Predicted change in eccentricity from tidal circularization, Δ ln e, and observed eccentricity for all APOGEE binary systems. Change in eccentricity is computed assuming that the semimajor axis of the systems remain constant during eccentricity evolution, and assuming that all stars have a primary mass of M1 = 1.4 M_⊙ and a companion mass of M₂ = 0.5 M_⊙ (the median values from all systems with measured masses). Most systems with large predicted Δ ln e have small observed eccentricities, with the exception of a few outlier systems.