of the spectrum. Fig. \[J0008-2901\] shows our best fit result of the [H]{}[i]{} lines.

3.  QSO J0041-4936 ($z_{\rm em}=3.240$). A damped absorber is known in this quasar from the Calán Tololo survey [@maza95]. From a low-resolution spectrum, @lopez01 measured the equivalent width of the [H]{}[i]{} absorption line to be ${\rm EW_{obs}}=34.60\,\AA$ but state that they cannot measure the [H]{}[i]{} column density due to the limited spectral resolution. Using the high-resolution UVES spectrum, we are able to measure the column density of the DLA to be log $N_{{\rm H}\,{\sc \rm I}}=20.46\pm0.13$ and $b=29\pm3.9$ km s$^{-1}$ at $z_{\rm abs}=2.248$ detected down to Ly$\beta$. Metal lines from [O]{}[i]{} $\lambda$ 1302, [Fe]{}[ii]{} $\lambda\lambda$ 1608, 1611, [Si]{}[ii]{} $\lambda\lambda\lambda\lambda$ 1260, 1304, 1526, 1808, [C]{}[ii]{} $\lambda$ 1334, [Al]{}[ii]{} $\lambda$ 1670, [Zn]{}[ii]{} $\lambda$ 2026, [Al]{}[iii]{} $\lambda\lambda$ 1854, 1862, and [C]{}[iv]{} $\lambda\lambda$ 1548, 1550 associated with the DLA are detected in the red part of the spectrum. Fig. \[J0041-4936\] shows the best fit result of the [H]{}[i]{} lines.

4.  QSO B0128-2150 ($z_{\rm em}=1.900$). This quasar was discovered during the course of the Montréal-Cambridge-Tololo survey [@lamontagne00]. Two absorbing systems at $z_{\rm abs}=1.64$ and 1.85 are reported in the UVES observing proposal. We find that the system at $z_{\rm abs}=1.857$ is 