Fit solutions for the three outlying flares. (a) Same as Fig. 7, but for the three flares that require high inclinations and large separations. The secondary peaks are not described by the flare models, but instead are modeled by the Gaussian process component. (b) Same as panel (a), but showing fit results for a spinning black hole (a = 0.99), which allows for smaller ISCOs and thus shorter orbital periods (r₀ ∼ 5.1 R_g). Here the secondary peaks are described by the flare model.