  Environment plays a pivotal role in shaping the evolution of satellite
galaxies. Analyzing the properties related to the cold gas phase of satellites
provides insights into unravelling the complexity of environmental effects. We
use the hydro-dynamical simulations Illustris TNG and Eagle, and the
semi-analytic models (SAMs) GAEA and L-Galaxies, in comparison with recent
observations from the Westerbork Synthesis Radio Telescope (WSRT), to
investigate the properties of satellite galaxies hosted by halos with mass
$M_{200}>10^{12.8}M_\odot$, and within projected regions $\le 1.1$ virial
radius $R_{200}$. Generally, satellite galaxies selected from semi-analytic
models have more HI than those selected from hydro-dynamical simulations across
all projected radii, e.g. more than 30% of satellites in the two
hydro-simulations are HI depleted, while this fraction is almost zero in SAMs.
Furthermore, both hydro-dynamical simulations and SAMs reproduce the observed
decrease of HI content and specific star-formation rate (sSFR) towards the halo
centre. However, the trend is steeper in two hydro-dynamical simulations TNG
and EAGLE, resulting in a better agreement with the observational data,
especially in more massive halos. By comparing the two version of GAEA, we find
that the inclusion of ram-pressure stripping of cold gas significantly improves
the predictions on HI fractions. The refined hot gas stripping method employed
in one of the two L-Galaxies models also yields improved results.
