and those identified by [trunk-1]{} are indicated.

Our method correctly identifies 100% of the lines in this band, which we have tested for different widths of the identification window. A similar analysis is performed using a synthetic spectra based on Model B (Table 2), where on top of the two warm absorber components, a third component due to galactic absorption is included (ism). This latter component only includes the continuum (bound-free) photoelectric absorption, thus while it modifies the model continuum it does not introduces any additional absorption features. In order to illustrate the virtues and caveats of the method we show in Figure \[cases1\], six (6) possible cases which are easily solved by it. In panel (a) we have the simplest possible case. One observed feature $\lambda(O)_1$, has an IW $\Delta \lambda_0$, and only the theoretical line $\lambda(T)_1$ is within the IW. Then $\lambda(O)_1$ is easily identified as $\lambda(T)_1$. In panel (b), theoretical lines $\lambda(T)_1$ and $\lambda(T)_2$ are within $\Delta \lambda_0$. In this case we simply take the one with the largest optical depth. If we assign $\tau_1$ to $\lambda(T)_1$ and $\tau_2$ to $\lambda(T)_2$ with $\tau_1 > \tau_2$, then $\lambda(O)_1$ is simply identified as $\lambda(T)_1$. In panel (c) we now 