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Using deep narrow-band and broad-band imaging, we identify 401 z~0.40 and 249z~0.49 H-alpha line-emitting galaxies in the Subaru Deep Field. Compared toother H-alpha surveys at similar redshifts, our samples are unique since theyprobe lower H-alpha luminosities, are augmented with multi-wavelength(rest-frame 1000AA--1.5 microns) coverage, and a large fraction (20%) of oursamples has already been spectroscopically confirmed. Our spectra allow us tomeasure the Balmer decrement for nearly 60 galaxies with H-beta detected above5-sigma. The Balmer decrements indicate an average extinction ofA(H-alpha)=0.7^{+1.4}_{-0.7} mag. We find that the Balmer decrementsystematically increases with higher H-alpha luminosities and with largerstellar masses, in agreement with previous studies with sparser samples. Wefind that the SFRs estimated from modeling the spectral energy distribution(SED) is reliable---we derived an "intrinsic" H-alpha luminosity which is thenreddened assuming the color excess from SED modeling. The SED-predicted H-alphaluminosity agrees with H-alpha narrow-band measurements over 3 dex (rms of 0.25dex). We then use the SED SFRs to test different statistically-based dustcorrections for H-alpha and find that adopting one magnitude of extinction isinappropriate: galaxies with lower luminosities are less reddened. We find thatthe luminosity-dependent dust correction of Hopkins et al. yields consistentresults over 3 dex (rms of 0.3 dex). Our comparisons are only possible byassuming that stellar reddening is roughly half of nebular reddening. Thestrong correspondence argue that with SED modeling, we can derive reliableintrinsic SFRs even in the absence of H-alpha measurements at z~0.5.

Dust Attenuation and H-alpha Star Formation Rates of z~0.5 Galaxies