Verification of the bulge versus hot inner stellar halo decomposition. Shown are the probability density p_hot (top panel) and metallicity Z_hot/Z_⊙ (bottom panel) of the hot orbits as a function of radius for TNG50 468590, TNG50 375073, TNG50 220596, and TNG50 2, from Panel (a) to Panel (d). In each panel, the red curve is the true profile from the simulation, and the thick and dashed black curves are the mean and 1σ scatter of our best fitting models. The vertical lines mark the position of r = 3.5 kpc, where we separate the bulge from hot inner stellar halo.