2 - The bulge Cluster APOgee Survey: I. Overview and initial ASPCAP results
AU - Geisler, D.
AU - Villanova, S.
AU - O'Connell, J. E.
AU - Cohen, R. E.
AU - Moni Bidin, C.
AU - Fernández-Trincado, J. G.
AU - Muñoz, C.
AU - Minniti, D.
AU - Zoccali, M.
AU - Rojas-Arriagada, A.
AU - Contreras Ramos, R.
AU - Catelan, M.
AU - Mauro, F.
AU - Cortés, C.
AU - Ferreira Lopes, C. E.
AU - Arentsen, A.
AU - Starkenburg, E.
AU - Martin, N. F.
AU - Tang, B.
AU - Parisi, C.
AU - Alonso-García, J.
AU - Gran, F.
AU - Cunha, K.
AU - Smith, V.
AU - Majewski, S. R.
AU - Jönsson, H.
AU - García-Hernández, D. A.
AU - Horta, D.
AU - Mészáros, S.
AU - Monaco, L.
AU - Monachesi, A.
AU - Muñoz, R. R.
AU - Brownstein, J.
AU - Beers, T. C.
AU - Lane, R. R.
AU - Barbuy, B.
AU - Sobeck, J.
AU - Henao, L.
AU - González-DÍaz, D.
AU - Miranda, R. E.
AU - Reinarz, Y.
AU - Santander, T. A.
N1 - Funding Information: Acknowledgements. This paper is dedicated to the memory of George Wallerstein. George was a true pioneer in the field of detailed abundance studies of globular clusters, as well as making many other stellar contributions. He was the founding father of the Astronomy Department of the University of Washington, where he taught many generations of future astronomers, and was the thesis advisor of both the first author and V.S. We would like to warmly acknowledge SDSS-IV and especially all of those who have contributed to the outstanding success of both APOGEE North and South, including M. Skrutskie and J. Wilson for the original idea, S. Majewski and K. Cunha for the original science motivation, Majewski, Skrutskie and Wilson for putting together and carrying out the project, V. Smith, K. Cunha and C. Allende-Prieto for helping identify species and their transitions, and Allende-Prieto, J. Holtzman and D. Nide-ver for developing the ASPCAP pipeline. We are deeply grateful to all those responsible for carrying out all phases of the CAPOS observations, especially the observation of the last field, which was the only bulge field observed by APOGEE-2S during all of 2019. We thank David Nataf, Louise Howes and Martin Asplund, who provided us access to the EMBLA sources. D.G., S.V., J.E.O., M.C., D.M., M.Z., J.A.-G., F.M. and R.R.M. gratefully acknowledge 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 Programa de Incentivo a la Investigación de Académi-cos (PIA-DIDULS), as well as the moral and amorous support of M.E. Bar-raza. S.V. gratefully acknowledges the support provided by FONDECYT Regular No. 1170518. J.G.F-T is supported by FONDECYT No. 3180210 and Becas Iberoamérica Investigador 2019, Banco Santander Chile. D.M. is also supported by the ANID – Millennium Science Initiative Project ICN12_009, awarded to the Millenium Institute of Astrophysics (MAS) and by Proyecto FONDECYT No. 1170121. Support for M.C., D.M., M.Z., J.A.-G, and F.M. is also provided by MAS and by FONDECYT projects #1171273 and #1191505. C.M. thanks the support provided by ANID through Beca Postdoctorado en el Extranjero convo-catoria 2018 folio 74190045. C.M. thanks the support provided by FONDECYT Postdoctorado No.3210144. Financial support for C.C. is provided by Proyecto FONDECYT Iniciación a la Investigación 11150768 and MAS. B.T. gratefully acknowledges support from the National Natural Science Foundation of China under grant No. U1931102 and support from the Hundred-Talent Project of Sun Yat-sen University. J.A.-G. acknowledges support by Proyecto Fondecyt Regular 1201490. A.M. and C.M. acknowledge support by FONDECYT Regular 1181797. C. E. F. L. acknowledges a postdoctoral fellowship from the CNPq and to MCTIC/FINEP (CT-INFRA grant 0112052700) and the EmbraceSpace Weather Program for the computing facilities at INPE. D.G.D. acknowledges support from call N.785 of 2017 of the Colombian Departamento Administra-tivo de Ciencia, Tecnología e Innovación, COLCIENCIAS. A.A. and E.S. gratefully acknowledge funding by the Emmy Noether program from the Deutsche Forschungsgemeinschaft (DFG). N.F.M. gratefully acknowledges support from the French National Research Agency (ANR) funded project “Pristine” (ANR-18-CE31-0017) along with funding from CNRS/INSU through the Programme National Galaxies et Cosmologie and through the CNRS grant PICS07708. A.A., E.S. and N.F.M. thank the International Space Science Institute, Bern, Switzerland for providing financial support and meeting facilities to the international Funding Information: team “Pristine”. SzM has been supported by the János Bolyai Research Scholarship of the Hungarian Academy of Sciences, by the Hungarian NKFI Grants K-119517 of the Hungarian National Research, Development and Innovation Office, and by the ÚNKP-20-4 New National Excellence Program of the Ministry for Innovation and Technology. Funding for LH was provided by the Chilean National Agency for Research and Development (ANID)/CONICYT-PFCHA/DOCTORADO NACIONAL/2017-21171231 grant. 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. R.R.M. also acknowledges partial support from FONDECYT project N◦1170364. C.M. also acknowledges the support provided by FONDECYT No. 1181797. F.G. acknowledges support by CONICYT-PCHA Doctorado Nacional 2017-21171485. D.A.G.H. acknowledges 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. We also thank the referee for useful comments that improved the paper. Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the US 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. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www. cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. Based on observations obtained through the Chilean National Telescope Allocation Committee through programs CN2017B-37, CN2018A-20, CN2018B-46, CN2019A-98 and CN2019B-31. Partly based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l’Univers of the Centre National de la Recherche Scien-tifique (CNRS) of France, and the University of Hawaii. We gratefully acknowledge the use of data from the ESO Public Survey program ID 179.B-2002 taken with the VISTA telescope and data products from the Cambridge Astronomical Survey Unit. Publisher Copyright: © ESO 2021.
PY - 2021/8/1
Y1 - 2021/8/1
N2 - Context. Bulge globular clusters (BGCs) are exceptional tracers of the formation and chemodynamical evolution of this oldest Galactic component. However, until now, observational difficulties have prevented us from taking full advantage of these powerful Galactic archeological tools. Aims. CAPOS, the bulge Cluster APOgee Survey, addresses this key topic by observing a large number of BGCs, most of which have only been poorly studied previously. Even their most basic parameters, such as metallicity, [α/Fe], and radial velocity, are generally very uncertain. We aim to obtain accurate mean values for these parameters, as well as abundances for a number of other elements, and explore multiple populations. In this first paper, we describe the CAPOS project and present initial results for seven BGCs. Methods. CAPOS uses the APOGEE-2S spectrograph observing in the H band to penetrate obscuring dust toward the bulge. For this initial paper, we use abundances derived from ASPCAP, the APOGEE pipeline. Results. We derive mean [Fe/H] values of -0.85 ± 0.04 (Terzan 2), -1.40 ± 0.05 (Terzan 4), -1.20 ± 0.10 (HP 1), -1.40 ± 0.07 (Terzan 9), -1.07 ± 0.09 (Djorg 2), -1.06 ± 0.06 (NGC 6540), and -1.11 ± 0.04 (NGC 6642) from three to ten stars per cluster. We determine mean abundances for eleven other elements plus the mean [α/Fe] and radial velocity. CAPOS clusters significantly increase the sample of well-studied Main Bulge globular clusters (GCs) and also extend them to lower metallicity. We reinforce the finding that Main Bulge and Main Disk GCs, formed in situ, have [Si/Fe] abundances slightly higher than their accreted counterparts at the same metallicity. We investigate multiple populations and find our clusters generally follow the light-element (anti)correlation trends of previous studies of GCs of similar metallicity. We finally explore the abundances of the iron-peak elements Mn and Ni and compare their trends with field populations. Conclusions. CAPOS is proving to be an unprecedented resource for greatly improving our knowledge of the formation and evolution of BGCs and the bulge itself.
AB - Context. Bulge globular clusters (BGCs) are exceptional tracers of the formation and chemodynamical evolution of this oldest Galactic component. However, until now, observational difficulties have prevented us from taking full advantage of these powerful Galactic archeological tools. Aims. CAPOS, the bulge Cluster APOgee Survey, addresses this key topic by observing a large number of BGCs, most of which have only been poorly studied previously. Even their most basic parameters, such as metallicity, [α/Fe], and radial velocity, are generally very uncertain. We aim to obtain accurate mean values for these parameters, as well as abundances for a number of other elements, and explore multiple populations. In this first paper, we describe the CAPOS project and present initial results for seven BGCs. Methods. CAPOS uses the APOGEE-2S spectrograph observing in the H band to penetrate obscuring dust toward the bulge. For this initial paper, we use abundances derived from ASPCAP, the APOGEE pipeline. Results. We derive mean [Fe/H] values of -0.85 ± 0.04 (Terzan 2), -1.40 ± 0.05 (Terzan 4), -1.20 ± 0.10 (HP 1), -1.40 ± 0.07 (Terzan 9), -1.07 ± 0.09 (Djorg 2), -1.06 ± 0.06 (NGC 6540), and -1.11 ± 0.04 (NGC 6642) from three to ten stars per cluster. We determine mean abundances for eleven other elements plus the mean [α/Fe] and radial velocity. CAPOS clusters significantly increase the sample of well-studied Main Bulge globular clusters (GCs) and also extend them to lower metallicity. We reinforce the finding that Main Bulge and Main Disk GCs, formed in situ, have [Si/Fe] abundances slightly higher than their accreted counterparts at the same metallicity. We investigate multiple populations and find our clusters generally follow the light-element (anti)correlation trends of previous studies of GCs of similar metallicity. We finally explore the abundances of the iron-peak elements Mn and Ni and compare their trends with field populations. Conclusions. CAPOS is proving to be an unprecedented resource for greatly improving our knowledge of the formation and evolution of BGCs and the bulge itself.
KW - Galaxy: bulge
KW - Globular clusters: general
KW - Stars: abundances
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U2 - 10.1051/0004-6361/202140436
DO - 10.1051/0004-6361/202140436
M3 - Article
AN - SCOPUS:85113667943
SN - 0004-6361
VL - 652
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A157
ER -