Molecular Outflows From the Protocluster, Serpens South
  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.
