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We present an analysis of the dust attenuation of star forming galaxies at$z=2.5-4.0$ through the relationship between the UV spectral slope ($\beta$),stellar mass ($M_{\ast}$) and the infrared excess(IRX$=L_{\rm{IR}}/L_{\rm{UV}}$) based on far-infrared continuum observationsfrom the Atacama Large Millimeter/sub-millimeter Array (ALMA). Our studyexploits the full ALMA archive over the COSMOS field processed by theA$^3$COSMOS team, which includes an unprecedented sample of $\sim1500$ galaxiesat $z\sim3$ as primary or secondary targets in ALMA band 6 or 7 observationswith a median continuum sensitivity of 126 $\rm{\mu Jy/beam}$ (1$\sigma$). Thedetection rate is highly mass dependent, decreasing drastically below $\log(M_{\ast}/M_{\odot})=10.5$. The detected galaxies show that the IRX-$\beta$relationship of massive ($\log M_{\ast}/M_{\odot} > 10$) main sequence galaxiesat $z=2.5-4.0$ is consistent with that of local galaxies, while starbursts aregenerally offset by $\sim0.5\,{\rm dex}$ to larger IRX values. At the low massend, we derive upper limits on the infrared luminosities through stacking ofthe ALMA data. The combined IRX-$M_{\ast}$ relation at$\rm{log\,(M_{\ast}/M_{\odot})>9}$ exhibits a significantly steeper slope thanreported in previous studies at similar redshifts, implying little dustobscuration at $\log M_{\ast}/M_{\odot}<10$. However, our results areconsistent with early measurements at $z\sim5.5$, indicating a potentialredshift evolution between $z\sim2$ and $z\sim6$. Deeper observations targetinglow mass galaxies will be required to confirm this finding.

A$^3$COSMOS: The Dust Attenuation of Star-Forming Galaxies at $z=2.5-4.0$ from the COSMOS-ALMA Archive