  We present the serendipitous discovery of 8 distant ($>$ 50 pc) late M dwarfs
with plausible associated radio emission at 144 MHz. The M dwarf nature of our
sources has been confirmed with optical spectroscopy performed using HET/LRS2
and Subaru/FOCAS, and their radio flux densities are within the range of
0.5-1.0 mJy at 144 MHz. Considering the radio-optical source separation and
source densities of the parent catalogues, we suggest that it is statistically
probable the M dwarfs are associated with the radio emission. However, it
remains plausible that for some of the sources the radio emission originates
from an optically faint and red galaxy hiding behind the M dwarf. The isotropic
radio luminosities ($\sim10^{17-18}$ erg s$^{-1}$ Hz$^{-1}$) of the M dwarfs
suggest that if the association is real, the radio emission is likely driven by
a coherent emission process produced via plasma or electron-cyclotron maser
instability processes, which is potentially caused by binary interaction. Long
term monitoring in the radio and high-resolution radio follow-up observations
are necessary to search for any variability and pinpoint the radio emission to
determine whether our tentative conclusion that these ultracool dwarfs are
radio emitting is correct. If the low-frequency radio emission is conclusively
associated with the M dwarfs, this would reveal a new population of optically
faint and distant ($>$ 50 pc) radio emitting M dwarfs.
