Properties of all 1.3 × 10⁶ unresolved binary WD pairs in our simulation box (maximum magnitude G = 35), for our standard model. Contour lines mark the regions in which 33%, 67% and 95% of the binaries are located. Higher density regions are given darker colours. The 1% binaries in the tail of the distribution are indicated by the scattered points. Compared to Fig. 6, this figure hardly has statistical noise because of the large number of halo WDs we expect to find in the Milky Way halo if we would go up to magnitude G = 35.