Average TESS FFDs for stars with reliable P_rot in the early (M2.5–M3.5) and late (M4.5–M5) SpT range derived in Sect. 4.6 (black) and constructed X-ray FFDs based on the energy conversion derived in Sect. 5.1.3 (red). Error bars on E_X represent the uncertainty caused by this conversion. Error bars on the flare rate are the same for the observed TESS (black) and constructed XMM-Newton (red) FFDs and result from Eq. (4). The green line represents the extrapolation to small flare energies for the observed X-ray FFD that Getman & Feigelson (2021) found for PMS stars with masses ≤1 M_⊙. The slopes of our power law fits are given in Table 4.