2020
DOI: 10.1093/mnras/staa2929
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Abstract: 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 anti-correlates 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 cluste… Show more

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Cited by 8 publications
(5 citation statements)
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“…In the ancient clusters, the complex CMDs are caused mainly by star-to-star chemical abundance variations (see reviews by Bastian & Lardo 2018;Gratton et al 2019). Similar variations have been observed in massive Magellanic Cloud clusters with ages of ∼ 2 Gyr or above (e.g., Saracino et al 2020;Martocchia et al 2020;Cadelano et al 2022), while they appear to be absent in the stars observed in even younger clusters (e.g., Mucciarelli et al 2014). Instead, stellar rotation has been suggested as the dominant cause of the unexpected features in the young clusters (e.g., Bastian & de Mink 2009;D'Antona et al 2015).…”
supporting
confidence: 71%
“…In the ancient clusters, the complex CMDs are caused mainly by star-to-star chemical abundance variations (see reviews by Bastian & Lardo 2018;Gratton et al 2019). Similar variations have been observed in massive Magellanic Cloud clusters with ages of ∼ 2 Gyr or above (e.g., Saracino et al 2020;Martocchia et al 2020;Cadelano et al 2022), while they appear to be absent in the stars observed in even younger clusters (e.g., Mucciarelli et al 2014). Instead, stellar rotation has been suggested as the dominant cause of the unexpected features in the young clusters (e.g., Bastian & de Mink 2009;D'Antona et al 2015).…”
supporting
confidence: 71%
“…Na variations have also been found, by first using integrated light techniques in quite young clusters (∼2-3 Gyr, Bastian et al 2019). Subsequently, Saracino et al (2020b) and Martocchia et al (2020b) showed that Na variations are present in massive star clusters at different ages (∼ 2 − 7.5 Gyr), by combining the power of HST and VLT/MUSE, a technique introduced by Latour et al (2019).…”
Section: Introductionmentioning
confidence: 99%
“…Instead of a simple population of coeval stars formed from a chemically homogeneous protocluster cloud, individual GCs associated with the Milky Way and to several galaxies of the Local Group host stars formed with large variations of their content in C, N, O, Na, and Al, with Mg also varying in the most massive and/or most metal-poor Galactic GCs (Cohen 1978;Peterson 1980;Carretta et al 2009Carretta et al , 2010Mészáros et al 2015Mészáros et al , 2020Pancino et al 2017;Schiavon et al 2017;Wang et al 2017;O'Malley & Chaboyer 2018;Mucciarelli et al 2009;Schiavon et al 2013;Dalessandro et al 2016;Carretta et al 2017;Niederhofer et al 2017;Gilligan et al 2019;Milone et al 2020;Vanaraj et al 2021;Leath et al 2022;Larsen et al 2022). Hints for the presence of MSP with similar characteristics are also found in intermediate-age (down to ∼ 2 Gyr) massive star clusters in the Magellanic Clouds (Hollyhead et al 2017(Hollyhead et al , 2019Saracino et al 2020;Martocchia et al 2020Martocchia et al , 2021Asa'd et al 2022;Cadelano et al 2022;Salgado et al 2022). While the epoch when the clusters formed is thus not critical for MSP to be present, the mass of the cluster is.…”
Section: Introductionmentioning
confidence: 93%