a sub-DLA with log $N_{{\rm H}\,{\sc \rm I}}=20.21\pm0.09$ and $b=25\pm2.6$ km s$^{-1}$. Metal lines from [O]{}[i]{} $\lambda$ 1302, [Fe]{}[ii]{} $\lambda\lambda\lambda$ 2344, 2374, 2382, [Si]{}[ii]{} $\lambda\lambda\lambda$ 1260, 1304, 1808, [C]{}[ii]{} $\lambda$ 1334, and [Al]{}[iii]{} $\lambda\lambda$ 1854, 1862 at the redshift of the absorber are observed in the red part of the spectrum. Fig. \[B0128-2150\] shows our best fit result of the [H]{}[i]{} column density. The absorbing system at $z_{abs}=1.64$ is below sub-DLA limit.

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5.  J021741.8-370100 ($z_{\rm em}=2.910$). Damped absorbers have been known in this quasar from the Calán Tololo survey [@maza96]. The column densities for these DLAs have not been reported before. We measure log $N_{{\rm H}\,{\sc \rm I}}=20.62\pm0.08$ at $z_{\rm abs}=2.429$ and log $N_{{\rm H}\,{\sc \rm I}}=20.46\pm0.09$ at $z_{\rm abs}=2.514$. Both absorbers are seen down to Ly$\beta$. The $b$ parameter is fixed to $b=30$ km s$^{-1}$ for both absorbers. Due to limited wavelength coverage only a few metal lines associated with the absorbers are seen in the spectrum. Metal lines from [O]{}[i]{} $\lambda$ 1302 and [Si]{}[ii]{} $\lambda\lambda\lambda\lambda$ 1190, 1193, 1260, 1304 are covered for the absorber at $z_{\rm abs}=2.429$. The lines from [Fe]{}[ii]{} $\lambda$ 1144 and [Si]{}[ii]{} $\lambda\lambda\lambda$ 1190, 1193, 1260 associated with the absorber at $z_{\rm abs}=2.514$ are 