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Fig. 10

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Kennicutt-Schmidt relation for the simulations involved in this study. We use two panels for clarity; in the bottom panel we only plot the MIRAGE sample, while in the top panel we overplot the MASSIV data on the MIRAGE sample for comparison. In both panels, we also display the relation obtained in Daddi et al. (2010b) (red solid line for the relation and dashed line for the associated 1σ dispersion). Simulations plotted at different times are represented with different colors, with values measured inside the stellar disk scalelength. In case of merger, we plot only snapshots where the coalescence has been reached. The mergers and isolated disks are respectively plotted with “+” and “Δ”. The MASSIV sample (Contini et al. 2012) positions are computed using the half-mass stellar radius for a typical gas fraction of 45%, and are plotted using black diamonds for isolated galaxies, triangles for minor mergers, and squares for major mergers. The associated error bars are computed using the errors on Hα flux, stellar size, and the assumption that the gas fraction fg lies in the range [0.25, 0.65].

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