Comparison of three illustrative two-planet dynamical models fitted to HD 332231. Each row corresponds to a different perturber configuration with orbital periods of about 81 days (a), 196 days (b), and 307 days (c); the corresponding masses and orbital eccentricities are also provided. Left panels: modelled RV signals overlaid on HIRES and APF data points (red and orange points, respectively). Right panels: corresponding TTV model compared to observed mid-transit times. In analogy to Fig. 2, blue points come from TESS light curves, and the green square is from spectral observations by Knudstrup & Albrecht (2022).