Combined Effects of Rotation and Age Spreads on Extended Main-Sequence Turn Offs

Combined Effects of Rotation and Age Spreads on Extended Main-Sequence Turn OffsGossage, SethConroy, CharlieDotter, AaronCabrera-Ziri, IvanDolphin, Andrew E.Bastian, NateDalcanton, Julianne J.Goudfrooij, PaulJohnson, L. CliftonWilliams, Benjamin F.Rosenfield, PhilipKalirai, JasonFouesneau, MorganDOI: info:10.3847/1538-4357/ab5717v. 887199
Gossage, Seth, Conroy, Charlie, Dotter, Aaron, Cabrera-Ziri, Ivan, Dolphin, Andrew E., Bastian, Nate, Dalcanton, Julianne J., Goudfrooij, Paul, Johnson, L. Clifton, Williams, Benjamin F., Rosenfield, Philip, Kalirai, Jason, and Fouesneau, Morgan. 2019. "Combined Effects of Rotation and Age Spreads on Extended Main-Sequence Turn Offs." The Astrophysical Journal 887:199. https://doi.org/10.3847/1538-4357/ab5717
ID: 154536
Type: article
Authors: Gossage, Seth; Conroy, Charlie; Dotter, Aaron; Cabrera-Ziri, Ivan; Dolphin, Andrew E.; Bastian, Nate; Dalcanton, Julianne J.; Goudfrooij, Paul; Johnson, L. Clifton; Williams, Benjamin F.; Rosenfield, Philip; Kalirai, Jason; Fouesneau, Morgan
Abstract: The extended main-sequence turn offs (eMSTOs) of several young to intermediate age clusters are examined in the Magellanic Clouds and the Milky Way. We explore the effects of extended star formation (eSF) and a range of stellar rotation rates on the behavior of the color─magnitude diagram, paying particular attention to the MSTO. We create synthetic stellar populations based on MESA stellar models to simulate observed Hubble Space Telescope and Gaia star cluster data. We model the effect of rotation as a nonparametric distribution, allowing for maximum flexibility. In our models the slow rotators comprise the blueward, and fast rotators the redward portion of the eMSTO. We simulate data under three scenarios: nonrotating eSF, a range of rotation rates with a single age, and a combination of age and rotation effects. We find that two of the five clusters (the youngest and oldest) favor an age spread, but these also achieve the overall worst fits of all clusters. The other three clusters show comparable statistical evidence between rotation and an age spread. In all five cases, a rotation-rate distribution alone is capable of qualitatively matching the observed eMSTO structure. In future work, we aim to compare our predicted V\sin i with observations in order to better constrain the physics related to stellar rotation.