Infrared Photometry of Red Supergiants in Young Clusters in the Magellanic Clouds

We present broad-band infrared photometry for 52 late-type supergiants in the young Magellanic Clouds clusters NGC 330, NGC 1818, NGC 2004 and NGC 2100. Standard models are seen to differ in the temperature they predict for the red supergiant population on the order of 300K. It appears that these differences most probably due to the calibration of the mixing-length parameter, $\alpha_{P}$, in the outermost layers of the stellar envelope. Due to the apparent model dependent nature of $\alpha_{P}$ we do not quantitatively compare $\alpha_{P}$ between models. Qualitatively, we find that $\alpha_{P}$ decreases with increased stellar mass within standard models. We do not find evidence for a metallicity dependence of $\alpha_{P}$.