A flexible subhalo abundance matching model for galaxy clustering in
  redshift space
  We develop an extension of subhalo abundance matching (SHAM) capable of
accurately reproducing the real and redshift-space clustering of galaxies in a
state-of-the-art hydrodynamical simulation. Our method uses a low-resolution
gravity-only simulation and it includes orphan and tidal disruption
prescriptions for satellite galaxies, and a flexible amount of galaxy assembly
bias. Furthermore, it includes recipes for star formation rate (SFR) based on
the dark matter accretion rate. We test the accuracy of our model against
catalogues of stellar-mass- and SFR-selected galaxies in the TNG300
hydrodynamic simulation. By fitting a small number of free parameters, our
extended SHAM reproduces the projected correlation function and redshift-space
multipoles for number densities $10^{-3} - 10^{-2}\, h^{3}{\rm Mpc}^{-3}$, at
$z=1$ and $z=0$, and for scales $r \in [0.3 - 20] h^{-1}{\rm Mpc}$.
Simultaneously, the SHAM results also retrieve the correct halo occupation
distribution, the level of galaxy assembly bias, and higher-order statistics
present in the TNG300 galaxy catalogues. As an application, we show that our
model simultaneously fits the projected correlation function of the SDSS in 3
disjoint stellar mass bins, with an accuracy similar to that of TNG300
galaxies. This SHAM extension can be used to get accurate clustering prediction
even when using low and moderate-resolution simulations.
