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 a 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 about \sim 3 Myr , have masses at or below the substellar limit and , 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 TTauri phase and form like stars , from colapse and fragmentation of a molecular cloud .