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Fig. 13

image

Mass-luminosity distribution of the whole sample. The gray tracks are evolutionary models used by Molinari et al. (2008). The dash-dotted colored lines show a linear fit to the corresponding class of sources. The horizontal dashed line shows the luminosity of a B1.5 star as calculated by Mottram et al. (2011a, Table 1), whereas the vertical dashed line shows the threshold of 650 M beyond which clumps are likely to host massive dense clumps or high-mass protostars (Csengeri et al. 2014).

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