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Fig. 5.

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Radial range of star-forming region (RRSF) versus the relative strength of the metallicity gradient for different ages, for the four highlighted galaxies in Figure 4. The correlation between ∇[Fe/H](τ) and Range [ Fe / H ] ( age ) $ \mathrm{Range}\widetilde{\mathrm{[Fe/H]}}\mathrm{(age)} $ is given in the bottom left of each panel, below the subhalo ID. The top panels depict situations in which the evolution of the metallicity gradient can be recovered from the scatter in [Fe/H], while the bottom row illustrates two examples of galaxies where the gradient cannot be recovered in this fashion due to the gradient being steepest during a time of a lower star-forming region.

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