Distribution of the metallicity gradients calculated for the simulated systems presented in Revaz & Jablonka (2018), on the left panel as a function of their stellar mass and color-coded according to their t₉₀, while inverting these two variables in the right panel. Numbers identify the individual halos mentioned in the main text, while the gradient values for the Local Group dwarf galaxies presented in this work are shown as grey circles with their associated error bars. We have assumed in this case a stellar mass-to-light ratio of one.