Toy model of H I removal in the cluster. The best results to reproduce Fig. 5, showing what we would observe every 0.2 Gyr. The grey diamonds are the CVn galaxies, the dashed black line shows the linear fit used to populate infalling galaxies to the CVn galaxies and the dotted lines show the 3σ scatter. The blue filled circles are galaxies in the cluster and the red dashed lines are the observational constraints both in M_r′ and M_HI, such that we would not detect a galaxy in H I in the red shaded regions. With N_infall = 100 Gyr⁻¹ and t_1/2 = 0.03 Gyr we are able to qualitatively reproduce what we observe in Fig. 5.