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We use a sample of 149 spectroscopically confirmed UV-selected galaxies at$z\sim 2$ to investigate the relative dust attenuation of the stellar continuumand the nebular emission lines. For each galaxy in the sample, at least onerest-frame optical emission line (H$\alpha$/[NII]$\lambda6583$ or[OIII]$\lambda5007$) measurement has been taken from the litterature, and 41galaxies have additional Spitzer/MIPS 24$\mu$m observations that are used toinfer infrared luminosities. We use a spectral energy distribution (SED)fitting code that predicts nebular line strengths when fitting the stellarpopulations of galaxies in our sample, and we perform comparisons between thepredictions of our models and the observed/derived physical quantities. We findthat on average our code is able to reproduce all the physical quantities(e.g., UV $\beta$ slopes, infrared luminosities, emission line fluxes), but weneed to apply a higher dust correction to the nebular emission compared to thestellar emission for the largest SFR($\log\mathrm{(SFR/M}_\odot\mathrm{yr}^{-1})>1.87$, Salpeter IMF). We find acorrelation between SFR and the difference in nebular and stellar colorexcesses, which could resolve the discrepant results regarding nebular dustcorrection at $z\sim2$ from previous results.

Dust attenuation of the nebular regions and optical emission lines of $z\sim2$ star-forming galaxies