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We present results on the dust attenuation of galaxies at redshift $\sim3-6$by studying the relationship between the UV spectral slope ($\beta_{\rm UV}$)and the infrared excess (IRX; $L_{\rm IR}$/$L_{\rm UV}$) using ALMAfar-infrared continuum observations. Our study is based on a sample of 67massive, star-forming galaxies with a median mass of $M_{\ast}\sim10^{10.7}\,M_{\rm \odot}$ spanning a redshift range $z=2.6-3.7$ (median$z=3.2$) that were observed with ALMA at $\lambda_{rest}=300\,{\rm \mu m}$.Both the individual ALMA detections (41 sources) and stacks including allgalaxies show the IRX-$\beta_{\rm UV}$ relationship at $z\sim3$ is mostlyconsistent with that of local starburst galaxies on average. However, we findevidence for a large dispersion around the mean relationship by up to $\pm0.5$dex. Nevertheless, the locally calibrated dust correction factors based on theIRX-$\beta_{\rm UV}$ relation are on average applicable to main-sequence$z\sim3$ galaxies. This does not appear to be the case at even higherredshifts, however. Using public ALMA observations of $z\sim4-6$ galaxies wefind evidence for a significant evolution in the IRX-$\beta_{\rm UV}$ and theIRX-$M_{\ast}$ relations beyond $z\sim3$ toward lower IRX values. We discussseveral caveats that could affect these results, including the assumed dusttemperature. ALMA observations of larger $z>3$ galaxy samples will be requiredto confirm this intriguing redshift evolution.

The Dust Attenuation of Star-forming Galaxies at $z\sim3$ and Beyond: New Insights from ALMA Observations