A recreation of Figure 4 in S. N. Quinn et al. (2014). The system age τ_age is plotted against the tidal circularization timescale τ_cir in logarithmic space, with color contours indicating orbital eccentricity. The dashed line marks where τ_cir = τ_age, based on Q_p = 4.9 × 10⁵. The shaded region reflects the uncertainty in Q_p. Marker size corresponds to planetary mass, and planets with only mass upper limits are excluded. Planets with fully constrained eccentricities are shown as circles, those with upper limits are triangles, and assumed circular orbits are indicated by squares. Dynamically old but eccentric outliers are highlighted in orange, while disk migration candidate hot Jupiters (a < 0.1 au) are highlighted in blue. We note that ﹩{({\tau }_{{\rm{cir}}}/{\tau }_{{\rm{age}}})}_{{\rm{median}}}\gt 1﹩ does not strictly imply τ_cir,median/τ_age,median > 1, and vice versa. This results in one planet to the left of the dashed line being highlighted in blue, and another to the right not being highlighted.