Is the turbulence in cluster-forming regions internally driven by stellar outflows or the consequence of a large-scale turbulent cascade ?
We address this question by studying the turbulent energy spectrum in NGC 1333 .
Using synthetic ^ { 13 } CO maps computed with a snapshot of a supersonic turbulence simulation , we show that the VCS method of Lazarian and Pogosyan provides an accurate estimate of the turbulent energy spectrum .
We then apply this method to the ^ { 13 } CO map of NGC 1333 from the COMPLETE database .
We find the turbulent energy spectrum is a power law , E ( k ) \propto k ^ { - \beta } , in the range of scales 0.06 pc \leq \ell \leq 1.5 pc , with slope \beta = 1.85 \pm 0.04 .
The estimated energy injection scale of stellar outflows in NGC 1333 is \ell _ { inj } \approx 0.3 pc , well resolved by the observations .
There is no evidence of the flattening of the energy spectrum above the scale \ell _ { inj } predicted by outflow-driven simulations and analytical models .
The power spectrum of integrated intensity is also a nearly perfect power law in the range of scales 0.16 pc < \ell < 7.9 pc , with no feature above \ell _ { inj } .
We conclude that the observed turbulence in NGC 1333 does not appear to be driven primarily by stellar outflows .