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tokens: by l b = ( π b + M b ) modulus 360deg. For CARMENES and the HARPS data sets, the total RV jitter is comparable at ≲ 2 m s −1 , while it is 5.62 m s −1 for the HIRES data. With 1.77 m s −1 , the root mean square of the residuals of the model fits is lowest for the HARPS post-upgrade data, followed by the HARPS pre-upgrade (2.15 m s −1 ) and the CARMENES (2.66 m s −1 ) data. Again, HIRES shows the highest value, with 6.02 m s −1 . Compared to the formal uncertainties of the measurements (see Sect. 3 ), this means a factor of around three for HIRES and the HARPS pre-upgrade, and a factor of two for the HARPS post-upgrade and the CARMENES data. The GLS periodogram of the residuals does not show any significant signals (lower panel Fig. 1 ). However, there is some power at periods around 45 days and its overtones. This can be attributed to the rotation period P rot = 46.04 d of the host star. Moreover, the strongest peak at around P ≈ 190 d nearly reaches the 1% FAP level. The source of this signal is currently unknown, although the activity indicators hint at stellar activity. We also analyzed the residuals for possible long-term structures, but found the results inconclusive. While the entire data set shows only a negligible drift term of 0.03 ms −1 yr −1 , it is more significant for the residuals of the most recent RV measurements. A linear fit to the combined residuals from the HARPS post-upgrade epoch together with the CARMENES data gives a slope of around 0.5 ms −1 yr −1 . This could be an indication for an additional long-term signal, which in the HIRES data might be obscured by the comparably high scatter. In order to investigate the robustness of our fit results against possible contributions from correlated noise and additional RV or activity signals, we studied five additional models, using the concepts of moving averages (MA) and Gaussian process (GP) regression. The results from this analysis and their discussion can be found in Appendix. B . They agree with the orbital parameters reported here. Fig. 2 Unfolded ( left ) and phase-folded ( right ) RV measurements of the individual instruments for HD 180617, together with the best fit overplotted. 4.3 Activity analysis Periodic variability in RV measurements can also be introduced by stellar activity. Chromospheric emission, chromatic dependence of the RVs, and changes in line profiles are indicative of stellar activity. In Fig. 4 we provide GLS periodograms for some of these quantities, derived from the available CARMENES spectra. The H α index, the chromatic index (CRX), and the differential line width (dLW), shown in the three uppermost panels, are derived from the time series of activity indicators directly provided by SERVAL ( Zechmeister et al. 2018 ). While the chromatic index reflects wavelength dependencies of the measured RVs in the different échelle orders, which can result from the temperature surface structure onthe star (spots or faculae), the differential line width