Millilens model with mass 10⁷ M_⊙ near the critical curve and magnifying LS1. The millilens is farther from the critical curve than in Fig. 14 but still forms critical curves at the position of LS1. This simulation includes both LS1 and i LS1′ as well as the knot image pair b and b′. The geometry of the simulation mimics the observations, with a separation between b and b′ of 045 and a tangential separation (i.e., in the vertical direction) between LS1 and knot b′ of 30 mas. The numbers in yellow indicate the approximate magnification at the position of the corresponding counterimage. In this configuration, LS1′ is ≈2.5 mag fainter than LS1 and therefore unobserved. For this mass, the effect on knots b and b′ is noticeable with the magnification of b′ affected by the millilens. Stars in the intracluster medium with a surface mass density of 5 M_⊙ pc⁻² blur the critical curves and reshuffle large magnifications away from the critical curve. The red double-arrow segment shows the width of the saturation region as predicted by Diego et al. (2018, their Eq. (15)).