  Dusty debris disks around pre- and main-sequence stars are potential
signposts for the existence of planetesimals and exoplanets. Giant planet
formation is therefore expected to play a key role in the evolution of the
disk. This is indirectly confirmed by extant sub-millimeter near-infrared
images of young protoplanetary and cool dusty debris disks around main sequence
stars usually showing substantial spatial structures. A majority of recent
discoveries of imaged giant planets have been obtained around young, early-type
stars hosting a circumstellar disk. In this context, we have carried out a
direct imaging program designed to maximize our chances of giant planet
discovery and targeting twenty-two young, early-type stars. About half of them
show indication of multi-belt architectures. Using the IRDIS dual-band imager
and the IFS integral field spectrograph of SPHERE to acquire high-constrast
coronagraphic differential near-infrared images, we have conducted a systematic
search in the close environment of these young, dusty and early-type stars. We
confirmed that companions detected around HIP 34276, HIP 101800 and HIP 117452
are stationary background sources and binary companions. The companion
candidates around HIP 8832, HIP 16095 and HIP 95619 are determined as
background contamination. For stars for which we infer the presence of debris
belts, a theoretical minimum mass for planets required to clear the debris gaps
can be calculated . The dynamical mass limit is at least $0.1 M_J$ and can
exceed $1 M_J$. 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 limits
tightly constrain the possible planetary systems present around each target.
These systems will be probably detectable with the next generation of planet
imagers.
