The Discovery of a Planetary Companion Interior to Hot Jupiter WASP-132 b
Abstract
Hot Jupiters are generally observed to lack close planetary companions, a trend that has been interpreted as evidence for high-eccentricity migration. We present the discovery and validation of WASP-132 c (TOI-822.02), a 1.85 ± 0.10 R ⊕ planet on a 1.01 day orbit interior to the hot Jupiter WASP-132 b. Transiting Exoplanet Survey Satellite and ground-based follow-up observations, in conjunction with vetting and validation analysis, enable us to rule out common astrophysical false positives and validate the observed transit signal produced by WASP-132 c as a planet. Running the validation tools vespa and TRICERATOPS on this signal yields false-positive probabilities of 9.02 × 10-5 and 0.0107, respectively. Analysis of archival CORALIE radial velocity data leads to a 3σ upper limit of 28.23 ms-1 on the amplitude of any 1.01 day signal, corresponding to a 3σ upper mass limit of 37.35 M ⊕. Dynamical simulations reveal that the system is stable within the 3σ uncertainties on the planetary and orbital parameters for timescales of ~100 Myr. The existence of a planetary companion near the hot Jupiter WASP-132 b makes the giant planet's formation and evolution via high-eccentricity migration highly unlikely. Being one of just a handful of nearby planetary companions to hot Jupiters, WASP-132 c carries with it significant implications for the formation of the system and hot Jupiters as a population.
- Publication:
-
The Astronomical Journal
- Pub Date:
- July 2022
- DOI:
- 10.3847/1538-3881/ac6f57
- arXiv:
- arXiv:2205.02501
- Bibcode:
- 2022AJ....164...13H
- Keywords:
-
- Exoplanet astronomy;
- Exoplanet systems;
- Exoplanets;
- Hot Jupiters;
- Extrasolar gaseous planets;
- Transit photometry;
- 486;
- 484;
- 498;
- 753;
- 2172;
- 1709;
- Astrophysics - Earth and Planetary Astrophysics
- E-Print:
- 19 pages, 8 figures, Accepted for publication in AJ