of the equatorial column density of the torus of the unobscured AGN in the [*Chandra*]{}/HEG sample of @Shu:2010zr. A slope consistent within $1\sigma$ with our fit to the X-ray Baldwin effect in the Seyfert regime is obtained for $N_{\rm\,H}^{\rm\,T}\geq 10^{23.1}\rm\,cm^{-2}$ for the $\theta_{\mathrm{OA}}-L_{\mathrm{X}}$ relationship of @Hasinger:2008ve, for $N_{\rm\,H}^{\rm\,T}\gtrsim 10^{23.2}\rm\,cm^{-2}$ for that of @Burlon:2011cr, and for $N_{\rm\,H}^{\rm\,T}\lesssim10^{23}\rm\,cm^{-2}$ for the relationship of @Maiolino:2007bh. Comparing the value of the intercept obtained by the simulations with that resulting from our fit of the X-ray Baldwin effect in the Seyfert regime, we found that only a narrow range of average equatorial column densities of the torus can reproduce the observations (right panel of Fig.\[fig:slope\_NH\]). For the $\theta_{\mathrm{OA}}-L_{\mathrm{X}}$ relationship of @Maiolino:2007bh we found $22.9 \lesssim \log N_{\rm\,H}^{\rm\,T} \lesssim 23$, while for those of @Burlon:2011cr and @Hasinger:2008ve we obtained $\log N_{\rm\,H}^{\rm\,T} \simeq 23.2$. Using both the values of $A$ and $B$, it is possible to extract the average values of $N_{\rm\,H}^{\rm\,T}$ that can explain the X-ray Baldwin effect. As it can be seen from the two figures for both the $\theta_{\mathrm{OA}}-L_{\mathrm{X}}$ relationship of @Hasinger:2008ve and @Burlon:2011cr the only value of column density consistent with both the observed intercept and slope is $\log N_{\rm\,H}^{\rm\,T}\simeq 23.2$, while for the 