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The rate at which interstellar gas is converted into stars, and itsdependence on environment, is one of the pillars on which our understanding ofthe visible Universe is build. We present a comparison of the surface densityof young stars (Sigma_*) and dust surface density (Sigma_d) across NGC346 (N66)in 115 independent pixels of 6x6 pc^2. We find a correlation between Sigma_*and Sigma_d with a considerable scatter. A power law fit to the data yields asteep relation with an exponent of 2.6+-0.2. We convert Sigma_d to gas surfacedensity (Sigma_g) and Sigma_* to star formation rate (SFR) surface densities(Sigma_SFR), using simple assumptions for the gas-to-dust mass ratio and theduration of star formation. The derived total SFR (4+-1 10^-3 M_sun/yr) isconsistent with SFR estimated from the Ha emission integrated over the Hanebula. On small scales the Sigma_SFR derived using Ha systematicallyunderestimates the count-based Sigma_SFR, by up to a factor of 10. This is dueto ionizing photons escaping the area, where the stars are counted. We findthat individual 36 pc^2 pixels fall systematically above integrateddisc-galaxies in the Schmidt-Kennicutt diagram by on average a factor of ~7.The NGC346 average SFR over a larger area (90 pc radius) lies closer to therelation but remains high by a factor of ~3. The fraction of the total mass(gas plus young stars) locked in young stars is systematically high (~10 percent) within the central 15 pc and systematically lower outside (2 per cent),which we interpret as variations in star formation efficiency. The inner 15 pcis dominated by young stars belonging to a centrally condensed cluster, whilethe outer parts are dominated by a dispersed population. Therefore, theobserved trend could reflect a change of star formation efficiency betweenclustered and non-clustered star-formation.

Star-formation rates from young-star counts and the structure of the ISM across the NGC346/N66 complex in the SMC