ner_tags: O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject O O O B-CelestialObject I-CelestialObject O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O B-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject O O O O O O O B-Model O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject B-CelestialObject I-CelestialObject O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O B-Model O O O O O O O O B-Telescope I-Telescope O B-Telescope O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject B-CelestialObject I-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O
tokens: B ). The trend is still visible with a lower slope 0.23 ms −1 d −1 . We present the RV and corrected RV of HD 186704A in Fig. 3 . The difference of one order of magnitude on the slope of the trend between Nidever et al. (2002) observations and ours can be explained by the fact that our observations were made when the SB was closer to the periastron or apoastron of its orbit. 3.1.6 HD 181321 We confirm that HD 181321 is an SB. Nordström et al. (2004) report a variation of 2.3 km s −1 over 9 yr, Guenther Esposito (2007) report a trend with a slope of 1.4 km s −1 yr −1 . Our observations spread on 3757 days (10.3 yr) cover at least two orbital periods. The star is active and show BVS variations with a period of 2−2.5 days that should correspond to the rotational period of the star. We use yorbit to fit the RV with two Keplerian models, one to fit the stellar activity variation and an another to fit the binary variations. We find two possible solutions for the companion, one with a period of 1600 days (2.7 au) and a minimum mass of 0.1 M ⊙ , and a second with a period of 3200 days (4.4 au) and a minimum mass of 0.18 M ⊙ . In both cases, the eccentricity is ~0.5. We present those two solutions in Fig. 4 . More data are needed in order to distinguish between those two solutions. Fig. 4 Solutions of HD 181321 RV fit by the sum of two Keplerian ( top ) and their residuals ( bottom ). Left : 1600 days solution. Right : 3200 days solution. 3.1.7 HD 206893 HD 206893 is a F5V star that hosts a directly imaged BD companion at a separation of 270 mas ( Milli et al. 2017 ; Delorme et al. 2017 ). We recently reported in Grandjean et al. (2019) a long-term trend in the star RV coupled with pulsations with periods slightly less than one day. We performed an MCMC on both the RV trend, imaging data, and H IPPARCOS - Gaia proper motion measurements to constrain the orbit and dynamical mass of the BD. We concluded that the trend can not be attributed to the BD as it leads to dynamical masses incompatible with the object’s spectra. The presence of an inner companion that contributes significantly to the RV trend is suggested with a mass of 15 M Jup , and a period between 1.6 and 4 yr. 3.1.8 HD 217987 HD 217987 is a M 2V, high proper motion star and exhibits a long-term RV trend induced by its secular acceleration. We therefore corrected the RV from the star secular acceleration in its proper motion we deduced from its paralax and proper motion reported in Gaia Collaboration (2018) (see Fig. 5 ). The corrected RV presents short period variations. The RV and BVS are correlated which indicate that the signal might be dominated by spots or plages (see Fig. 5 ). We observe a long-term variation in log , FWHM, and RV which are better fitted by a second degree polynomial model than with a linear model (see Fig. 5 ). This variation could be then attributed to a magnetic cycle of the star with a period greater than 5000 days. An analysis on a large number of M dwarf was