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Fig. 8


Upper panel: gaseous protocluster mass-size relation defined with gas kinematics overplotted with measurements of star-forming clumps summarized by Fall et al. (2010, light gray dots) and Urquhart et al. (2014, dark gray dots). The total mass of the cluster is used (gas plus sinks). Lower panel: sink cluster number-size relation overplotted with embedded cluster concluded by Adams et al. (2006, dark gray dots) and Gutermuth et al. (2009, light gray dots). The gray line indicates the number-size relation R (pc) ∝ (N/ 300)1/2 by Adams et al. (2006). Simulations with four different levels of turbulent support are plotted. The blue solid, green dashed, red dot-dashed, and cyan dotted curves have virial parameters αvir = 0.12, 0.64, 0.96, 1.78, respectively. The curves represent the time sequence. As the protoclusters accrete, they gain in mass and move from left to right in the figure. Time steps before 2 Myr are plotted with thinner lines.

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