SIMBAD references

We have obtained a series of high-resolution optical spectra for 2MASSW J1207334-393254 (2M 1207). Two consecutive observing nights at the ESO Very Large Telescope with the Ultraviolet and Visual Echelle Spectrograph yielded a time series with a resolution of ∼12 minutes. Additional high-resolution optical spectra were obtained months apart at the Magellan Clay telescope using the Magellan Inamori Kyocera Echelle (MIKE) instrument. Combined with previously published results, these data allow us to investigate changes in the emission line spectrum of 2M 1207 on timescales of hours to years. Most of the emission line profiles of 2M 1207 are broad, in particular that of Hα, indicating that the dominant fraction of the emission must be attributed to disk accretion rather than to magnetic activity. From the Hα 10% width, we deduce a relatively stable accretion rate between 10^–10.1 and 10^–9.8 M_☉/yr for two nights of consecutive observations. Therefore, either the accretion stream is nearly homogeneous over (sub)stellar longitude, or the system is seen face-on. Small but significant variations are evident throughout our near-continuous observation, and they reach a maximum after ∼8 hr, roughly the timescale on which maximum variability is expected across the rotation cycle. Together with past measurements, we confirm that the accretion rate of 2M 1207 varies by more than 1 order of magnitude on timescales of months to years. Such variable mass accretion yields a plausible explanation for the observed spread in the M{dot}-M diagram. The magnetic field required to drive the funnel flow is on the order of a few hundred G. Despite the obvious presence of a magnetic field, neither radio nor X-ray emission has been reported for 2M 1207. It is possible that strong accretion suppresses magnetic activity in brown dwarfs, similar to the findings for higher mass T Tauri stars.