Kavli Affiliate: Sara Seager
| First 5 Authors: Benjamin J. Hord, Knicole D. Colón, Travis A. Berger, Veselin Kostov, Michele L. Silverstein
| Summary:
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 $pm$
0.10 $R_{oplus}$ planet on a 1.01 day orbit interior to the hot Jupiter
WASP-132 b. Transiting Exoplanet Survey Satellite (TESS) 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 texttt{vespa} and texttt{triceratops} on this signal yield
false positive probabilities of $9.02 times 10^{-5}$ and 0.0107, respectively.
Analysis of archival CORALIE radial velocity data leads to a 3$sigma$ upper
limit of 28.23 ms$^{-1}$ on the amplitude of any 1.01-day signal, corresponding
to a 3$sigma$ upper mass limit of 37.35 $M_{oplus}$. Dynamical simulations
reveal that the system is stable within the 3$sigma$ uncertainties on
planetary and orbital parameters for timescales of $sim$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.
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