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The calculation was performed with the {\sc orion} adaptive mesh refinement (AMR) code \cite{truelove98,klein99}. The simulation follows the collapse of an isolated, turbulent low-mass core. It begins with an initially uniform, cold $4\msun$ sphere of radius $R_c=2\times 10^{17}$cm, density $\rho_c=2\times 10^{-19}$ g cm$^{-3}$ and temperature $T_c=10$ K . This core is embedded in a warm, diffuse gas with $\rho=rho_c/100$ and $T=100 T_c$ K. The dense gas is initialized with a grid of random velocity perturbations such that the initial rms velocity dispersion is 0.5 km s$^{-1}$.   Additional levels of adaptive mesh refinement (AMR) are inserted as the core collapses under the influence of gravity. The core itself is resolved with a minimum cell size of $\Delta_{\rm min}\simeq 0.001$ pc, where the maximum level of refinement has $\Delta_{\rm min}\simeq 26 AU$. Once the central region exceeds the maximum grid resolution ($\rho_{\rm max}\simeq 6.5 \times 10^{-15}$ g cm$^{-3}$, e.g., \citealt{truelove98}), a ``star" forms. This star, which is represented by a Lagrangian sink particle, accretes, radiates and launches a collimated bipolar outflow \citep{krumholz04, Offner09, cunninham11}. \citep{krumholz04,Offner09,cunninham11}.  The rate of mass loss due to the outflow is set to a fixed fraction of the instantaneous accretion rate: $\dot m_w = \f_w \dot m_*$, where $f_w = 0.3$ is the outflow launching rate given by the X-wind model \citep{shu88}. The distribution of outflow momentum is parameterized by a fixed collimation angle, $\theta_0=0.1$, which is empirically determined to be similar to that of observed outflows \citep{matzner99,cunningham11}. Although $\theta_0$ is constant in time, the outflow injection into the AMR grid occurs on such small scales that the outflow properties such as the opening angle and morphology evolve hydrodynamically; these appear to agree well with observed low-mass outflows \citep{Offner11,Offner14}.   By the end of the calculation ($t= 0.5$ Myr), the simulation contains a single star with a mass of $\sim$1.45 $\msun$.   %Over the evolution, the outflow unbinds and ejects a significant fraction of the gas from the domain, producing a star formation efficiency of 47\%, which is comparable to observational and theoretical estimates for dense cores (e.g., \citealt{matzner00,alves07}).