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Fig. 7.

image

Scatter plot between the clumpiness and the distance from the main sequence (c vs. distMS) for our sample. Each galaxy in the plot is color-coded according to its mergerness value. Morphological mergers identified in the Gini-M20 diagram (mergerness > 0) are shown with white filled circles, and their fraction fmerg (compared to the whole population) constantly increases toward higher distMS (upper histogram). Median clumpiness values and 1σ errors are calculated for mergers and not merger systems in seven bins of distMS of 0.2 dex approximately. The violet line and shaded area indicate, respectively, the best-fit linear correlation for Gini-M20 mergers (whose equation is reported in the legend) and the corresponding 1σ error region. The annotation below the legend indicates the Pearson correlation coefficient ρ and p-value for the same galaxies, along with the 1σ scatter of morphological mergers around the best-fit line. The histogram on the left compares instead the clumpiness distribution for morphologically selected mergers (mergerness > 0, in white) and not mergers (gray region, derived from the black circles in the scatter plot). In this case, a larger discrepancy is observed between the two distributions compared to Fig. 6, confirmed by the higher significance of the KS test (KS = 0.432, p-value = 2 × 10−8).

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