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Fig. 7


Bound fraction as a function of gas removal velocity for different εSFE, here for clusters with an initial stellar mass of 104M and a HMR of 0.3 pc. Approximating the gas removal to be instantaneous might make the assumption of an unusually high εSFE necessary, as otherwise simulations might not have any surviving cluster after gas expulsion. Every data point corresponds to a single simulation.

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