EDP Sciences
Free access
Volume 425, Number 2, October II 2004
Page(s) L29 - L32
Section Letters
DOI http://dx.doi.org/10.1051/0004-6361:200400056

A&A 425, L29-L32 (2004)
DOI: 10.1051/0004-6361:200400056


A giant planet candidate near a young brown dwarf

Direct VLT/NACO observations using IR wavefront sensing
G. Chauvin1, A.-M. Lagrange2, C. Dumas1, B. Zuckerman3, D. Mouillet4, I. Song3, J.-L. Beuzit2 and P. Lowrance5

1  European Southern Observatory, Casilla 19001, Santiago 19, Chile
    e-mail: gchauvin@eso.org
2  Laboratoire d'Astrophysique, Observatoire de Grenoble, 414 rue de la piscine, Saint-Martin d'Hères, France
3  Department of Physics & Astronomy and Center for Astrobiology, University of California, Los Angeles, 8371 Math Science Building, Box 951562, CA 90095-1562, USA
4  Laboratoire d'Astrophysique, Observatoire Midi-Pyrénées, Tarbes, France
5  Spitzer Science Center, Infrared Processing and Analysis Center, MS 220-6, Pasadena, CA 91125, USA

(Received 22 July 2004 / Accepted 12 August 2004)

We present deep VLT/NACO infrared imaging and spectroscopic observations of the brown dwarf 2MASSWJ 1207334-393254, obtained during our on-going adaptive optics survey of southern young, nearby associations. This ~25  $M_{\rm {Jup}}$ brown dwarf, located ~70 pc from Earth, has been recently identified as a member of the TW Hydrae Association (age ~ 8 Myr). Using adaptive optics infrared wavefront sensing to acquire sharp images of its circumstellar environment, we discovered a very faint and very red object at a close separation of ~780 mas (~55 AU). Photometry in the H, ${K}_{\rm s}$ and L' bands and upper limit in J-band are compatible with a spectral type L5-L9.5. Near-infrared spectroscopy is consistent with this spectral type estimate. Different evolutionary models predict an object within the planetary regime with a mass of ${M}=5\pm2~M_{\rm {Jup}}$ and an effective temperature of ${T}_{\rm {eff}}=1250\pm200$ K.

Key words: 2MASSWJ 1207334-393254 -- brown dwarf -- giant planet -- adaptive optics imaging and spectroscopy

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© ESO 2004

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