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Close-in gas giants present a surprising range of stellar obliquity, theangle between a planet's orbital axis and its host star's spin axis. It isunclear whether the obliquities reflect the planets' dynamical history (e.g.,aligned for in situ formation or disk migration versus misaligned forhigh-eccentricity tidal migration) or whether other mechanisms (e.g.,primordial misalignment or planet-star interactions) are more important insculpting the obliquity distribution. Here we present the stellar obliquitymeasurement of TOI-1268 (TIC-142394656, $V_{\rm mag} {\sim} 10.9$), a youngK-type dwarf hosting an 8.2-day period, Saturn-sized planet. TOI-1268's lithiumabundance and rotation period suggest the system age between the ages ofPleiades cluster (${\sim}120$ Myr) and Praesepe cluster (${\sim}670$ Myr).Using the newly commissioned NEID spectrograph, we constrain the stellarobliquity of TOI-1268 via the Rossiter-McLaughlin (RM) effect from both radialvelocity (RV) and Doppler Tomography (DT) signals. The 3$\sigma$ upper boundsof the projected stellar obliquity $|\lambda|$ from both models are below60$^\circ$. The large host star separation ($a/R_\star {\sim} 17$), combinedwith the system's young age, makes it unlikely that the planet has realignedits host star. The stellar obliquity measurement of TOI-1268 probes thearchitecture of a young gas giant beyond the reach of tidal realignment($a/R_\star {\gtrsim} 10$) and reveals an aligned or slightly misalignedsystem.

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