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Protostellar outflows have been shown theoretically to be capable ofmaintaining supersonic turbulence in cluster-forming clumps and keeping thestar formation rate per free-fall time as low as a few percent. We aim to testtwo basic predictions of this outflow-regulated cluster formation model, namely(1) the clump should be close to virial equilibrium and (2) the turbulencedissipation rate should be balanced by the outflow momentum injection rate,using recent outflow surveys toward 8 nearby cluster-forming clumps (B59,L1551, L1641N, Serpens Main Cloud, Serpens South, $\rho$ Oph, IC 348, and NGC1333). We find, for almost all sources, that the clumps are close to virialequilibrium and the outflow momentum injection rate exceeds the turbulencemomentum dissipation rate. In addition, the outflow kinetic energy issignificantly smaller than the clump gravitational energy for intermediate andmassive clumps with $M_{\rm cl} \gtrsim {\rm a \ few} \times 10^2 M_\odot$,suggesting that the outflow feedback is not enough to disperse the clump as awhole. The number of observed protostars also indicates that the star formationrate per free-fall time is as small as a few percent for all clumps. Theseobservationally-based results strengthen the case for outflow-regulated clusterformation.

Confronting Outflow-Regulated Cluster Formation Model with Observations