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Using Spitzer Space Telescope and Chandra X-ray Observatory data, we identifyYSOs in the Rosette Molecular Cloud (RMC). By being able to select clustermembers and classify them into YSO types, we are able to track the progressionof star formation locally within the cluster environments and globally withinthe cloud. We employ nearest neighbor method (NNM) analysis to explore thedensity structure of the clusters and YSO ratio mapping to study ageprogressions in the cloud. We find a relationship between the YSO ratios andextinction which suggests star formation occurs preferentially in the densestparts of the cloud and that the column density of gas rapidly decreases as theregion evolves. This suggests rapid removal of gas may account for the low starformation efficiencies observed in molecular clouds. We find that the overallage spread across the RMC is small. Our analysis suggests that star formationstarted throughout the complex around the same time. Age gradients in the cloudappear to be localized and any effect the HII region has on the star formationhistory is secondary to that of the primordial collapse of the cloud.

The Progression of Star Formation in the Rosette Molecular Cloud