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The Star Formation Rate (SFR) is one of the main parameters used to analyzethe evolution of galaxies through time. The need for recovering the lightreprocessed by dust commonly requires the use of low spatial resolutionfar-infrared data. Recombination-line luminosities provide an alternative,although uncertain dust-extinction corrections based on narrow-band imaging orlong-slit spectroscopy have traditionally posed a limit to their applicability.Integral Field Spectroscopy (IFS) is clearly the way to overcome suchlimitation. We obtain integrated H{\alpha}, ultraviolet (UV) and infrared(IR)-based SFR measurements for 272 galaxies from the CALIFA survey at 0.005 <z < 0.03 using single-band and hybrid tracers. We provide updated calibrations,both global and split by properties (including stellar mass and morphologicaltype), referred to H{\alpha}. The extinction-corrected H{\alpha} luminosityagrees with the updated hybrid SFR estimators based on either UV or H{\alpha}plus IR luminosity over the full range of SFRs (0.03-20 M$_{\odot}$ yr$^{-1}$).The coefficient that weights the amount of energy produced by newly-born starsthat is reprocessed by dust on the hybrid tracers, a$_{IR}$, shows a largedispersion. However, it does not became increasingly small at highattenuations, as expected if significant highly-obscured H$\alpha$ emissionwould be missed. Lenticulars, early-type spirals and type-2 AGN host galaxiesshow smaller coefficients due to the contribution of optical photons and AGN todust heating. In the Local Universe the H{\alpha} luminosity derived from IFSobservations can be used to measure SFR, at least in statistically-significant,optically-selected galaxy samples. The analysis of the SFR calibrations bygalaxies properties could be potentially used by other works to study theimpact of different selection criteria in the SFR values derived.

Star Formation in the Local Universe from the CALIFA sample. I. Calibrating the SFR using IFS data