Relation between mass and effective radius for the clumps in G304.74. The solid line shows the least squares fit to the data, i.e., log (M) ≈ 3.1 + 2.8log (R). The dotted line represents the mass-radius threshold for massive-star formation proposed by Kauffmann & Pillai (2010), i.e., M(R) = 870 M⊙ × (R/pc)1.33.
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