A new outflow from the Class 0/I binary system [BHB2007]11 revealed by ALMA

During the early stages of star formation, accretion processes such as infall from the envelope and molecular streamers, and ejection of matter through winds and jets, take place simultaneously and distribute the angular momentum of the parent molecular cloud. The Class 0/I binary [BHB2007]11 shows evidence for accretion and ejection at the scales of the circumbinary disk and the inner close binary. Recent observations, however, show two elongated structures with hints of outflowing motion in the direction perpendicular to the main CO outflow launched from the circumbinary disk. We have analyzed these structures with molecular data obtained with ALMA within the FAUST Large Program. The gas kinematics are consistent with outflowing motions in the direction perpendicular to the main CO outflow. Plus, elongated, compact SiO emission close to the binary system has a similar orientation to that observed for the larger-scale structures, suggesting that it likely arises from the shocked material at the base of a new second outflow. We derive mass loss rates and evaluate the rotation of this potential new outflow. The observations trace the material moving at velocities closer to the ambient cloud velocity, which could not be probed in previous observations of the self-absorbed emission of CO. This work illustrates the importance of tracing different spatial scales and velocity ranges with a rich molecular dataset to understand the complex dynamics in the evolution of protostars.