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Fig. 1


Top: schematic of the usual barycentric photo-centre displacement ΔαB used in astrometry to detect a planet of mass MC at distance a from the barycentre with the star of mass M. Bottom: the photo-centre displacement Δαph is now caused by an inhomogeneity of flux Iinh at distance a orbiting around a star of flux I and possibly surrounded by a disc shown with yellow lines.

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