  We probe the HI properties and the gas environments of three early-type
barred galaxies harbouring counter-rotating ionized gas, NGC 128, NGC 3203 and
NGC 7332. Each system has one or more optically-identified galaxy, at a similar
or as yet unknown redshift within a 50 kpc projected radius. Using HI synthesis
imaging data, we investigate the hypothesis that the counter-rotating gas in
these galaxies has been accreted from their neighbours. In NGC 128 and NGC
3203, we find 9.6e7 and 2.3e8 Msun of HI, respectively, covering almost the
entire stellar bodies of dwarf companions that appear physically connected.
Both the HI morphology and kinematics are suggestive of tidal interactions. In
NGC 7332, we do not find any directly-associated HI. Instead, NGC 7339, a
neighbour of a comparable size at about 10 kpc, is found with 8.9e8 Msun of HI
gas. More recently in a single dish observation, however, another group
discovered a large HI structure which seems to be an extension of NGC 7339's HI
disc and also covers NGC 7332. All these observations thus suggest that HI gas
is being accreted in these three galaxies from their companions, which is
likely responsible for the kinematically-decoupled gas component present in
their central region. Considering the incompleteness of existing studies of the
faint dwarf galaxy population both in the optical and in HI, accretion from
cold gas blobs, presumably gas-rich dwarfs, is expected to occur even more
frequently than what is inferred from such cases that have been observed to
date.
