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The ages of young star clusters are fundamental clocks to constrain theformation and evolution of pre-main-sequence stars and their protoplanetarydisks and exoplanets. However, dating methods for very young clusters oftendisagree, casting doubts on the accuracy of the derived ages. We propose a newmethod to derive the kinematic age of star clusters based on the evaporationages of their stars. The method is validated and calibrated using hundreds ofclusters identified in a supernova-driven simulation of the interstellar mediumforming stars for approximately 40 Myr within a 250 pc region. We demonstratethat the clusters' evaporation-age uncertainty can be as small as about 10% forclusters with a large enough number of evaporated stars and small but realisticobservational errors. We have obtained evaporation ages for a pilot sample of10 clusters, finding a good agreement with their published isochronal ages. Theevaporation ages will provide important constraints for modeling thepre-main-sequence evolution of low-mass stars, as well as to investigate thestar-formation and gas-evaporation history of young clusters. These ages can bemore accurate than isochronal ages for very young clusters, for whichobservations and models are more uncertain.

Evaporation Ages: a New Dating Method for Young Star Clusters