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We update the spectral modeling code MAGPHYS to include a 2175\AA\ absorptionfeature in its UV-to-near-IR dust attenuation prescription. This allows us todetermine the strength of this feature and the shape of the dust attenuationcurve in ~5000 star-forming galaxies at 0.1<z<3 in the COSMOS field. We findthat a 2175\AA\ absorption feature of ~1/3 the strength of that in the MilkyWay is required for models to minimize residuals. We characterize the totaleffective dust attenuation curves as a function of several galaxy propertiesand find that the UV slopes of the attenuation curve for COSMOS galaxies show astrong dependence with star formation rate (SFR) and total dust attenuation($A_V$), such that galaxies with higher SFR and $A_V$ have shallower curves andvice versa. These results are consistent with expectations from radiativetransfer that attenuation curves become shallower as the effective dust opticaldepth increases. We do not find significant trends in the strength of the2175\AA\ absorption feature as a function of galaxy properties, but this mayresult from the high uncertainties associated with this measurement. Theupdated code is publicly available online.

The Strength of the 2175\AA\ Feature in the Attenuation Curves of Galaxies at 0.1