$\log L_{\rm\,max}=44.2$ for @Hasinger:2008ve, $\log L_{\rm\,max}=43.8$ for @Burlon:2011cr and $\log L_{\rm\,max}=45.0$ for @Maiolino:2007bh. Due to its limitations in the values of $\theta_{\mathrm{OA}}$ permitted, the model of @Ikeda:2009nx restricts most of the simulations to the Seyfert regime ($\log L_{\mathrm{X}}\leq \log L_{\mathrm{X}}^{\mathrm{Q}}=44.2$).

To extend our study to the quasar regime ($L_{\mathrm{X}}> L_{\mathrm{X}}^{\mathrm{Q}}$) we simulated the X-ray Baldwin effect using the spectral model of @Brightman:2011oq. This model considers the same geometry as @Ikeda:2009nx, but has $R_{\mathrm{in}}=0$, a $\theta_{\,\mathrm{i}}$-independent $N_{\rm\,H}$, and it allows different values of $\theta_{\mathrm{OA}}$ ($26^{\circ}$ to $84^{\circ}$). The higher maximum half-opening angle permitted by this model allows to reach higher maximum luminosities in the simulations for the relationships of @Hasinger:2008ve ([-@Hasinger:2008ve]; $\log L_{\rm\,max}=45.3$) and @Maiolino:2007bh ([-@Maiolino:2007bh]; $\log L_{\rm\,max}=46.2$), while that of @Burlon:2011cr is flat ($f_{\rm\,obs}\simeq0.2$) in the quasar regime. However, the lower boundary of $\theta_{\mathrm{OA}}$ in the model of @Brightman:2011oq limits the lower luminosity we can reach in the simulations, in particular $\log L_{\rm\,min}\simeq 43$ for the relation of @Maiolino:2007bh. Thus, we used the model of @Ikeda:2009nx to study the X-ray Baldwin effect in the Seyfert regime ($42\leq\log L_{\mathrm{X}} \leq 44.2$), and the model of @Brightman:2011oq to probe the quasar regime ($\log L_{\mathrm{X}} > 44.2$).

![Equivalent width of the iron K$\alpha$ 