The Effect of Stellar Rotation on Colour-Magnitude Diagrams: On the apparent presence of multiple populations in intermediate age stellar clusters

TL;DR

This paper demonstrates that stellar rotation can mimic multiple populations in intermediate age clusters' colour-magnitude diagrams, challenging the interpretation of age spreads in these clusters.

Contribution

It introduces a model showing how stellar rotation effects can explain observed features without invoking multiple stellar populations.

Findings

Rotation rates of 20-50% of critical match observations

Rotation effects can mimic age spreads in CMDs

Rotation unlikely causes in old globular clusters

Abstract

A significant number of intermediate age clusters (1-2 Gyr) in the Magellanic Clouds appear to have multiple stellar populations within them, derived from bi-modal or extended main sequence turn offs. If this is interpreted as an age spread, the multiple populations are separated by a few hundred Myr, which would call into question the long held notion that clusters are simple stellar populations. Here we show that stellar rotation in stars with masses between 1.2-1.7 Msun can mimic the effect of a double or multiple population, whereas in actuality only a single population exists. The two main causes of the spread near the turn-off are the effects of stellar rotation on the structure of the star and the inclination angle of the star relative to the observer. Both effects change the observed effective temperature, hence colour, and flux of the star. In order to match observations, the required rotation rates are 20-50% of the critical rotation, which are consistent with observed rotation rates of similar mass stars in the Galaxy. We provide scaling relations which can be applied to non-rotating isochrones in order to mimic the effects of rotation. Finally, we note that rotation is unlikely to be the cause of the multiple stellar populations observed in old globular clusters, as low mass stars (<1 Msun) are not expected to be rapid rotators.