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