Notes. (1) ID CALIFA identifier; (2) galaxy name; (3) morphological type; (4) distance in Mpc calculated from redshift; (5) minor-to-major axis ratio as given by the RC3 catalog, i.e., measured in the D25 B-band isophote; (6) observed-Hα flux using an elliptical aperture with a semimajor axis of 36 arcsec; (7) attenuation obtained using the Balmer decrement. As explained in Sect. 3.1.4, we have assumed an intrinsic Hα/Hβ ratio of 2.86 (although lower values are also physically possible in HII regions, depending on the electron density, effective temperature, and therefore on the chemical abundance. This leads to a number of galaxies for which we assumed A(Hα) = 0 that also appeared in this table). The errors listed here only use the Hα flux uncertainty, an additional 7% uncertainty in the Hβ flux have been taken into account for the errors in the Hα luminosities, Col. (8), and SFRs, Col. (9) and in the attenuations used in the paper; (8) observed Hα luminosity corrected for aperture effects; (9) Balmer-corrected and aperture-corrected Hα SFR values; (10) observed FUV luminosity; (11) observed NUV luminosity; (12) UV color in AB system; (13) TIR luminosity defined as the total infrared emission in the range 8−1000 μm; (14) 22 μm (aperture photometry) luminosity. As explained in Sect. 3.3, it has been pointed out by several authors (Wright et al. 2010; Jarrett et al. 2013; Brown et al. 2014) that SF galaxies measured with the WISE 22 μm filter are systematically brighter by ~10 % than that inferred from Spitzer IRS and 24 μm data. For that reason, the 22 μm luminosity values given in Col. (14) have to be multiplied by 1/1.1. Note that galaxies UGC 00987 and UGC 03973 are classified as type-1 AGN within our sample. As a consequence, they have been excluded from the SFR analysis.