the turbulent velocity field will have a power spectrum that is somewhat steeper than the standard Kolmogorov (1941) description for incompressible flows. However, this deviation is small and we note that the the ability of a cloud to fragment is only weakly dependent on the power spectrum of the turbulence [@ddetal04]. The three-dimensional root-mean-squared velocity in the turbulent field – which we will refer to as $\Delta v_{\rm turb}$ – is then scaled to some fraction of the sound speed in the initial conditions. For the simulations presented here we use four different rms velocities: 0.1, 0.2, 0.4 and 0.8 $c_{\rm s}$. For an isothermal sound speed and an adiabatic index of $\gamma = 5/3$, the corresponding ratios of the turbulent to thermal energy are given by $1/3(\Delta v_{\rm turb}/c_{\rm s})^{2}$, yielding 0.0033, 0.0133, 0.0533 and 0.2133 respectively, for our chosen values of $c_{\rm s}$. In order to focus on the effects of the turbulence, we do not include any ordered rotation of the initial gas cloud. Note, however, that this does not imply that the initial angular momentum of the cloud is zero, since the imposed turbulent velocity field gives the cloud a small amount of angular momentum. Note 