The CALIFA survey across the Hubble sequence: How galaxies grow their
  bulges and disks
  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
$M_\star \sim 10^9$ to $7 \times 10^{11}$ $M_\odot$. We derive the stellar mass
surface density ($\mu_\star$), light-weighted and mass-weighted ages ($\langle
{\rm log}\,age\rangle _L$, $\langle {\rm log}\,age\rangle _M$), and
mass-weighted metallicity ($\langle {\rm log}\,Z_\star\rangle _M$), applying
the spectral synthesis technique. We study the mean trends with galaxy stellar
mass, $M_\star$, and morphology (E, S0, 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$_\star$, which evidences that
quenching is related to morphology, but not driven by mass.
