We characterize in detail the radial structure of the stellar population properties of 300 galaxies in the nearby universe, observed with integral field spectroscopy in the CALIFA survey. The sample covers a wide range of Hubble types, from spheroidal to spiral galaxies, ranging in stellar masses from M_* ~ 10~9 to 7 × 10~(11) M_⊙. We derive the stellar mass surface density (μ_*), light-weighted and mass-weighted ages (_L, _M）, and mass-weighted metallicity (_M), applying the spectral synthesis technique. We study the mean trends with galaxy stellar mass, M_*, and morphology (E, SO, Sa, Sb, Sbc, Sc and Sd). We confirm that more massive galaxies are more compact, older, more metal rich, and less reddened by dust. Additionally, we find that these trends are preserved spatially with the radial distance to the nucleus. Deviations from these relations appear correlated with Hubble type: earlier types are more compact, older, and more metal rich for a given M_*, which evidences that quenching is related to morphology, but not driven by mass.
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