Hot Jupiters generally do not have nearby planet companions, as they may have cleared out other planets during their inward migration from more distant orbits. This gives evidence that hot Jupiters more often migrate inward via high-eccentricity migration due to dynamical interactions between planets rather than more dynamically cool migration mechanisms through the protoplanetary disk. Here we further refine the unique system of WASP-132 by characterizing the mass of the recently validated 1. 0-day period super-Earth WASP-132c (TOI-822. 02), interior to the 7. 1-day period hot Jupiter WASP-132b. Additionally, we announce the discovery of a giant planet at a 5-year period (2. 7 AU). We also detected a long-term trend in the radial velocity data indicative of another outer companion. Using over nine years of CORALIE radial velocities (RVs) and over two months of highly sampled HARPS RVs, we determined the masses of the planets from smallest to largest orbital period to be {M₂} = 6. 26 - ₁. ₈₃^ + 1. 84M_, {M₁} = 0. 428 - ₀. ₀₁₅^ + 0. 015M{₉ₔ}, and {M₃} i = 5. 16 - ₀. ₅₂^ + 0. 52M{₉ₔ}, respectively. Using TESS and CHEOPS photometry data, we measured the radii of the two inner transiting planets to be {R₂} = 1. 841 - ₀. ₀₉₃^ + 0. 094R_ and {R₁} = 0. 901 - ₀. ₀₃₈^ + 0. 038R{₉ₔ}. We find a bulk density of ₂ = 5. 47 - ₁. ₇₁^ + 1. 96g\, \, c{m^ - 3} for WASP-132c, which is slightly above the Earth-like composition line on the mass-radius diagram. WASP-132 is a unique multi-planetary system in that both an inner rocky planet and an outer giant planet are in a system with a hot Jupiter. This suggests it migrated via a rarer dynamically cool mechanism and helps to further our understanding of how hot Jupiter systems form and evolve.
Grieves et al. (2025) studied this question.