The gas and stellar mass of low-redshift damped Lyman-$\alpha$ absorbers
  We report Hubble Space Telescope Cosmic Origins Spectrograph far-ultraviolet
and Arecibo Telescope H{\sc i} 21cm spectroscopic studies of six damped and
sub-damped Lyman-$\alpha$ absorbers (DLAs and sub-DLAs, respectively) at $z
\lesssim 0.1$, that have yielded estimates of their H{\sc i} column density,
metallicity and atomic gas mass. This significantly increases the number of
DLAs with gas mass estimates, allowing the first comparison between the gas
masses of DLAs and local galaxies. Including three absorbers from the
literature, we obtain H{\sc i} masses $\approx (0.24 - 5.2) \times 10^9 \: {\rm
M}_\odot$, lower than the knee of the local H{\sc i} mass function. This
implies that massive galaxies do not dominate the absorption cross-section for
low-$z$ DLAs. We use Sloan Digital Sky Survey photometry and spectroscopy to
identify the likely hosts of four absorbers, obtaining low stellar masses,
$\approx 10^7-10^{8.7} M_\odot$, in all cases, consistent with the hosts being
dwarf galaxies. We obtain high H{\sc i} 21\,cm or CO emission line widths,
$\Delta V_{20} \approx 100-290$~km~s$^{-1}$, and high gas fractions, $f_{\rm
HI} \approx 5-100$, suggesting that the absorber hosts are gas-rich galaxies
with low star formation efficiencies. However, the H{\sc i} 21\,cm velocity
spreads ($\gtrsim 100$~km~s$^{-1}$) appear systematically larger than the
velocity spreads in typical dwarf galaxies.
