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Fig. 8.

image

Top: normalized distribution (continuous line) and medians (vertical dashed lines) of the clumpiness for four types of galaxies: main sequence galaxies with mergerness < 0 and > 0 (in black and cyan, respectively), and starbursts (in orange those with mergerness < 0 and in red the morphological merger subset). We notice that the merger-selected starbursts dominate the high clumpiness tail, while the remaining SBs are basically indistinguishable from the population of main sequence galaxies with mergerness < 0. A substantial contribution to the high clumpiness population also comes from mergers inside the MS, as shown by the cyan excess at 0.06 < c < 0.12. A Kolmogorov–Smirnov (KS) test between merger and not-merger MS systems (cyan and black subsets) yields 0.302 (p-value = 0.094). Bottom: same histograms as above, but considering visual mergers instead of the automatic morphological classification.

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