Rotation curve (left panels) and velocity dispersions (right panels) of a boxy bulge formed from a thin stellar disk (square symbols) compared to ARGOS data (colored curves). In the N-body model, only stars at | x | ≤ 2.5 kpc and | y | ≤ 3 kpc from the galaxy center are shown. An initial radial metallicity profile [ Fe/H ] = 0.5−0.4R in the disk is assumed, similar to Martinez-Valpuesta & Gerhard (2013). Three different metallicity bins are shown, from top to bottom in decreasing [Fe/H], corresponding to the populations A, B, and C, as defined by Ness et al. (2013a). For each plot, four different latitudes are shown for the modeled galaxy: b = −4° (yellow squares), b = −6° (red squares), b = −8° (pale blue squares), b = −10° (dark blue squares). For comparison, ARGOS fields at b = −5° (orange, solid curve), b = −7.5° (pale blue, dashed curve), b = −10° (dark blue, dotted curve) for populations A, B, and C are also given. The thickness of the curves corresponds to the ± 1σ error in the observational data.