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We present measurements of the dust attenuation of H\alpha-selectedemission-line galaxies at z=0.8 from the NewH\alpha\ narrowband survey. Theanalysis is based on deep follow-up spectroscopy with Magellan/IMACS, whichcaptures the strong rest-frame optical emission lines from [OII] \lambda 3727to [OIII] \lambda 5007. The spectroscopic sample used in this analysis consistsof 341 confirmed H\alpha\ emitters. We place constraints on the AGN fractionusing diagnostics which can be applied at intermediate redshift. We find thatat least 5% of the objects in our spectroscopic sample can be classified as AGNand 2% are composite, i.e. powered by a combination of star-formation and AGNactivity. We measure the dust attenuation for individual objects from theratios of the higher order Balmer lines. The H\beta\ and H\gamma\ pair of linesis detected with S/N>5 in 55 individual objects and the H\beta\ and H\delta\pair is detected in 50 individual objects. We also create stacked spectra toprobe the attenuation in objects without individual detections. The medianattenuation at H\alpha\ based on the objects with individually detected linesis A(H\alpha)=0.9+-1.0 magnitudes, in good agreement with the attenuation foundin local samples of star-forming galaxies. We find that the z=0.8 galaxiesoccupy a similar locus of attenuation as a function of magnitude, mass and SFRas a comparison sample drawn from the SDSS DR4. Both the results from theindividual z=0.8 galaxies and from the stacked spectra show consistency withthe mass -- attenuation and SFR -- attenuation relations found in the localUniverse, indicating that these relations are also applicable at intermediateredshift.

Nebular Attenuation in H\alpha-selected Star-forming Galaxies at z=0.8 from the NewH\alpha\ Survey