Bolometric flare frequency distribution of LP 89-187 as derived from three sectors of TESS data shown in blue. The blue arrow indicates the upper limit derived from the HiPERCAM observations. We show the bolometric flare frequency distribution of stars in the β Pic moving group in orange (spectral type ≲ M2) and in red (spectral type ≳ M3). We also show the flare frequency distribution of TRAPPIST-1 analogue stars (dashed black line) and TRAPPIST-1 using K2 data (dashed brown line) taken from Fig. 21 of Seli et al. (2021).