Volume 460, Number 2, December III 2006
|Page(s)||635 - 640|
|Section||Planets and planetary systems|
|Published online||12 September 2006|
Are isolated planetary-mass objects really isolated?
A brown dwarf-exoplanet system candidate in the σ Orionis cluster
Instituto de Astrofísica de Canarias, 38205 La Laguna, Tenerife, Spain e-mail: email@example.com
2 Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
3 University of Central Florida, Department of Physics, PO Box 162385, Orlando, FL 32816-2385, USA
4 Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH, UK
5 LAEFF-INTA, PO Box 50727, 28080, Madrid, Spain
Accepted: 30 August 2006
Context.Free-floating planetary-mass objects have masses below the deuterium burning mass limit at about 13 Jupiter masses, and have mostly been found in very young open clusters. Their origin and relationship to stars and brown dwarfs are still a mystery.
Aims.The recent detection by direct imaging of three giant planets at wide separation (50–250 AU) from their primaries has raised the question about the true “isolation” of planetary-mass objects in clusters. Our goal was to test the possibility that some free-floating planetary-mass objects could in fact be part of wide planetary systems.
Methods.We searched in the literature for stellar and brown-dwarf candidates members of the σ Orionis cluster (~3 Ma, ~360 pc) at small angular separations from published candidate planetary-mass objects. We found one candidate planetary system composed of an X-ray source, SE 70, and a planetary-mass object, S Ori 68, separated by only 4.6 arcsec. In order to assess the cluster membership of the X-ray source, we obtained mid-resolution optical spectroscopy using ISIS on the William Herschel Telescope. We also compiled additional data on the target from available astronomical catalogues.
Results.We have found that SE 70 follows the spectrophotometric sequence of the cluster and displays spectroscopic features of youth, such as lithium in absorption and chromospheric Hα emission. The radial velocity is consistent with cluster membership. Hence, SE 70 is very probably a member of the σ Orionis cluster. The projected physical separation between SE 70 and S Ori 68 is AU at the distance of the cluster. If a common proper motion is confirmed in the near future, the system would be composed of an M5–6 brown dwarf with an estimated mass of ~45 MJup and an L5 ± 2 giant planet with an estimated mass of ~5 MJup. It would be the widest and one of the lowest-mass planetary systems known so far.
Key words: stars: low-mass, brown dwarfs / planetary systems / open clusters and associations: individual: σ Orionis
© ESO, 2006
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