How ram pressure and SMBHs affect the gas contents of TNG-Cluster satellite galaxies. For the gas-rich $M_{\mathrm{gas}}^{\mathrm{sat}}>{10}^9{M}_{\odot }$ satellites at a fixed cluster $M_{200\mathrm{c}}^{\mathrm{host}}\sim {10}^{15}{M}_{\odot }$ and satellite $M_{\star }^{\mathrm{sat}}\sim {10}^{10},{10}^{10.75}{M}_{\odot }$ (top versus bottom panels) mass, we show total gas density radial profiles colored by current ram pressure (left column) and SMBH mass (right column). The thick curves show the medians of the top and bottom quartiles of ram pressure and SMBH mass, and the thin curves are the profiles of the individual satellites. Ram pressure tends to truncate the gas profiles at large distances and slightly compress the ISM gas, while SMBH feedback tends to eject and decrease the density of the ISM gas for more massive satellites.