Stellar mass versus quiescent fraction in our simulations of LMC-mass hosts versus observed (points) LG galaxies and simulated (shaded regions) LG- or MW-like haloes. MC12 (McConnachie 2012) and W15 (Weisz et al. 2015) report data for the LG itself, while M21 (Mao et al. 2021) report data for observed MW analogues. We define the quiescent fraction as the number of galaxies in each mass bin that have t_quench < 13.2 Gyr (i.e. selecting all galaxies that have not formed a star particle within the last 500 Myr) to allow for variations that may arise from finite time-steps and star particle mass limits. We find that LMC-mass hosts are able to quench their satellite population to nearly the same degree as MW- or LG-like hosts, perhaps a surprising result given their significantly smaller halo masses and baryonic content. References: FIRE MW + LG – Samuel et al. (2022); CHANGA – Akins et al. (2021); MC12 – McConnachie (2012) (as compiled by Wetzel et al. 2015b); W15 – Weisz et al. (2015); M21 – Mao et al. (2021).