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Fig. 6


The detection limit (dashed line) for wide orbit planets from the observations of the target HR 8799 in the NIRI CH4s filter (left) and K′ filter (right) compared to the DUSTY (red line) and COND (black line) evolutionary models (Chabrier et al. 2000; Baraffe et al. 2003). The DUSTY model mass-magnitude grid does not extend to magnitudes as faint as the detection limits. The current estimates of the HR 8799 planet masses (Marois et al. 2010b) are also plotted, and the empirical masses are consistent with the COND magnitudes within the error bars.

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