Nominal X-ray fluxes from eRASSl vs. optical brightness for stars in our sample. For stars with an apparent Gaia magnitude brighter than 4mag, there is a clear trend towards high apparent eRASS fluxes, which can be attributed to optical loading. Some individual bright stars named in the plot can be expected to be only weak X-ray emitters because they are either lacking an outer convective envelope (ß Pic) or are coronal graveyard-type giants (Ayres et al. 2003). Furthermore, these specific stars are known to be X-ray dim from previous observations by other X-ray telescopes.