Closure phases and amplitudes for Model F at 230 GHz (period 2.8 hr). The colored lines indicate the closure quantities that would be obtained in the absence of noise. The abscissa shows the time range over which Sgr A* is above 5° elevation at least three western hemisphere telescopes. Due to changing baseline orientations, closure phases and amplitudes do not approximately repeat, although significant deviations are seen simultaneously on most subarrays. Very small spikes seen in some of the lines are artifacts of the modeling.