  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 $\alpha_{88}^{1110} = -1.80 \pm 0.09$ and $\alpha_{88}^{944} =
-1.13 \pm 0.09$ for the radio halos in Abell 3404 and Abell 141, respectively.
Each cluster is noted to have 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.
