  We investigate the flare-frequency distributions of 5 M-dwarfs that
experienced superflares with energies in excess of $10^{33}$ erg detected by
ASAS-SN. We use K2 and TESS short-cadence observations along with archival
ASAS-SN data to categorise the flaring behaviour of these stars across a range
of flare energies. We were able to extract a rotation period for 4 of the
stars. They were all fast rotators ($P_{\mathrm{rot}} \leq 6 \textrm{d}$),
implying relative youth. We find that the flare-frequency distributions for
each of the stars are well fit by a power-law, with slopes between $\alpha =
1.22$ and $\alpha= 1.82$. These slopes are significantly flatter than those of
fast-rotating M-dwarfs not selected for their superflaring activity,
corresponding to an increased number of high energy flares. Despite our
specific selection of superflaring stars with shallow flare-rate distributions
and more power in higher-energy flares, we find that the implied UV flux is
insufficient to deplete the ozone of earth-sized planets in the habitable zone
around these stars. Furthermore, we find that the flares detected on the stars
in our sample are insufficient to produce the UV flux needed to fuel
abiogenetic processes. These results imply that given available models, even
M-dwarfs selected for extreme flaring properties may have insufficient UV
emission from flares to impact exolife on earth-sized planets in the habitable
zones around M-dwarfs.
