EDP Sciences
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Volume 422, Number 2, August I 2004
Page(s) 631 - 636
Section Stellar structure and evolution
DOI http://dx.doi.org/10.1051/0004-6361:20047122

A&A 422, 631-636 (2004)
DOI: 10.1051/0004-6361:20047122

High resolution spectroscopy of brown dwarfs in Taurus

Detection of accretion in KPNO-Tau-3
D. Barrado y Navascués

Laboratorio de Astrofísica Espacial y Física Fundamental, INTA, PO Box 50727, 2808 Madrid, Spain
    e-mail: barrado@laeff.esa.es

(Received 3 February 2004 / Accepted 11 March 2004)

We present high resolution optical spectroscopy of three candidate members of the Taurus-Auriga star forming region. Based on the spectral type, the strength, profile and width of the H $\alpha$ line, the detected lithium at 6708 Å, the location of these objects in the H-R diagram and the comparison with similar objects belonging to young stellar associations, we determine that they are bona fide members of the SFR with ages of ~3 Myr, and have masses at or below the substellar limit. At least in one case, there is active accretion from a circum(sub)stellar disk. This result suggests that high mass brown dwarfs go through a classical T Tauri phase and form, as stars do, from the collapse and fragmentation of a molecular cloud.

Key words: open clusters and associations: individual: Taurus -- stars: brown dwarfs

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© ESO 2004