Institution(s): 1. Institut d' Astrophysique Spatiale, 2. NAOJ
Super star clusters (SSCs), likely the progenitors of globular clusters, are one of the most extreme forms of star formation. Stellar feedback from such massive clusters is vital to galaxy evolution and star formation history in the Universe, as the intense radiation and stellar winds produced by massive stars are important in unbinding and dispersing large molecular clouds and affecting star formation efficiency and sequential star formation. Nearby galaxy mergers are ideal sites to investigate massive star feedback, and to form local analogous in high-redshift galaxies. Based on ALMA and VLT observations, we study this process in a SSC in the Antennae galaxies (NGC 4038/39, 22 Mpc), a spectacular example of a burst of star formation triggered by the encounter of two galaxies. We analyze a massive (~107 M⊙) and young (3.4 Myr) SSC, B1, which is associated with compact molecular and ionized emission, suggesting that it is still embedded in its parent molecular cloud. However, we found that the observed CO linewidth yields a conservative velocity expansion, the radiation pressure does not accelerate today the gas and the matter surrounding the cluster is clumpy, indicating that SSC B1 is not embedded in its parent cloud after all. We propose that radiation pressure was highly enhanced at the early stages of the SSC formation, early disrupting the parent cloud (< 3 Myr). The gas observed today surrounding the cluster did not participate on the cluster formation but are nearby clouds and/or gas accreted from the SGMC. We present evidences that outflowing gas from the parent cloud may be still observed in the broader, high velocity component of the CO gas, which has a bubble-like shape structure distributed around SSC B1. Higher angular resolution observations are needed to validate this interpretation and to understand the origin and fate of the component seen to be associated with SSC B1.