Weak-lensing mass-observed richness relation measured for the clusters at redshift z = 0.22 run with GadgetX. The different panels consider different minimum stellar mass cuts M_{star,  min}, from 10¹⁰ to 10^10.75 h⁻¹ M_⊙. The weak-lensing masses M_wl are rescaled with respect to the pivot value M_p = 3 × 10¹⁴ h⁻¹ M_⊙. The blue points with the corresponding error bars show the results for the observed richness calculated as in Eq. (14) and the derived weak-lensing mass from the tangential shear profile. For the magenta triangles, the mass is not M_wl, but M₂₀₀; correspondingly we show the number λ_int of galaxies within R₂₀₀. The green circles show the results when using M_wl and the number of subhaloes in a sphere with radius R₂₀₀. The solid blue line displays the results of our fit performed using MCMC on the blue data points, and in cyan, the 1σ uncertainty. The orange dash-dotted line is the best fit of the inverse relation; see Eq. (18). Black dotted lines display the model presented in this work, WLOR relation as in Eq. (15) considering the values reported in Table 1.