"Our team measured the ingress of TOI-2202b's transit on UT 2022 August 24 using one of the 0.7m Minerva-Australis telescopes located at the University of Southern Queensland's Mount Kent Observatory. The telescope is equipped with a 2000x2000pixel Andor CCD with pixel scale 0.608"", and we used a 15pixel radius (9.12"") aperture to extract the photometry. We measured one partial transit of TOI-2202b on UT 2022 September 9 using the Las Cumbres Observatory Global Network (LCOGT) Siding Spring Observatory (SSO) 0.4 and 1m telescopes, in New South Wales in Australia. Observations were taken in the Sloan i' band with 170s exposures on the 0.4m telescope and 43s exposures on the 1m telescope. We also measured two transit ingress events for TOI-2202b on UT 2022 October 10 and 2022 October 10, as well as one full transit on UT 2022 November 4, using the LCOGT Cerro Tololo Inter-American Observatory (CTIO) 0.4m telescope located 80km east of La Serena, Chile. The UT 2022 October 10 ingress was simultaneously observed using the LCOGT CTIO 1m telescope. Observations were taken in the Sloan i' band, with 170s exposures for the 0.4m telescope observations and 43s exposures for the 1m telescope observations. We measured one transit egress event for TOI-2202b on UT 2022 October 11 using the TRAPPIST-South 0.6m robotic telescope at La Silla Observatory in the Atacama Desert of Chile. Continuous 30s observations were taken with the Astrodon ""i+z"" filter. The TRAPPIST-South observing sequence spanned 2.16hr prior to the transit ingress, as well as 1.76 in-transit hours of observations. Our team measured two full transits of TOI-2202b on UT 2022 October 23 and UT 2022 November 4 using the station of the Observatoire Moana located in El Sauce Observatory in Chile. Observations were taken in the Sloan r band with continuous 100s exposures."

The geometries of near-resonant planetary systems offer a relatively pristine window into the initial conditions of exoplanet systems. 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. Incorporating the full census of spin-orbit measurements for near-resonant systems, we demonstrate that the current set of near-resonant systems with period ratios P2/P1<~4 is generally consistent with a quiescent formation pathway, with some room for low-level (<~20{deg}) protoplanetary disk misalignments or post-disk- dispersal spin-orbit excitation. Our result constitutes the first population- wide analysis of spin-orbit geometries for near-resonant planetary systems.

Financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033

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