For fitting $N_{{\rm H}\,{\sc \rm I}}$, we usually used the components from $\ion{O}{i}$. The other low ionization line components are used to fit $N_{{\rm H}\,{\sc \rm I}}$ for the cases where there is no $\ion{O}{i}$ covered by our data. Table \[dlamet\] summarizes the properties of the DLAs/sub-DLAs for which we obtained ${\rm H}\,{\sc \rm I}$ column density for the first time and provides quasar emission redshifts, absorption redshifts, [H]{}[i]{} column densities and metal line lists.

Moreover, the majority of the $N_{{\rm H}\,{\sc \rm I}}$ measurements of the DLAs/sub-DLAs towards the 250 EUADP quasars comes from high-resolution data mostly from UVES or Keck/HIRES. In 7 cases, we cover the DLA/sub-DLA in our data but the $N_{{\rm H}\,{\sc \rm I}}$ in the literature is obtained from low/moderate resolution spectra. For these 7 cases, we refitted the DLA/sub-DLA using the EUADP data and new $N_{{\rm H}\,{\sc \rm I}}$ are reported in Table \[newNH\]. For most of the cases, we find consistent results with the low resolution studies. In the case of QSOB1114-0822, @storrie00 reported a DLA with log $N_{{\rm H}\,{\sc \rm I}}=20.3$ at $z_{\rm abs}=4.258$ while we find a sub-DLA with log $N_{{\rm H}\,{\sc \rm I}}=20.02\pm0.12$.

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