Baraffe et al. (1998, and Baraffe et al. (2015, stellar evolutionary models with isochrones ranging from 8 − 30 − 120 − 300 − 500 Myr. Earlier models combined with the photometry from Daemgen et al. (2007) suggest that the BC components of J1036 are ≈300 Myr old and close to 0.16 M_⊙ in mass. More recent models, however, do not agree with the current measurements and would argue for the components being far younger and less massive, and for them being in the brown dwarf regime where hydrogen has yet to begin nuclear fusion. Neither model corresponds well with our estimates of the individual dynamical mass of B and C of 0.24 M_⊙, indicated by the blue markers in the lower plot, which are within 1σ of the models predictions where the uncertainty is dominated by the error from the distance of 20.1 ± 2.0 pc. The red crosses in the lower plot are earlier mass estimates, where the observed brightness has been interpolated with the 300 Myr isochrone. The length of the arms of the red crosses do not represent the errors.