Closeby Habitable Exoplanet Survey (CHES). III. Retrieval of Planetary Masses in Binaries Using the <i>N</i>-body Model with Radial Velocity and Astrometry Synergy

Abstract Given that secular perturbations in a binary system not only excite high orbital eccentricities but also alter the planetary orbital inclination, the classical Keplerian orbital model is no longer applicable for orbital retrieval. The combination of a dynamical model and observational data is essential for characterizing the configuration and planetary mass in close binaries. We calculate the theoretical radial velocity (RV) signal in the N -body framework and observe a drift in the RV semiamplitude, which leads to a reduction in the m sin i detection threshold by 20 M ⊕ , with ∼100% detection probability in the m 1 sin i 1 – a 1 parameter space. High-precision RV data with an accuracy of 1 m s −1 can detect such dynamical effects. For four close-in binaries—GJ 86, GJ 3021, HD 196885, and HD 41004—the deviation between the minimum mass derived from the Keplerian and N -body models is found to be &gt;0.2 M Jup . High-precision astrometric data are also necessary to resolve the 3D orbits and true masses of exoplanets. We generate astrometric simulation data with accuracies corresponding to Gaia (57.8 μ as) and the Closeby Habitable Exoplanet Survey (CHES; 1 μ as), respectively. Joint orbit fitting is performed for RV+Gaia and RV+CHES synergy methods. Compared with the fitting results from the astrometry-only model, the synergy models more effectively constrain the range of orbital inclinations. Using simulation data, we derive precise uncertainties for the true planetary mass, which are critical for determining the evolution of planets around binary stars and multiplanet systems.