Table 1: Molecular hydrogen abundances and dust contents $\tilde{k}$ in cosmological H2-bearing clouds.
\begin{displaymath}{ \begin{tabular}{l c r @{$\;\pm\;$} l c c c l} \hline \hline... ...002$ & Levshakov et~al. (\cite{Lev00})\\ \hline \end{tabular}}\end{displaymath}
Note: column densities N(H I) and N(H2) are given in cm-2; $^\dagger$ tentative H2 identification; $^\ast$ photospheric solar abundances for Cr and Zn are taken from Grevesse & Sauval (1998), for Mg and Fe from Holweger (2001), see Eq. (3).
a High resolution UVES data reveal a few H2 subcomponents spread over $\sim$700 km s-1 (Petitjean et al. 2002); b Srianand et al. (2000); c Ledoux et al. (2003); d Levshakov & Foltz (1988); e M$\o$ller & Warren (1993); f Prochaska & Wolfe (1999); g Levshakov et al. (2001).

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