Exploring the nature and synchronicity of early cluster formation in the Large Magellanic Cloud V: Multiple Populations in ancient Globular Clusters. (arXiv:2003.09473v1 [astro-ph.GA])

Exploring the nature and synchronicity of early cluster formation in the Large Magellanic Cloud V: Multiple Populations in ancient Globular Clusters. (arXiv:2003.09473v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Gilligan_C/0/1/0/all/0/1">Christina K. Gilligan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chaboyer_B/0/1/0/all/0/1">Brian Chaboyer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cummings_J/0/1/0/all/0/1">Jeffrey D. Cummings</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mackey_D/0/1/0/all/0/1">Dougal Mackey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cohen_R/0/1/0/all/0/1">Roger E. Cohen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Geisler_D/0/1/0/all/0/1">Douglas Geisler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grocholski_A/0/1/0/all/0/1">Aaron J. Grocholski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Parisi_M/0/1/0/all/0/1">M. C. Parisi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sarajedini_A/0/1/0/all/0/1">Ata Sarajedini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ventura_P/0/1/0/all/0/1">Paolo Ventura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Villanova_S/0/1/0/all/0/1">Sandro Villanova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_S/0/1/0/all/0/1">Soung-Chul Yang</a>

We examine four ancient Large Magellanic Cloud (LMC) globular clusters (GCs)
for evidence of multiple stellar populations using the Advanced Camera for
Surveys and Wide Field Camera 3 on the Hubble Space Telescope Programme
GO-14164. NGC 1466, NGC 1841, and NGC 2257 all show evidence for a redder,
secondary population along the main-sequence. Reticulum does not show evidence
for the presence of a redder population, but this GC has the least number of
stars and Monte Carlo simulations indicate that the sample of main sequence
stars is too small to robustly infer whether a redder population exists in this
cluster. The second, redder, population of the other three clusters constitutes
$sim30-40%$ of the total population along the main-sequence. This brings the
total number of ancient LMC GCs with known split or broadened main-sequences to
five. However, unlike for Hodge 11 and NGC 2210 (see arXiv:1904.01434), none of
the clusters show evidence for multiple populations in the horizontal branch.
We also do not find evidence of a second population along the Red Giant Branch
(RGB).

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