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Dust attenuation affects nearly all observational aspects of galaxyevolution, yet very little is known about the form of the dust-attenuation lawin the distant Universe. Here, we model the spectral energy distributions(SEDs) of galaxies at z = 1.5--3 from CANDELS with rest-frame UV to near-IRimaging under different assumptions about the dust law, and compare the amountof inferred attenuated light with the observed infrared (IR) luminosities. Someindividual galaxies show strong Bayesian evidence in preference of one dust lawover another, and this preference agrees with their observed location on theplane of infrared excess (IRX, $L_{\text{TIR}}/L_{\text{UV}}$) and UV slope($\beta$). We generalize the shape of the dust law with an empirical model,$A_{\lambda,\delta}=E(B-V)\ k_\lambda\ (\lambda/\lambda_V)^\delta$ where$k_\lambda$ is the dust law of Calzetti et al. (2000), and show that thereexists a correlation between the color excess ${E(B-V)}$ and tilt $\delta$ with${\delta=(0.62\pm0.05)\log(E(B-V))}$+ ${(0.26~\pm~0.02)}$. Galaxies with highcolor excess have a shallower, starburst-like law, and those with low colorexcess have a steeper, SMC-like law. Surprisingly, the galaxies in our sampleshow no correlation between the shape of the dust law and stellar mass,star-formation rate, or $\beta$. The change in the dust law with color excessis consistent with a model where attenuation is caused by by scattering, amixed star-dust geometry, and/or trends with stellar population age,metallicity, and dust grain size. This rest-frame UV-to-near-IR method showspotential to constrain the dust law at even higher ($z>3$) redshifts.

Breaking the Curve with CANDELS: A Bayesian Approach to Reveal the Non-Universality of the Dust-Attenuation Law at High Redshift