2004/03/12 by D. Barrado, David Barrado y Navascues
Chemistry · Physics and Astronomy · #Astrophysics and Star Formation Studies #Molecular Spectroscopy and Structure #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1051/0004-6361:20047122
published as Astron.Astrophys. 422 (2004) 631-636 · Astronomy & Astrophysics, accepted March 11, 2004
arxiv created 2004/03/12 · openalex publication_date 2004/07/09 · arxiv updated 2009/12/01 · openalex created_date 2022/10/03 · openalex updated_date 2026/04/05
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 line, the detected lithium at 6708 , 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.