We use the near--infrared Brgamma hydrogen recombination line as a reference star formation rate (SFR) indicator to test the validity and establish the calibration of the {it Herschel} PACS 70 mu m emission as a SFR tracer for sub--galactic regions i
n external galaxies. Brgamma offers the double advantage of directly tracing ionizing photons and of being relatively insensitive to the effects of dust attenuation. For our first experiment, we use archival CFHT Brgamma and Ks images of two nearby galaxies: NGC,5055 and NGC,6946, which are also part of the {it Herschel} program KINGFISH (Key Insights on Nearby Galaxies: a Far-Infrared Survey with Herschel). We use the extinction corrected Brgamma emission to derive the SFR(70) calibration for H{sc ii} regions in these two galaxies. A comparison of the SFR(70) calibrations at different spatial scales, from 200 pc to the size of the whole galaxy, reveals that about 50% of the total 70mu m emission is due to dust heated by stellar populations that are unrelated to the current star formation. We use a simple model to qualitatively relate the increase of the SFR(70) calibration coefficient with decreasing region size to the star formation timescale. We provide a calibration for an unbiased SFR indicator that combines the observed Halpha with the 70 mu m emission, also for use in H{sc ii} regions. We briefly analyze the PACS 100 and 160 mu m maps and find that longer wavelengths are not as good SFR indicators as 70mu m, in agreement with previous results. We find that the calibrations show about 50% difference between the two galaxies, possibly due to effects of inclination.
