Clump masses as a function of clump radius. a) The upper panel shows the distribution of massive star forming clumps identified by cross-matching dense clumps with methanol masers, massive young stellar objects and compact HII regions, all of which are excellent tracers of embedded massive stars and their associated proto-clusters (Urquhart et al. 2014). The dashed red line shows the results of a power-law fit to the clump size-mass distribution. b) Comparison between the clump data by Urquhart et al. and the cluster data of Fig. 4a. c) Possible range of star formation efficiencies derived from the mass-radius relations for gas clumps and embedded star clusters in the solar neighbourhood. The red-dashed line indicates in all three plots the fit of Urquhart et al. (2014) and the black full line the fit to the Lada & Lada (2003) data. The symbols are the same as in Figs. 1 and 3.
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