Similarly to Galactic GCs, the RGB width of Magellanic Cloud (MC) GCs correlates with cluster mass after removing the dependence from metallicity. This fact demonstrates that cluster mass is the main factor affecting the properties of MPs.
We suggest that a small variation in metals and binarity governs the color spread of the 1G in the ChM and that evolved BSs contribute to the bluest tail of the 1G sequence.
A new _economic_ combination of HST filter reveals the presence of four stellar populations with extreme Helium variations in the massive outer-halo globular cluster NGC2419.
This is a two-orbits proposal to explore pre-main sequence (pre-MS) stars in Large Magellanic Cloud young clusters to assess, once and for all, if multiple bursts of star formation can be supported by these systems.
Internal variation of helium content cannot reproduce all the observational constraints at the same time. The origin of the first generation colour spread is therefore still without a straightforward explanation.
By comparing the observations with simulated CMDs, we find that a simple population composed of coeval stars that span a wide range of rotation rates is unable to reproduce the color spread of the cluster’s MSs. We suggest that variable stars, binary interactions, and stellar rotation affect the eMSTO morphology of these very young.
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