Companions of Hot Jupiters: two decades of radial velocity monitoring with CORALIE
Authors: Léna Parc, João P. Faria, François Bouchy, Jana Baron, Siddharth Bhatnagar, Nicolas Billot, Yann Carteret, Guillaume Chaverot, Adrien Deline, Jean-Baptiste Delisle, Pedro Figueira, Emile Fontanet, Nathan C. Hara, Mathilde Houelle, Maxime Marmier, Marion Neveu-VanMalle, Louise D. Nielsen, Javiera Rey, Damien Ségransan, Manu Stalport, Stéphane Udry
Abstract
Hot Jupiters are thought to form through multiple pathways, some of which can leave observable signatures in the architecture of their planetary systems. Massive outer companions, in particular, can provide important constraints on the dynamical histories of hot Jupiters. We aim to characterize the occurrence rate and orbital properties of additional giant companions in hot Jupiter systems, and to investigate whether these companions provide evidence for the role of dynamical interactions in shaping the hot Jupiter population. We perform a homogeneous long-term radial-velocity analysis of 147 WASP hot Jupiter systems observed with the CORALIE spectrograph between 2007 and 2025. We identify or refine 13 outer giant companions and use individual radial-velocity posteriors within a Bayesian occurrence-rate framework to measure the frequency of giant companions over orbital periods of 10--6250 days. The occurrence rate of additional giant companions increases strongly with orbital period, from {2}lt;0.01$ and 0.02 at 10--50 and 50--250 days to 0.05 and 0.17 at 250--1250 and 1250--6250 days, respectively, in agreement with the giant-planet occurrence of the general FGK population and with previous estimates of outer companions to hot Jupiters. Hot Jupiters with detected companions have longer orbital periods and higher eccentricities than those without. We also find that companion eccentricity decreases with hot Jupiter period, and that the companion-to-hot-Jupiter mass ratio increases with period ratio, both consistent with expectations from high-eccentricity migration (HEM). Our results support HEM as the mechanism shaping hot Jupiters with outer companions. Combining long-baseline radial velocities with future Gaia astrometry will further constrain companion masses, mutual inclinations, and dynamical histories.
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Abstract
Direct imaging (DI) campaigns are uniquely suited to probing the outer regions around young stars and looking for giant exoplanet and brown dwarf companions, hence providing key complementary information to radial velocity (RV) and transit searches for the purpose of demographic studies. However, the critical 5-20 au region, where most giant planets are thought to form, remains poorly explored, lying in-between RV and DI capabilities. Significant gains in detection performances can be attained at no instrumental cost by means of advanced post-processing techniques. In the context of the COBREX project, we have assembled the largest collection of archival DI observations to date in order to u…
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Abstract
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Abstract
Precise mass constraints are vital for the characterisation of brown dwarfs and exoplanets. Here, we present how the combination of data obtained by Gaia and GRAVITY can help enlarge the sample of substellar companions with measured dynamical masses. We show how the Non-Single-Star (NSS) two-body orbit catalogue contained in Gaia DR3 can be used to inform high angular resolution follow-up observations with GRAVITY. Applying the method presented in this work for eight Gaia candidate systems, we detect all eight predicted companions, seven of which being previously unknown and five of substellar nature. Among the sample is Gaia DR3 2728129004119806464 B, which - detected at a angular separatio…
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Abstract
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Abstract
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Abstract
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Abstract
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Abstract
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