  We study the morphology of the stellar periphery of the Magellanic Clouds in
search of substructure using near-infrared imaging data from the VISTA
Hemisphere Survey (VHS). Based on the selection of different stellar
populations using the ($J-K_\mathrm{s}$, $K_\mathrm{s}$) colour-magnitude
diagram, we confirm the presence of substructures related to the interaction
history of the Clouds and find new substructures on the easter side of the LMC
disc which may be owing to the influence of the Milky Way, and on the northern
side of the SMC, which is probably associated to the ellipsoidal structure of
the galaxy. We also study the luminosity function of red clump stars in the SMC
and confirm the presence of a bi-modal distance distribution, in the form of a
foreground population. We find that this bi-modality is still detectable in the
eastern regions of the galaxy out to a 10 deg distance from its centre.
Additionally, a background structure is detected in the North between 7 and 10
deg from the centre which might belong to the Counter Bridge, and a foreground
structure is detected in the South between 6 and 8 deg from the centre which
might be linked to the Old Bridge.
