Data colors and symbols are the same as in Fig. 8, but for GJ 876. Panel a: the total amount of 622 precise RVs from HARPS, HIRES and CARMENES are fitted with a four-planet Newtonian model. Panel b: zoomed extent of the CARMENES data, which clearly follow the four planet model with a very low rms = 2.97 m s^-1, very similar to the HARPS data with rms = 2.95 m s^-1, but better than the HIRES data whose rms scatter is 4.35 m s^-1. Panel c: GLS power spectrum of the residuals from the four-planet dynamical model for GJ 876 showing several peaks above FAP = 0.1% near 106.0 d, 90.6 d and 441.1 d. However, these are unlikely planetary signals (see text for details). Panel d: our updated four-planet dynamical fit is stable for 10 Myr and is consistent with a chaotic Laplace 1:2:4 MMR orbital evolution between planets b, c and e, already known for this system. Our best fit and orbital evolution of the planetary system, however, suggests smaller (compared to the literature) eccentricity (e_d = 0.082) of the innermost planet GJ 876 d.