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Context. Measuring star formation at a local scale is important to constrainstar formation laws. Yet, it is not clear whether and how the measure of starformation is affected by the spatial scale at which a galaxy is observed. Aims.We want to understand the impact of the resolution on the determination of thespatially resolved star formation rate (SFR) and other directly associatedphysical parameters such as the attenuation. Methods. We have carried out amulti-scale, pixel-by-pixel study of the nearby galaxy M33. Assembling FUV,Halpha, 8, 24, 70, and 100 micron maps, we have systematically compared theemission in individual bands with various SFR estimators from a resolution of33 pc to 2084 pc. Results. We have found that there are strong,scale-dependent, discrepancies up to a factor 3 between monochromatic SFRestimators and Halpha+24 micron. The scaling factors between individual IRbands and the SFR show a strong dependence on the spatial scale and on theintensity of star formation. Finally, strong variations of the differentialreddening between the nebular emission and the stellar continuum are seen,depending on the specific SFR (sSFR) and on the resolution. At the finestspatial scales, there is little differential reddening at high sSFR. Thedifferential reddening increases with decreasing sSFR. At the coarsest spatialscales the differential reddening is compatible with the canonical value foundfor starburst galaxies. Conclusions. Our results confirm that monochromaticestimators of the SFR are unreliable at scales smaller than 1 kpc. Furthermore,the extension of local calibrations to high redshift galaxies presentsnon-trivial challenges as the properties of these systems may be poorly known.

Measuring star formation with resolved observations: the test case of M33