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We employ a recently developed population-orbit superposition technique tosimultaneously fit the stellar kinematic and age maps of 82 CALIFA spiralgalaxies and obtain the ages of stars in different dynamical structures. Wefirst evaluated the capabilities of this method on CALIFA-like mock datacreated from the Auriga simulations. The recovered mean ages of dynamicallycold, warm, and hot components match the true values well, with anobservational error of up to $20\%$ in the mock age maps. For CALIFA spiralgalaxies, we find that the stellar ages of the cold, warm, and hot componentsall increase with the stellar mass of the galaxies, from $\overline{t_{\rmcold}}\sim2.2$ Gyr, $\overline{t_{\rm warm}}\sim2.3$ Gyr, and $\overline{t_{\rmhot}}\sim2.6$ Gyr for galaxies with stellar mass $M_*<10^{10}\,\rm M_{\odot}$,to $\overline{t_{\rm cold}}\sim4.0$ Gyr, $\overline{t_{\rm warm}}\sim5.1$ Gyr,and $\overline{t_{\rm hot}}\sim5.9$ Gyr for galaxies with $M_*>10^{11}\,\rmM_{\odot}$. About $80\%$ of the galaxies in our sample have $t_{\rm hot}>t_{\rmcold}$, and the mean values of $t_{\rm hot}-t_{\rm cold}$ also increase withstellar mass, from $0.7_{-0.2}^{+0.6}$ Gyr in low-mass galaxies ($10^{8.9}\,\rmM_{\odot}<M_*\le10^{10.5}\,\rm M_{\odot}$) to $1.7_{-0.2}^{+0.7}$ Gyr inhigh-mass galaxies ($10^{10.5}\,\rm M_{\odot}<M_*<10^{11.3}\,\rm M_{\odot}$).The stellar age is younger in disks than in bulges, on average. This suggeststhat either the disks formed later and/or that they experienced a moreprolonged and extensive period of star formation. Lower-mass spiral galaxieshave younger bulges and younger disks, while higher-mass spiral galaxiesgenerally have older bulges, and their disks span a wide range of ages. This isconsistent with the scenario in which the bulges in more massive spirals formedearlier than those in less massive spirals.

Quantifying the stellar ages of dynamically separated bulges and disks of CALIFA spiral galaxies