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It has been shown that hot Jupiters systems with massive, hot stellarprimaries exhibit a wide range of stellar obliquities. On the other hand, hotJupiter systems with low-mass, cool primaries often have stellar obliquitiesclose to zero. Efficient tidal interactions between hot Jupiters and theconvective envelopes present in lower-mass main sequence stars have been apopular explanation for these observations. If this explanation is accurate,then aligned systems should be older than misaligned systems. Likewise, theconvective envelope mass of a hot Jupiter's host star should be an effectivepredictor of its obliquity. We derive homogeneous stellar parameters --including convective envelope masses -- for hot Jupiter host stars withhigh-quality sky-projected obliquity inferences. Using a thin disk stellarpopulation's Galactic velocity dispersion as a relative age proxy, we find thathot Jupiter host stars with larger-than-median obliquities are older than hotJupiter host stars with smaller-than-median obliquities. The relative agedifference between the two populations is larger for hot Jupiter host starswith smaller-than-median fractional convective envelope masses and issignificant at the 3.6-$\sigma$ level. We identify stellar mass, not convectiveenvelope mass, as the best predictor of stellar obliquity in hot Jupitersystems. The best explanation for these observations is that many hot Jupitersin misaligned systems arrived in the close proximity of their host stars longafter their parent protoplanetary disks dissipated. The dependence of observedage offset on convective envelope mass suggests that tidal realignmentcontributes to the population of aligned hot Jupiters orbiting stars withconvective envelopes.

Evidence for the Late Arrival of Hot Jupiters in Systems with High Host-star Obliquities