low-resolution spectrum, @lopez01 measured the equivalent width of the [H]{}[i]{} absorption line to be ${\rm EW_{obs}}=13.52\,\AA$ 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 identify two main components in the system from the metal lines at 0 and -144 km s$^{-1}$. Fitting these components we measure the total column density of the sub-DLA to be log $N_{{\rm H}\,{\sc \rm I}}=19.30\pm0.10$ with $b$ parameter of $b=26\pm3.4$ and fixed 20 km s$^{-1}$ (at 0 and -144 km s$^{-1}$). The component at 0 km s$^{-1}$ is stronger and heavily dominates over the component at 144 km s$^{-1}$. Metal lines from [Fe]{}[ii]{} $\lambda\lambda\lambda\lambda$ 1144, 2344, 2382, 2586, [Si]{}[ii]{} $\lambda\lambda\lambda$ 1193, 1260, 1526, [C]{}[ii]{} $\lambda$ 1334, [Al]{}[iii]{} $\lambda\lambda$ 1854, 1862, [Si]{}[iv]{} $\lambda\lambda$ 1393, 1402, and [C]{}[iv]{} $\lambda\lambda$ 1548, 1550 associated with the sub-DLA are detected in the red part of the spectrum. Fig. \[Q1036-2257\] shows the best fit result of the [H]{}[i]{} column density.

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10. QSO B1036-268 ($z_{\rm em}=2.460$). A low-resolution slit spectrum of the quasar has been previously published [@jakobsen92]. We find four strong velocity components in the system at $z_{\rm abs}=2.235$ from the 