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Context. The formation of planetary systems is a common, yet complexmechanism. Numerous stars have been identified to possess a debris disk, aproto-planetary disk or a planetary system. The understanding of such formationprocess requires the study of debris disks. These targets are substantial andparticularly suitable for optical and infrared observations. Sparse Aperturemasking (SAM) is a high angular resolution technique strongly contributing toprobe the region from 30 to 200 mas around the stars. This area is usuallyunreachable with classical imaging, and the technique also remains highlycompetitive compared to vortex coronagraphy. Aims. We aim to study debris diskswith aperture masking to probe the close environment of the stars. Our goal iseither to find low mass companions, or to set detection limits. Methods. Weobserved eight stars presenting debris disks ( $\beta$ Pictoris, AUMicroscopii, 49 Ceti, $\eta$ Telescopii, Fomalhaut, g Lupi, HD181327 andHR8799) with SAM technique on the NaCo instrument at the VLT. Results. No closecompanions were detected using closure phase information under 0.5 ofseparation from the parent stars. We obtained magnitude detection limits thatwe converted to Jupiter masses detection limits using theoretical isochronesfrom evolutionary models. Conclusions. We derived upper mass limits on thepresence of companions in the area of few times the diffraction limit of thetelescope around each target star.

astronomy and astrophysics

Sparse aperture masking at the VLT II. Detection limits for the eight  debris disks stars $\beta$ Pic, AU Mic, 49 Cet, $\eta$ Tel, Fomalhaut, g Lup,  HD181327 and HR8799