Volume 612, April 2018
|Number of page(s)||5|
|Section||Planets and planetary systems|
|Published online||08 May 2018|
Institut de Planétologie et d’Astrophysique de Grenoble,
38041 Grenoble Cedex 9, France
2 Max-Planck-Institut fuer Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
3 European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile
4 INAF – Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy
5 Institute for Astronomy, The University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK
6 Instituto de Fisica y Astronomía, Facultad de Ciencias, Universidad de Valparaiso, Av. Gran Bretana 1111, 5030 Casilla, Valparaiso, Chile
7 CNRS, UMR 7095, Institut d’Astrophysique de Paris, 98bis boulevard Arago, 75014 Paris, France
8 Istituto Nazionale di AstroFisica, Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, Italy
Accepted: 12 April 2017
Context. The search for extrasolar planets has been limited so far to close orbit (typ. ≤5 au) planets around mature solar-type stars on the one hand, and to planets on wide orbits (≥10 au) around young stars on the other hand. To get a better view of the full giant planet population, we have started a survey to search for giant planets around a sample of carefully selected young stars.
Aims. This paper aims at exploring the giant planet population around one of our targets, β Pictoris, over a wide range of separations. With a disk and a planet already known, the β Pictoris system is indeed a very precious system for studies of planetary formation and evolution, as well as of planet–disk interactions.
Methods. We analyse more than 2000 HARPS high-resolution spectra taken over 13 years as well as NaCo images recorded between 2003 and 2016. We combine these data to compute the detection probabilities of planets throughout the disk, from a fraction of au to a few dozen au.
Results. We exclude the presence of planets more massive than 3 MJup closer than 1 au and further than 10 au, with a 90% probability. 15+ MJup companions are excluded throughout the disk except between 3 and 5 au with a 90% probability. In this region, we exclude companions with masses larger than 18 (resp. 30) MJup with probabilities of 60 (resp. 90) %.
Key words: techniques: radial velocities / stars: individual: β Pictoris / techniques: high angular resolution / planets and satellites: detection
Based on data obtained with the ESO3.6 m/HARPS spectrograph at La Silla, and with NaCO on the VLT.
The RV data are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (220.127.116.11) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/612/A108
© ESO 2018
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