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Recent observations with the James Webb Space Telescope are yieldingtantalizing hints of an early population of massive, bright galaxies at $z >10$, with Atacama Large Millimeter Array (ALMA) observations indicatingsignificant dust masses as early as $z\sim 7$. To understand the implicationsof these observations, we use the DELPHI semi-analytic model that jointlytracks the assembly of dark matter halos and their baryons, including the keyprocesses of dust enrichment. Our model employs only two redshift- andmass-independent free parameters (the maximum star-formation efficiency and thefraction of supernova energy that couples to gas) that are tuned against allavailable galaxy data at $z \sim 5-9$ before it is used to make predictions upto $z \sim 20$. Our key results are: (i) the model under-predicts the observedultraviolet luminosity function (UV LF) at $z > 12$; observations at $z>16$ lieclose to, or even above, a "maximal" model where all available gas is turnedinto stars; (ii) UV selection would miss 34\% of the star formation ratedensity at $z \sim 5$, decreasing to 17\% by $z \sim 10$ for bright galaxieswith $\rm{M_{UV}} < -19$; (iii) the dust mass ($M_d$) evolves with the stellarmass ($M_*$) and redshift as $\log(M_d) = 1.194\log(M_*) + 0.0975z - 5.433$;(iv) the dust temperature increases with stellar mass, ranging between $30-33$K for $M_* \sim 10^{9-11}M_\odot$ galaxies at $z \sim 7$. Finally, we predictthe far infrared LF at $z \sim 5-20$, testable with ALMA observations, andcaution that spectroscopic redshifts and dust masses must be pinned down beforeinvoking unphysical extrema in galaxy formation models.

The dust enrichment of early galaxies in the JWST and ALMA era