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Fig. 15.

image

Most massive fragment mass as a function of clump properties for sources at a distance of 2−4 kpc (dots) and 1−2 kpc (triangles). Left: mass of the most massive fragment as a function of clump luminosity-to-mass ratio. Vertical lines mark the luminosity-to-mass ratio of 1 and 10. Middle: mass of the most massive fragment mass as a function of clump mass. Gray lines show the 30% and 100% proportion of clump mass; the blue dashed line shows the result of a linear fit on logarithmic scale to sources in the 2−4 kpc distance range of Mfragments = 0.96log Mclumps − 1.18. The relation between cluster mass and maximum stellar mass is indicated by the red dash-dotted line, which is an analytical relation from Weidner et al. (2013), and is scaled up by 3.3 assuming a 30% star-formation efficiency. The eft and middle plots share the same color bar. The clumps are color-coded according to their sizes. Right: surface density of the most massive fragment as a function of clump surface density. Vertical line marks the 0.2 g cm−2 empirical limit from Butler & Tan (2012). The blue dashed line shows the result of a linear fit to sources in the 2−4 kpc distance range of log Σfragments = 1.03log Σclumps + 0.43.

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