Left: disk membership probability plotted against position angle from the disk line of nodes (Ω = 96 3) for the 10 simulations with f _disk = 0.2. True disk members are shown as red circles ( N = 240), while stars from the isotropic population are marked as black squares ( N = 960). Stars with significant acceleration detections are marked with an "x." For disk stars, the probability of disk membership is a function of the angular offset from the disk's line of nodes. Non-accelerating disk stars with small angular offsets (<20°) show relatively large scatter in disk membership probability. We compute the median and standard deviation of the probability in angular offset bins of 10° for all non-accelerating disk stars. The median and 3σ lower-limit values are shown as the green solid and dashed curves, respectively. Right: same plot, but for the observed sample of N = 116 stars. The 3σ lower-limit curve is overplotted. Points above this curve represent the most likely members of the clockwise disk. The 3 B stars that are likely disk members are indicated with the letter "B."