Predicted rms eccentricity (black curves) of 50 stars, each with mass M = 25 M _☉ , resulting from two-body interactions within a stellar disk with various mass function slopes. This is a version of Figure 4 in Alexander et al. (2007), which has been updated to reflect the latest black hole mass estimates (4 × 10 ⁶ M _☉ ) and a recent estimate of the age of the young star population from Lu et al. (2013) of 3.65 ± 0.87 Myr. From bottom to top, the three curves represent the rms eccentricity after 2.78 Myr, 3.65 Myr, and 4.52 Myr, respectively. The red point shows the rms eccentricity and estimated uncertainty of our best measured stars ( e ^{2 1/2} = 0.28 ± 0.07) and the latest estimate of the mass function slope (α = 1.7 ± 0.2) from Lu et al. (2013). The observed values are within 1σ of the predicted values from the Alexander et al. model.