Astronomy and Astrophysics, volume 595A, 31-31 (2016/11-1)
Sparse aperture masking at the VLT. II. Detection limits for the eight debris disks stars β Pic, AU Mic, 49 Cet, η Tel, Fomalhaut, g Lup, HD 181327 and HR 8799.
GAUCHET L., LACOUR S., LAGRANGE A.-M., EHRENREICH D., BONNEFOY M., GIRARD J.H. and BOCCALETTI A.
Abstract (from CDS):
Context. The formation of planetary systems is a common, yet complex mechanism. Numerous stars have been identified to possess a debris disk, a proto-planetary disk or a planetary system. The understanding of such formation process requires the study of debris disks. These targets are substantial and particularly suitable for optical and infrared observations. Sparse aperture masking (SAM) is a high angular resolution technique strongly contributing to probing the region from 30 to 200mas around the stars. This area is usually unreachable with classical imaging, and the technique also remains highly competitive compared to vortex coronagraphy.
Aims. We aim to study debris disks with aperture masking to probe the close environment of the stars. Our goal is either to find low-mass companions, or to set detection limits.
Methods. We observed eight stars presenting debris disks (β Pictoris, AU Microscopii, 49 Ceti, η Telescopii, Fomalhaut, g Lupi, HD 181327, and HR 8799) with SAM technique on the NaCo instrument at the Very Large Telescope (VLT).
Results. No close companions were detected using closure phase information under 0.5'' of separation from the parent stars. We obtained magnitude detection limits that we converted to Jupiter masses detection limits using theoretical isochrones from evolutionary models.
Conclusions. We derived upper mass limits on the presence of companions in the area of a few times the telescope's diffraction limits around each target star.
© ESO, 2016
instrumentation: high angular resolution - planetary systems - planets and satellites: formation
VizieR on-line data:
<Available at CDS (J/A+A/595/A31): list.dat fits/*>
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