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Fig. 8

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Comparison of the W43-MM2&MM3 CMF (blue histogram, see Fig. 5a) with power-laws fitted to the high-mass end, >1 M, of CMFs measured in three star-forming regions. The proto-typical CMF of low-mass star-forming regions, derived in Aquila (green line, Könyves et al. 2015), resembles the Salpeter slope of the canonical IMF (dashed magenta line, Salpeter 1955). In contrast, the CMFs in W43-MM2&MM3 and in the two high-mass star-forming protoclusters W43-MM1 and G28.37+0.07 (red dot-dashed and orange dotted lines, Motte et al. 2018b; Kong 2019) are top-heavy.

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