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In recent years, significant growth in the amount of data available toastronomers has opened up the possibility to uncover fundamental correlations,linking the dust component of a galaxy to its star formation rate (SFR). Inthis paper, we re-examine these correlations, investigating the origin of theobserved scatter, and the ability of the James Webb Space Telescope (JWST) toexplore such relations in the early Universe. We defined a sample of about 800normal star-forming galaxies with photometries in the range of 0.15 < $\lambda$< 500 microns and analysed them with different spectral energy distribution(SED) fitting methods. With the SEDs extracted, we investigated the detectionrate at different redshifts with the MId-Infrared instruments (MIRI) onboardthe JWST. Dust luminosity (L$_d$) and SFR show a strong correlation, but forSFR < 2 M$_\odot$ yr$^{-1}$, the correlation scatter increases dramatically. Weshow that selection based on the fraction of ultraviolet (UV) emission absorbedby dust, that is, the UV extinction, greatly reduces the data dispersion.Reproducing the sensitivity of the Cosmic Evolution Early Release ScienceSurvey (CEERS) and classifying galaxies according to their SFR and stellar mass(M$_\ast$), we investigated the MIRI detection rate as a function of thephysical properties of the galaxies. Fifty percent of the objects with SFR$\sim$ 1 M$_\odot$yr$^{-1}$ at $z$ = 6 are detected with F770, which decreasesto 20% at $z$ = 8. For such galaxies, only 5% of the subsample will be detectedat 5$\sigma$ with F770 and F1000 at $z$ = 8, and only 10% with F770, F1000, andF1280 at $z$ = 6. The link between dust and star formation is complex, and manyaspects remain to be fully understood. In this context, the JWST willrevolutionise the field, allowing investigation of the dust--star interplaywell within the epoch of reionisation.

The dust-star interplay in late-type galaxies at z < 0.5: forecasts for the JWST