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The nature of dust in distant galaxies is not well understood, and untilrecently few direct dust measurements have been possible. We investigate dustin distant star-forming galaxies using near-infrared grism spectra of the3D-HST survey combined with archival multi-wavelength photometry. These dataallow us to make a direct comparison between dust around star-forming regions($A_{V,\mathrm{HII}}$) and the integrated dust content ($A_{V,\mathrm{star}}$).We select a sample of 163 galaxies between $1.36\le{}z\le1.5$ with H$\alpha$signal-to-noise ratio $\ge5$ and measure Balmer decrements from stacked spectrato calculate $A_{V,\mathrm{HII}}$. First, we stack spectra in bins of$A_{V,\mathrm{star}}$, and find that$A_{V,\mathrm{HII}}=1.86\,A_{V,\mathrm{star}}$, with a significance of$\sigma=1.7$. Our result is consistent with the two-component dust model, inwhich galaxies contain both diffuse and stellar birth cloud dust. Next, westack spectra in bins of specific star formation rate ($\log\,\mathrm{SSFR}$),star formation rate ($\log\,\mathrm{SFR}$), and stellar mass ($\log{}M_*$). Wefind that on average $A_{V,\mathrm{HII}}$ increases with SFR and mass, butdecreases with increasing SSFR. Interestingly, the data hint that the amount ofextra attenuation decreases with increasing SSFR. This trend is expected fromthe two-component model, as the extra attenuation will increase once olderstars outside the star-forming regions become more dominant in the galaxyspectrum. Finally, using Balmer decrements we derive dust-corrected H$\alpha$SFRs, and find that stellar population modeling produces incorrect SFRs ifrapidly declining star formation histories are included in the exploredparameter space.

Direct measurements of dust attenuation in z~1.5 star-forming galaxies from 3D-HST: Implications for dust geometry and star formation rates