Simulating galaxy formation in f(R) modified gravity: Matter, halo, and
  galaxy-statistics
  We present an analysis of the matter, halo and galaxy clustering in
$f(R)$-gravity employing the SHYBONE full-physics hydrodynamical simulation
suite. Our analysis focuses on the interplay between baryonic feedback and
$f(R)$-gravity in the matter power spectrum, the matter and halo correlation
functions, the halo and galaxy-host-halo mass function, the subhalo and
satellite-galaxy count and the correlation function of the stars in our
simulations. Our studies of the matter power spectrum in full physics
simulations in $f(R)$-gravity show, that it will be very difficult to derive
accurate fitting formulae for the power spectrum enhancement in $f(R)$-gravity
which include baryonic effects. We find that the enhancement of the halo mass
function due to $f(R)$-gravity and its suppression due to feedback effects do
not show significant back-reaction effects and can thus be estimated from
independent GR-hydro and $f(R)$ dark matter only simulations. Our simulations
furthermore show, that the number of subhalos and satellite-galaxies per halo
is not significantly affected by $f(R)$-gravity. Low mass halos are
nevertheless more likely to be populated by galaxies in $f(R)$-gravity. This
suppresses the clustering of stars and the galaxy correlation function in the
theory compared to standard cosmology.
