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tokens: and the detailed shape of the break. In fact, this is what we show in Fig. 5 . Type-II galaxies with strong breaks (less influenced by radial redistribution, especially accretion) display steeper stellar age and metallicity profiles than type-II systems with weak breaks or even type-I galaxies. A consistent behaviour is also found in the case of the age profiles for type-III galaxies in which systems with weak breaks (less affected by accretion) display steeper profiles than galaxies with strong breaks; in which case, even positive gradients are displayed. However, in the case of the metallicity gradients, this trend is inverted. Type-III galaxies with weak breaks have shallower profiles than systems with strong breaks (which are more affected by accretion). This inverted trend can be explained by the characteristics of the accreted stars. In Ruiz-Lara et al. (2016a) we showed that accreted stars populating the RaDES galaxies are mainly old, metal-poor stars. As a consequence, the accumulation of accreted stars in the outer parts of type-III galaxies giving rise to these kind of systems causes the outer parts to be old (positive age gradients) and relatively metal-poor (producing steeper negative profiles). Based on Fig. 5 we can conclude that, not only does radial redistribution of material affect the shape of observed light distributions, but also accretion has to play a key role in shaping observed stellar age and metallicity profiles. All these results and the similarities between the observational results (TRL17) and the theoretical work presented in this paper seem to indicate that radial redistribution of material and accretion shape the SB profiles and generally flatten the age and the metallicity profiles with the exception of the metallicity profiles for type-III galaxies due to the accumulation of metal-poor, accreted stars in the outer disc. The greater the efficiency of this redistribution, the larger the flattening effect. As a consequence, we would expect steeper age and metallicity gradients at birth than what we observe presently due to the effect of the radial redistribution of material. To shed light on this aspect and the true role of this redistribution in shaping the age and metallicity profiles we have also analysed the inner gradients of these stellar parameters in the absence of radial motions, that is, considering birth locations (see Fig. 6 ). Figure 6 shows the same information as Fig. 4 but focusing on the effect of radial motion of stars on the stellar age and metallicity gradients. In this case we show mean values for type-I, II and III systems, not the values for all the individual galaxies. Grey circles represent the mean values of the stellar age and metallicity gradients (averaging among SB types) considering stars located at their current locations. Grey squares represent the same mean quantities but this time computed using stars located at their birth locations (thus avoiding the effect of radial