  We report on the detection of a giant radio halo in the cluster Abell 3404 as
well as confirmation of the radio halo observed in Abell 141 (with linear
extents $\sim 770$ kpc and $\sim 850$ kpc, respectively). We use the Murchison
Widefield Array (MWA) in conjunction with the Australian Square Kilometre Array
Pathfinder (ASKAP) and the Australia Telescope Compact Array (ATCA) to
characterise the emission and intervening radio sources from $\sim100$-$1000$
MHz; power law models are fit to the spectral energy distributions with
spectral indices $\alpha_{88}^{1110} = -1.66 \pm 0.07$ and $\alpha_{88}^{944} =
-1.06 \pm 0.09$ for the radio halos in Abell 3404 and Abell 141, respectively.
We find strong correlation between radio and X-ray surface brightness for
Abell~3404 but little correlation for Abell~141. We note each cluster has an
atypical morphology for a radio-halo--hosting cluster, with Abell 141 having
been previously reported to be in a pre-merging state, and Abell 3404 is
largely relaxed with only minor evidence for a disturbed morphology. We find
that the radio halo power is consistent with the current radio halo sample and
$P_\nu$-$M$ scaling relations, but note that the radio halo in Abell 3404 is an
ultra-steep-spectrum radio halo (USSRH) and, as with other USSRHs lies slightly
below the best-fit $P_{1.4}$-$M$ relation. We find that an updated scaling
relation is consistent with previous results and shifting the frequency to 150
MHz does not significantly alter the best-fit relations with a sample of 86
radio halos. We suggest that the USSRH halo in Abell 3404 represents the faint
class of radio halos that will be found in clusters undergoing weak mergers.
