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tokens: more massive galaxies, LTGs have the same negative gradient regardless of mass. Metallicity gradients steepening for more massive ETGs is consistent with other studies from the MaNGA survey, Oyarzún et al. ( 2019 ) (after noting that they probe larger radii) and Lacerna et al. ( 2020 ). For C and Mg, at low masses the radial gradients are slightly positive, and they become shallower or slightly negative as galaxy mass increases. The gradients are independent of the type of galaxy. For the heavier elements, ETGs display similar gradients at all masses for [Ca/Fe], and become slightly negative as mass increases for [Ti/Fe]. High-mass spirals show larger variation in gradients with mass. The overall trend for Ca is unclear, but for Ti, the gradients become more negative as galaxy mass increases, like ETGs. N gradients go from slightly positive or shallow at low masses, to negative at high masses for both types. Finally, for Na, ETGs display a slight steepening in the gradient for the most massive galaxies while gradients are consistent for both types at intermediate masses. This suggests that the mass or some other property drives Na abundance variation rather than galaxy type. Briefly, we find several interesting features while studying these radial gradients in these parameters for different galaxy types. The most striking difference is in the age gradients. While ETGs display relatively flat age gradients, at all masses, LTGs show negative age gradients, which become steeper with mass. Metallicity behaves exactly the opposite way, with negative gradients steepening with mass for ETGs and negative gradients overall for LTGs. These properties could provide clues into how these different galaxy types and their stellar populations assembled and evolved. C and Mg abundances and radial gradients are remarkably similar for both types, suggesting that star formation time-scales are independent of galaxy type but rather depend on some other physical property i.e. galaxy mass or velocity dispersion. Na behaves in the same way as metallicity, showing negative gradients for LTGs, and negative gradients that steepen with mass for ETGs. We explore relations with velocity dispersion in the following section. 3.2.4 Local versus global relationships Along with radial gradients, it is informative to look at trends with velocity dispersion. We plot the spatially resolved parameters for both galaxy types, in different mass bins, so that we can identify local deviations (radial) from the global relation with velocity dispersion. The increased sample size and inclusion of different morphologies considerably expands our parameter space compared to P19, section 3.3. Fig. 18 shows all our derived stellar population parameters against the velocity dispersion. These velocity dispersion profiles shown in Fig. 5 have been calculated by combining the dispersions from the individual spectra belonging to each bin. The symbols represent three key pieces of information: (i)