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Super star clusters (SSCs), likely the progenitors of globular clusters, areone of the most extreme forms of star formation. Understanding how SSCs form isan observational challenge. Theoretical studies establish that, to form suchclusters, the dynamical timescale of their parent clouds has to be shorter thanthe timescale of the disruption of their parent clouds by stellar feedback.However, due to insufficient observational support, it is still unclear howfeedback from SSCs acts on their surrounding matter. Studying feedback in SSCsis essential to understand how such clusters form. Based on ALMA and VLTobservations, we study this process in a SSC in the overlap region of theAntennae galaxies. We analyze a unique massive (~10^7 Msun) and young (1-3.5Myr) SSC, still associated with compact molecular and ionized gas emission. Thecluster has two CO velocity components, a low velocity one spatially associatedwith the cluster and a high velocity one distributed in a bubble-like shapearound the cluster. Our results on the low velocity component suggest that thisgas did not participate in the formation of the SSC. We propose that most ofthe parent cloud has already been blown away, accelerated at the early stagesof the SSC evolution by radiation pressure, in a timescale ~1 Myr. The highvelocity component may trace outflowing molecular gas from the parent cloud.Supporting evidence is found in shock heated H2 gas. The low velocity componentmay be gas that was near the SSC when it formed but not part of its parentcloud or clumps that migrated from the SGMC environment. This gas would bedispersed by stellar winds and supernova explosions. Within ~100 pc from thecluster, we estimate SFE>17%, smaller than the theoretical limit of 30% neededto form a bound cluster. Further higher spatial resolution observations areneeded to test and quantify our proposed scenario.

The impact of a massive star cluster on its surrounding matter in the Antennae overlap region