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Title:
The search for multiple populations in Magellanic Cloud clusters - IV. Coeval multiple stellar populations in the young star cluster NGC 1978
Authors:
Martocchia, S.; Niederhofer, F.; Dalessandro, E.; Bastian, N.; Kacharov, N.; Usher, C.; Cabrera-Ziri, I.; Lardo, C.; Cassisi, S.; Geisler, D.; Hilker, M.; Hollyhead, K.; Kozhurina-Platais, V.; Larsen, S.; Mackey, D.; Mucciarelli, A.; Platais, I.; Salaris, M.
Affiliation:
AA(Astrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool L3 5RF, UK), AB(Leibniz-Institut für Astrophysik Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany), AC(INAF -- Osservatorio di Astrofisica and Scienza dello Spazio, via Gobetti 93/3, I-40129 Bologna, Italy), AD(Astrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool L3 5RF, UK), AE(Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany), AF(Astrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool L3 5RF, UK 0000-0002-7383-7106), AG(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AH(Laboratoire d'Astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire, CH-1290 Versoix, Switzerland 0000-0002-4295-8773), AI(INAF -- Osservatorio Astronomico d'Abruzzo, sn., I-64100 Teramo, Italy), AJ(Departamento de Astronomia, Universidad de Concepcion, Casilla 160-C, Chile), AK(European Southern Observatory, Karl-Schwarzschild-Straße 2, D-85748 Garching bei München, Germany), AL(Department of Astronomy, Oscar Klein Centre, Stockholm University, AlbaNova, SE-10691 Stockholm, Sweden), AM(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA), AN(Department of Astrophysics/IMAPP, Radboud University, PO Box 9010, NL-6500 GL Nijmegen, the Netherlands), AO(Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, Australia), AP(INAF -- Osservatorio di Astrofisica and Scienza dello Spazio, via Gobetti 93/3, I-40129 Bologna, Italy; Dipartimento di Fisica and Astronomia, Università degli Studi di Bologna, via Gobetti 93/2, I-40129 Bologna, Italy), AQ(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA), AR(Astrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool L3 5RF, UK)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 477, Issue 4, p.4696-4705 (MNRAS Homepage)
Publication Date:
07/2018
Origin:
OUP
Astronomy Keywords:
stars: abundances, Hertzsprung--Russell and colour--magnitude diagrams, galaxies: individual: LMC, galaxies: individual: NGC 1978
Abstract Copyright:
2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society
DOI:
10.1093/mnras/sty916
Bibliographic Code:
2018MNRAS.477.4696M

Abstract

We have recently shown that the ˜2 Gyr old Large Magellanic Cloud star cluster NGC 1978 hosts multiple populations in terms of star-to-star abundance variations in [N/Fe]. These can be seen as a splitting or spread in the subgiant and red giant branches (SGB and RGB) when certain photometric filter combinations are used. Because of its relative youth, NGC 1978 can be used to place stringent limits on whether multiple bursts of star formation have taken place within the cluster, as predicted by some models for the origin of multiple populations. We carry out two distinct analyses to test whether multiple star formation epochs have occurred within NGC 1978. First, we use ultraviolet colour-magnitude diagrams (CMDs) to select stars from the first and second population along the SGB, and then compare their positions in optical CMDs, where the morphology is dominantly controlled by age as opposed to multiple population effects. We find that the two populations are indistinguishable, with age differences of 1 ± 20 Myr between them. This is in tension with predictions from the asymptotic giant branch scenario for the origin of multiple populations. Second, we estimate the broadness of the main-sequence turn-off (MSTO) of NGC 1978 and we report that it is consistent with the observational errors. We find an upper limit of ˜65 Myr on the age spread in the MSTO of NGC 1978. This finding is in conflict with the age spread scenario as origin of the extended MSTO in intermediate-age clusters, while it fully supports predictions from the stellar rotation model.
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