Letters to the Editor

X-shooter observations of the accreting brown dwarf J053825.4-024241^⋆

¹ Osservatorio Astrofisico di Arcetri, INAF, Largo E. Fermi 5, 50125 Firenze, Italy
e-mail: erigliaco@arcetri.astro.it
² Università di Firenze, Dipartimento di Astronomia, Largo E.Fermi 2, 50125 Firenze, Italy
³ School of Cosmic Physics, Dublin Institute for Advanced Studies, Dublin 2, Republic of Ireland
⁴ ESO, Karl Schwarschild Strasse 2, 85748 Garching bei München, Germany
⁵ Osservatorio Astronomico di Capodimonte, INAF, 80131 Napoli, Italy
⁶ Max-Planck-Institut fur extraterrestriche Physik, 85741 Garching bei München, Germany

Received: 26 October 2010
Accepted: 9 December 2010

Abstract

We present the first observations of a probable brown dwarf, obtained with the new spectrograph X-shooter mounted on the UT2@VLT. The target (2MASS J053825.4-024241) is a 0.06 M_⊙ object in the star-formation region σ Ori. The X-shooter spectrum covers simultaneously the whole range from UV to NIR (300–2500 nm). The J053825.4-024241 spectrum is rich in emission lines that are typical of accreting young object and clearly shows the Balmer jump. Moreover, many photospheric atomic and molecular absorption lines yield the spectral type and confirm that the object is young. We compute the mass accretion rate from all available observed accretion diagnostics. We find that there is a large spread in the Ṁ_acc values (up to a factor 40) that is not caused by variability; some of this spread may be intrinsic, i.e., owing to different physical conditions of the emitting region for the same Ṁ_acc. However, within the large error bars all Ṁ_acc measurements agree, and the mean value is logṀ_acc ~ −9.86 ± 0.45 M_⊙/y. The hydrogen Balmer lines are clearly detected up to n = 25. Their ratios suggest that the emitting region is cold (T ~ 2000−3000 K), dense and in thermal equilibrium (LTE), and that the lines are optically thick up to n ~ 21. We briefly discuss the implications of this result for magnetospheric accretion models.