Volume 546, October 2012
|Number of page(s)||8|
|Section||Planets and planetary systems|
|Published online||16 October 2012|
INAF – Osservatorio Astronomico di Padova, Vicolo dell’ Osservatorio
2 Dipartimento di Astronomia – Universitá di Padova, Vicolo dell’Osservatorio 2, Padova, Italy
3 INAF – Centro Galileo Galilei, Calle Alvarez de Abreu 70, 38700 Santa Cruz de La Palma ( TF), Spain
4 McDonald Observatory, The University of Texas at Austin, Austin, TX 78712, USA
5 INAF – Osservatorio Astrofisico di Catania, via S. Sofia 78, Catania, Italy
6 INAF – Osservatorio Astrofisico di Torino, via Osservatorio 20, 10025 Pino Torinese, Italy
7 Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388 Marseille, France
Received: 17 July 2012
Accepted: 13 August 2012
We have performed radial velocity (RV) monitoring of the components of the binary system HD 106515 over almost 11 years using the high-resolution spectrograph SARG at Telescopio Nazionale Galileo (TNG). The primary shows long-period radial velocity variations that indicate the presence of a low-mass companion whose projected mass is in the planetary regime (msini = 9.33 MJ). The 9.8 year orbit is quite eccentric (e = 0.57), as is typical for massive giant planets. Our results confirm the previously made preliminary announcement of the planet by Mayor et al. (2011, A&A, submitted [arXiv:1109.2497]). The secondary instead does not show significant RV variations. The two components do not differ significantly in chemical composition, as was also found for other pairs of which one component hosts giant planets. Adaptive optics images obtained with TNG/AdOpt do not reveal additional stellar companions. From the analysis of the relative astrometry of the components of the wide pair we compute an upper limit on the mass of the newly detected companion of about 0.25 M⊙. State-of-the-art or near-future instrumentation can provide true mass determination, thanks to the availability of the wide companion HD106515B as reference. Therefore, HD 106515Ab will allow a deeper insight into the transition region between planets and brown dwarfs.
Key words: stars: individual: HD 106515A / planetary systems / binaries: visual / techniques: radial velocities / brown dwarfs / techniques: high angular resolution
Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundacion Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias.
Tables 3 and 4 are available in electronic form at http://www.aanda.org
© ESO, 2012
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