the Galactic tide would not have yet had time to disrupt the pair nor to disperse fully the common (sub)halo they inhabit. As a result, most other dwarf companions of the Clouds should still lie in their close vicinity. Such “Magellanic satellites” have long been speculated [see, e.g., @Lynden-Bell1995], and their existence would be consistent with the relatively common occurrence of dwarf galaxy associations in the nearby Universe [@Tully2006]. The immediate surroundings of the Clouds should thus be a fertile ground to search for new dwarfs, as proposed by @Sales2011 [S11 hereafter].

A full search for satellites around the Clouds would be extremely valuable. One reason is that, in $\Lambda$CDM, the satellite luminosity function is expected to be a nearly scale-free function when expressed in units of the luminosity of the primary [@Sales2013]. In other words, to first order, the Galactic satellite abundance should be simply a scaled-up version of that of the Clouds. A complete catalogue of Magellanic faint and ultra-faint satellites would be easier to compile (the relevant survey volume is much smaller than the full Galactic halo) and could therefore help to constrain the incompleteness of all-sky surveys of Galactic satellites. In general, the surrounding of dwarf 