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Fig. 15


Projected separation (top panel) and estimated reflected-light contrast in the WFIRST blue channel (bottom panel) for GJ 676A b as a function of time. The solid line shows the best-fit model and the grey band encompasses the 1σ interval for orbital solutions drawn from the MCMC posterior distribution, i.e. it takes into account all uncertainties except for the one in GJ 676A’s mass. In the bottom panel, dashed, solid, and dash-dotted lines represent albedos of 0.4, 0.5, and 0.6, respectively. The vertical dashed line indicates the maximum separation of 110 mas for which we estimated a contrast of 2.6 × 10-9 for an albedo of 0.5.

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