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