|Reference : Deep near-infrared interferometric search for low-mass companions around β Pictoris|
|Scientific journals : Article|
|Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics|
|Deep near-infrared interferometric search for low-mass companions around β Pictoris|
|Absil, Olivier [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Astroph. extragalactique et observations spatiales (AEOS) >]|
|Le Bouquin, Jean-Baptiste [ > > ]|
|Lebreton, Jérémy [ > > ]|
|Augereau, Jean-Charles [ > > ]|
|Benisty, Myriam [ > > ]|
|Chauvin, Gaël [ > > ]|
|Hanot, Charles [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Astroph. extragalactique et observations spatiales (AEOS) >]|
|Mérand, Antoine [ > > ]|
|Montagnier, Guillaume [ > > ]|
|Astronomy and Astrophysics|
|[en] stars: individual: β Pic ; planets and satellites: detection ; techniques: interferometric ; planetary systems|
|[en] Aims. We search for low-mass companions in the innermost region (<300 mas, i.e., 6 AU) of the β Pic planetary system.
Methods. We obtained interferometric closure phase measurements in the K-band with the VLTI/AMBER instrument used in its medium spectral resolution mode. Fringe stabilization was provided by the FINITO fringe tracker.
Results. In a search region of between 2 and 60 mas in radius, our observations exclude at 3σ significance the presence of companions with K-band contrasts greater than 5×10^-3 for 90% of the possible positions in the search zone (i.e., 90% completeness). The median 1σ error bar in the contrast of potential companions within our search region is 1.2×10^-3. The best fit to our data set using a binary model is found for a faint companion located at about 14.4 mas from β Pic, which has a contrast of 1.8×10^-3 ± 1.1×10^-3 (a result consistent with the absence of companions). For angular separations larger than 60 mas, both time smearing and field-of-view limitations reduce the sensitivity.
Conclusions. We can exclude the presence of brown dwarfs with masses higher than 29 MJup (resp. 47 MJup) at a 50% (resp. 90%) completeness level within the first few AUs around β Pic. Interferometric closure phases offer a promising way to directly image low-mass companions in the close environment of nearby young stars.
|http://www.aanda.org/index.php?option=com_article&access=doi&doi=10.1051/0004-6361/201015156&Itemid=129 - Copyright ESO 2010, published by EDP Sciences|
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