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For the first time both H$\alpha$ and far-ultraviolet (FUV) observations froman HI-selected sample are used to determine the dust-corrected star formationrate density (SFRD: $\dot{\rho}$) in the local Universe. Applying the two starformation rate indicators on 294 local galaxies we determine log($\dot{\rho}$$_{H\alpha}) = -1.68~^{+0.13}_{-0.05}$ [M$_{\odot} $ yr$^{-1} $ Mpc$^{-3}]$ andlog($\dot{\rho}_{FUV}$) $ = -1.71~^{+0.12}_{-0.13}$ [M$_\odot $ yr$^{-1} $Mpc$^{-3}]$. These values are derived from scaling H$\alpha$ and FUVobservations to the HI mass function. Galaxies were selected to uniformlysample the full HI mass (M$_{HI}$) range of the HI Parkes All-Sky Survey(M$_{HI} \sim10^{7}$ to $\sim10^{10.7}$ M$_{\odot}$). The approach leads torelatively larger sampling of dwarf galaxies compared to optically-selectedsurveys. The low HI mass, low luminosity and low surface brightness galaxypopulations have, on average, lower H$\alpha$/FUV flux ratios than theremaining galaxy populations, consistent with the earlier results of Meurer.The near-identical H$\alpha$- and FUV-derived SFRD values arise with the lowH$\alpha$/FUV flux ratios of some galaxies being offset by enhanced H$\alpha$from the brightest and high mass galaxy populations. Our findings confirm thenecessity to fully sample the HI mass range for a complete census of local starformation to include lower stellar mass galaxies which dominate the localUniverse.

Near-identical star formation rate densities from H$\alpha$ and FUV at redshift zero