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We use a newly assembled large sample of 3,545 star-forming galaxies withsecure spectroscopic, grism, and photometric redshifts at z=1.5-2.5 toconstrain the relationship between UV slope (beta) and dust attenuation(L(IR)/L(UV)=IRX). Our sample benefits from the combination of deep HubbleWFC3/UVIS photometry from the Hubble Deep UV (HDUV) Legacy survey and existingphotometric data compiled in the 3D-HST survey, and extends the range of UVluminosity and beta probed in previous UV-selected samples. IRX is measuredusing stacks of deep Herschel/PACS 100 and 160 micron data, and the results arecompared with predictions of the IRX-beta relation for different assumptions ofthe stellar population model and obscuration curve. We find that z=1.5-2.5galaxies have an IRX-beta relation that is consistent with the predictions foran SMC extinction curve if we invoke sub-solar metallicity models that arecurrently favored for high-redshift galaxies, while the commonly assumedstarburst attenuation curve over-predicts the IRX at a given beta by a factorof ~3. The IRX of high-mass (M*>10^9.75 Msun) galaxies is a factor of >4 largerthan that of low-mass galaxies, lending support for the use of stellar mass asa proxy for attenuation. The commonly observed trend of fainter galaxies havingbluer beta may simply reflect bluer intrinsic UV slopes for such galaxies,rather than lower obscurations. The IRX-beta for young/low-mass galaxiesimplies a dust curve that is steeper than the SMC, suggesting a lowerattenuation at a given beta relative to older/more massive galaxies. The lowerattenuations and higher ionizing photon output implied by low metallicitystellar population models point to Lyman continuum production efficiencies,xi_ion, that may be elevated by a factor of ~2 relative to the canonical valuefor L* galaxies, aiding in their ability to keep the universe ionized at z~2.[Abridged]

The HDUV Survey: A Revised Assessment of the Relationship between UV Slope and Dust Attenuation for High-Redshift Galaxies