An imaged 15 M Jup companion within a hierarchical quadruple system

Chomez, A.; Squicciarini, V.; Lagrange, A.-M.; Delorme, P.; Viswanath, G.; Janson, M.; Flasseur, O.; Chauvin, G.; Langlois, M.; Rubini, P.; Bergeon, S.; Albert, D.; Bonnefoy, M.; Desidera, S.; Engler, N.; Gratton, R.; Henning, T.; Mamajek, E. E.; Marleau, G.-D.; Meyer, M. R.; ... (2023). An imaged 15 M Jup companion within a hierarchical quadruple system. Astronomy and astrophysics, 676 EDP Sciences 10.1051/0004-6361/202347044

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Context. Since 2019, the direct imaging B-star Exoplanet Abundance STudy (BEAST) at SPHERE@VLT has been scanning the surroundings of young B-type stars in order to ascertain the ultimate frontiers of giant planet formation. Recently, the 17+3−4 Myr HIP 81208 was found to host a close-in (∼50 au) brown dwarf and a wider (∼230 au) late M star around the central 2.6 M primary.
Aims. Alongside the continuation of the survey, we are undertaking a complete reanalysis of archival data aimed at improving detection performances so as to uncover additional low-mass companions.
Methods. We present here a new reduction of the observations of HIP 81208 using the patch covariance algorithm (PACO), a recent and powerful algorithm dedicated to processing high-contrast imaging datasets, as well as more classical algorithms and a dedicated point spread function subtraction approach. The combination of different techniques allowed for a reliable extraction of astrometric and photometric parameters.
Results. A previously undetected source was recovered at a short separation from the C component of the system. Proper motion analysis provided robust evidence for the gravitational bond of the object to HIP 81208 C. Orbiting C at a distance of ∼20 au, this 15 MJup brown dwarf becomes the fourth object of the hierarchical HIP 81208 system.
Conclusions. Among the several BEAST stars which are being found to host substellar companions, HIP 81208 stands out as a particularly striking system. As the first stellar binary system with substellar companions around each component ever found by direct imaging, it yields exquisite opportunities for thorough formation and dynamical follow-up studies.

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