dashed line with $\Delta \lambda = 0.1$ Å, and dotted line with $\Delta \lambda = 0.2$ Å). However we see that the density function of these velocities are very small compared with the components made by right identification.

Discussion & Conclusions {#discu1}
========================

In this paper we show how important is to correctly define the level of continuum for EW measurements, which could differ up to $\sim 80$ %, including or not interstellar absorption. We also show that [xline-id]{} is better than 90% in the identification of absorption lines, where more than one absorber is present.

Once we have inferred the gas density from the spectral lines, we can take equation (\[xi11\]) and compute $r$ from it. What is deduced, using the relation $n_H  \propto r^{-2} $, and Figure \[distance1\], is a suggestion of the MIP located at distances of $r_{MIP}\simeq (0.18-1.80)$ lt-days ($\log r \simeq 14.7-15.7$ \[cm\]), and the LIP located at distances of $r_{LIP}\simeq (0.51-5.13)$ lt-days ($\log r\simeq 15.1-16.1$ \[cm\]).

The global picture that emerges from this is that highly ($\log \xi \sim 2$) ionized material with gas density ($n_H \sim 10^{12}$ ) is located closer than the less ionized (colder $\log T\sim 4.7$ K) gas. There was 