Relationships between ICL amount as a function of M_vir. Top panel: luminosity of the ICL component as a function of the M_vir. The best fit for the linear correlation is shown by the dark-red solid line. The best fit equation is log(L_ICL) = (0.41 ± 0.11)*log(M_vir)−(5 ± 1.5), with R² = 28% and p-value = 0. Lower panel: ICL fraction (f_ICL) vs. M_vir obtained for the VEGAS targets (magenta symbols), compared with the values of f_ICL available in the literature, for targets at z ≤ 0.05 (black points). These are the compact groups from Da Rocha & Mendes de Oliveira (2005), Da Rocha et al. (2008), Pildis et al. (1995), Poliakov et al. (2021) Ragusa et al. (2021, stars), the Coma cluster (Jiménez-Teja et al. 2019, octagon), the Virgo cluster (Mihos et al. 2017, cross) and the Abell 85 cluster (Montes et al. 2021, square). The clusters of galaxies from Kluge et al. (2021) are also included in this plot (diamonds). The virial masses for the cluster in the latter sample are from Kluge (2020), when available. For systems with no estimation of the viral mass, we used the velocity dispersion of the member galaxies reported in Kluge (2020) to estimate it following Munari et al. (2013). The solid line indicates the best fit for the linear correlation. The best fit equation is f_ICL = (0.02 ± 0.02)*log(M_vir)−(0.07 ± 0.34), with R² = 1.6 % and p-value = 0.47. The theoretical prediction obtained by Contini et al. (2014; blue contours) and Rudick et al. (2011; light blue area) are included for comparison.