First determination of the dynamical mass of a binary L dwarf

We present here the results of astrometric, photometric and spectroscopic observations leading to the determination of the orbit and dynamical masses of the binary L dwarf 2MASSW J0746425+2000321. High angular resolution observations spread over almost 4 years and obtained with the Hubble Space Telescope (HST), the ESO Very Large Telescope (VLT), and a the W. M. Keck Observatory (Keck) allow us to cover similar to36% of the period, corresponding to 60% of the orbit, and, for the first time. to derive a precise estimate of the total and individual masses of such a late-type object. We find an orbital period of 3850.9(-767)(+904) days. The corresponding total mass is 0.146(-0.006)(+0.016) M-circle dot with uncertainties depending on the distance. Spatially resolved low resolution optical (550-1025 nm) spectra have been obtained with HST/STIS, allowing us to measure the spectral types of the two components (L0 +/- 0.5 for the primary and L1.5 +/- 0.5 for the secondary). We also present precise photometry of the individual components measured on the high angular resolution images obtained with HST/ACS and WFPC2 (visible), VLT/NACO (J. H and K-S bands) and Keck I (K-S band). These spectral and photometric measurements enable us to estimate their effective temperatures and mass ratio, and to place the object accurately in a H-R diagram. The binary system is most likely formed by a primary with a mass of 0.085 +/- 0.010 M. and a secondary with a mass of 0.066 (sic) 0.006 M., thus clearly substellar. for an age of approximately 300 +/- 150 Myr. Halpha variability indicates chromospheric and/or magnetic activity.