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Fig. 6


The relative motions between planet host stars and the candidate companions where observations over several epochs are available. The black lines show the expected motion if the detected star were a distant background star, assuming that such a star would have negligible proper motion compared to the foreground planet host star. The shaded areas indicate the 1σ uncertainties on the motions, based on the errors in proper motion. The dashed blue line is the best fit assuming no relative motion between the two stars. The symbols indicate the source of each point: blue circles – this work; green squares – Wöllert et al. (2015), Wöllert & Brandner (2015); red upwards triangles – Faedi et al. (2013); cyan downwards triangles – Ngo et al. (2015); magenta hexagons – Adams et al. (2013); yellow diamonds – Ginski et al. (2013); black pentagons – 2MASS.

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