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We study the relation between the UV-slope, $\beta$, and the ratio betweenthe infrared- and UV-luminosities (IRX) of galaxies from TNG50, the latestinstallment of the IllustrisTNG galaxy formation simulations. We select 7280star-forming main-sequence (SFMS) galaxies with stellar mass $10^9M_\odot$ atredshifts $0 \leq z \leq 4$ and perform radiative transfer with SKIRT to modeleffects of interstellar medium dust on the emitted stellar light. Assuming aMilky Way (MW) dust type and a dust-to-metal ratio of 0.3, we find that TNG50SFMS galaxies generally agree with observationally-derived IRX-$\beta$relations at $z \lesssim 1$. However, we find a redshift-dependent systematicoffset with respect to empirically-derived local relations, with the TNG50IRX-$\beta$ relation shifting towards lower $\beta$ and steppening at higherredshifts. This is partially driven by variations in the dust-uncorrectedUV-slope of galaxies, due to different star-formation histories of galaxiesselected at different cosmic epochs; we suggest the remainder of the effect iscaused by differences in the effective dust attenuation curves (EDACs) ofgalaxies as a function of redshift. We find a typical galaxy-to-galaxyvariation of 0.3 dex in IRX at fixed $\beta$, correlated with intrinsic galaxyproperties: galaxies with higher star-formation rates, star-formationefficiencies, gas metallicities and stellar masses exhibit larger IRX values.We demonstrate a degeneracy between stellar age, dust geometry and dustcomposition: $z=4$ galaxies with a Small Magellanic Cloud dust type follow thesame IRX-$\beta$ relation as low-redshift galaxies with MW dust. We provide aredshift-dependent fitting function for the IRX-$\beta$ relation for MW dustbased on our models.

A redshift-dependent IRX-$\beta$ dust attenuation relation for TNG50 galaxies