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Fig. 4
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Inverse cumulative distribution function of ρ for the dense gas (for r > 10−15g cm−3) outside the main star cluster, that is, for r > 0.1 pc for both models at SFE=0.05 (dotted lines) and SFE=0.1 (plain lines). One can clearly see that the outflows promote fragmentation between SFE=0.05 and SFE=0.1.
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