The top panels show the logarithmic density of giants in Magellanic Bridge coordinates. In the region between the Clouds, there exists a population of stars whose nature we would like to probe. On selecting stars falling within the black rectangle, we show their metallicity along the bridge in the panel below. The column-normalized density shows the evolution of giant metallicity upon the passage from the SMC to the LMC. Between the Clouds, it appears as if they are joined by a constant ridge at ∼−1 dex, a value consistent with both the outer regions of the LMC and the median value of all SMC giants. On moving outwards from the SMC, there appear to be two sequences: the ridge that connects to the LMC and a metal-poorer population that extends out to X_MB ∼ −13°. The lower two panels show the proper motions of the stars through the bridge region, with a relatively smooth transition between the Clouds being apparent. The motion along ﹩{\mu }_{{X}_{\mathrm{MB}}}﹩ shows a degree of dispersion that is consistent with Figure 15.