Left: stellar masses of TNG subhalos by their association to their supposed host galaxy (black and blue lines) and estimates for the MATLAS dwarfs from (red line; Habas et al. 2020). The latter estimates were made by assuming that the observed dwarfs lie at the same distance as their field’s target host galaxy. Stellar masses for the subset of MATLAS dwarfs for which independent distance estimates are available are plotted as a red dotted line. TNG50’s baryonic resolution m_gas is indicated by the hatched region. 97% of MATLAS-like dwarfs in TNG50 are sufficiently resolved with at least 100 stellar particles. Right: impact of simulation resolution on dwarf populations. The lower panel is taken from Fig. 2 and shows the distribution of luminous subhalo properties in R_e − M_g space in TNG50 (m_gas = 8.5 × 10⁴ M_⊙), while the upper panel instead displays results for the lower-resolution TNG100 run (m_gas = 1.4 × 10⁶ M_⊙). MATLAS-like dwarfs satisfying the selection criteria are plotted in black. The broadening in R_e due to insufficient stellar particles occurs at around M_g > −12 in TNG100, but only affects M_g > −9 in TNG50 at a regime much fainter than the MATLAS-like dwarfs.