2020MNRAS.499.1200M


C.D.S. - SIMBAD4 rel 1.7 - 2021.05.06CEST05:43:03

2020MNRAS.499.1200M - Mon. Not. R. Astron. Soc., 499, 1200-1211 (2020/November-3)

Leveraging HST with MUSE: II. Na-abundance variations in intermediate age star clusters.

MARTOCCHIA S., KAMANN S., SARACINO S., USHER C., BASTIAN N., REJKUBA M., LATOUR M., LARDO C., CABRERA-ZIRI I., DREIZLER S., KACHAROV N., KOZHURINA-PLATAIS V., LARSEN S., MANCINO S., PLATAIS I. and SALARIS M.

Abstract (from CDS):

Ancient (>10 Gyr) globular clusters (GCs) show chemical abundance variations in the form of patterns among certain elements, e.g. N correlates with Na and anticorrelates with O. Recently, N abundance spreads have also been observed in massive star clusters that are significantly younger than old GCs, down to an age of ∼2 Gyr. However, so far N has been the only element found to vary in such young objects. We report here the presence of Na abundance variations in the intermediate age massive star clusters NGC 416 (∼6.5 Gyr old) and Lindsay 1 (∼7.5 Gyr old) in the Small Magellanic Cloud, by combining Hubble Space Telescope (HST) and European Southern Observatory Very Large Telescope MUSE observations. Using HST photometry, we were able to construct 'chromosome maps' and separate subpopulations with different N content, in the red giant branch of each cluster. MUSE spectra of individual stars belonging to each population were combined, resulting in high signal-to-noise spectra representative of each population, which were compared to search for mean differences in Na. We find a mean abundance variation of Δ[Na/Fe] = 0.18 ± 0.04 dex for NGC 416 and Δ[Na/Fe] = 0.24 ± 0.05 dex for Lindsay 1. In both clusters, we find that the population that is enhanced in N is also enhanced in Na, which is the same pattern to the one observed in ancient GCs. Furthermore, we detect a bimodal distribution of core-helium-burning red clump (RC) giants in the UV colour-magnitude diagram of NGC 416. A comparison of the stacked MUSE spectra of the two RCs shows the same mean Na abundance difference between the two populations. The results reported in this work are a crucial hint that star clusters of a large age range share the same origin: they are the same types of objects, but only separated in age.

Abstract Copyright: © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): stars: abundances - galaxies: individual: SMC - galaxies: star clusters: individual: NGC 416 - galaxies: star clusters: individual: Lindsay 1 - Hertzprung-Russell and colour-magnitude diagrams - techniques: spectroscopy - techniques: photometry

Status at CDS : Large table(s) will be appraised for possible ingestion in VizieR.

Simbad objects: 17

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Number of rows : 17

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 Cl Lindsay 1 Cl* 00 03 54 -73 28.3   11.7       ~ 99 0
2 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 11298 1
3 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9780 1
4 NGC 416 Cl* 01 07 59.0 -72 21 20 12.73 12.55 11.76   10.71 ~ 132 1
5 NAME Fornax Dwarf Spheroidal G 02 39 59.3 -34 26 57   9.02 7.4     ~ 1533 1
6 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5921 1
7 NGC 1316 GiP 03 22 41.789 -37 12 29.52 9.81 9.15 8.53 7.66   ~ 1232 1
8 [GMK2001] 114 GlC 03 22 42.4375 -37 12 41.516   19.63 18.46     ~ 22 1
9 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 15333 1
10 NGC 1978 GlC 05 28 45.330 -66 14 12.04   10.7 10.70     ~ 280 0
11 NGC 2808 GlC 09 12 03.10 -64 51 48.6   7.77 5.69     ~ 1289 0
12 M 3 GlC 13 42 11.62 +28 22 38.2     6.39     ~ 2310 0
13 NGC 6362 GlC 17 31 54.99 -67 02 54.0   9.72 8.86     ~ 505 0
14 NAME SDG G 18 55 03.1 -30 28 42   4.5 3.6     ~ 1836 2
15 M 54 GlC 18 55 03.33 -30 28 47.5           ~ 943 0
16 NGC 7252 IG 22 20 44.7751096408 -24 40 41.905677809 12.26 12.46 12.06 11.57   ~ 671 1
17 NAME Local Group GrG ~ ~           ~ 7251 0

    Equat.    Gal    SGal    Ecl

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2021.05.06-05:43:03

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