We present the results of CO ( J = 3 - 2 ) and HCO ^ { + } ( J = 4 - 3 ) mapping observations toward a nearby embedded cluster , Serpens South , using the ASTE 10 m telescope .
Our CO ( J = 3 - 2 ) map reveals that many outflows are crowded in the dense cluster-forming clump that can be recognized as a HCO ^ { + } clump with a size of \sim 0.2 pc and mass of \sim 80 M _ { \odot } .
The clump contains several subfragments with sizes of \sim 0.05 pc .
By comparing the CO ( J = 3 - 2 ) map with the 1.1 mm dust continuum image taken by AzTEC on ASTE , we find that the spatial extents of the outflow lobes are sometimes anti-correlated with the distribution of the dense gas and some of the outflow lobes apparently collide with the dense gas .
The total outflow mass , momentum , and energy are estimated at 0.6 M _ { \odot } , 8 M _ { \odot } km s ^ { -1 } , and 64 M _ { \odot } km ^ { 2 } s ^ { -2 } , respectively .
The energy injection rate due to the outflows is comparable to the turbulence dissipation rate in the clump , implying that the protostellar outflows can maintain the supersonic turbulence in this region .
The total outflow energy seems only about 10 percent the clump gravitational energy .
We conclude that the current outflow activity is not enough to destroy the whole cluster-forming clump , and therefore star formation is likely to continue for several or many local dynamical times .