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Fig. 8.

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SFHs for NGC 1433 in different galactocentric radii for the original data (left) and the ND data (right). In the y-axis we display the fraction of mass formed. In the upper part of each panel we use arrows to display the mean age for each SFH, following the same colour coding with respect to the distance to the centre. For both data cubes, it is clear that the farther from the centre, the younger the SFH is (with the exception of the last curve), meaning that the fraction of younger stars increases. This is shown even more strikingly with the subtracted data cube: it is clear that the outskirts of the ND are in fact younger, in accordance with the inside-out growth scenario of Bittner et al. (2019).

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