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The dust attenuation for a sample of $\sim$10000 local ($z\lesssim0.1$) starforming galaxies is constrained as a function of their physical properties. Weutilize aperture-matched multi-wavelength data available from the GalaxyEvolution Explorer (GALEX) and the Sloan Digital Sky Survey (SDSS) to ensurethat regions of comparable size in each galaxy are being analyzed. We followthe method of Calzetti et al. (1994) and characterize the dust attenuationthrough the UV power-law index, $\beta$, and the dust optical depth, which isquantified using the difference in Balmer emission line optical depth,$\tau_B^l=\tau_{\mathrm{H}\beta} - \tau_{\mathrm{H}\alpha}$. The observedlinear relationship between $\beta$ and $\tau_B^l$ is similar to the localstarburst relation, but the large scatter ($\sigma_{\mathrm{int}}=0.44$)suggests there is significant variation in the local Universe. We derive aselective attenuation curve over the range$1250\mathrm{\AA}<\lambda<8320\mathrm{\AA}$ and find that a single attenuationcurve is effective for characterizing the majority of galaxies in our sample.This curve has a slightly lower selective attenuation in the UV compared topreviously determined curves. We do not see evidence to suggest that a 2175\AA\feature is significant in the average attenuation curve. Significant positivecorrelations are seen between the amount of UV and optical reddening and galaxymetallicity, mass, star formation rate (SFR), and SFR surface density. Thisprovides a potential tool for gauging attenuation where the stellar populationis unresolved, such as at high-$z$.

Characterizing Dust Attenuation in Local Star Forming Galaxies: UV and Optical Reddening