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Fig. 10.


Top row: empirical templates fitted to 2M2022. We find a best-fit model to be of M9γ/β ± 1 for both components, suggesting a pair of young BDs around ∼100 Myr old. Due to the small relative separation between the two components we expect there to be substantial contamination from each of them influencing the other. Nevertheless, we find that they are of almost equal brightness and expect them to share the same spectral type. The spectral type is consistent with the age of the AB Dor moving group at around 120–200 Myr, suggesting that the binary is a pair of ≈50 MJup BDs. Lower plots: best-fit theoretical evolutionary models from BT-Settl CIFIST to each individual component, where we find the Teff = 2800 K and logg = 3.5−4.0 models to be the best fit to both components. The light-blue, green, and yellow shaded areas indicate the spectral features from FeH, Na I, and CO, respectively.

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