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We use Atacama Large Millimeter Array CO(3-2) observations in conjunctionwith optical observations from the Hubble Space Telescope to determine theratio of stellar to gas mass for regions in the Antennae Galaxies. We adopt theterm "instantaneous mass ratio" IMR(t) = M$_{stars}$/(M$_{gas}$ +M$_{stars}$),that is equivalent to the star formation efficiency for an idealized system att = 0. We use two complementary approaches to determining the IMR(t) based on1) the enclosed stellar and molecular mass within circular apertures centeredon optically-identified clusters, and 2) a tessellation algorithm that definesregions based on CO emission. We find that only a small number of clustersappear to have IMR(0) = SFE > 0.2, which suggests that only a small fraction ofthese clusters will remain bound. The results suggest that by ages of$10^{6.7}$ years, some clusters will have lost all of their associatedmolecular gas, and by $10^{7.5}$ years this is true for the majority ofclusters. There appears to be slight dependence of the IMR(t) on the CO surfacebrightness, which could support the idea that dense molecular environments aremore likely to form bound clusters. However, the IMR(t) appears to have astrong dependence on extinction, which likely traces the evolutionary state ofclusters.

Resolved Star Formation Efficiency in the Antennae Galaxies