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We present the results of a new study of dust attenuation at redshifts $3 < z< 4$ based on a sample of $236$ star-forming galaxies from the VANDELSspectroscopic survey. Motivated by results from the First Billion Years (FiBY)simulation project, we argue that the intrinsic spectral energy distributions(SEDs) of star-forming galaxies at these redshifts have a self-similar shapeacross the mass range $8.2 \leq$ log$(M_{\star}/M_{\odot}) \leq 10.6$ probed byour sample. Using FiBY data, we construct a set of intrinsic SED templateswhich incorporate both detailed star formation and chemical abundancehistories, and a variety of stellar population synthesis (SPS) modelassumptions. With this set of intrinsic SEDs, we present a novel approach fordirectly recovering the shape and normalization of the dust attenuation curve.We find, across all of the intrinsic templates considered, that the averageattenuation curve for star-forming galaxies at $z\simeq3.5$ is similar in shapeto the commonly-adopted Calzetti starburst law, with an averagetotal-to-selective attenuation ratio of $R_{V}=4.18\pm0.29$. We show that theoptical attenuation ($A_V$) versus stellar mass ($M_{\star}$) relationpredicted using our method is consistent with recent ALMA observations ofgalaxies at $2<z<3$ in the \emph{Hubble} \emph{Ultra} \emph{Deep} \emph{Field}(HUDF), as well as empirical $A_V - M_{\star}$ relations predicted by aCalzetti-like law. Our results, combined with other literature data, suggestthat the $A_V - M_{\star}$ relation does not evolve over the redshift range$0<z<5$, at least for galaxies with log$(M_{\star}/M_{\odot}) \gtrsim 9.5$.Finally, we present tentative evidence which suggests that the attenuationcurve may become steeper at log$(M_{\star}/M_{\odot}) \lesssim 9.0$.

The VANDELS survey: Dust attenuation in star-forming galaxies at $\mathbf{z=3-4}$