...1,2,

Alexander von Humboldt Fellow at the Max-Planck-Institut für Astronomie.

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...2006)

The mass is derived from the comparison between theoretical luminosities of Chabrier et al. (2000) and the luminosities of the objects. The latter are computed from the J-band absolute magnitude and an I-J colour-dependent bolometric correction.

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...2005)

The tight pair [W96] 4771-899 AB and [W96] 4771-899 C (aka S Ori J053847.7-022711, at $\rho = 7.63 \pm 0.10$ arcsec) is in fact a triple stellar system. There is an additional binary system candidate formed by a very low-mass star, S Ori J0539268-026614, and a faint brown dwarf at 4.4 arcsec ( $J = 16.21\pm0.09$ mag, not found in 2MASS or DENIS catalogues). Both of them show Li I in absorption (Zapatero Osorio, et al. in prep.).

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