The impact of ram pressure on cluster galaxies, insights from GAEA and TNG

Ram pressure stripping (RPS) has a non-negligible impact on the gas content of cluster galaxies. We used the semi-analytic model and the hydro-simulation to investigate whether cluster galaxies suffer from strong RPS that is sufficient to remove a significant fraction of their gas during the first pericentric passage. We estimated that a ram pressure of 10^-10.5 can remove $90%$, $50%$, and $20%$ of the cold gas reservoir from low-mass galaxies with $9< ⋆ M ⊙ <9.5$, assuming the gas can be stripped instantaneously. We then used this information to divide the phase space diagram into ``strong'', ``moderate'', ``weak'', and ``no'' RPS zones. By tracing the orbit of galaxies since 2.5R_vir, we find in both and that about half of the galaxies in Virgo-like halos (log M_h / ⊙ ∼ 14 ) did not suffer strong RPS during the first pericentric passage. In Coma-like halos (log M_h / M_ ⊙ ∼ 15), almost all galaxies have suffered strong RPS during the first pericentric passage, which can remove all gas from low-mass galaxies but is insufficient to significantly reduce the gas content of more massive galaxies. In general, results from and are consistent, with the RPS being only slightly stronger in than in GAEA. Our findings suggest that most cluster galaxies maintain a notable fraction of their gas and continue forming stars after the first pericentric passage, except for those with a low stellar mass (log ⋆ M ⊙ <9.5) in very massive halos (log M_ h M ⊙