The dearth of difference between central and satellite galaxies II.
  Comparison of observations with L-GALAXIES and EAGLE in star formation
  quenching
  As we demonstrated in Paper I, the quenched fractions of central and
satellite galaxies as function of halo mass are extremely similar, as long as
one controls for stellar mass. The same holds for the quenched fractions as a
function of central velocity dispersion, which is tightly correlated with black
hole mass, as long as one controls for both stellar and halo mass. Here we use
mock galaxy catalogs constructed from the latest semi-analytic model,
L-GALAXIES, and the state-of-the-art hydrodynamical simulation, EAGLE, to
investigate whether these models can reproduce the trends seen in the data. We
also check how the group finder used to identify centrals and satellites
impacts our results. We find that L-GALAXIES fails to reproduce the trends. The
predicted quenched fraction of central galaxies increases sharply with halo
mass around $10^{12.5}h^{-1}M_{\odot}$ and with black hole mass around
$\sim10^{6.5}M_{\odot}$, while the predicted quenched fraction of satellites
increases with both halo and black hole masses gradually. In contrast, centrals
and satellites in EAGLE follow almost the same trend as seen in the data. We
discuss the implications of our results for how feedback processes regulate
galaxy quenching.
