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Fig. 9

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For each W43-MM2&MM3 subregion, the power-law index of the CMF high-mass end plotted against the slope coefficient of the second η-PDF tail (panel a) and the protostellar fraction (panel b). Horizontal arrows represent lower limits for s2 in panel a. We avoid fitting the correlation trends observed in panels a–b because they rely on too few subregions.

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