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The discovery of potentially habitable planets around the ultracool dwarfstar Trappist-1 naturally poses the question: could Trappist-1 planets be hometo life? These planets orbit very close to the host star and are mostsusceptible to the UV radiation emitted by the intense and frequent flares ofTrappist-1. Here we calculate the UV spectra (100 - 450 nm) of a superflareobserved on Trappist-1 with the K2 mission. We couple radiative transfer modelsto this spectra to estimate the UV surface flux on planets in the habitablezone of Trappist-1 (planets $e$, $f$, and $g$), assuming atmospheric scenariosbased on a pre-biotic and an oxygenic atmosphere. We quantify the impact of theUV radiation on living organisms on the surface and on a hypothetical planetocean. Finally, we find that for non-oxygenic planets, UV resistant lifeformswould survive on the surface of planets f and g. Nevertheless, more fragileorganisms (i.e. \textit{E. coli}) could be protected from the hazardous UVeffects at ocean depths greater than 8m. If the planets have an ozone layer,any lifeforms studied here would survive in the HZ planets.

Surface and oceanic habitability of Trappist-1 planets under the impact of flares