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Fig. 9.

image

Top row: empirical templates fitted to the spectra of the components to 2M1510, suggesting best fits for M9γ or an earlier type for both components. Due to the contrast and proximity of the companion to the primary, it is very likely that much of the shape of the spectrum of the secondary component is contributed by the primary. The companion is about 0.2 times the brightness of the primary, and it is unlikely they would be of the same spectral type (although this discrepancy may be mitigated if the primary is an unresolved binary). Lower plots: best-fit theoretical evolutionary models from BT-Settl CIFIST to each individual component. We find the best-fit models to be Teff = 2700 K with logg = 3.5 for the primary and Teff = 2700 K with logg = 4.5 for the secondary. The contrast in magnitude between the components is estimated to be ΔMH ≈ 2, and we would expect the secondary component to be cooler than what is predicted by our best-fit model.

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