  Using the largest sample of galaxies observed with an optical integral field
unit (IFU, the SDSS-IV MaNGA survey, $\sim$10000 targets), we derive the radial
distribution of the physical properties obtained from the stellar continuum and
the ionized-gas emission lines. Given the large sample, we are able to explore
the impact of the total stellar mass and morphology by averaging those radial
distributions for different bins of both global properties. We use a piece-wise
analysis to characterize the slopes of the gradients from those properties at
different galactocentric distances. In general we find that most of the
properties -- derived from both the stellar continuum and the ionized gas
emission lines -- exhibit a negative gradient with a secondary impact by global
properties such as the total stellar mass or morphology. Our results confirm
the intimate interplay between the properties of the stellar component and
those of the ionized gas at local (kpc) scales in order to set the observed
gradients. Furthermore, the resemblance of the gradients for similar global
properties (in particular for the stellar parameters) indicates statistical
similar histories of star formation and chemical enrichment with an initial
radial gas distribution following the potential of the galaxy.
