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Fig. 2


Upper panel: mass of the cluster as a function of its radius as predicted by Eq. (12), i.e. for a turbulent type accretion for which  ∝ M0.75. Three values of α∗,c are displayed. The stars correspond to the embedded clusters listed in Table 1 of Lada & Lada (2003) for which the mass has been multiplied by 5 to account for a star formation efficiency of about 20%. Lower panel: same as lower panel for  ∝ M. The thick solid line corresponds to the solid line of the upper panel for comparison.

This figure is made of several images, please see below:

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