We investigate dust obscuration as parameterised by the infrared excess IRX$equiv$$L_{rm IR}/L_{rm UV}$ in relation to global galaxy properties, using a sample of $sim$32$,$000 local star-forming galaxies (SFGs) selected from SDSS, GALEX and WISE. We show that IRX generally correlates with stellar mass ($M_ast$), star formation rate (SFR), gas-phase metallicity ($Z$), infrared luminosity ($L_{rm IR}$) and the half-light radius ($R_{rm e}$). A weak correlation of IRX with axial ratio (b/a) is driven by the inclination and thus seen as a projection effect. By examining the tightness and the scatter of these correlations, we find that SFGs obey an empirical relation of the form $IRX$=$10^alpha,(L_{rm IR})^{beta},R_{rm e}^{-gamma},(b/a)^{-delta}$ where the power-law indices all increase with metallicity. The best-fitting relation yields a scatter of $sim$0.17$,$dex and no dependence on stellar mass. Moreover, this empirical relation also holds for distant SFGs out to $z=3$ in a population-averaged sense, suggesting it to be universal over cosmic time. Our findings reveal that IRX approximately increases with $L_{rm IR}/R_{rm e}^{[1.3 - 1.5]}$ instead of $L_{rm IR}/R_{rm e}^{2}$ (i.e., surface density). We speculate this may be due to differences in the spatial extent of stars versus star formation and/or complex star-dust geometries. We conclude that not stellar mass but IR luminosity, metallicity and galaxy size are the key parameters jointly determining dust obscuration in SFGs.
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