F Philipot
email: florian.philipot@obspm.fr

A.-M Lagrange

F Kiefer

P Rubini

P Delorme

A Chomez

A multi-technique approach to identifying and/or constraining radial-velocity substellar companions

Keywords: radial velocities -techniques, high angular resolution -astrometry -planets and satellites, gaseous planets -brown dwarfs -stars, low-mass A107,

Context. Although more than one thousand substellar companions have already been detected with the radial velocity (RV) method, many new companions remain to be detected in the public RV archives. Aims. We wish to use the archival data obtained with the ESO/HARPS spectrograph to search for substellar companions. Methods. We used the astronomic acceleration measurements of stars obtained with the HIPPARCOS and Gaia satellites to identify anomalies that could be explained by the presence of a companion. Once hints for a companion were found, we combined the RV data with absolute astrometry data and, when available, relative astrometry data, using a Markov chain Monte Carlo algorithm to determine the orbital parameters and mass of the companion. Results. We find and characterize three new brown dwarfs (GJ 660.1 C, HD 73256 B, and HD 165131 B) and six new planets (HD 75302 b, HD 108202 b, HD 135625 b, HD 185283 b, HIP 10337 b, and HIP 54597 b) with separations between 1 and 6 au and masses between 0.6 and 100 M Jup . We also constrain the orbital inclination of ten known substellar companions and determine their true mass. Finally, we identify twelve new stellar companions. This shows that the analysis of proper motion anomalies enables the optimization of the RV search for substellar companions and their characterization.

Introduction

Since the first discovery of a planet orbiting a solar-type star (Mayor & Queloz 1995), various radial velocity (RV) surveys have detected hundreds of extrasolar planets and brown dwarfs (Mayor et al. 2011;Hébrard et al. 2016;Wittenmyer et al. 2020;Rosenthal et al. 2021). In the long term, these surveys aim to estimate the minimum mass and radial distributions of these companions and compare these values with results obtained by different population synthesis models [START_REF] Mordasini | Handbook of Exoplanets[END_REF]Emsenhuber et al. 2021).

Despite the many detections, numerous RV data available in the public archives have never been published and could potentially contain the signals of unknown companions. The proper motion acceleration measurements published in Gaia Data Release 3 (hereafter DR3) for more than 1.4 billion stars can be used to select the targets with the highest probability of having a companion. Indeed, the study of the stars' proper motion accelerations has recently allowed the detection in highcontrast imaging (hereafter HCI) of a few substellar companions (e.g., Bonavita et al. 2022a;Swimmer et al. 2022;Franson et al. 2023;Kuzuhara et al. 2022).

Absolute astrometry based on position and proper motion measurements obtained with Gaia (Gaia Collaboration 2020) and HIPPARCOS (Perryman et al. 1997;van Leeuwen 2007) can furthermore remove the indetermination on the companion orbital inclination that is left with the RV method. For instance, using only the RV data, Kane et al. (2019) report a planet candidate with a minimum mass of about 10 M Jup , while Li et al. (2021), combining the RV data with absolute astrometry, found a highly inclined orbit and a true mass of about 20 M Jup . Since the first Gaia data release, the combination of these two techniques has allowed us to improve the characterization of tens of substellar companions (Grandjean et al. 2019;Brandt et al. 2019Brandt et al. , 2021a,b;,b;Kiefer et al. 2019Kiefer et al. , 2021;;Damasso et al. 2020;Venner et al. 2021;Li et al. 2021;Feng et al. 2022;Philipot et al. 2023).

However, the precise mass of a companion can only be determined if the orbital parameters are properly constrained, which remains difficult when the orbital period (P) is much larger than the RV baseline Lagrange et al. (2023). In the case of poorly constrained periods, the addition of relative astrometry from HCI or interferometry allows us to significantly improve the characterization of the companion. This is, for instance, the case with HD 211847 B, which was first reported using only RV data as a low-mass brown dwarf candidate with very poorly constrained orbital parameters and minimum mass (Sahlmann et al. 2011), then reported as a massive brown dwarf adding absolute astrometry (Feng et al. 2022), and finally identified as a low-mass star by adding relative astrometry data (Philipot et al. 2023).

In this paper, we study the proper motion anomalies of the stars observed with the HARPS/ESO spectrograph, with the aim of detecting new substellar companions. We also combine the available RV data and absolute astrometry with HIPPARCOS

Sample

Proper motion anomaly for stars observed by HARPS-South

We first selected the 734 stars observed with the High Accuracy Radial velocity Planet Searcher (HARPS) spectrograph mounted on the 3.6 m ESO telescope at La Silla (Mayor et al. 2003) that are listed in the HARPS-RVBANK archive (Trifonov et al. 2020) with more than 30 RV data points spread on a temporal baseline greater than 1000 days. Secondly, we used the astrometric acceleration of stars (the so-called proper motion anomaly, Kervella et al. 2019, hereafter PMa) determined by the difference in proper motion (hereafter PM) between the average HIPPARCOS-Gaia PM (24.5 yr time baseline) and the "instantaneous" PM published in the Gaia DR3 to select systems with the highest probability of hosting a substellar companion. To do so, we selected the stars with a PMa 2σ larger than the noise. We simulated many samples of Gaia DR3 measurements for single stars of similar G-magnitudes and Gb -Gr colors, out of which we fit a PMa solely based on pure noise. For any of the 734 stars, we obtained PMa distributions of them as if they were single. The percentile of the PMa, measured in Kervella et al. (2022), within these distributions determines by how many σ they exceed the noise. To focus our study on the detection of substellar companions, we then excluded systems for which the predicted mass of a companion orbiting at 10 au that could account for the measured PMa value is larger than 200 M Jup . We obtained a sample of 116 stars.

Selection of systems with a substellar companion

For the selected sample of stars, we then retrieved all the RV measurements available in the public archives of 12 different spectrographs (see below) and analyzed them to identify the presence of companion(s). For this step, we used the DPASS genetic algorithm 1 (Lagrange et al. 2019) to detect periodicity in the data and make a rapid estimate of the orbital properties and the minimum mass of the companion(s). We thus find 20 multiple systems (two or more companions) and 80 single systems (one companion). Then, we selected the systems for which the orbital parameters of the companion are properly determined and the mass is lower than about 80 M Jup , corresponding to substellar companions. To do so, we combined the RV data with astrometry to determine the orbital inclination of the companion and obtain its 1 DPASS uses an evolutionary algorithm to fit RV data with one or more Keplerian orbits. This algorithm converges to the solution corresponding to the smallest root-mean-square (hereafter rms) of the RV residuals.

true mass. We used a Markov chain Monte Carlo (MCMC) algorithm to estimate the uncertainties of the different parameters. In the first step, we used the orvara (Orbits Using Radial Velocity, Absolute, and/or Relative Astrometry) algorithm (Brandt et al. 2021d), which enables the RV data to be combined with the absolute astrometry and the available HCI data. Orvara converges faster than most other algorithms (Brandt et al. 2021c) and enables us to quickly estimate the orbital parameters and mass of the companion and exclude stellar companions. However, Lagrange et al. (2023) have shown that, when the orbital period is not well covered by the RV data points, MCMC algorithms have difficulties exploring very eccentric solutions. Therefore, we then used our MCMC algorithm (described in Sect. 3.4) based on the MCMC sampling tool used by Lagrange et al. (2023) to enable a better exploration of the possible solutions.

In 27 cases, the coupling of the different methods does not properly constrain the orbit of companions, mainly due to the poor coverage of their periods by RV data. We also report on 25 stellar companions, for which the orbital parameters and the mass can be retrieved in Table C.3. Finally, we obtain a sample of 27 substellar companions for which it is possible to estimate all the orbital parameters and true masses.

Data available in the sample systems

Radial velocity data

We used the archival data obtained with the HARPS spectrograph available in the European Southern Observatory (ESO) archives2 . To characterize as well as possible the different systems, we combined the HARPS data with all other publicly available RV data points. We retrieved from the literature the data obtained with the University College London Echelle Spectrograph (UCLES, Diego et al. 1990), the Lick Observatory Hamilton Echelle Spectrometer (Lick, Vogt 1987), the Automated Planet Finder (APF, Vogt et al. 2014), the Coudé Echelle Spectrometer (CES, Enard 1982) long camera (LC) and very long camera (VLC), the Magellan Inamori Kyocera Echelle spectrograph (MIKE, Bernstein et al. 2003), the Carnegie Planet Finder Spectrograph (PFS, Crane et al. 2010), the High-Resolution Spectrograph (HRS, Tull 1998), and the High-Resolution Echelle Spectrometer (HIRES, Vogt et al. 1994). We retrieved from the DACE archive3 the data obtained with the CORALIE echelle spectrograph (Queloz et al. 1999) and from the Observatoire de Haute-Provence (OHP) archive4 the data obtained with the ELODIE (Baranne et al. 1996) and SOPHIE (Perruchot et al. 2008) spectrographs. For the 53 systems with a characterized companion, the considered RV datasets are listed in Appendix B (Table B.1).

Due to a major optical fiber upgrade in 2015 (Lo Curto et al. 2015), an RV offset may be present between HARPS data obtained before and after this upgrade. We, therefore, separated these data into two different sets as if they were obtained from two different instruments. We labeled the datasets obtained before May 19, 2015 "H03" and the datasets obtained after June 3, 2015 "H15". As for HARPS, a major upgrade has been performed on the HIRES (Tal-Or et al. 2019) and SOPHIE (Bouchy et al. 2013) spectrographs and two major upgrades have been performed on the CORALIE spectrograph (Ségransan et al. 2010). We labeled the HIRES datasets obtained A107, page 2 of 71 Philipot, F., et al.: A&A, 678, A107 (2023) Table 1. Characteristics of the reduced HCI observations.

Star

Date obs. Instrument Filter NDIT×DIT(s)×Nframe ( * ) Seeing ( ′′ ) Airmass τ 0 (ms) (a) Notes. ( * ) NDIT is the number of sub-integration within a DIT. DIT is the detector integration time per frame. τ 0 corresponds to the coherence time.

before and after August 7, 2004 "Hir94" and "Hir04", respectively, the SOPHIE datasets obtained before and after June 17, 2011 "SOPHIE" and "SOPHIE+", respectively, and the CORALIE datasets obtained before June 2007, between June 2007 and November 2014, and after November 2014 "C98", "C07", and "C14", respectively.

Relative astrometry data

Whenever possible, we used high-contrast imaging data available in the literature as well as new relative astrometry measurements obtained from observations in the NAOS+CONICA (NACO; Rousset et al. 2003;Lenzen et al. 2003) and the Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE; Beuzit et al. 2019) archives. The observing logs for the analyzed observations are summarized in Table 1.

For the NACO observations, even when they are quite shallow, these HCI data are precious in identifying large-separation stellar companions that could mimic the astrometric signature of closer-in substellar objects. Given the low contrast and wide separation of such stellar companions, we carried out a very simple reduction, by just stacking and subtracting one to another raw data cubes acquired at two different offset positions within the same observation, which subtracts the dark and thermal background. In spite of this simple reduction, we detect five high S/N stellar companions (Fig. 1) in the systems HD 1388, HD 78612, HD 93351, and HD 207700. Since we chose to use only noncoronographic observations even when deeper coronographic data did exist, we were also able to measure very accurately the position of the host star and of the high S/N stellar companions, using the moffatian fit of their diffraction-limited cores.

For the SPHERE observations, we detect a massive stellar companion in the system HD 21175. This companion is outside the field of view of the integral field spectrograph (IFS), and hence only the data from the near-infrared imager and spectrograph (IRDIS) are used. All the pre-reduction steps (dark and background subtraction, flat-field correction, bad pixel correction, and centering) were performed on the SPHERE data center [START_REF] Delorme | Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics[END_REF]) using tools provided in the ESO data reduction and handling pipeline (Pavlov et al. 2008). Due to the stellar nature of the companion, its point spread function (PSF) on the residual image provided by angular differential imaging (ADI) based algorithms using the science sequence is completely saturated and prevents any fitting of it. We thus chose to extract the astrometry of the companion using the off-axis unsaturated PSF frames of the primary star taken before and after the coronographic sequence. We created a 4D dataset containing only the PSF frames. We used a simple No-ADI algorithm embedded into the SPHERE speckle calibration tool (SPECAL) software Notes. Since the companion of HD 93351 is binary, we considered the average separation in RA and Dec of the two companions. (Galicher et al. 2018) installed in the SPHERE data center. The astrometry and photometry were extracted by SPECAL from the residual stack produced by the No-ADI reduction, taking into account the neutral density filter used during the off-axis calibration frames (ND_3.5).

The separations and position angles (hereafter SEP and PA) found for the new detections can be retrieved in Table 2. For GJ 680, HD 101198, HD 111031, HD 195564, HD 221146, and HIP 113201, we used the separations and position angles published in the literature. All considered relative astrometry values are summarized in Table B.2.

Absolute astrometry data

We used the position and proper motion values from the HIPPARCOS-Gaia Catalog of Accelerations (HGCA) published by Brandt (2021) from HIPPARCOS and Gaia early DR3 (Gaia Collaboration 2016, 2021) measurements to determine the stellar acceleration of each selected target. For each star, the difference between the position measurements obtained by HIPPARCOS and Gaia divided by the mean interval between the two measurements (∼25 yr) gives a more accurate tangential proper motion. The corresponding values are provided in Table A.1.

Orbit fitting

We used our MCMC algorithm presented in Philipot et al. (2023) to fit the RV and/or relative astrometry and/or absolute astrometry data, assuming Keplerian orbits. Our tool is based on the emcee 3.0 Python package (Foreman-Mackey et al. 2013). We used the HTOF package (Brandt et al. 2021d)

+ ∆ 2 pa σ 2 pa (1 -ρ 2 sep,pa ) + 2ρ sep,pa * ∆ sep * ∆ pa σ sep σ pa (1 -ρ 2 sep,pa ) (1) LLH 2 RV = -0.5 *        ∆ 2 RV σ 2 RV + jitter 2 + log(σ 2 err + jitter 2 )        (2) LLH 2 HG = (µ H,o -μ -pµ H ) T C -1 H (µ H,o -μ -pµ H ) + (µ HG,o -μ -pµ HG ) T C -1 HG (µ HG,o -μ -pµ HG ) + (µ G,o -μ -pµ G ) T C -1 G (µ G,o -μ -pµ G ), (3)
where ∆ sep , ∆ pa , and ∆ RV are the difference between the measured and predicted separations, the position angle, and the RV. ρ sep,pa is the correlation coefficient between the separation and the position angle measurement. σ sep , σ pa , and σ err correspond to the uncertainty on the measured separation, the PA, and the RV, respectively. σ RV is the variance in the RV, and jitter is the stellar jitter measured. For the likelihood of the proper motions measurements, µ x,o and µ x correspond to the predicted and observed proper motion, p is the parallax, C -1 x is the inverse of the covariance matrix, and μ corresponds to the center-of-mass motion of the system's barycenter.

Unlike orvara or other similar packages, our code uses modular arithmetic computations for angles, wherever appropriate, to alleviate artifacts at the range boundaries. To minimize multimodality effects, the MCMC code uses a mix of move functions, in particular the Differential Evolution (DE) move function suggested in the Emcee package documentation for these situations (Foreman-Mackey et al. 2013).

We considered ten free parameters for each system: the host star mass, the parallax 5 , the semi-major axis (a), the eccentricity (ecc), the orbital inclination (I), the longitude of the ascending node (Ω), the argument of periastron (ω), the periastron passage time (P time ) 6 , the companion mass, and a stellar jitter. It is important to note that in the fitting process we considered √ ecc cos ω and √ ecc sin ω instead of ecc and ω. In addition, to combine data from different instruments, we added an instrumental offset for each instrument as a free parameter of the model (see above). We considered uniform priors for all fitting parameters, except for the host star mass and the distance of the system, for which we considered Gaussian priors, and for the orbital inclination, for which we considered a sin(I) prior.

When the orbital period of a companion is much shorter than the Gaia DR3 observing window (1038 days), the PMa does not allow us to constrain the orbital inclination. In such cases, we fit Keplerian orbits with our MCMC, considering only the RV data points. We then used GASTON (Gaia Astrometric Noise Simulation to derive Orbit incliNation; (Kiefer et al. 2019(Kiefer et al. , 2021)), updated to the improved Gaia DR3 accuracy, to model the DR3 astrometric excess noise (hereafter AEN) with a motion of the system's photocenter induced by the orbiting RV companion at an optimal orbital inclination. This leads to a new estimate of the true mass of the companion. The principle of GASTON is to assume the presence of this companion and (i) simulate Gaia's observations of the system with many possible orbits of the photocenter, (ii) fit out the 5-parameters linear model, as performed by Gaia, that includes position, proper motion, and parallax, (iii) calculate the AEN from the residuals, and (iv) compare the DR3 AEN to the outcomes of the simulations and perform an optimization of the orbital inclination. The GASTON method has been improved since the EDR3 release. It now accounts for the dependence of the noise intrinsic to Gaia's acquisitions and data reductions (instrumental jitter, spacecraft's attitude, and modeling) on magnitude (G-band) and color (Gb -Gr) (Lindegren et al. 2021). It also accounts for a parallax offset due to the orbital motion and produces a corrected parallax.

New companions

4.1. Brown dwarfs 4.1.1. GJ 660.1 GJ 660.1 is a binary system composed of a M1V star (GJ 660.1 A) and another low mass star of type M9.5 ± 0.3 (GJ660.1 B, Aganze et al. 2016). The projected separation between the two M dwarfs is estimated at 122 ± 9 au (Schneider et al. 2011). For this system, 59 RV data points were obtained with the HARPS spectrograph between 2009 and 2019 for GJ 660.1 A. A periodicity is clearly present in the periodogram of the data with a peak at about 615 days. Using DPASS, we find the best solution, corresponding to an additional brown dwarf candidate with a minimum mass of 16 M Jup and a period of 620 days (Fig. D.1).

The significant AEN in the Gaia DR3 data for GJ 660.1 of 2.633 mas (83σ larger than noise) is dominated by orbital signals with a period shorter than 100 yr (a < 16 au). The effect of GJ660.1 B is thus negligible, and we assume that the AEN is only due to GJ660.1 C. We used Gaston to fit the AEN, considering the RV solution found with our MCMC algorithm (Fig. 2), considering 300 000 iterations (burn-in = 50 000) and 1000 walkers, and varying the orbital inclination and the longitude of the ascending node. We find a semi-major axis of 1.12 ± 0.02 au (P = 618.6 ± 0.1 d), an eccentricity of 0.65 +0.11 -0.08 , a minimum mass of 59 +34 -15 M Jup , and an inclination of 87 +39 -43 °. This leads to a true mass within 78 +38

-16 M Jup . The posteriors obtained for each free parameter of the MCMC are reported in Table 3 and the corner plot is available in Appendix D (Fig. D.12). Note that, even if the orbital period is properly covered by the RV data, additional measurements near the periastron are necessary to better constrain the mass and eccentricity of GJ660.1 C and define the precise nature of the companion.

Looking at the periodogram of the RV data, corrected for the signal of GJ660.1 C, we observe a significant peak at about 200 days. No correlation between RV variations and bisector velocity span (BVS) variations that may explain this peak is observed. This signal could therefore correspond to the presence of an additional companion located at 0.5 au (P = 206 d) with a minimum mass of 0.3 M Jup (Fig. D.1). It should be noted that, given the mass and semi-major axis of this candidate companion, the AEN induced by it would be negligible compared with that induced by GJ 660.1 C.

HD 73256

Eighty-two RV data points were obtained for the G8IV star HD 73256, 26 RV HARPS measurements were obtained between A107, page 5 of 71 Philipot, F., et al.: A&A, 678, A107 (2023) 2003 and 2012, 38 RV CORALIE measurements were obtained between 2001 and 2003, and 18 RV HIRES measurements were obtained between 2004 and 2016. Udry et al. (2003) reported a hot Jupiter with a minimum mass of 1.87 ± 0.49 M Jup and a period of 2.54858 ± 0.00016 days, considering the CORALIE data points. Considering all the RV data points available, a periodicity appears in the periodogram of the data with a strong peak around 2.5 days corresponding to the companion identified by Udry et al. (2003). Once the planet signal is removed, a periodicity appears in the periodogram with a peak around 3000 d. Using DPASS, we find the best two-planet solution with inner planet orbital parameters and minimum mass close to those reported by Udry et al. (2003) and a new, outer giant planet candidate with a minimum mass of 10 M Jup and a period of 2777 days (Fig. D.2). After removing both planets' signals, a periodicity is again present around 14 days, which corresponds to the rotation period of the host star (Udry et al. 2003).

As the orbital period of HD 73256 b is much smaller than the duration of Gaia DR3, the proper motion induced by the inner planet can be neglected. We thus simultaneously fit all the RV data points available, corrected for the signal of the inner planet, with the absolute astrometry (Fig. 3) with our MCMC, considering 300 000 iterations (burn-in = 50 000) and 1000 walkers. We find a semi-major axis of 3.8 ± 0.1 au (P = 2690 +60 -102 d) and an eccentricity of 0.16 ± 0.07, and constrained the orbital inclination of HD 73256 c to either 29 +5 -3 °or 152 +8 -7 °. We find a true mass of 16 ± 1 M Jup , corresponding to a low-mass brown dwarf. The posteriors obtained for each free parameter of the MCMC are reported in Table 3 and By simultaneously fitting RV HARPS measurements and absolute astrometry with our MCMC (Fig. 4), and considering 300 000 iterations after 50 000 iterations and 1000 walkers, we characterized the orbital parameters of the companion and constrained the orbital inclination to either 70 +11 -9 °or 109 +10 -12 °. We find a semi-major axis of 3.59 +0.06 -0.07 au (P = 2343 ± 2 d), an eccentricity of 0.672 ± 0.003 and a true mass of 19 +2

-1 M Jup . The posteriors obtained for each free parameter of the MCMC are reported in Table 3 a minimum mass of 5.3 M Jup , and an eccentricity of 0.88. However, we observe a significant correlation between RV variations and bisector velocity span (BVS) variations (Fig. D.9), indicating a possible stellar activity signal. Correcting the RV data with the linear regression between RVs and the bisector velocity span (Melo et al. 2007), we obtain a new RV dataset, for which a strong peak is present in the periodogram around 3000 days. Considering these data corrected for the stellar activity, we find the best solution for the companion corresponding to a planet that is less massive and eccentric (m p sin i = 2.7 M Jup and e = 0.44) but that has a similar period (Fig. D.11).

Combining the corrected RV data with absolute astrometry with our MCMC (Fig. 5), considering 300 000 iterations (burnin = 50 000) and 1000 walkers, we find a well-constrained orbital solution for HD 75302 b, and we constrained its orbital inclination to either 29 ± 5°or 150 +5 -6 °. We find a semi-major axis of 5.3 +0.2 -0.1 au (P = 4356 +173 -112 d), an eccentricity of 0.39 +0.10 -0.11 , and a true mass of 5.4 +0.5 -0.4 M Jup . The posteriors obtained for each free parameter of the MCMC are reported in Table 4 and

HD 108202

Forty-two RV data points were obtained with the HARPS spectrograph between 2005 and 2022 for the K4/5V star HD 108202. A periodicity is present in the periodogram of the data, with a peak of around 3000 days. Using DPASS, we find the best solution, corresponding to a giant planet candidate with a minimum mass of 2.4 M Jup and a period of 2990 days (Fig.

D.3).

By simultaneously fitting RV data and absolute astrometry with our MCMC (Fig. 6), and considering 200 000 iterations (burn-in = 50 000) and 1000 walkers, we characterized the orbital parameters of the companion. We find an orbital inclination of either 56 +19

-13 °or 130 +14 -24 °, a semi-major axis of 3.7 ± 0.1 au (P = 2990 +54 -51 d), an eccentricity of 0.52 +0.04 -0.03 , and a true mass of 3.0 +0.7 -0.5 M Jup . The posteriors obtained for each free parameter of the MCMC are reported in Table 4 and

HD 135625

Ninety-nine RV data points were obtained with the HARPS spectrograph between 2004 and 2021 for the G3IV/V star By simultaneously fitting RV data and absolute astrometry with our MCMC (Fig. 7), and considering 200 000 iterations (burn-in = 30 000) and 1000 walkers, we characterized the orbital parameters of the companion. Absolute astrometry does not allow us to properly constrain the orbital inclination. We can only exclude the solutions corresponding to a high inclined orbit and we find an orbital inclination of 93 +39 -43 °. We find a semi-major axis of 5.4 ± 0.1 au (P = 4055 +45 -44 d), an eccentricity of 0.16 Notes. The median and 1σ confidence interval are given for each parameter.

HD 185283

Seventy-eight RV data points were obtained with the HARPS spectrograph between 2004 and 2021 for the K3V star HD 185283. A periodicity is clearly present in the periodogram of the data, with a strong peak at about 4500 days. Using DPASS, we find the best solution, corresponding to a giant planet candidate with a minimum mass of 1.5 M Jup and a period of 4000 days (Fig. D.6). By simultaneously fitting RV data and absolute astrometry with our MCMC (Fig. 8), and considering 300 000 iterations (burn-in = 30 000) and 1000 walkers, we characterized the orbital parameters of the companion and constrained the orbital inclination to be of 91 +30 -31 °. We find a semi-major axis of 4.6 +0.2 -0.1 au (P = 4060 +148 -112 d), an eccentricity of 0.07 +0.05 -0.04 , and a true mass of 1.3 +0.3 -0.1 M Jup . The posteriors obtained for each free parameter of the MCMC are reported in Table 4 andthe

HIP 10337

One hundred and eight RV data points were obtained for the K7V star HIP 10337. 90 RV HARPS measurements were obtained between 2005 and 2022 and 18 RV HIRES measurements were obtained between 2008 and 2014. A periodicity is present in the periodogram of the data, with a large peak at about 8000 days. Using DPASS, we find the best solution, corresponding to a giant planet candidate with a minimum mass of 2.9 M Jup and a period of 6400 days (Fig. D.7).

By simultaneously fitting RV data and absolute astrometry with our MCMC (Fig. 9), and considering 300 000 iterations (burn-in = 30 000)and 1000 walkers, we characterized the orbital parameters of the companion and constrained the orbital inclination to either 33 +5 -4 °or 146 +4 -5 °. We find a semi-major axis of 5.9 ± 0.1 au (P = 6240 +151 -156 d), an eccentricity of 0.43 ± 0.05, and a true mass of 4.8 ± 0.6 M Jup . The posteriors obtained for each free parameter of the MCMC are reported in Table 4 and the corner plots are available in the appendix (Figs. D.20 and D.21).

HIP 54597

Sixty-nine RV data points were obtained with HARPS between 2006 and 2022 for the K5V star HIP 54597. A periodicity is clearly present in the periodogram of the data, with a strong peak at about 3300 days. Using DPASS, we find the best solution, corresponding to a giant planet candidate with a minimum mass of 2.3 M Jup and a period of 3270 days (Fig. D.8).

By simultaneously fitting RV data and absolute astrometry with our MCMC (Fig. 10), and considering 300 000 iterations (burn-in = 30 000) and 1000 walkers, we characterized the orbital parameters of the companion and constrained the orbital inclination to either 62 +16 -13 °or 116 +13 -14 °. We find a semi-major axis of 4.0 ± 0.1 au (P = 3274 +47 -46 d), an eccentricity of 0.03 +0.03 -0.02 , and a true mass of 2.4 +0.4 -0.2 M Jup . The posteriors obtained for each free parameter of the MCMC are reported in Table 4 andthe

Long-term stellar activity

The long-term magnetic activity of the host star can lead to variations in the RVs over periods similar to the orbital periods of the companions detected in our study (2-15 yr, Meunier et al. 2019). In order to estimate the amplitude of these RV variations, Meunier & Lagrange (2019) simulated the impact of the magnetic activity for F-G-K type stars considering a log R ′ HK between -5.1 and -4.6. They show that long-term magnetic activity can induce an RV jitter between 1 m s -1 for quiet stars and up to 10 m s -1 for the most active stars. These RV variations A107, page 8 of 71 can thus significantly impact the detection of sub-Jupiter planets with a minimum mass typically lower than 0.6 M Jup (Lagrange et al. 2023). All the newly detected companions have a minimum mass higher than 1.5 M Jup , corresponding to RV amplitudes higher than 40 m s -1 , well above the expected activity signal.

Concerning eventual short-term activity, we did not note a significant correlation between BVS and VR for any of these systems (except for HD 75302, see above). This result is consistent with the fact that these companions orbit around mature stars (> typ. 1 Gyr), the stellar jitters of which are generally smaller than those for young systems (Tran et al. 2021).

Improved parameters of known RV companions

Long-period companions (P > 1000 d)

By combining RV and absolute astrometry data, we properly characterized 14 substellar companions that have already been reported in the literature. We significantly improve the characterization and determine the exact nature of ten companions, and

HD 16905

Fifty-two RV data points were obtained with the HARPS spectrograph between 2003 and 2020 for the K3V star HD 16905. By coupling HARPS RV measurements obtained before February 2018 (Julian day: 2 458 160) with absolute astrometry, Feng et al. (2022) report an eccentric, massive giant planet with a mass of 9.1 +1.3 -1.4 M Jup , an orbital inclination of 19.7 +3.3 -1.9 °, a semi-major axis of 6.4 +1.6 -0.4 au, and an eccentricity of 0.67 +0.06 -0.07 . By fitting all the available RV data and the absolute astrometry data with our MCMC (Figs. D.23 and D.24), and considering 300 000 iterations (burn-in = 50 000) and 1000 walkers, we find significantly different solutions, with a semi-major axis of 8.8 +0.4 -0.3 au (P = 10 256 +618 -522 d), a mass of 11.3 +0.6 -0.7 M Jup , and an orbital inclination of either 43 ± 3°or 136 ± 3°.

A107, page 9 of 71 In each plot, the black curve corresponds to the best fit. The color bar indicates the log-likelihood corresponding to the different fits plotted.

HD 28254

Seventy-two RV data points were obtained with the HARPS spectrograph between 2003 and 2021 for the G5V star HD 28254. Naef et al. (2010) reported a very eccentric giant planet candidate with a minimum mass of 1.16 +0.10 -0.06 M Jup , a semimajor axis of 2.15 +0.04 -0.05 au, and an eccentricity of 0.81 +0.05 -0.02 based on the RV HARPS data obtained before April 2009 (Julian day: 2 454 931).

The baseline of RV data used by Naef et al. (2010) fully covers the period of HD 28254 b. Combining all HARPS RV measurements available with absolute astrometry with our MCMC (Figs. D.25 and D.26), and considering 600 000 iterations (burn-in = 100 000) and 1000 walkers, we find a solution with a semi-major axis very close to that reported by Naef et al. (2010) but more eccentric: a = 2.45 +0.03 -0.04 au (P = 1333 ± 4 d) and ecc = 0.95 +0.03 -0.04 . We also estimate the orbital inclination to be at either 21 +38 -11 °or 162 +7 -27 and the true mass to be between 1.5 and 6.5 M Jup . Hence, HD 28254 b is a giant planet.

HD 62364

Eighty-seven RV data points were obtained with the HARPS spectrograph between 2004 and 2021 for the F7V star HD 62364. By coupling the HARPS RV measurements obtained before February 2018 (Julian day: 2 458 160) with absolute astrometry, Feng et al. (2022) report two companions: a first, 17.4 +1.6 -1.7 M Jup brown dwarf at 18.9 +1.6 -1.1 au and a second 24.9 +2.7 -2.9

M Jup brown dwarf at 36.98 +3.0 -2.8 au. By fitting the RV data considering a one-companion system with DPASS, using three years of additional HARPS RV measurements, we find a significantly different result: a single companion at approximately 6.4 au and no additional signal in the RV residuals. Moreover, when considering a two-companion system, we find an offset of about 78 m s -1 between the HARPS RV measurements obtained before and after the fiber upgrade, while the average offset for a star of this spectral type is smaller than 20 m s -1 (Lo Curto et al. 2015), which is in agreement with the offset of 17 m s -1 found for a one-companion system. We A107, page 10 of 71 conclude that there is no evidence for the presence of a second companion.

Combining all the RV data points available and the absolute astrometry data with our MCMC, considering a one-companion system (Figs. D.27 and D.28), 300 000 iterations (burn-in = 30 000) and 1000 walkers, we find an eccentric brown dwarf with a mass of 19 +2 -1 M Jup , a semi-major axis of 6.4 ± 0.1 au (5 = 5172 ± 30 d), an eccentricity of 0.610 +0.004 -0.005 , and an orbital inclination of either 42 ± 2°or 131 ± 2°.

HD 89839

Ninety-eight RV data points were obtained with HARPS between 2004 and 2021 for the F7V star HD 89839. Moutou et al. (2011) reported a giant planet candidate based on the RV HARPS measurements obtained before June 2010 (Julian day: 2 455 353). However, this dataset does not fully cover the orbit of the companion, which is consequently poorly characterized. The reported orbital parameters are therefore poorly constrained, with a semi-major axis of 6.8 +3.3 -2.4 au and an eccentricity of 0.32 ± 0.20. The available data allow us to reasonably well constrain the amplitude of RV variations, corresponding to a minimum mass of 3.9 ± 0.4 M Jup .

The additional data points obtained between 2010 and 2021 now allow us to properly constrain the orbital parameters of HD 89839 b and, by simultaneously fitting all the RV data points available with the absolute astrometry with our MCMC (Figs. D.29 and D.30), and considering 300 000 iterations (burnin = 30 000) and 1000 walkers, we constrained the orbital inclination to either 53 +16 -9 °or 129 +9 -15 °. Thus, we find a semimajor axis of 4.9 ± 0.1 au (P = 3448 ± 26 d), an eccentricity of 0.20 ± 0.02, and a true mass of 5.2 ± 0.8 M Jup . Hence, HD 89839 b is a giant planet. M Jup , respectively. As the orbital period of HD 114783 b is much smaller than the duration of Gaia DR3, the proper motion induced by the planet can be neglected. We thus simultaneously fit all the RV data points available, corrected for the signal of the inner planet, with the absolute astrometry with our MCMC (Figs. D.31 and D.32), considering 300 000 iterations (burn-in = 100 000) and 1000 walkers. We find orbital parameters close to those reported by Rosenthal et al. (2021), with a semi-major axis of 5.0 ± 0.1 au (P = 4352 +88 -76 d) and an eccentricity of 0.05 +0.04 -0.03 . We constrained the orbital inclination of HD 114783 c to either 21 +7

-4 °or 159 +4 -6 °. We find a true mass of 2.0 ± 0.4 M Jup . Hence, HD 114783 c is a giant planet.

HD 140901

Four hundred and forty-three RV data points were obtained for the G7IV star HD 140901. 52 RV HARPS measurements were obtained between 2004 and 2007, 321 RV AAT measurements were obtained between 1998 and 2014, and 70 RV PFS measurements were obtained between 2011 and 2022. Considering all the RV data points available and the absolute astrometry, Feng et al. (2022) report a massive planet with a semi-major axis of 7.42 +0.32 -0.58 au, an inclination of 169.4 +2.2 -55.4 °, a mass of 6.3 +1.3 -5.0 M Jup , and an eccentricity of 0.61 +0.03 -0.04 . They also report the presence of an inner planet with a minimum mass of 0.049 +0.002 -0.008 M Jup located at 0.085 +0.003 -0.004 au. However, the study does not detail the analysis of the system. Although a significant peak is present in the periodogram of the data around ten days, once the signal of the external planet is subtracted the amplitude of the dispersion of the RV measurements is greater than the signal induced by the potential planet. It is not possible to confirm the presence of the planet.

A107, page 11 of 71 Philipot, F., et al.: A&A, 678, A107 (2023) In any case, as the orbital period of the planet candidate is much smaller than the duration of Gaia DR3, the proper motion induced by this potential planet is negligible. Thus, by simultaneously fitting the same RV dataset as Feng et al. (2022) and the absolute astrometry with our MCMC (Figs. D.33 and D.34), and by considering 400 000 iterations (burn-in = 100 000) and 1000 walkers, we find a semi-major axis of 11.8 +4.1 -2.5 au (P = 14 386 +8099 -4415 d), an inclination of either 40 +18 -11 °or 138 +12 -21 °, a mass of 1.8 ± 0.5 M Jup , and an eccentricity of 0.77 +0.06 -0.07 . This solution is within the error bars associated with the values found by Feng et al. (2022) and confirms that HD 140901 b is a giant planet.

HD 143361

One hundred and twenty RV data points were obtained for the G6V star HD 143361. 47 By simultaneously fitting all the available RV data points with the absolute astrometry with our MCMC (Figs. D.35 and D.36), and considering 300 000 iterations (burn-in = 50 000) and 1000 walkers, we find orbital parameters close to those reported by Jenkins et al. (2017), with a semi-major axis of 2.05 ± 0.03 au (P = 1040 ± 1) and an eccentricity of 0.198 +0.007 0.006 . We constrained the orbital inclination of HD 143361 b to either 50 +19

-12 °or 128 +18 -27 °. Thus, we find a true mass between 3.9 and 6.3 M Jup . Hence, HD 143361 b is a giant planet.

HD 167677

Forty-four RV data points were obtained with HARPS between 2005 and 2019 for this G5V star HD 167677. Moutou et al. (2011) reported a giant planet candidate with a minimum mass of 1.36 ± 0.12 M Jup , a semi-major axis of 2.90 ± 0.12 au, and an eccentricity of 0.17 ± 0.07. They considered the RV HARPS measurements obtained before October 2010 (Julian day: 2 455 495), which properly cover the period of the companion.

By simultaneously fitting all the available HARPS RV measurements with the absolute astrometry with our MCMC (Figs. D.37 and D.38), and considering 200 000 iterations (burnin = 50 000) and 1000 walkers, we find orbital parameters close to those reported by Moutou et al. (2011), with a semi-major axis of 2.9 ± 0.1 au (P = 1804 ± 73 d) and an eccentricity of 0.35 +0.25 -0.15 . We constrained the orbital inclination of HD 167677 b to either 20 +14 -6 °or 155 +6 -12 °. Thus, we find a true mass of 3.7 +1.6 -1.1 M Jup . Hence, HD 167677 b is a giant planet.

HD 169830

Two hundred and seventy-seven RV data points were obtained for the F7V star HD 169830. 86 RV HARPS measurements were obtained between 2004 and 2009, 106 RV CORALIE measurements were obtained between 1999 and 2003, and 85 RV HIRES measurements were obtained between 2000 and 2019. Firstly, Naef et al. (2001) reported a giant planet candidate with a minimum mass of 2.94 ± 0.12 M Jup , a semi-major axis of 0.82 au, and an eccentricity of 0.35 ± 0.04, considering the RV CORALIE measurements obtained before May 2000 (Julian day: 2 451 668).

A second giant planet candidate was then identified by Mayor et al. (2004) and characterized by Rosenthal et al. (2021), considering all available RV data points. They found a minimum mass of 3.51 ± 0.12 M Jup , a semi-major axis of 3.283 +0.035 -0.036 au, and an eccentricity of 0.257 ± 0.019 for HD 169830 c. Recently, combining all the RV data points with absolute astrometry, Feng et al. (2022) report an orbital inclination of 24.47 +12.74 -7.21 °and a true mass of 7.67 +1.94 -2.76 M Jup for HD 169830 c 7 . By simultaneously fitting the same RV dataset as Feng et al. (2022), corrected for the signal of HD 169830 b, and the absolute astrometry with our MCMC (Figs. D.39 and D.40), and considering 300 000 iterations (burn-in = 50 000) and 1000 walkers, we find a semi-major axis of 3.29 +0.04 -0.05 au (P = 1832 ± 7 d), an inclination of either 23 +12 -6 °or 158 +5 -9 °, a mass of 8.9 +2.8 -2.6 M Jup , and an eccentricity of 0.23 +0.03 -0.02 . This solution is within the error bars associated with the values found by Feng et al. (2022) and confirms that HD 169830 c is a giant planet.

HD 196050

One hundred and thirty-one RV data points were obtained for the G3V star HD 196050 A. 56 RV HARPS measurements were obtained between 2004 and 2021, 31 RV CORALIE measurements were obtained between 1999 and 2003, and 44 RV UCLES measurements were obtained between 1998 and 2005. Based on NACO high contrast imaging observations, Eggenberger et al. (2007) reported a binary companion orbiting at about 500 au from HD 196050 A and composed of an M1.5-M4.5 low-mass star with a mass of 0.29 ± 0.02 M ⊙ and an M2.5-M5.5 low-mass star with a mass of 0.19 ± 0.02 M ⊙ . Given the separation and mass of the HD 196050 B/C pair, their movement will induce negligible variations in RV and proper motion. Jones et al. (2002) reported a giant planet candidate with a minimum mass of 2.8 ± 0.5 M Jup , a semi-major axis of 2.4 ± 0.5 au, and an eccentricity of 0.19 ± 0.09, considering the RV UCLES measurements obtained before June 2002 (Julian day: 2 452 455). Considering the RV CORALIE measurements, Mayor et al. (2004) reported orbital parameters and a minimum mass for HD 196050 Ab close to those reported by Jones et al. (2002).

By simultaneously fitting all the available RV data points with the absolute astrometry with our MCMC (Figs. D.41 and D.42), and considering 300 000 iterations (burn-in = 30 000) and 1000 walkers, we improved the orbital parameters with a semi-major axis of 2.65 ± 0.03 au (P = 1392 ± 4 d) and an eccentricity of 0.20 ± 0.01. We constrained the orbital inclination of HD 196050 Ab to either 42 +11 -7 °or 141 +7 -12 °. Thus, we find a semimajor axis of 2.65 ± 0.03 au, an eccentricity of 0.20 ± 0.01, and a true mass of 4.7 ± 0.8 M Jup . Hence, HD 196050 Ab is a giant planet.

HD 204961

Two hundred and thirty-eight RV data points were obtained for the M 2/3V star HD 204961. 183 RV HARPS measurements were obtained between 2003 and 2019, 39 RV AAT measurements were obtained between 1998 and 2013, and 16 RV PFS measurements were obtained between 2011 and 2013. Bailey et al. (2009) reported a giant planet candidate with a minimum mass of 0.64 ± 0.06 M Jup and a period of 3416 ± 131 days. An inner super-Earth was reported by Wittenmyer et al. (2014) with a minimum mass of 5.4 ± 1 M Earth ; however, the signal 7 As the orbital period of HD 169830 b is much smaller than the duration of Gaia DR3, the proper motion induced by this planet is negligible.

A107, page 12 of 71 Philipot, F., et al.: A&A, 678, A107 (2023) corresponding to this potential inner planet was then identified as corresponding to the rotation period of the host star by Gorrini et al. (2022).

By simultaneously fitting all the available RV data points with the absolute astrometry with our MCMC (Figs. D.43 and D.44), and considering 300 000 iterations (burn-in = 30 000) and 1000 walkers, we find orbital parameters close to those reported by Gorrini et al. (2022), with a semi-major axis of 3.7 ± 0.1 au (P = 3853 +51 -47 d) and an eccentricity of 0.05 ± 0.03. We constrained the orbital inclination of HD 204961 b to either 51 ± 3°or 134 ± 3°. We find a true mass of 0.99 +0.09 -0.08 M Jup . Hence, HD 204961 b is a giant planet.

HD 216437

One hundred and sixty RV data points were obtained for the G1V star HD 216437. 100 RV HARPS measurements were obtained between 2007 and 2021, 31 RV CORALIE measurements were obtained between 1999 and 2003, and 39 RV UCLES measurements were obtained between 1998 and 2005. Jones et al. (2002) reported a giant planet candidate with a minimum mass of 2.1 ± 0.3 M Jup , a semi-major axis of 2.4 ± 0.5 au, and an eccentricity of 0.33 ± 0.09, considering the RV UCLES measurements obtained before June 2002 (Julian day: 2 452 456). Considering the RV CORALIE measurements, Mayor et al. (2004) reported orbital parameters and minimum mass for HD 216437 b close to those reported by Jones et al. (2002).

By simultaneously fitting all the available RV data points with the absolute astrometry with our MCMC (Figs. D.45 and D.46), and considering 400 000 iterations (burn-in = 100 000) and 1000 walkers, we improved the orbital parameters and constrained the orbital inclination of HD 216437 b to either 36 +8 -6 °or 148 +5 -7 °. Thus, we find a semi-major axis of 2.57 ± 0.04 au (P = 1359 ± 1 d), an eccentricity of 0.31 ± 0.01, and a true mass of 4.2 ± 0.7 M Jup . Hence, HD 216437 b is a giant planet.

HD 221420

Two hundred and three RV data points were obtained for the G1V star HD 221420. 77 RV HARPS measurements were obtained between 2003 and 2018, 88 RV AAT measurements were obtained between 1998 and 2015, and 38 RV PFS measurements were obtained between 2012 and 2021. Kane et al. (2019) report a giant planet candidate with a minimum mass of 9.7 +1.1 -1.0 M Jup , a semi-major axis of 18.5 ± 2.3 au, and an eccentricity of 0.42 +0.05 -0.07 , considering the RV AAT measurements. Recently, combining the RV AAT and HARPS measurements with absolute astrometry, Li et al. (2021) report an orbital inclination of either 17.8 +2.9

-2.8 °or 162.2 +2.8 -2.9 °and a true mass of 20.6 +2.0

-1.6
M Jup , corresponding to a brown dwarf. Moreover, they obtain a better constraint on the other orbital parameters and find a semi-major axis of 9.99 +0.74 -0.70 au and an eccentricity of 0.162 +0.035 -0.030 . By simultaneously fitting all the available RV data points with the absolute astrometry with our MCMC (Figs. D.47 and D.48), and considering 300 000 iterations (burn-in = 50 000) and 1000 walkers, we find a semi-major axis of 10.1 ± 0.7 au (P = 10 066 +929 -1125 d), an inclination of either 14 ± 1°or 162 ± 2°, a mass of 22 ± 2 M Jup , and an eccentricity of 0.12 +0.04 -0.03 . This solution is within the error bars associated with the values found by Li et al. (2021) and confirms that HD 221420 B is a brown dwarf.

HIP 70849

Fifty-nine RV data points were obtained with HARPS between 2006 and 2021 for the K7V star HIP 70849. Ségransan et al. (2011) reported the detection of a very poorly constrained companion with a minimum mass between 3 and 15 M Jup , a semi-major axis between 4.5 and 36 au, and an eccentricity between 0.47 and 0.96 (3σ confidence interval), considering the RV HARPS measurements obtained before June 2010 (Julian day: 2 455 374). In Philipot et al. (2023), we already used our MCMC (Fig. D.49) to combine available HARPS data points with absolute astrometry, considering 300 000 iterations (burn-in = 30 000) and 1000 walkers. We found a semi-major axis of 3.99 +0.06 -0.07 au (P = 3649 ± 18 d), an inclination of 96 ± 16°, a mass of 4.5 +0.4 -0.3 M Jup , and an eccentricity of 0.65 +0.02 -0.01 , confirming that HIP70849 b is a giant planet. In this study, as we consider the same dataset and the same fitting tools as Philipot et al. (2023), we obtain the same solution.

Short-period companions (P < 1000 d)

Four companions (HD 44219 b, HD 100777 b, HD 111998 b, and HD 215497 c) have an orbital period smaller than the duration of Gaia data as delivered in the DR3. It is therefore not possible to precisely determine their inclination and hence their true mass from the variations of proper motion. We therefore fit only the radial velocities with I fixed at 90°and ω fixed at 0°to obtain the other orbital parameters and the minimum mass of the four companions. We then used GASTON to estimate the maximum orbital inclination and the maximum mass, which can explain the AEN measured by the Gaia DR3.

HD 44219

Sixty-five RV data points were obtained with HARPS between 2003 and 2021 for the G3V star HD 44219. Naef et al. (2010) reported a giant planet candidate with a minimum mass of 0.58 +0.06 -0.04 M Jup , a semi-major axis of 1.19 ± 0.02 au, and an eccentricity of 0.61 +0.07 -0.09 , considering the HARPS data points obtained before April 2009 (Julian day: 2 454 932).

By fitting all the HARPS data points available with our MCMC, and considering 200 000 iterations (burn-in = 50 000) and 1000 walkers (Fig. D.50), we find orbital parameters close to those reported by Naef et al. (2010), with a semi-major axis of 1.26 +0.02 -0.07 au (P = 472 +3 -4 d) and an eccentricity of 0.41 +0.12 -0.14 . Using Gaston, we could estimate that the orbital inclination of HD 44219 b is between 4°and 176°(confidence interval at 3σ), and thus that the maximum mass of the planet is 11 M Jup . Hence, HD 44219 b is a giant planet.

HD 100777

Thirty-seven RV data points were obtained with HARPS between 2004 and 2007 for the G8V star HD 100777. Naef et al. (2007) reported a giant planet candidate with a minimum mass of 1.16 ± 0.03 M Jup , a semi-major axis of 1.03 ± 0.03 au, and an eccentricity of 0.36 ± 0.02, considering all the available HARPS data.

By fitting the same dataset as the one considered by Naef et al. (2007) with our MCMC, and considering 200 000 iterations (burn-in = 50 000) and 1000 walkers (Fig. D.50), we find orbital parameters close to those reported by Naef et al. (2007), with a semi-major axis of 1.06 +0.02 -0.01 au (P = 383 ± 1 d) and an eccentricity of 0.38 ± 0.02. Using Gaston, we could estimate that the orbital inclination of HD 100777 b is between 4°and 176°( confidence interval at 3σ), and thus that the maximum mass of the planet is 18 M Jup . Hence, the use of the AEN measured by Gaia does not allow us to determine with certainty the nature of A107, page 13 of 71 Philipot, F., et al.: A&A, 678, A107 (2023) the companion. Moreover, it is important to note that the PMa does not seem to agree with that induced by HD 100777 b. This difference could be explained by the presence of an external companion. However, there is no significant signal present in the RV data. This could be due to the short RV temporal baseline (∼1200 d).

HD 111998

One hundred and fifty RV data points were obtained with the HARPS spectrograph between 2006 and 2014 for HD 111998. As HD 111998 is a fast-rotating F6V star, the HARPS DRS is not able to properly compute the radial velocity of the star. For this reason, Borgniet et al. (2017) used the SAFIR (Spectroscopic data via Analysis of the Fourier Interspectrum Radial velocities) software (Galland et al. 2005) to compute the RV. They report a giant planet candidate with a minimum mass of 4.51 ± 0.50 M Jup , a semi-major axis of 1.82 ± 0.07 au, and an eccentricity of 0.03 ± 0.04.

By fitting the same dataset as the one considered by Borgniet et al. (2017) with our MCMC, and considering 300 000 iterations (burn-in = 100 000) and 1000 walkers (Fig. D.50), we find orbital parameters close to those reported by Borgniet et al. (2017), with a semi-major axis of 1.91 +0.02 -0.03 au (P = 810 +6 -5 d) and an eccentricity of 0.13 +0.05 -0.04 . Using Gaston, we could estimate that the orbital inclination of HD 111998 b is between 23°and 154°(confidence interval at 3σ), and thus that the maximum mass of the planet is 12.8 M Jup . Hence, HD 111998 is a giant planet. Morover, it is important to note that, as for HD 100777, the PMa measured for HD 111998 does not seem to agree with that induced by the HD 111998 b. This difference could be due to an additional companion, which could explain the long-term trend reported in Borgniet et al. (2017).

HD 215497

One hundred and fifteen RV data points were obtained with HARPS between 2004 and 2009 for the K3V star HD 215497. Lo Curto et al. ( 2010) reported a super-Earth candidate with a minimum mass of 6.6 M Earth , a semi-major axis of 0.047 au, and en eccentricity of 0.16 ± 0.09 and a giant planet candidate with a minimum mass of 0.33 M Jup , a semi-major axis of 1.28 au, and an eccentricity of 0.49 ± 0.04, considering all the available HARPS data points.

HD 215467 b is not massive enough to induce a significant PMa or AEN. We have therefore considered only HD 215497 c. By fitting the HARPS data points, corrected for the signal of HD 215497 b, with our MCMC, and considering 400 000 iterations (burn-in = 100 000) and 1000 walkers (Fig. D.50), we find a semi-major axis of 1.31 ± 0.02 au (P = 566 ± 4 d), a minimum mass of 0.35 ± 0.02 M Jup , and an eccentricity of 0.47 +0.03 -0.04 . The solution found by Lo Curto et al. ( 2010) is within the error bars associated with our values. Using Gaston, we could estimate that the orbital inclination of HD 215467 c is between 4°and 176°( confidence interval at 3σ), and thus that the maximum mass of the planet is 5.0 M Jup . Hence, HD 215497 c is a giant planet.

Stellar companions

Among the 116 selected stars, we detect and confirm the nature of 27 stellar companions, including 12 new detections (Table C.3). These companions orbit between 0.56 and 90 au and have masses between 0.1 and 1.1 M ⊙ (uncertainties included).

Even if the addition of absolute astrometry can allow us to lift the sin(I) indetermination and determine the true mass of a companion, the fit of the variations of the proper motion of a star does not always allow us to choose between a prograde and a retrograde orbit for the companion. For almost all the systems presented in this study, when the orbital period is properly constrained we find very close semi-major axes and masses for the prograde and retrograde solutions. One exception is the system HIP 39470, for which the 32 RV data obtained with HARPS between 2004 and 2019 do not fully cover the orbital period of the companion. Thanks to the significant PMa of the star, adding the absolute astrometry allows us to significantly improve the constraints on the companion's orbital parameters compared to the RV alone. However, considering a prograde and a retrograde solution (I = 22 +2 -3 °and I = 170 ± 1°respectively), we find two different solutions, with a semi-major axis of 8.8 ± 0.2 or 7.6 ± 0.1 au and a mass of 0.138 +0.007 -0.008 or 0.147 ± 0.005 M ⊙ , respectively. In the two cases, we find that the new companion HIP 39470 B is a stellar companion. The epoch astrometry of Gaia, expected with the fourth data release (at the end of 2025), or HCI observation, when possible, could constrain the exact orbital inclination of the companions and significantly improve the characterization of HIP 39470 B.

The study of these stellar mass companions shows us the importance of properly determining the orbital inclination of a companion. Indeed, using only RV data, the minimum masses found for three of these companions were in the brown dwarfs' regime. Indeed, we find a minimum mass of about 37 and 52 M Jup for the new companions HD 56380 B and HD 221638 B, and [START_REF] Moutou | [END_REF] reported a minimum mass of about 18 M Jup for HD 131664 B. However, coupling the RV data with absolute astrometry, we find an inclination of either 6.1 ± 0.1°o r 173.6 ± 0.1°, either 31 ± 1°or 150 ± 1°, and either 9.3 ± 0.3°o r 170.4 ± 0.3°, respectively, corresponding to a true mass of 0.39 ± 0.02, 0.132 ± 0.006, and 0.109 ± 0.005 M ⊙ (410 ± 19, 138 ± 6, and 114 ± 5 M Jup ), respectively. These three companions are thus, in reality, low-mass stars. We note that Feng et al. (2021) had already identified HD 131664 B as a stellar companion by coupling RV HARPS measurements with absolute astrometry.

Moreover, in most cases, when the period of the companion is much larger than the available RV baseline, the orbital parameters and the mass of the companion cannot be properly characterized. In these cases, the addition of relative astrometry significantly improves the constraint on the orbit of the companion and, consequently, its mass. Good examples are the cases of GJ680 B and HD 111031 B. Feng et al. (2022) combine RV data points obtained with HARPS between 2004 and 2012 for GJ680, and with HIRES between 1997 and 2016 for HD 111031, and absolute astrometry. They report a semi-major axis of 10.1 +1.8 -1.7 and 13.1 (Dalba et al. 2021). In this study, we consider the same RV dataset for GJ680 and, for HD 111031, we consider the RV HARPS measurements obtained between 2004 and 2013, the RV HIRES data obtained between 1997 and 2020, the RV APF measurements obtained between 2013 and 2020, and the RV LICK measurements obtained in 2001. Combining these RV data with absolute astrometry and relative astrometry data, we find significantly different results from those published by Feng et al. (2022) for the two companions. We find semi-major A107, page 14 of 71 Philipot, F., et al.: A&A, 678, A107 (2023) Fig. 11. Semi-major axis and masses of the different substellar companions. For known companions, the dotted black lines enable the solutions obtained in this study, represented by a star, to be compared with those obtained in previous studies, represented by a square. The orange arrow corresponds to the maximum mass of the planet at 3σ found with Gaston. The dotted gray horizontal line corresponds to the deuterium burning limit (∼13 M Jup ).

axes of 32 +9

-6 and 21.1 ± 0.6 au and true masses of 0.178 ± 0.004 and 0.129 ± 0.003 M ⊙ (186 ± 4 and 135 ± 3 M Jup ), respectively, corresponding to low-mass stars instead of a brown dwarf.

As seen above, the algorithm used for this study, based on the MCMC sampling tool used by Lagrange et al. (2023), allows us to obtain a better exploration of the mass and orbital values compatible with the data. For example, in the case of GJ680 B, the orbit of which is poorly constrained, we obtain, by considering only RV and absolute astrometry data, solutions corresponding to a 1σ (resp. 3σ) confidence interval for the semi-major axis and the companion mass between 16 and 28 au (resp. 12 and 35 au) and between 70 and 160 M Jup (resp. 50 and 190 M Jup ), respectively. We notice that the solutions found by adding the HCI observations are well explored by the MCMC, but it is not possible without the imaging to come to any conclusions about the orbital parameters and the mass of the companion.

Finally, thanks to the HCI observations of HD 93351 obtained with NACO, we find that the companion is actually a stellar binary with a combined mass of 0.70 ± 0.05 M ⊙ . However, the combination of RV, HCI, and absolute astrometry data does not allow us to properly determine the orbital parameters of the binary. We can only obtain an estimate for the semi-major axis, with a solution at 83 +18 -19 au.

Conclusion

Using the PMa of the stars as given by Gaia DR3 and HIPPARCOS, observed with HARPS RV data points spread over at least 1000 days, we identified good candidates to host longperiod substellar companions, which allowed us to optimize our search for substellar companions. We detect at least one companion, stellar or substellar, for 86% of the selected stars, including systems hosting multiple companions as well as those with companion's orbit poorly constrained. Moreover, 23% of the systems are composed of at least one confirmed substellar companion (41% considering companions detected in multiple systems with a minimum mass smaller than 80 M Jup ). This is significantly higher than the detection rates obtained in the case of the large RV surveys (Mayor et al. 2011;Wittenmyer et al. 2020;Rosenthal et al. 2021), which do not use selection criteria to optimize the detection of substellar companions. Among our sample, we have detected three new brown dwarfs (GJ 660.1 C, HD 73256 C, and HD 165131 B) and six new planets (HD 75302 b, HD 108202 b, HD 135625 b, HD 185283 b, HIP 10337 b, and HIP 54597 b). As already demonstrated in the direct imaging study (Bonavita et al. 2022a, Swimmer et al. 2022, Kuzuhara et al. 2022), we confirm that the study of the PMa enables the selection of targets for the search of substellar companions to be optimized. However, this method remains sensitive only to massive objects (typically >1 M Jup ) and is not adapted for the detection of low-mass planets (super-Earths and mini-Neptunes).

Combining RV data with absolute astrometry data allows us to properly characterize the orbital parameters of these ten new companions and in particular their orbital inclination. We thus determine their true mass and their exact nature. Moreover, by applying the same method, we are able to improve the characterization and determine precisely the true mass of ten known substellar companions and, using GASTON, we are able to confirm the planetary nature of three known candidate planets (Fig. 11). We determined the properties of 25 stellar companions, A107, page 15 of 71 Philipot, F., et al.: A&A, 678, A107 (2023) including 12 new detections. We show also that five companions previously reported as brown dwarfs are indeed low-mass stars: GJ 680 B, HD 56380 B, HD 111031 B, HD 131664 B, and HD 221638 B.

The coupling of HIPPARCOS/Gaia measurements with RV data does not always permit the accurate characterization of the orbit of a companion, in particular when its period is not completely covered by the RV data. The addition of HCI data allows for better constraining of the orbit of the companion and, consequently, measuring its mass. However, most of the companions revealed in this study have not been detected or observed in imaging. Thus, neither the orbital parameters nor the exact nature of 27 of the 80 single companions found in our sample can be determined.

In summary, we conclude that studying the PMa of stars allows the search for substellar companions in RV to be optimized so that they can then be properly characterized by combining RV, absolute astrometry, and, when available, relative astrometry data. However, this method is not sensitive to lowmass planets and therefore does not enable Earth-like planets to be searched for. Ghazaryan et al. (2019). 16 Ammler-von Eiff & Reiners (2012). 17 Rice & Brewer (2020). 18 Borgniet et al. (2017). 19 Costa Silva et al. (2020). 20 Hojjatpanah et al. (2019). 21 Sousa et al. (2018). 22 Brandt (2021). 23 Schneider et al. (2011). 24 Maldonado et al. (2020). 25

Appendix C: Additional results

Table C.1: Summary of posteriors obtained with our MCMC algorithm for known planets. The median and 1σ confidence interval are given for each parameter. * corresponds to the solutions found considering only the RV data points. The reported masses are therefore the minimum masses. In these cases, the maximum value of the true mass of the companions, estimated with Gaston, with a confidence index of 3σ, are noted between parentheses.

) C07 = 3 ± 2 Hir94 = -2 ± 3 C98 = 61348 +2 -1 AAT = 0 ± 1 UCLES = 0 ± 1 AAT = 43 +4 -5 -35 ± 1 Hir04 = -2 +2 -1 UCLES = 0 ± 1 PFS = -12 ± 1 C98 = -2276 ± 1 PFS = 25 +4 -6
A107, page 24 of 71 Notes: HG corresponds to (HIPPARCOS/Gaia) absolute astrometry data. For HD42659 B, the reported mass is the minimum mass.

  Fig. 1. Images of new stellar companions detected in HCI. The observations considered come from the NACO and SPHERE ESO archives.

Fig. 2 .

 2 Fig. 2. Fit of the GJ660.1 A RV measurements. The black curve corresponds to the best fit. The color bar indicates the log-likelihood corresponding to the different fits plotted.

  The median and 1σ confidence interval are given for each parameter. ( * ) Values obtained with Gaston.

  the corner plots are available in the appendix (Figs. D.13 and D.14). 4.1.3. HD 165131 Sixty-nine RV data points were obtained with the HARPS spectrograph between 2006 and 2021 for the G3/5V star HD 165131. A periodicity is clearly present in the periodogram of the data, with a peak at about 2350 days. Using DPASS, we find the best solution, corresponding to a brown dwarf candidate with a minimum mass of 18 M Jup and a period of 2344 days (Fig. D.5).

Fig. 3 .

 3 Fig. 3. Fit of the orbit of HD 73256. Top: fit of the HD 73256 RV measurements after subtracting the signal of the inner planet. Bottom: fit of the HD 73256 astrometric acceleration in right ascension (left) and declination (right). The black points correspond to the HIPPARCOS and Gaia EDR3 proper motion measurements. In each plot, the black curve corresponds to the best fit. The color bar indicates the log-likelihood corresponding to the different fits plotted.

  Fig. 4. Fit of the orbit of HD 165131. Top: fit of the HD 165131 RV measurements. Bottom: fit of the HD 165131 astrometric acceleration in right ascension (left) and declination (right). The black points correspond to the HIPPARCOS and Gaia EDR3 proper motion measurements. In each plot, the black curve corresponds to the best fit. The color bar indicates the log-likelihood corresponding to the different fits plotted.

  the corner plot is available in Appendix D (Fig. D.16).

Fig. 5 .

 5 Fig. 5. Fit of the orbit of HD 75302. Top: fit of the HD 75302 RV measurements. Bottom: fit of the HD 75302 astrometric acceleration in right ascension (left) and declination (right). The black points correspond to the HIPPARCOS and Gaia EDR3 proper motion measurements. In each plot, the black curve corresponds to the best fit. The color bar indicates the log-likelihood corresponding to the different fits plotted.

  corner plot is available in Appendix D (Fig. D.19).

  corner plot is available in Appendix D (Fig. D.22).

Fig. 6 .

 6 Fig. 6. Fit of the orbit of HD 108202. Top: fit of the HD 108202 RV measurements. Bottom: fit of the HD 108202 astrometric acceleration in right ascension (left) and declination (right). The black points correspond to the HIPPARCOS and Gaia EDR3 proper motion measurements. In each plot, the black curve corresponds to the best fit. The color bar indicates the log-likelihood corresponding to the different fits plotted.

Fig. 7 .

 7 Fig. 7. Fit of the orbit of HD 135625. Top: fit of the HD 135625 RV measurements. Bottom: fit of the HD 135625 astrometric acceleration in right ascension (left) and declination (right). The black points correspond to the HIPPARCOS and Gaia EDR3 proper motion measurements. In each plot, the black curve corresponds to the best fit. The color bar indicates the log-likelihood corresponding to the different fits plotted.

Fig. 8 .

 8 Fig. 8. Fit of the orbit of HD 185283. Top: fit of the HD 185283 RV measurements. Bottom: fit of the HD 185283 astrometric acceleration in right ascension (left) and declination (right). The black points correspond to the HIPPARCOS and Gaia EDR3 proper motion measurements. In each plot, the black curve corresponds to the best fit. The color bar indicates the log-likelihood corresponding to the different fits plotted.

Fig. 9 .

 9 Fig. 9. Fit of the orbit of HIP 10337. Top: fit of the HIP 10337 RV measurements. Bottom: fit of the HIP 10337 astrometric acceleration in right ascension (left) and declination (right). The black points correspond to the HIPPARCOS and Gaia EDR3 proper motion measurements. In each plot, the black curve corresponds to the best fit. The color bar indicates the log-likelihood corresponding to the different fits plotted.

Fig. 10 .

 10 Fig. 10. Fit of the orbit of HIP 54597. Top: fit of the HIP 54597 RV measurements. Bottom: fit of the HIP 54597 astrometric acceleration in right ascension (left) and declination (right). The black points correspond to the HIPPARCOS and Gaia EDR3 proper motion measurements. In each plot, the black curve corresponds to the best fit. The color bar indicates the log-likelihood corresponding to the different fits plotted.

  5.1.5. HD 114783 Two hundred and eighty-two RV data points were obtained for the K1V star HD 114783. 91 RV HARPS measurements were obtained between 2004 and 2016, 157 RV HIRES measurements were obtained between 1998 and 2019, and 34 RV HRS measurements were obtained between 2004 and 2007. Firstly, Vogt et al. (2002) reported a giant planet candidate with a minimum mass of 1 M Jup and a period of 501 days. Bryan et al. (2016) report an outer companion with a minimum mass of 0.611 +0.056 -0.053 M Jup and a period of 4319 +151 -130 days. Considering the RV HIRES measurements, Rosenthal et al. (2021) report a two planets system at 1.164 ± 0.016 au and 4.97 +0.12 -0.11 au (P = 4344 +33 -14 d), with a minimum mass of 1.033 +0.034 -0.033 M Jup and 0.660 +0.046 -0.047

  Fig. C.1: Semi-major axis and masses of the different stellar companions.For known companions, when previous characterization is available, the dotted lines allow the solutions obtained in this study to be compared with those obtained in previous studies. The dotted gray line corresponds to the hydrogen burning limit (∼80 M Jup ).

Fig. D. 11 :

 11 Fig. D.11: Fit of the HD75302 RV measurements before (left) and after (right) correction of the star's short-term activity.

Table 2 .

 2 New relative astrometry.

	Companion	JD -2 400 000 SEP (mas)	PA (deg)
	HD 1388 B	53 940.39	1490 ± 10	85.6 ± 1
	HD 21175 B	57 665.35	2628.0 ± 2.5 122.75 ± 0.08
	HD 78612 B	53 739.29	613 ± 5	272.3 ± 1
	HD 93351 B/C	56 093.02	1684 ± 30	76.3 ± 1
	HD 207700 B	56 092.36	1090 ± 20	284.2 ± 1

Table 3 .

 3 Summary of posteriors for new brown dwarfs.

	Parameter	GJ660.1 C	HD 73256 C	HD 165131 B
						-0.07
	P (days)	618.6 ± 0.1	2690 +60 -102	2343 ± 2
	Ecc	0.65 +0.11 -0.08	0.16 ± 0.07	0.672 ± 0.003
	I (°)	87 +39 -43	( * )	29 +5 -3 or 152 +8 -7	93 +39 -43
	Mass (M Jup )	78 +38 -16	( * )	16 ± 1	19 +2 -1
	Ω (°)	112 +122 -123	( * )	303 +5 -6 or 269 +8 -7	141 +20 -19
	ω (°)	188 +1 -2	300 +37 -53	3.1 ± 0.4
	P time (days) √ ecc cos(ω) √ ecc sin(ω)	540 +2 -3 -0.80 +0.06 -0.07 -0.12 +0.02 -0.01	244 +134 -179 0.42 +0.08 -0.12 -0.07 +0.13 -0.14	1588 ± 2 0.818 +0.002 -0.001 0.044 ± 0.006
	Jitter (m s -1 )	3.4 +0.6 -0.5	23 +3 -2	5.6 ± 0.6
	rms (m s -1 )	4.6 +1.6 -0.2	24.2 +3.8 -1.6	6.3 +0.2 -0.1

a (au)

1.12 ± 0.02 3.8 ± 0.1 3.59

+0.06

  and the corner plot is available in Appendix D (Fig. D.18).

	4.2. New planets
	4.2.1. HD 75302
	Eighty-two RV data points were obtained for this G5V star,
	HD 75302. 35 RV HARPS measurements were obtained between
	2012 and 2018, 26 RV ELODIE measurements were obtained
	between 1997 and 2005, and 21 RV SOPHIE measurements were
	obtained between 2008 and 2018. A periodicity appears in the
	periodogram of the data, with a weak peak around 2000 days
	(Fig. D.10). Using DPASS, we find the best solution, correspond-
	ing to an eccentric planet candidate with a period of 4300 days,

Table 4 .

 4 Jup . The posteriors obtained for each free parameter of the MCMC are reported in Table 4 and the corner plot is available in Appendix D (Fig. D.17). Summary of posteriors for new planets.

	+0.04 -0.03 ,

  RV HARPS measurements were obtained between 2007 and 2019, 44 RV CORALIE measurements were obtained between 2010 and 2014, and 29 RV MIKE measurements were obtained between 1998 and 2005. Jenkins et al. (2017) report a giant planet candidate with a minimum mass of 3.48 ± 0.24 M Jup , a semi-major axis of 1.98 ± 0.07 au, and an eccentricity of 0.193 ± 0.015, considering the RV MIKE and CORALIE measurements and the RV HARPS measurements obtained before June 2013 (Julian day: 2 456 462).

Table A .

 A 2: Table A.1 continued.

					Philipot, F., et al.: A&A, 678, A107 (2023)
	Star	σ PMa a Mb at 10au	Parallax b	µ α Hip	µ δ Hip	µ α EDR3	µ δ EDR3	µ α Hip-EDR3	µ δ Hip-EDR3	No. of
			(MJup)	(mas)	(mas/yr)	(mas/yr)	(mas/yr)	(mas/yr)	(mas/yr)	(mas/yr)	companion(s)
	HD129191	> 4	11	18.4622 ± 0.0242	26.520 ± 0.042	-152.832 ± 0.035	26.278 ± 1.394	-152.293 ± 1.540	26.058 ± 0.039	-152.433 ± 0.038	1 *
	HD131664	> 4	99	19.1360 ± 0.0829	8.008 ± 0.105	22.284 ± 0.126	14.979 ± 0.710	28.685 ± 0.740	11.370 ± 0.022	25.899 ± 0.023
	HD131977	> 4	3.7	169.8843 ± 0.0653 1031.472 ± 0.093 -1723.619 ± 0.075	1035.702 ± 1.343	-1725.446 ± 1.007 1032.968 ± 0.051 -1724.781 ± 0.033
	HD135625	2.0	0.1	18.9018 ± 0.0191	72.385 ± 0.026	-16.574 ± 0.027	72.305 ± 0.974	-17.487 ± 0.728	72.283 ± 0.023	-16.433 ± 0.016
	HD140901	2.0	0.1	26.2048 ± 0.0179	-4.040 ± 0.019	-176.046 ± 0.025	-3.664 ± 0.508	-176.463 ± 0.808	-4.053 ± 0.015	-176.132 ± 0.022
	HD142070	> 4	81	5.5771 ± 0.0307	-14.315 ± 0.043	-24.244 ± 0.033	-15.266 ± 1.073	-25.030 ± 1.016	-13.895 ± 0.031	-23.580 ± 0.023
	HD143361	3.0	3.0	14.5456 ± 0.0202 -156.561 ± 0.026 -120.231 ± 0.019	-157.333 ± 1.362	-119.387 ± 1.039 -156.630 ± 0.040 -120.369 ± 0.027
	HD150139	2.3	0.1	20.5407 ± 0.0251	139.201 ± 0.044	-143.615 ± 0.037	138.903 ± 0.807	-142.494 ± 0.594	139.101 ± 0.031	-143.648 ± 0.023	1 *
	HD156079	> 4	4.4	17.5648 ± 0.0239	-69.179 ± 0.031	-165.076 ± 0.023	-69.736 ± 0.909	-164.554 ± 0.561	-68.923 ± 0.028	-165.238 ± 0.015
	HD156274	> 4	9.9	113.7513 ± 0.0725 1029.609 ± 0.117	106.935 ± 0.101	1036.484 ± 1.039	109.036 ± 0.520	1033.069 ± 0.039	107.932 ± 0.021	1 *
	HD165131	> 4	15	17.2691 ± 0.0317	-61.918 ± 0.043	-124.587 ± 0.030	-59.570 ± 1.126	-125.994 ± 0.717	-62.476 ± 0.036	-124.074 ± 0.023
	HD166724	3.2	1.6	37.4641 ± 0.0253	-43.140 ± 0.040	72.728 ± 0.037	-43.593 ± 0.393	73.244 ± 0.361	-43.414 ± 0.013	72.873 ± 0.012	1 *
	HD167677	3.2	3.0	16.7894 ± 0.0166	33.127 ± 0.020	12.219 ± 0.017	33.530 ± 1.050	12.868 ± 0.828	33.235 ± 0.035	12.392 ± 0.027
	HD169830	2.0	0.1	27.1461 ± 0.1469	-0.341 ± 0.221	16.103 ± 0.158	-0.721 ± 0.881	15.434 ± 0.537	0.064 ± 0.023	16.374 ± 0.014
	HD171587	2.0	0.1	28.5668 ± 0.0217	126.024 ± 0.029	-193.681 ± 0.025	126.315 ± 0.938	-194.794 ± 0.733	125.979 ± 0.034	-193.715 ± 0.023
	HD174429	3.1	2.1	21.1621 ± 0.0223	16.272 ± 0.025	-85.519 ± 0.024	17.353 ± 1.217	-83.766 ± 0.830	16.081 ± 0.035	-85.590 ± 0.025
	HD179346	> 4	53	18.0318 ± 0.0942	-7.800 ± 0.126	-53.982 ± 0.116	-9.922 ± 0.877	-52.875 ± 0.720	-4.943 ± 0.030	-53.287 ± 0.021
	HD181433	> 4	2.1	37.0511 ± 0.0211 -230.723 ± 0.018	235.806 ± 0.025	-230.886 ± 0.841	235.382 ± 0.996	-230.958 ± 0.030	235.640 ± 0.029
	HD183414	2.2	0.2	36.1158 ± 0.0264	1.440 ± 0.037	-174.330 ± 0.042	2.701 ± 0.701	-174.656 ± 0.464	1.268 ± 0.023	-174.389 ± 0.015
	HD185283	2.3	0.8	31.9046 ± 0.0217 -163.887 ± 0.022	-53.650 ± 0.017	-162.481 ± 1.218	-53.718 ± 1.109	-163.982 ± 0.033	-53.707 ± 0.025
	HD191797	> 4	58	22.7336 ± 0.0272	-8.443 ± 0.038	51.173 ± 0.033	-12.621 ± 2.324	54.340 ± 1.456	-5.479 ± 0.051	48.047 ± 0.033
	HD195145	> 4	3.1	16.6547 ± 0.0305	4.132 ± 0.052	-4.200 ± 0.050	1.989 ± 0.769	-4.698 ± 0.481	4.050 ± 0.021	-4.430 ± 0.012
	HD195564	> 4	21	40.4241 ± 0.0497	309.736 ± 0.068	109.910 ± 0.051	307.694 ± 0.651	107.216 ± 0.518	308.366 ± 0.021	108.386 ± 0.012
	HD196050	> 4	6.1	22.2309 ± 0.0234 -219.316 ± 0.041 -179.612 ± 0.039	-219.148 ± 0.675	-180.370 ± 0.547 -219.413 ± 0.026 -179.984 ± 0.023
	HD196385	> 4	24	20.9103 ± 0.0239	73.036 ± 0.031	-16.412 ± 0.024	73.293 ± 0.772	-15.056 ± 0.445	73.633 ± 0.022	-15.383 ± 0.012	1 *
	HD202206	3.2	2.2	22.2420 ± 0.0740	352.541 ± 0.107	-31.590 ± 0.064	350.543 ± 0.977	-32.314 ± 0.509	352.754 ± 0.031	-31.388 ± 0.022
	HD204313	> 4	11	20.7705 ± 0.0343	42.751 ± 0.054	-270.443 ± 0.034	42.551 ± 0.747	-271.125 ± 0.483	42.234 ± 0.027	-270.727 ± 0.018
	HD204961	> 4	0.7	201.3252 ± 0.0237 -45.917 ± 0.032	-816.875 ± 0.025	-45.677 ± 1.028	-817.318 ± 0.656	-46.049 ± 0.030	-816.302 ± 0.025
	HD207700	> 4	11	26.0873 ± 0.0172 -196.563 ± 0.025 -437.609 ± 0.030	-195.605 ± 0.674	-438.053 ± 0.573 -195.753 ± 0.019 -437.915 ± 0.018
	HD207869	3.1	1.6	19.5789 ± 0.0118 -156.358 ± 0.014 -248.956 ± 0.017	-157.311 ± 0.951	-249.431 ± 0.807 -156.228 ± 0.032 -248.970 ± 0.030
	HD210797	> 4	13	15.4128 ± 0.0210	258.946 ± 0.027	-122.008 ± 0.024	258.354 ± 1.303	-118.366 ± 1.076	258.487 ± 0.037	-121.500 ± 0.036	1 *
	HD212036	> 4	69	19.1167 ± 0.0803	21.555 ± 0.105	-234.978 ± 0.116	29.075 ± 1.182	-224.715 ± 1.505	22.904 ± 0.036	-231.443 ± 0.033
	HD215257	> 4	6.0	23.6251 ± 0.0251	150.456 ± 0.035	333.617 ± 0.033	150.934 ± 0.889	331.705 ± 0.653	150.716 ± 0.026	333.292 ± 0.020	1 *
	HD215497	2.0	0.1	24.6569 ± 0.0152	-54.666 ± 0.016	-61.147 ± 0.019	-53.881 ± 0.939	-60.575 ± 0.933	-54.665 ± 0.031	-61.222 ± 0.033
	HD216437	2.8	1.7	26.9269 ± 0.0154	52.792 ± 0.025	215.141 ± 0.027	51.858 ± 0.767	214.317 ± 0.865	52.863 ± 0.026	214.857 ± 0.028
	HD218396	2.1	3.5	28.2075 ± 0.0230 -179.085 ± 0.037	-6.549 ± 0.023	-196.276 ± 10.121	-9.146 ± 5.480	-179.244 ± 0.344	-6.934 ± 0.226
	HD219834	> 4	0.1	173.5740 ± 0.0170 -135.692 ± 0.015 -719.178 ± 0.023	-137.136 ± 0.575	-713.779 ± 0.834 -136.426 ± 0.018 -715.027 ± 0.028
	HD221146	> 4	29	27.5348 ± 0.0247	-10.513 ± 0.033	-24.287 ± 0.024	-11.763 ± 1.093	-28.467 ± 0.843	-11.268 ± 0.030	-25.794 ± 0.022
	HD221420	> 4	16.3	32.1023 ± 0.0325	16.306 ± 0.056	0.736 ± 0.058	15.885 ± 0.437	1.647 ± 0.385	14.973 ± 0.014	0.455 ± 0.012
	HD221638	> 4	40	19.1599 ± 0.0269	56.624 ± 0.041	72.839 ± 0.042	52.210 ± 0.623	77.925 ± 0.609	55.789 ± 0.019	74.527 ± 0.019
	HD222237	> 4	3.7	87.3724 ± 0.0187	143.736 ± 0.030	-736.907 ± 0.032	141.756 ± 0.524	-736.300 ± 0.507	142.849 ± 0.018	-736.651 ± 0.017	1 *
	HD223238	2.5	0.1	17.8497 ± 0.0171	-1.916 ± 0.016	-202.994 ± 0.018	-2.808 ± 1.100	-202.424 ± 1.016	-1.814 ± 0.037	-203.140 ± 0.035
	HIP9603	> 4	109	18.8225 ± 0.0866 -111.175 ± 0.143	257.497 ± 0.147	-110.184 ± 0.933	245.727 ± 0.990	-119.933 ± 0.033	255.468 ± 0.033
	HIP10337	> 4	1.9	42.1225 ± 0.0167	375.454 ± 0.019	55.718 ± 0.020	377.499 ± 1.622	55.290 ± 1.164	375.597 ± 0.051	55.414 ± 0.040
	HIP39470	> 4	91	22.6284 ± 0.0325	16.231 ± 0.044	-82.449 ± 0.047	9.228 ± 1.155	-82.499 ± 1.131	18.669 ± 0.039	-76.357 ± 0.041
	HIP54597	2.3	0.1	19.3611 ± 0.0183	40.676 ± 0.019	53.190 ± 0.025	41.256 ± 0.462	54.595 ± 0.690	40.793 ± 0.016	53.317 ± 0.022
	HIP70849	> 4	4.6	41.4618 ± 0.0175	-44.051 ± 0.023	-201.577 ± 0.028	-47.003 ± 2.099	-203.284 ± 1.890	-44.428 ± 0.060	-202.047 ± 0.044
	HIP113201	> 4	132	68.7356 ± 0.0272	341.147 ± 0.037	-219.108 ± 0.034	343.238 ± 2.100	-218.067 ± 3.265	341.100 ± 0.055	-219.083 ± 0.063
										A107, page 19 of 71

Table A .

 A 3: Characteristics of the 53 stars with characterized companions. Notes: 1 Kervella et al. (2022). 2 Trifonov et al. (2020). 3 Gomes da Silva et al. (2021). 4 Reiners & Zechmeister (2020). 5 Liebing et al. (2021). 6 Stanford-Moore et al. (2020). 7 Astudillo-Defru et al. (2017). 8 Yee et al. (2017). 9 Gondoin (2020). 10 Boro Saikia et al. (2018). 11 Hojjatpanah et al. (2020). 12 Stelzer et al. (2013). 13 Llorente de Andrés et al. (2021). 14 Hojjatpanah et al. (2020). 15

	Name	HIP	Mass 1 (M ⊙ )	Distance 1 (pc)	Spectral 2 type	V 2 (mag)	logR ′ HK	Vsin(I) (km s -1 )	Age (Gyr)	χ 2 22
	GJ660.1	84212 0.43 ± 0.01 23.10 ± 0.21	M1V	11.62	-5.30 7	-	> 2 23		69
	GJ680	86057 0.47 ± 0.01 9.676 ± 0.003	M3V	10.13	-5.16 7	3.0 12	8.1 ± 4.2 24	8601
	HD1388	1444 1.18 ± 0.06 26.90 ± 0.02	G0V	6.50	-4.98 6	3.1 13	4.6 ± 1.7 25	4141
	HD16160	12114 0.80 ± 0.04	7.23 ± 0.02	K3V	5.60 3	-4.87 3	4.7 13	4.7 ± 3.9 13	6078
	HD16548 12350 1.31 ± 0.07 52.81 ± 0.07	G5V	6.98	-5.13 3	5.2 13	4.9 ± 0.3 25	11460
	HD16905 12436 0.85 ± 0.04 39.80 ± 0.02	K3V	9.46	-4.72 3	1.5 14	6.1 ± 4.7 25	184
	HD21175	15799 0.86 ± 0.04 17.68 ± 0.01	K0V	6.90	-4.74 6	1.8 14	3.7 +3.3 -1.7	6	69960
	HD28254 20606 1.10 ± 0.05 55.16 ± 0.08	G5V	7.68	-5.17 3	2.3 5	6.0 ± 1.3 25	10.3
	HD42659 29365 2.20 ± 0.11	128.5 ± 0.6	A3	6.75	-	19.0 15	-		15
	HD44219	30114 1.20 ± 0.06 52.84 ± 0.06	G3V	7.70	-5.04 3	2.2 13	8.4 ± 0.9 25	23
	HD46569	31079 1.50 ± 0.07 36.87 ± 0.07	F8V	5.57	-4.93 6	5.9 16	7.6 +3.2 -3.0	6	6232
	HD56380 34961 0.98 ± 0.05	53.1 ± 0.3	G8V	9.20	-5.00 3	0.5 14	12.2 ± 1.1 25	3697
	HD61383	37233 1.17 ± 0.06 53.05 ± 0.08	G3V	7.57	-5.02 3	2.7 13	11.4 ± 0.2 13	36110
	HD62364 36941 1.30 ± 0.06 52.95 ± 0.08	F7V	7.31	-4.95 3	3.6 13	3.9 ± 0.7 25	364
	HD73256	42214 1.00 ± 0.05 36.68 ± 0.04	G8IV	8.06	-4.46 5	3.50 13	2.2 ± 2.1 25	2040
	HD75302 43297 1.06 ± 0.05 30.29 ± 0.03	G5V	7.46 4	-4.62 6	0.46 17	2.1 +2.6 -1.1	6	299
	HD78612	44896 1.20 ± 0.06 40.85 ± 0.04	G3V	7.15	-4.98 3	1.6 13	10.2 ± 0.8 25	20060
	HD89839 50653 1.30 ± 0.06 50.10 ± 0.07	F7V	7.64	-4.94 3	4.2 14	1.6 ± 0.9 25	56
	HD93351 52720 0.98 ± 0.05 55.72 ± 0.05	G6V	9.14	-4.98 3	-	4.3 ± 3.9 13	143
	HD96116	54102 1.08 ± 0.05 57.05 ± 0.06	G3V	8.69	-4.69 3	1.7 13	2.1 ± 1.8 25	28020
	HD100777 56572 1.08 ± 0.05 49.52 ± 0.08	G8V	8.42	-5.09 3	1.8 13	5.7 ± 3.3 25	173
	HD101198 56802 1.33 ± 0.07 26.82 ± 0.03	F6.5V	5.48	-4.87 6	5 18	6.2 +3.2 -2.6	6	1529
	HD107094 60051 0.98 ± 0.05 53.54 ± 0.07	G5V	9.13	-4.83 3	1.8 13	8.6 ± 4.0 25	1225
	HD108202 60648 0.74 ± 0.04 38.65 ± 0.03	K4/5V	10.22	-4.50 3	-	6.5 ± 4.0 28	28
	HD111031 62345 1.17 ± 0.06 31.19 ± 0.02	G5V	6.87	-5.09 3	1.9 13	4.1 ± 1.6 25	8191
	HD111998 62875 1.40 ± 0.07 33.39 ± 0.05	F6V	6.11	-4.58 6	20.0 18	1.7 +3.4 -0.9	6	27
	HD114783 64457 0.90 ± 0.04 21.01 ± 0.02	K1V	7.55	-4.97 3	2.0 13	6.0 ± 4.9 25	33
	HD131664 73408 1.16 ± 0.06	52.2 ± 0.3	G3V	8.13	-4.85 5	3.0 13	1.2 ± 1.0 25	1823
	HD135625 74856 1.28 ± 0.06 56.58 ± 0.07	G3IV/V	7.71	-4.99 6	4.5 13	4.4 ± 0.9 25	7
	HD140901 77358 1.06 ± 0.05 15.24 ± 0.01	G7IV	6.01	-4.79 6	2.0 13	3.2 ± 2.8 25	18
	HD143361 78521 1.06 ± 0.05 68.62 ± 0.10	G6V	9.16	-5.01 5	0.68 5	6.3 ± 3.7 29	21
	HD165131 88595 1.10 ± 0.06	57.8 ± 0.1	G3/5V	8.41	-4.98 3	2.3 19	2.7 ± 2.0 25	264
	HD167677 89583 1.00 ± 0.05 54.59 ± 0.07	G5V	8.92	-4.98 3	0.7 19	11.5 ± 1.7 25	22
	HD169830 90485 1.40 ± 0.07	36.8 ± 0.2	F7V	5.90	-4.95 5	3.4 13	2.2 ± 0.2 25	12
	HD179346 94370 1.16 ± 0.06	55.4 ± 0.3	G0V	8.05	-4.84 3	3.8 13	0.79 ± 0.68 25	496
	HD185283 96861 0.80 ± 0.04 31.32 ± 0.02	K3V	8.95	-4.94 3	0.9 14	6.0 ± 4.7 25	9

Table A .

 A 4: Table A.3 continued.

				Philipot, F., et al.: A&A, 678, A107 (2023)
	Appendix B:
	Name	HIP	Mass 1 (M ⊙ )	Distance 1 (pc)	Spectral 2 type	V 2 (mag)	logR ′ HK	Vsin(I) (km s -1 )	Age (Gyr)		χ 2 22
	HD191797	99695 0.85 ± 0.04	43.94 ± 0.06	K0V	9.50	-4.37 3	3.6 13	4.6 ± 4.3	6461
	HD195564 101345 1.24 ± 0.06	24.71 ± 0.04	G2.5IV	5.65	-5.18 3	1.9 13	7.4 ± 0.3	1054
	HD196050 101806 1.27 ± 0.06	50.49 ± 0.05	G3V	7.49	-4.98 5	3.3 13	4.3 ± 0.9	655
	HD204961 106440 0.45 ± 0.01 4.966 ± 0.001	M2/3V	8.67	-5.18 7	2.1 20	8.1 ± 4.2	278
	HD207700 108158 1.16 ± 0.06	38.31 ± 0.03	G4V	7.43	-5.10 5	1.2 13	9.9 ± 1.6	655
	HD212036 110440 1.08 ± 0.05	52.2 ± 0.3	G5V	8.47	-4.86 6	1.3 14	5.7 ± 3.2	894
	HD215497 112441 0.92 ± 0.05	40.53 ± 0.02	K3V	8.95	-5.07 3	-	5.8 ± 4.9	4
	HD216437 113137 1.22 ± 0.06	26.68 ± 0.02	G1V	6.05	-5.04 9	3.7 13	4.9 ± 1.0 13	46
	HD221146 115951 1.24 ± 0.06	36.27 ± 0.04	G1V	6.89	-4.98 5	2.9 13	6.4 ± 1.1	2220
	HD221420 116250 1.34 ± 0.07	31.14 ± 0.04	G1V	6.89	-5.28 3	0.7 13	3.7 ± 0.5	541
	HD221638 116350 1.20 ± 0.06	52.15 ± 0.09	F6V	7.55	-4.86 3	7.2 13	2.2 ± 1.4	1586
	HIP9603	9603	0.60 ± 0.01	27.8 ± 0.1	K7V	11.10	-	-	-		6339
	HIP10337	10337 0.69 ± 0.01 23.725 ± 0.010	K7V	9.83	-4.43 10	3.2 5	4.0 +9.5 -2.8	8	62
	HIP39470	39470 0.69 ± 0.01	44.16 ± 0.07	M0	10.83	-	-	5.1 ± 4.6 10660
	HIP54597	54597 0.80 ± 0.04	39.51 ± 0.02	K5V	9.82	-5.04 11	0.5 14	4.3 ± 4.0 13	9
	HIP70849	70849 0.65 ± 0.01	24.10 ± 0.01	K7V	10.38 -4.48 10	0.3 21	1 -5 26	119
	HIP113201 113201 0.53 ± 0.01	23.5 ± 0.2	M4V	11.51	-4.42 7	-	1.2 ± 0.1	4869
									A107, page 21 of 71

Data considered for orbital fits

  Table B.1: RV data considered for orbital fits.

					Philipot, F., et al.: A&A, 678, A107 (2023)
	Star	Instrument ∆T (days) N obs	Reference	Star	Instrument ∆T (days) N o bs	Reference
	GJ660.1	HARPS	3649	59	ESO archive	HD140901	HARPS	52	ESO archive
	GJ680	HARPS	3008	39	ESO archive	HD140901	HARPS	52	ESO archive
	HD1388	HARPS	5082	212	ESO archive	HD140901	AAT	321	Feng et al. (2022)
	HD1388	HIRES	8357	53	Rosenthal et al. (2021)	HD140901	PFS	70	Feng et al. (2022)
	HD16160	HARPS	1776	229	ESO archive	HD143361	HARPS	59	ESO archive
	HD16160	HIRES	4858	146	Rosenthal et al. (2021)	HD143361 CORALIE	45	Jenkins et al. (2017)
	HD16160	APF	2216	252	Rosenthal et al. (2021)	HD143361	MIKE	17	Jenkins et al. (2017)
	HD16160	LICK	8153	81	Rosenthal et al. (2021)	HD165131	HARPS	69	ESO archive
	HD16548	HARPS	6333	52	ESO archive	HD167677	HARPS	44	ESO archive
	HD16548	LICK	1349	9	Fischer et al. (2014)	HD169830	HARPS	86	ESO archive
	HD16905	HARPS	6263	52	ESO archive	HD169830 CORALIE	106	Mayor et al. (2004) *
	HD21175	HARPS	1147	61	ESO archive	HD169830	HIRES	85	Rosenthal et al. (2021)
	HD28254	HARPS	6338	72	ESO archive	HD179346	HARPS	44	ESO archive
	HD42659	HARPS	1535	49	Hartmann & Hatzes (2015) HD185283	HARPS	78	ESO archive
	HD44219	HARPS	6353	65	ESO archive	HD191797	HARPS	42	ESO archive
	HD46569	HARPS	1297	63	ESO archive	HD195564	HARPS	95	ESO archive
	HD46569	LC	1925	53	Zechmeister et al. (2013)	HD195564	HIRES	56	Rosenthal et al. (2021)
	HD46569	VLC	2040	54	Zechmeister et al. (2013)	HD195564	APF	299 Rosenthal et al. (2021)
	HD56380	HARPS	6287	96	ESO archive	HD196050	HARPS	56	ESO archive
	HD61383	HARPS	6293	63	ESO archive	HD196050 CORALIE	31	Mayor et al. (2004) *
	HD62364	HARPS	6233	87	ESO archive	HD196050	UCLES	44	Butler et al. (2006) *
	HD73256	HARPS	2986	26	ESO archive	HD204961	HARPS	183	ESO archive
	HD73256 CORALIE	755	38	? *	HD204961	UCLES	32	Bailey et al. (2009) *
	HD73256	HIRES	4700	18	Butler et al. (2017) *	HD207700	HARPS	36	ESO archive
	HD75302	HARPS	2160	35	ESO archive	HD212036	HARPS	51	ESO archive
	HD75302	ELODIE	3218	26	OHP archive	HD215497	HARPS	99	?
	HD75302	SOPHIE	3227	20	OHP archive	HD216437	HARPS	100	ESO archive
	HD78612	HARPS	3073	31	ESO archive	HD216437 CORALIE	21	Mayor et al. (2004) *
	HD89839	HARPS	6191	98	ESO archive	HD216437	UCLES	39	Butler et al. (2006) *
	HD93351	HARPS	6537	40	ESO archive	HD221146	HARPS	69	ESO archive
	HD96116	HARPS	6296	40	ESO archive	HD221146	HRS	50	Bowler et al. (2021)
	HD100777	HARPS	1231	37	ESO archive	HD221420	HARPS	77	ESO archive
	HD101198	HARPS	1988	91	Borgniet et al. (2017)	HD221420	AAT	88	Feng et al. (2022)
	HD107094	HARPS	6566	98	ESO archive	HD221420	PFS	38	Feng et al. (2022)
	HD108202	HARPS	6088	42	ESO archive	HD221638	HARPS	57	ESO archive
	HD111031	HARPS	3337	40	ESO archive	HIP9603	HARPS	39	ESO archive
	HD111998	HARPS	2992	150	Borgniet et al. (2017)	HIP10337	HARPS	90	ESO archive
	HD114783	HARPS	4415	91	ESO archive	HIP10337	HIRES	18	Butler et al. (2017) *
	HD114783	HIRES	7849	157	Rosenthal et al. (2021)	HIP39470	HARPS	32	ESO archive
	HD114783	HRS	826	34	Wittenmyer et al. (2009)	HIP54597	HARPS	69	ESO archive
	HD131664	HARPS	6100	65	ESO archive	HIP70849	HARPS	59	ESO archive
	HD135625	HARPS	6292	99	ESO archive	HIP113201	HARPS	66	ESO archive
				Notes: * Data retrieved from the DACE archives.
	A107, page 22 of 71

Table B .

 B 2: Relative astrometry considered for orbital fits.

	Companion	JD -2400000	SEP (mas)	PA (deg)	Instrument	Reference
	GJ680 B	53491.03	3760 ± 50	325.4 ± 0.3	NACO	Ward-Duong et al. (2015)
	GJ680 B	54235.64	3940 ± 50	323.7 ± 0.3	NACO	Ward-Duong et al. (2015)
	HD1388 B	57999.50	1845.9 ± 1.3	85.8 ± 0.6	NESSI a	Dalba et al. (2021)
	HD1388 B	53940.39	1490 ± 10	85.6 ± 1	NACO	This paper
	HD21175 B	57665.35	2628.0 ± 2.5 122.75 ± 0.08	SPHERE	This paper
	HD78612 B	53739.29	613 ± 5	272.3 ± 1	NACO	This paper
	HD93351 B/C	56093.02	1684 ± 30	76.3 ± 1	NACO	This paper
	HD101198 B	54421.70	891.2 ± 13.6 250.36 ± 1.16	PUEO b	Ehrenreich et al. (2010)
	HD101198 B	54948.30	926.4 ± 6.3	251.23 ± 0.55	NACO	Ehrenreich et al. (2010)
	HD101198 B	54948.30	927.0 ± 10.6 250.93 ± 0.86	NACO	Ehrenreich et al. (2010)
	HD111031 B	58151.50	1055.8 ± 1.3	121.3 ± 0.6	NESSI	Dalba et al. (2021)
	HD195564 B	58006.70	1113.0 ± 1.3	49.4 ± 0.6	NESSI	Dalba et al. (2021)
	HD195564 B	58006.70	1104.9 ± 1.3	49.8 ± 0.6	NESSI	Dalba et al. (2021)
	HD207700 B	56092.36	1090 ± 20	284.2 ± 1	NACO	This paper
	HD221146 B	53262.30	1723.0 ± 5.0	28.6 ± 0.1	NIRC2 c	Bowler et al. (2021)
	HD221146 B	53571.14	1720.0 ± 5.0	28.5 ± 0.2	NIRC2	Bowler et al. (2021)
	HD221146 B	58041.14	1623.0 ± 5.0	25.10 ± 0.14	NIRC2	Bowler et al. (2021)
	HD221146 B	58480.47	1600.0 ± 5.0	24.33 ± 0.12	NIRC2	Bowler et al. (2021)
	HD221146 B	58480.47	1604.0 ± 5.0	24.26 ± 0.14	NIRC2	Bowler et al. (2021)
	HD221146 B	58676.11	1592.0 ± 5.0	24.4 ± 0.2	NIRC2	Bowler et al. (2021)
	HIP113201 B	57649.13	161.21 ± 0.38 182.36 ± 0.13	SPHERE	Bonavita et al. (2022b)
	HIP113201 B	57676.03	167.80 ± 0.53 180.90 ± 0.53	SPHERE	Bonavita et al. (2022b)
	HIP113201 B	57709.01	172.61 ± 1.36 177.72 ± 0.13	SPHERE	Bonavita et al. (2022b)
	HIP113201 B	57906.44	198.44 ± 1.76 162.72 ± 0.51	SPHERE	Bonavita et al. (2022b)
	HIP113201 B	58621.39	285.49 ± 1.29 123.59 ± 0.26	SPHERE	Bonavita et al. (2022b)

Notes:

a

  Scott et al. (2018). b Rigaut et al. (1998). c Service et al. (2016).

	Philipot, F., et al.: A&A, 678, A107 (2023)
	A107, page 23 of 71

Table C .

 C 2: Table C.1 continued.

Table C .

 C 3: Orbital parameters and mass of single stellar companions.

	Discovery reference	Ward-Duong et al. (2015)	Dalba et al. (2021)	Feng et al. (2021)	This paper	This paper	Hartmann & Hatzes (2015)	Zechmeister et al. (2013)	This paper	This paper	This paper	dos Santos et al. (2017)	Borgniet et al. (2017)	Santos et al. (2011)	Feng et al. (2022)	Moutou et al. (2009)	This paper	This paper	Dalba et al. (2021)	This paper	This paper	Bowler et al. (2021)	This paper	This paper	This paper	Biller et al. (2022)
	Methods	RV+HG+HCI	RV+HG+HCI	RV+HG	RV+HG	RV+HG+HCI	RV	RV+HG	RV+HG	RV+HG	RV+HG+HCI	RV+HG	RV+HG+HCI	RV+HG	RV+HG+HCI	RV+HG	RV+HG	RV+HG	RV+HG+HCI	RV+HG+HCI	RV+HG	RV+HG+HCI	RV+HG	RV+HG	RV+HG	RV+HG+HCI
																									0.4
	P time (years)	188 +102 -68	501 +149 -103	11.54 ± 0.01	105 +73 -43	134 +60 -24	0.05 ± 0.01	19.4 +0.5 -0.6	4.758 +0.002 -0.001	28.4 ± 0.2	37 +17 -8	73 +26 -16	70 +8 -6	357 +93 -72	53 +4 -3	0.01 ± 0.01	7.413 ± 0.003	0.46 ± 0.01	29.0 +1.0 -0.7	77 +90 -32	6.886 ± 0.001	172 +23 -10	16.71 ± 0.06	12.80 ± 0.04	4 18.2 ± 0.5 or 16.4 ±	8.96 ± 0.02
	ω (°)	60 +22 -20	283 +10 -13	133.5 ± 0.3	4 +9 -10	284 +48 -247	227 +9 -8	3 278.7 ± 0.3	24.0 ± 0.1	169 +2 -1	11 +22 -9	67 +22 -16	147 ± 6	257 ± 1	42 +3 -2	2 151.7 +0.5 -0.4	126.3 +0.2 -0.1	212 ± 1	270 ± 10	318 +75 -66	181.11 +0.06 -0.05	126 +10 -66	196.7 +0.9 -0.8	188 ± 3	2 151 ± 3 or 150 ±	317 ± 1
	I (°) Ω (°)	167 +4 -10 171 +18 -14	91 ± 2 86 ± 1	47 ± 1 307 ± 1	24 +5 -4 125 +13 -10	27 +9 -6 93 +248 -61	fix to 90 fix to 0	45 ± 1 or 138 ± 1 252 ± 3 or 313 ±	6.1 ± 0.1 314 ± 1	87 ± 4 222 ± 2	48 +11 -9 95.9 ± 0.8	55 ± 10 86 +2 -3	108 ± 3 227 ± 5	95.4 ± 0.4 278 +5 -6	137 +4 -3 325 +2 -1	9.3 ± 0.3 or 170.4 ± 0.3 268 ± 1 or 182 ±	67 ± 1 150 +2 -1	91 ± 6 315 ± 1	61 +7 -9 263 +24 -11	154 +10 -16 79 24 -30	104 +4 -7 35 +4 -7	142 +12 -15 350 +18 -69	149 ± 1 124 +2 -1	45 ± 1 71 ± 5	22 +2 -3 or 170 ± 1 260 ± 2 or 142 ±	144.8 ± 0.4 201 ± 2
																									0.04
	Ecc	0.75 +0.11 -0.13	0.43 +0.07 -0.05	0.635 ± 0.003	0.66 ± 0.06	0.23 ± 0.13	0.15 +0.02 -0.01	0.580 ± 0.004	0.650 ± 0.001	0.33 ± 0.02	0.42 +0.13 -0.17	0.40 +0.07 -0.08	0.64 +0.09 -0.12	0.81 ± 0.03	0.71 ± 0.01	0.69 ± 0.01	0.624 ± 0.002	0.78 ± 0.01	0.94 +0.02 -0.01	0.28 +0.29 -0.19	0.51 ± 0.01	0.89 +0.02 -0.07	0.68 ± 0.02	0.63 ± 0.05	0.005 0.33 +0.05 -0.06 or 0.26 ±	0.69 ± 0.01
	Mass (M ⊙ )	0.178 ± 0.004	0.474 +0.006 -0.005	0.099 ± 0.004	0.51 +0.07 -0.06	1.05 ± 0.05	0.50 ± 0.02	0.29 ± 0.01	0.40 ± 0.01	0.227 +0.007 -0.006	0.29 ± 0.01	0.41 +0.08 -0.05	0.50 ± 0.02	0.28 ± 0.1	0.129 ± 0.003	0.132 ± 0.006	0.192 ± 0.007	0.139 ± 0.005	0.42 +0.02 -0.01	0.13 ± 0.01	0.164 +0.006 -0.005	0.633 +0.009 -0.008	0.108 ± 0.005	0.21 ± 0.02	0.1 0.138 +0.007 -0.008 or 0.147 ±	0.118 ± 0.002
	Star a (au)	GJ680 32 +9 -6	HD1388 77 +13 -10	HD16160 17.1 ± 0.3	HD16548 30 +11 -8	HD21175 43 +6 -4	HD42659 0.561 +0.007 -0.008	HD46569 10.4 ± 0.2	HD56380 4.79 ± 0.07	HD61383 12.7 ± 0.2	HD78612 18.2 +3.5 -1.6	HD96116 23 +5 -3	HD101198 26 +2 -1	HD107094 54 +9 -8	HD111031 21.1 ± 0.6	HD131664 3.4 ± 0.1	HD179346 9.4 ± 0.2	HD191797 5.4 ± 0.1	HD195564 73 +17 -12	HD207700 40 +7 -9	HD212036 4.1 ± 0.1	HD221146 38.0 +3.3 -1.3	HD221638 7.2 ± 0.2	HIP9603 15 ± 3	HIP39470 8.8 ± 0.2 or 7.6 ±	HIP113201 9.7 ± 0.2

http://archive.eso.org

https://dace.unige.ch

http://atlas.obs-hp.fr

The host star mass and the parallax considered are those reported byKervella et al. (2022).

The periastron passage time is calculated considering an initial time at BJD-2 454 000. A107, page 4 of

Acknowledgements. This study was funded by a grant from PSL/OCAV. This project has also received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (COBREX; grant agreement n°885593). This work presents results from the European Space Agency (ESA) space mission Gaia. Gaia data are being processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC is provided by national institutions, in particular the institutions participating in the Gaia MultiLateral Agreement (MLA). The Gaia mission website is https://www.cosmos.esa.int/Gaia. The Gaia archive website is https://archives.esac.esa.int/Gaia. This publication makes use of The Data & Analysis Center for Exoplanets (DACE), which is a facility based at the University of Geneva (CH) dedicated to extrasolar planet data visualisation, exchange, and analysis. DACE is a platform of the Swiss National Centre of Competence in Research (NCCR) PlanetS, federating Swiss expertise in exoplanet research. The DACE platform is available at ttps://dace. unige.ch. This work has made use of the SPHERE Data Center, jointly operated by OSUG/IPAG (Grenoble), PYTHEAS/LAM/CeSAM (Marseille), OCA/Lagrange (Nice), Observatoire de Paris/LESIA (Paris), and Observatoire de Lyon (OSUL/CRAL). This research has made use of the SIMBAD database and VizieR catalogue access tool, operated at CDS in Strasbourg, France. It is also based on data retrieved from the SOPHIE archive at Observatoire de Haute-Provence (OHP), available at atlas.obs-hp.fr/sophie, on spectral data retrieved from the ELODIE archive at Observatoire de Haute-Provence (OHP), and on observations collected at the European Southern Observatory under ESO programmes. We finally thank our anonymous referee, whose feedback helped us to improve the quality of this study.

Appendix A: Target list