metallicity estimate. From the simultaneous Voigt-profile fit of the $\lambda$2026 with the $\lambda$1526, $\lambda$1808 and $\lambda$1608, $\lambda$1611 lines in the low resolution spectrum, performed with the MIDAS/FITLYMAN software [@Fontana95], we derive a log $(N_{\mathrm{Zn\,{\sc II}}}/$cm$^{-2})=13.53\pm0.14$ cm$^2$ (i.e. \[Zn/H\] $-0.93\pm0.18$, Doppler thermal broadening $b_{\textrm{th}}=0$ km s$^{-1}$, and turbulent broadening $b_{\textrm{tur}}=39.4\pm6.8$ km s$^{-1}$). The analysis seems to show that the $\lambda$2026 line is on the linear part of the curve of growth (i.e. unsaturated), despite the low spectral resolution of the data. The metallicities refer to the solar abundances reported by @Asplund09.\
Several lines are also identified in the medium resolution 1400V, 1200R and 600z spectra with the EWs listed in Table \[tab2\]. Many of the lines associated with the GRB host galaxy system show evidence for a two-component profile (component “a" and “b"). In order to derive reliable column densities and to study the kinematics of the gas, we select the , , and lines in the higher resolution grisms 1400V and 1200R that are neither too saturated nor blended with other transitions, and model them simultaneously with a two-component Voigt profile, using the VPFIT[^2] software. In this way, the line profile of all the species is modelled with the same 