NEID Rossiter-McLaughlin Measurement of TOI-1268b: A Young Warm Saturn Aligned with Its Cool Host Star

Close-in gas giants present a surprising range of stellar obliquity, the angle between a planet's orbital axis and its host star's spin axis. It is unclear whether the obliquities reflect the planets' dynamical history (e.g., aligned for in situ formation or disk migration versus misaligned for high-eccentricity tidal migration) or whether other mechanisms (e.g., primordial misalignment or planet-star interactions) are more important in sculpting the obliquity distribution. Here we present the stellar obliquity measurement of TOI-1268 (TIC-142394656, V-mag similar to 10.9), a young K-type dwarf hosting an 8.2 day period, Saturn-sized planet. TOI-1268's lithium abundance and rotation period suggest the system age between the ages of the Pleiades cluster (similar to 120 Myr) and the Prasepe cluster (similar to 670 Myr). Using the newly commissioned NEID spectrograph, we constrain the stellar obliquity of TOI-1268 via the Rossiter-McLaughlin effect from both radial velocity and Doppler tomography signals. The 3 sigma upper bounds of the projected stellar obliquity vertical bar lambda vertical bar from both models are below 60 degrees. The large host star separation (a/R-star similar to 17), combined with the system's young age, makes it unlikely that the planet has realigned its host star. The stellar obliquity measurement of TOI-1268 probes the architecture of a young gas giant beyond the reach of tidal realignment (a/R-star greater than or similar to 10) and reveals an aligned or slightly misaligned system.