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Fig. 3


Photo-centre displacement as a function of wavelength for a Keplerian dust cloud orbiting at 1au around a G2V star at 10 pc (solid lines). The thicker of the G2V lines is the numerical model. We also vary the spectral type of the host star using the analytical model. The dotted line is for an A6V star and the dashed line for an M8V star.

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