Fig. 3
Top panel: HD 113337 RV residuals from the Keplerian fit of planet b only vs time (black dots) and HD 113337 FWHM vs time (green triangles, same scale as RV). The Keplerian fit of candidate planet c is overplotted to the RV residuals of planet b (red). The average FWHM (~13.7 km s−1) has been set to 0 for clarity. Middle panel: FWHM vs RV residuals of planet b. Bottom panel: Pearson’s correlation coefficient of RV residuals of planet b vs FWHM for different FWHM phase shifts, considering a ~3265-day period (black solid line). The actual Pearson’s coefficient (for no FWHM phase shift) is displayed as a black dot.
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