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We investigate the flare-frequency distributions of 5 M-dwarfs thatexperienced superflares with energies in excess of $10^{33}$ erg detected byASAS-SN. We use K2 and TESS short-cadence observations along with archivalASAS-SN data to categorise the flaring behaviour of these stars across a rangeof flare energies. We were able to extract a rotation period for 4 of thestars. They were all fast rotators ($P_{\mathrm{rot}} \leq 6 \textrm{d}$),implying relative youth. We find that the flare-frequency distributions foreach 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 offast-rotating M-dwarfs not selected for their superflaring activity,corresponding to an increased number of high energy flares. Despite ourspecific selection of superflaring stars with shallow flare-rate distributionsand more power in higher-energy flares, we find that the implied UV flux isinsufficient to deplete the ozone of earth-sized planets in the habitable zonearound these stars. Furthermore, we find that the flares detected on the starsin our sample are insufficient to produce the UV flux needed to fuelabiogenetic processes. These results imply that given available models, evenM-dwarfs selected for extreme flaring properties may have insufficient UVemission from flares to impact exolife on earth-sized planets in the habitablezones around M-dwarfs.

Flares Big and Small: a K2 and TESS View of ASAS-SN Superflares