Table 1: UVES DLA sample: average metallicities and velocity widths of low-ionization line profiles$^\ast $.

Quasar		 Other name $z_{\rm em}$ $z_{\rm abs}$1 $\log N($H  I) [X/H]2   $\Delta V$ Selected
            X (km s-1) transition lines3
Q 0000-263 LBQS 0000-2619 4.11 3.390 $21.40\pm 0.08$ $-2.06\pm 0.09$ Zn 33 O  I$\lambda $950
Q 0010-002 LBQS 0010-0012 2.15 2.025 $20.95\pm 0.10$ $-1.43\pm 0.11$ Zn 32 Si  II$\lambda $1808
Q 0013-004 LBQS 0013-0029 2.09 1.973 $20.83\pm 0.05$ $-0.59\pm 0.05$ Zn 720 Fe  II$\lambda $1608
Q 0058-292 LBQS 0058-2914 3.09 2.671 $21.10\pm 0.10$ $-1.53\pm 0.10$ Zn 34 Si  II$\lambda $1808
Q 0100+130 LBQS 0100+1300 2.69 2.309 $21.35\pm 0.08$ $-1.58\pm 0.08$ Zn 37 Cr  II$\lambda $2056
Q 0102-190 LBQS 0102-1902 3.04 2.370 $21.00\pm 0.08$ $-1.90\pm 0.08$ S 17 Fe  II$\lambda $2374
Q 0102-190 LBQS 0102-1902 3.04 2.926 $20.00\pm 0.10$ $-1.50\pm 0.10$ Si 146 Si  II$\lambda $1526
Q 0112-306 LBQS 0112-3041 2.99 2.418 $20.50\pm 0.08$ $-2.42\pm 0.08$ Si 31 Si  II$\lambda $1526
Q 0112-306 LBQS 0112-3041 2.99 2.702 $20.30\pm 0.10$ $-0.49\pm 0.11$ Si 218 Fe  II$\lambda $1608
Q 0112+030 LBQS 0112+0300 2.81 2.423 $20.90\pm 0.10$ $-1.31\pm 0.11$ S 112 Fe  II$\lambda $1608
Q 0135-273 CTS 1005 3.21 2.107 $20.30\pm 0.15$ $-1.12\pm 0.16$ S 82/103 Fe  II$\lambda $2260/Fe  II$\lambda $2586
Q 0135-273 CTS 1005 3.21 2.800 $21.00\pm 0.10$ $-1.40\pm 0.10$ S 65/67 S  II$\lambda $1259/Fe  II$\lambda $1608
Q 0216+080 LBQS 0216+0803 2.99 1.769 $20.30\pm 0.10$ $-1.00\pm 0.12$ Zn 75 Fe  II$\lambda $2374
Q 0216+080 LBQS 0216+0803 2.99 2.293 $20.50\pm 0.10$ $-0.70\pm 0.11$ Zn 104 Si  II$\lambda $1808
Q 0336-017 LBQS 0336-0142 3.20 3.062 $21.10\pm 0.10$ $-1.41\pm 0.10$ Si 67 Si  II$\lambda $1808
Q 0347-383 LBQS 0347-3819 3.22 3.025 $20.73\pm 0.05$ $-1.17\pm 0.07$ Zn 93 Fe  II$\lambda $1608
Q 0405-443 CTS 247 3.02 1.913 $20.80\pm 0.10$ $-1.03\pm 0.10$ Zn 98 Si  II$\lambda $1808
Q 0405-443 CTS 247 3.02 2.550 $21.15\pm 0.15$ $-1.36\pm 0.16$ Zn 165 Si  II$\lambda $1808
Q 0405-443 CTS 247 3.02 2.595 $21.05\pm 0.10$ $-1.12\pm 0.10$ Zn 79 Si  II$\lambda $1808
Q 0405-443 CTS 247 3.02 2.622 $20.45\pm 0.10$ $-2.04\pm 0.10$ Si 182 Si  II$\lambda $1526
Q 0450-131 .... 2.25 2.067 $20.50\pm 0.07$ $-1.62\pm 0.08$ S 148 Fe  II$\lambda $1608
Q 0458-020 LBQS 0458-0203 2.29 2.040 $21.70\pm 0.10$ $-1.22\pm 0.10$ Zn 88 Cr  II$\lambda $2056
Q 0528-250 LBQS 0528-2505 2.77 2.141 $20.98\pm 0.05$ $-1.36\pm 0.06$ Zn 105 Si  II$\lambda $1808
Q 0528-250 LBQS 0528-2505 2.77 2.811 $21.35\pm 0.07$ $-0.91\pm 0.07$ Zn 304 S  II$\lambda $1253
Q 0551-366 .... 2.32 1.962 $20.70\pm 0.08$ $-0.35\pm 0.08$ Zn 468 Si  II$\lambda $1808
Q 0841+129 .... 2.50 1.864 $21.00\pm 0.10$ $-1.51\pm 0.11$ S 32 S  II$\lambda $1259
Q 0841+129 .... 2.50 2.375 $21.05\pm 0.10$ $-1.59\pm 0.10$ Zn 37 Fe  II$\lambda $1125
Q 0841+129 .... 2.50 2.476 $20.80\pm 0.10$ $-1.60\pm 0.10$ Zn 30 S  II$\lambda $1259
Q 0913+072 LBQS 0913+0715 2.78 2.618 $20.35\pm 0.10$ $-2.59\pm 0.10$ Si 22 Si  II$\lambda $1526
Q 1036-229 CTS 460 3.13 2.778 $20.93\pm 0.05$ $-1.36\pm 0.05$ S 80 Fe  II$\lambda $1081
Q 1108-077 BRI 1108-0747 3.92 3.482 $19.95\pm 0.07$ $-1.63\pm 0.07$ Si 49 Si  II$\lambda $1526
Q 1108-077 BRI 1108-0747 3.92 3.608 $20.37\pm 0.07$ $-1.59\pm 0.07$ Si 31 Fe  II$\lambda $1608
Q 1111-152 CTS 298 3.37 3.266 $21.30\pm 0.05$ $-1.65\pm 0.11$ Zn 140 Si  II$\lambda $1020
Q 1117-134 BR 1117-1329 3.96 3.350 $20.95\pm 0.10$ $-1.41\pm 0.11$ Zn 43/45 Si  II$\lambda $1808/Fe  II$\lambda $1608
Q 1157+014 .... 1.99 1.944 $21.80\pm 0.10$ $-1.44\pm 0.10$ Zn 89 Fe  II$\lambda $2260
Q 1209+093 LBQS 1209+0919 3.30 2.584 $21.40\pm 0.10$ $-1.01\pm 0.10$ Zn 214 Si  II$\lambda $1808
Q 1210+175 LBQS 1210+1731 2.54 1.892 $20.70\pm 0.08$ $-0.93\pm 0.08$ S 62 S  II$\lambda $1253
Q 1223+178 LBQS 1223+1753 2.94 2.466 $21.40\pm 0.10$ $-1.63\pm 0.10$ Zn 91 Si  II$\lambda $1808
Q 1232+082 LBQS 1232+0815 2.57 2.338 $20.90\pm 0.08$ $-1.43\pm 0.08$ S 85 Si  II$\lambda $1808
Q 1331+170 .... 2.08 1.776 $21.15\pm 0.07$ $-1.28\pm 0.08$ Zn 75 Fe  II$\lambda $2374
Q 1337+113 LBQS 1337+1121 2.92 2.508 $20.12\pm 0.05$ $-1.81\pm 0.06$ Si 32 Fe  II$\lambda $2344
Q 1337+113 LBQS 1337+1121 2.92 2.796 $21.00\pm 0.08$ $-1.86\pm 0.09$ Si 42 Fe  II$\lambda $1608
Q 1340-136 CTS 325 3.20 3.118 $20.05\pm 0.08$ $-1.42\pm 0.08$ S 153 Fe  II$\lambda $1608
Q 1409+095 LBQS 1409+0930 2.85 2.019 $20.65\pm 0.10$ $-1.62\pm 0.16$ Zn 39 Fe  II$\lambda $2374
Q 1409+095 LBQS 1409+0930 2.85 2.456 $20.53\pm 0.08$ $-2.06\pm 0.08$ Si 69 Si  II$\lambda $1526
Q 1441+276 PSS J 1443+2724 4.42 4.224 $20.95\pm 0.10$ $-0.63\pm 0.10$ S 130 Fe  II$\lambda $1081
Q 1444+014 LBQS 1444+0126 2.21 2.087 $20.25\pm 0.07$ $-0.80\pm 0.09$ Zn 294 Fe  II$\lambda $1608
Q 1451+123 LBQS 1451+1223 3.25 2.255 $20.35\pm 0.10$ $-1.07\pm 0.15$ Zn 103 Fe  II$\lambda $2374
Q 1451+123 LBQS 1451+1223 3.25 2.469 $20.40\pm 0.10$ $-2.27\pm 0.13$ Si 35 Fe  II$\lambda $2382
Q 1451+123 LBQS 1451+1223 3.25 3.171 $20.20\pm 0.20$ $-2.10\pm 0.21$ Si 45 Si  II$\lambda $1526
Q 2059-360 .... 3.09 2.507 $20.29\pm 0.07$ $-1.85\pm 0.20$ S 25 Fe  II$\lambda $2344
Q 2059-360 .... 3.09 3.083 $20.98\pm 0.08$ $-1.77\pm 0.09$ S 44 Fe  II$\lambda $1121
Q 2116-358 HES 2116-3550 2.34 1.996 $20.10\pm 0.07$ $-0.34\pm 0.11$ Zn 177 Fe  II$\lambda $1608
Q 2138-444 LBQS 2138-4427 3.17 2.383 $20.60\pm 0.05$ $-1.15\pm 0.10$ Zn 131 Fe  II$\lambda $2374
Q 2138-444 LBQS 2138-4427 3.17 2.852 $20.98\pm 0.05$ $-1.74\pm 0.05$ Zn 58/62 Si  II$\lambda $1808/Fe  II$\lambda $2374
Q 2152+137 PSS J 2155+1358 4.26 3.316 $20.50\pm 0.15$ $-1.37\pm 0.15$ Si 74 Fe  II$\lambda $1608
Q 2206-199 LBQS 2206-1958 2.56 1.921 $20.67\pm 0.05$ $-0.54\pm 0.05$ Zn 136 Si  II$\lambda $1808
Q 2206-199 LBQS 2206-1958 2.56 2.076 $20.44\pm 0.05$ $-2.32\pm 0.05$ Si 20 Si  II$\lambda $1304
Q 2230+025 LBQS 2230+0232 2.15 1.864 $20.90\pm 0.10$ $-0.81\pm 0.10$ S 148 S  II$\lambda $1253
Q 2231-002 LBQS 2231-0015 3.02 2.066 $20.55\pm 0.07$ $-0.65\pm 0.07$ S 145 S  II$\lambda $1253
Q 2243-605 HES 2243-6031 3.01 2.331 $20.65\pm 0.05$ $-0.85\pm 0.05$ Zn 173 Si  II$\lambda $1808
Q 2332-094 FIRST J 2334-0908 3.32 2.287 $20.07\pm 0.07$ $-0.33\pm 0.07$ Zn 43 Si  II$\lambda $1808
Q 2332-094 FIRST J 2334-0908 3.32 3.057 $20.50\pm 0.07$ $-1.33\pm 0.08$ S 111 Fe  II$\lambda $1608
Q 2343+125 .... 2.51 2.431 $20.40\pm 0.07$ $-0.92\pm 0.07$ Zn 289 Fe  II$\lambda $1608
Q 2344+125 .... 2.76 2.538 $20.50\pm 0.10$ $-1.81\pm 0.10$ Si 69 Fe  II$\lambda $1608
Q 2348-011 LBQS 2348-0108 3.01 2.426 $20.50\pm 0.10$ $-0.64\pm 0.10$ S 248 Fe  II$\lambda $1608
Q 2348-011 LBQS 2348-0108 3.01 2.615 $21.30\pm 0.08$ $-2.02\pm 0.08$ Si 95/105 Si  II$\lambda $1808/Si  II$\lambda $1526
Q 2348-147 .... 2.94 2.279 $20.63\pm 0.05$ $-2.10\pm 0.08$ S 55 Fe  II$\lambda $2586
Q 2359-022 LBQS 2359-0216 2.81 2.095 $20.65\pm 0.10$ $-0.84\pm 0.13$ Zn 146 Fe  II$\lambda $1608
Q 2359-022 LBQS 2359-0216 2.81 2.154 $20.30\pm 0.10$ $-1.62\pm 0.10$ Si 67 Si  II$\lambda $1526
$^\ast $ Total neutral hydrogen column density and metallicity measurements are from this work, except for the systems at $z_{\rm abs}=3.390$toward Q 0000-263 (Molaro et al. 2001), $z_{\rm abs}=3.025$ and 2.087 toward Q 0347-383 and Q 1444+014 (Ledoux et al. 2003), respectively, $z_{\rm abs}=1.962$toward Q 0551-366 (Ledoux et al. 2002), and $z_{\rm abs}=4.224$ toward Q 1441+276 (Ledoux et al. 2006).
Quoted uncertainties are $1\sigma$ standard deviations.
1 There are a few DLA systems with $c\vert z_{\rm em}-z_{\rm abs}\vert/(1+z_{\rm abs})<5000$ km s-1. These systems were not considered during the correlation analyses. However, their properties (metallicity, N(H  I), ionization level) do not resemble those of the associated systems. They are not associated with the central engine of the quasar, nor ejected by the quasar, but rather associated with dense gas in its surroundings (see text).
2 Average gaseous metallicities relative to solar, [X/H $]\equiv\log [N($X)/N(H $)]-\log [N($X)/N(H$)]_\odot$, calculated using solar abundances listed in Morton (2003), which are based on meteoritic data from Grevesse & Sauval (2002). The reference element was taken to be X = Zn when Zn  II is detected, or else either S or Si was used.
3 Transition lines used to determine the velocity widths of low-ionization line profiles. Whenever none of the observed lines satisfied the adopted criterion (see Sect. 2), we used the mean value of the velocity widths calculated from (i) a slightly more saturated line, and (ii) a slightly weaker line than what the criterion specifies.

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