of the spider (see §3.3), and telescope arrays can be simulated by placing a mask with appropriately located small holes.

Pupil masks allow to select a sub-sample of spatial frequencies and more accurately measure the corresponding complex visibilities since they will be less attenuated (as the overlap of the fringes is lower); hence, a better use of the maximum number of photons allowed by the detector. The price to pay is to perform an interpolation in the Fourier space (aperture synthesis, see methods in §5.1) and complementary observations to make the process more robust in the case of complex objects.

We made 3 pupil masks by drilling 0.7 mm holes into a 5-cm metallic disk, according to some of the complementary non-redundant networks from Golay (1971). They are displayed in Fig.   with the corresponding $(u,v)$ coverage. A successful image of HR 8652 was restored using these masks and the aperture synthesis method from Lannes (1989, 1991) and Anterrieu (1992). These method would work with any other configuration – there is no need for complementary networks –. We chose these masks because the corresponding $(u,v)$ coverage (Fig. ) was rather compact with only small gaps, which makes image restoration more robust.

