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We analyze the spatially resolved star formation history of 300 nearbygalaxies from the CALIFA integral field spectroscopic survey to investigate theradial structure and gradients of the present day stellar populationsproperties as a function of Hubble type and galaxy stellar mass. A fossilrecord method based on spectral synthesis techniques is used to recoverspatially and temporally resolved maps of stellar population properties ofspheroidal and spiral galaxies with masses $10^9$ to $7 \times 10^{11}$M$_\odot$. The results show that galaxy-wide spatially averaged stellarpopulation properties (stellar mass, mass surface density, age, metallicity,and extinction) match those obtained from the integrated spectrum, and thatthese spatially averaged properties match those at $R = 1$ HLR (half lightradius), proving that the effective radii are really effective.  Further, the individual radial profiles of the stellar mass surface density($\mu_\star$), luminosity weighted ages ($< {\rm log}\,age>_L$), and massweighted metallicity ($< \log Z_\star >_M$) are stacked in bins of galaxymorphology (E, S0, Sa, Sb, Sbc, Sc and Sd). All these properties show negativegradients as a sign of the inside-out growth of massive galaxies. However, thegradients depend on the Hubble type in different ways. For the same galaxymass, E and S0 galaxies show the largest inner gradients in $\mu_\star$; whileMW-like galaxies (Sb with $M_\star \sim 10^{11} M_\odot$) show the largestinner age and metallicity gradients. The age and metallicity gradients suggestthat major mergers have a relevant role in growing the center (within 3 HLR) ofmassive early type galaxies; and radial mixing may play a role flattening theradial metallicity gradient in MW-like disks.

CALIFA across the Hubble types: Spatially resolved properties of the stellar populations