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We present results on the dust attenuation curve of z~2 galaxies using earlyobservations from the MOSFIRE Deep Evolution Field (MOSDEF) survey. Our sampleconsists of 224 star-forming galaxies with nebular spectroscopic redshifts inthe range z= 1.36-2.59 and high S/N measurements of, or upper limits on, theH-alpha and H-beta emission lines obtained with Keck/MOSFIRE. We constructcomposite SEDs of galaxies in bins of specific SFR and Balmer optical depth inorder to directly constrain the dust attenuation curve from the UV throughnear-IR for typical star-forming galaxies at high redshift. Our results implyan attenuation curve that is very similar to the SMC extinction curve atwavelengths redward of 2500 Angstroms. At shorter wavelengths, the shape of thecurve is identical to that of the Calzetti relation, but with a lowernormalization (R_V). Hence, the new attenuation curve results in SFRs that are~20% lower, and log stellar masses that are 0.16 dex lower, than those obtainedwith the Calzetti attenuation curve. Moreover, we find that the difference inthe reddening---and the total attenuation---of the ionized gas and stellarcontinuum correlates strongly with SFR, such that for dust-corrected SFRslarger than 20 Msun/yr assuming a Chabrier IMF, the nebular emission linessuffer an increasing degree of obscuration relative to the continuum. A simplemodel that can account for these trends is one in which the UV through opticalstellar continuum is dominated by a population of less reddened stars, whilethe nebular line and bolometric luminosities become increasingly dominated bydustier stellar populations for galaxies with large SFRs, as a result of theincreased dust enrichment that accompanies such galaxies. Consequently, UV- andSED-based SFRs may underestimate the total SFR at even modest levels of ~20Msun/yr. [Abridged]

The MOSDEF Survey: Measurements of Balmer Decrements and the Dust Attenuation Curve at Redshifts z~1.4-2.6