Photometry obtained for TOI-2202b

Given that near-resonant systems have likely experienced minimal dynamical disruptions, the spin-orbit orientations of these systems inform the typical outcomes of quiescent planet formation, as well as the primordial stellar obliquity distribution. However, few measurements have been made to constrain the spin- orbit orientations of near-resonant systems.

We present a Rossiter-McLaughlin measurement of the near-resonant warm Jupiter TOI-2202b, obtained using the Carnegie Planet Finder Spectrograph on the 6.5m Magellan Clay Telescope. This is the eighth result from the Stellar Obliquities in Long-period Exoplanet Systems survey. We derive a sky-projected 2D spin-orbit angle {lambda}=26_-15_^+12^ and a 3D spin-orbit angle {psi}=31_-11_^+13^deg , finding that TOI-2202 b-the most massive near- resonant exoplanet with a 3D spin-orbit constraint to date-likely deviates from exact alignment with the host star's equator.