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\subsection{Numerical Simulations}  In this paper, we analyze the magneto-hydrodynamic simulations performed by \cite{Offner_2015}\cite{Offner_2015} \cite{Offner_2015}  of a small group of wind-launching stars, which are embedded in a turbulent molecular cloud. We refer the reader to that paper for full numerical details. Table \ref{simprop} summarizes the simulation properties for the specific evolutionary times we analyze here. In brief, the calculations are performed using the {\sc orion} adaptive mesh refinement code \citep[e.g.,]{li12}. They include supersonic turbulence, magnetic fields, and five star particles endowed with a prescription for launching isotropic stellar winds. The domain size for all runs is 5 pc and the molecular gas is initially 10 K with a velocity dispersion of $2.0$\kms. The turbulent realization, magnetic field strength and wind properties vary between runs as stated in Table \ref{simprop}. \subsection{CO Emission Modeling}  As in \citet{Offner15}, \cite{Offner_2015},  we post-process each output with the radiative transfer code {\sc radmc-3d}\footnote{http://www.ita.uni-heidelberg.de/~dullemond/software/radmc-3d/} in order to compute the $^{12}$CO (1-0) emission. We solve the equations of radiative statistical equilibrium using the Large Velocity Gradient (LVG) approach \citep{shetty11}. We perform the radiative transfer using the densities, temperatures, and velocities of the simulations flattened to a uniform $256^3$ grid. We convert to CO number density by defining $n_{\rm H_2} = \rho/(2.8 m_p)$ and adopting a CO abundance of [$^{12}$CO/H$_2$] =$10^{-4}$ \citep{frerking82}. Gas above 800 K or with $n_{\rm H_2} < 10$ cm$^{-3}$ is set to a CO abundance of zero. This effectively means that gas inside the wind bubbles is CO-dark. The CO abundance in regions with densities $n_{\rm H_2} > 2 \times 10^4$ cm$^{-3}$ is also set to zero, since CO freezes-out onto dust grains at higher densities \citep{Tafalla_2004}. In the radiative transfer calculation, we include sub-grid turbulent line broadening by setting a constant micro-turbulence of 0.25$\kms$. The data cubes have a velocity range of $\pm 10\kms$ and a spectral resolution of $\Delta v = 0.156~ \kms$. [Ryan - explain the next steps in 2-3 sentences]