MG2016+112, discovered by Lawrence et al. (1984) is one of the best–studied among multiply–imaged systems, but is still only partially understood. Ostensibly a three–image system consisting of images A, B and C of a quasar at z = 3.273, the observed lensing galaxy D (a giant elliptical at z = 1.01) at the centroid of the image system seems inadequate to provide the minimum mass of ∼ 2.5 × 1012 M⊙ within 10 kpc of its center (in projection along the l.o.s.) required to produce the observed 3.″9 image–splitting. C itself appears to consist of two components, radio emission that may be associated with the faint optical image counterpart of A and B (called C2, see Garrett et al. 1994) and flat-spectrum C1, which dominates radio observations of the system and apparently consists of at least three linearly stretched subcomponents, C11 to C13 (see Garrett et al. in these proceedings).