Notes. Col. 1: galaxy name;Col. 2: morphological classification adopted from the NASA/IPAC Extragalactic Database (NED);Col. 3: classification according to our study in P13, based on the mean τ ratio (Col. 12) for the extranuclear component (type i, i+, and ii);Col. 4: right ascension;Col. 5: declination;Col. 6: distance in Mpc adopted from NED;Col. 7: apparent r total magnitude from SDSS DR7;Col. 8: petrosian_50 radius in arcsec in the SDSS r band;Col. 9: integral Hα flux in units of 10^-16 erg s^-1 cm^-2, derived from CALIFA IFS data;Col. 10: integral Hα luminosity in units of 10³⁹ erg s^-1;Col. 11: logarithm of all stellar mass ever formed and present stellar mass in M_⊙, as obtained from spectral modeling with Starlight;Col. 12: mean τ ratio (from P13 in the case of ETGs);Col. 13: spectroscopic classification based on the emission-line ratios (panels i and j of Figs. 1, C.1–C.31 and D.1–D.5) of the nuclear (R^⋆≤ 3.̋8) CALIFA spectrum. The notation is as follows: H: Hii/star-forming, C: composite (cf. description of panels i and j of Fig. 1), L: LINER, S: Seyfert. When available, the spectroscopic classification from NED is included within brackets, and the index following the • symbol indicates that additional information is available at the NED on the morphology of the radio continuum: (1) radio jet, (2) narrow-angle tail radio source, (3) FR I source; Col. 14: tentative three-character kinematical classification: r: rotation-dominated kinematics, p: perturbed rotational pattern, o: gas outflow, and n: no distinguishable pattern or pressure-supported stellar kinematics. The first and third character refer to the kinematics of stars and gas, respectively, and the second character indicates in the case of stellar rotation (r or p) whether the kinematic and photometric major axes are roughly aligned (∥) or not (∦). The + symbol marks ETGs without detected stellar rotation (n) or with a nearly circular-symmetric morphology, thus uncertain photometric major axis. Galaxies NGC 7025, NGC 7236, and NGC 7436B overlap by a substantial fraction of their area with extended foreground/background sources that, even after subtraction, most likely introduce uncertainties of ~10% in the quoted Hα fluxes.