Illustration of how our method can be used to derive mass–observable relations at different redshifts. From top to bottom, we show example best fits to the M_star,tot–M_200m, M_bcg–M_200m, and N–M_200m relations at z ≈ 0.95 (black dashed line) and z ≈ 0.42 (pale red dashed line). For the values of the slopes, please refer to Table 1. Here we simply note that the slopes of both M_star,tot–M_200m and N–M_200m appear to be invariant with respect to redshift.