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Dusty debris disks around pre- and main-sequence stars are potentialsignposts for the existence of planetesimals and exoplanets. Giant planetformation is therefore expected to play a key role in the evolution of thedisk. This is indirectly confirmed by extant sub-millimeter near-infraredimages of young protoplanetary and cool dusty debris disks around main sequencestars usually showing substantial spatial structures. A majority of recentdiscoveries of imaged giant planets have been obtained around young, early-typestars hosting a circumstellar disk. In this context, we have carried out adirect imaging program designed to maximize our chances of giant planetdiscovery and targeting twenty-two young, early-type stars. About half of themshow indication of multi-belt architectures. Using the IRDIS dual-band imagerand the IFS integral field spectrograph of SPHERE to acquire high-constrastcoronagraphic differential near-infrared images, we have conducted a systematicsearch in the close environment of these young, dusty and early-type stars. Weconfirmed that companions detected around HIP 34276, HIP 101800 and HIP 117452are stationary background sources and binary companions. The companioncandidates around HIP 8832, HIP 16095 and HIP 95619 are determined asbackground contamination. For stars for which we infer the presence of debrisbelts, a theoretical minimum mass for planets required to clear the debris gapscan be calculated . The dynamical mass limit is at least $0.1 M_J$ and canexceed $1 M_J$. Direct imaging data is typically sensitive to planets down to$\sim 3.6 M_J$ at 1 $''$, and $1.7 M_J$ in the best case. These two limitstightly constrain the possible planetary systems present around each target.These systems will be probably detectable with the next generation of planetimagers.

VLT/SPHERE survey for exoplanets around young, early-type stars including systems with multi-belt architectures