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Fig. 2

image

Top: GLS periodogram of the RV data of HD 59686 A. The significant peaks at ~5000 and ~340 days represent the orbits of the stellar and planetary companions, respectively. The 5000-day period is the time frame of our observations, therefore it is much shorter than the actual stellar period. The dotted, dashed, and dash-dotted lines show FAPs of 0.1%, 1%, and 5%, respectively. Middle: periodogram of the residual RVs after the signal due to the stellar companion is removed from the data. Now the peak due to the planetary companion becomes much stronger and the alias period at ~400 days disappears. Additionaly, another alias period appears at ~1700 days. Bottom: periodogram of the residual RVs after subtracting the orbital fit (stellar+planetary companions); it shows no significant peaks.

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