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Table 3:

Interstellar absorption lines.

Ion
$\lambda_{\rm lab}$a f $z_{\rm abs}$b $\Delta\upsilon$c W0d $\sigma (W_0)$d $\log N_{\rm aod}$ $\sigma (\log N_{\rm aod})$ $\log N_{\rm adopt}$e $\sigma (\log N_{\rm adopt})$e [X/H]f $\sigma$([X/H])f
  (Å)     (km s-1) (Å) (Å) (cm-2) (cm-2) (cm-2) (cm-2)    
H I 1215.6700 0.41640             20.57 0.10    
O I 1302.1685 0.04887 B  -985 to +315 3.62 0.41 > $15.99^{\dag }$   >15.99   >-1.24  
N V 1238.8210 0.15700 2.7334  -260 to +50  0.24 0.03 14.13 0.09 14.23 0.10    
  1242.8040 0.07823 2.7335  -260 to +50  0.21 0.02 14.32 0.10        
C II 1334.5323 0.12780 2.7321  -985 to +315 4.04 1.73 > $15.84^{\dag }$   >15.84   >-1.12  
C IV 1548.1949 0.19080 B -1290 to +320 5.65 2.39 > $15.60^{\dag }$   >15.93      
  1550.7700 0.09522 B -1290 to +320 5.84 2.46 > $15.93^{\dag }$          
Si II 1260.4221 1.00700 2.7319  -845 to +315 3.23 0.56 > $14.72^{\dag }$   15.89 0.10 -0.19 0.14
  1304.3702 0.09400 B  -795 to +225 2.73 0.32 > $15.60^{\dag }$          
  1526.7065 0.12700 2.7319  -795 to +225 3.48 1.81 > $15.55^{\dag }$          
  1808.0129 0.00218 2.7324  -450 to +15  0.43 0.05 15.89 0.10        
Si II* 1264.7377 0.90340 2.7326  -450 to +15  0.48 0.06 13.67 0.10 13.62 0.10    
  1309.2758 0.14680 2.7329  -340 to +15  0.07 0.01 13.56 0.10        
  1533.4312 0.22930 Noisy  -450 to +95  0.25 0.03 <13.78          
Si IV 1393.7550 0.52800 2.7320 -1055 to +445 3.61 0.73 > $15.06^{\dag }$   >15.06      
  1402.7700 0.26200 2.7322 -1055 to +445 2.79 0.37 > $15.06^{\dag }$          
S II 1250.5840 0.00545 2.7333  -340 to +15  0.24 0.03 15.56 0.10 15.43 0.10 -0.28 0.14
  1253.8110 0.01088 2.7328  -340 to +15  0.24 0.03 15.26 0.10        
Al II 1670.7874 1.88000 2.7317  -795 to +225 3.19 0.45 > $14.12^{\dag }$   >14.12   >-0.82  
Al III 1854.7164 0.53900 2.7323  -415 to +30  1.81 0.40 14.36 0.22 14.38 0.18    
  1862.7896 0.26800 2.7326  -415 to +30  1.19 0.18 14.39 0.15        
Fe II 1608.4510 0.05850 2.7313  -795 to +150 1.28 0.13 15.11 0.09 15.14 0.11 -0.88 0.15
  2344.2129 0.11420 2.7317  -795 to +150 3.16 0.41 > $14.97^{\dag }$          
  2374.4612 0.03131 2.7326  -450 to +15  1.46 0.21 15.17 0.13        
  2382.7649 0.32000 2.7320  -795 to +225 4.16 1.25 > $14.76^{\dag }$          
Zn II 2026.1360 0.48900 2.7331  -340 to +15  0.47 0.05 13.48 0.09 <13.48   <+0.31  
  2062.6641 0.25600 B  -340 to +15  0.29 0.03 <13.53          
Cr II 2056.2539 0.10500 ND  -340 to +15  0.48 0.05 <14.16   <14.09   <-0.12  
  2062.2339 0.07800 ND  -340 to +15  0.32 0.03 <14.09          
Ni II 1317.2170 0.05700 ND  -340 to +15  0.16 0.02 <14.32   <14.32   <-0.48  
  1741.5531 0.04270 ND  -340 to +15  0.41 0.05 <14.62          

Notes. ``B'' indicates cases where a reliable value $z_{\rm abs}$ could not be measured because of strong blending. ``ND'' refers to cases where the line is not detected and only an upper limit to the ion column density could be derived. $^{\dag }$ Refers to saturated lines where only a lower limit to the ion column density could be determined.
(a) Vacuum wavelengths; (b) vacuum heliocentric and values measured from the centroid wavelength of the interstellar absorption lines; (c) velocity range for equivalent width and column density measurements relative to $z_{\rm sys} = 2.7350$; (d) rest-frame equivalent width and $1\sigma $ error; (e) adopted ion column density and $1\sigma $ error; (f) elemental abundance [X/H] = $\log {\rm (X/H)} - \log {\rm (X/H)}_{\odot}$ and $1\sigma $ error as derived from the adopted ion column density relative to the solar meteoritic abundance scale from Grevesse et al. (2007).


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