The top panel shows with green circles the observed stellar density multiplied by ﹩{r}_{q}^{2}﹩ as a function of flattened radius, r_q, compared to the best-fit triple power-law model (red solid line) and double power-law model (blue solid line). Error bars represent the 1σ uncertainties computed from 100 bootstrap subsamples of our K giants. Here the best-fit triple power-law model in this work (red solid line), that in J. J. Han et al. (2022; orange solid line), and the double power-law model (blue solid line) have been convolved with the angular and radial selection functions to have a fair direct comparison with the data (see Section 3.1). Two vertical black dotted lines in both the top and bottom panels represent the two break radii, r_b,1 and r_b,2, respectively. Two horizontal dashed gray lines in the bottom panels represent 10% regions of the model-predicted density over observed density, with the black dashed horizontal line marking y = 1. Both triple power-law and double power-law models fit the stellar halo within 70 kpc well, but the double power-law model shows a worse match of the outer stellar halo beyond ∼70 kpc.