Evolution of the star-forming clump. Top 6 maps: (x−y) column density maps of the two models integrated along the z direction at SFE=0.1. The top map shows the model without protostellar outflows. The bottom map shows the model with protostellar outflows. From left to right: we zoom toward sink 1, that is, near the center of the collapse. The outflows have a visible impact on the column density structures at scales below 0.1 pc. Clearly, more stars form in the presence of the outflows. Bottom 6 maps: same but for the mass weighted norm of the velocity. The outflows significantly modify the velocity field at scales smaller than 0.1 pc.