Table 3: Lines detected above 5$\sigma $ in the low- (lr) and high-resolution (hr) spectra.
$\lambda$(lr) ${\it EW}_{\rm rest}$(lr) $\lambda$(hr) ${\it EW}_{\rm rest}$(hr) IDb,c z
4484 9 (1)a     Ly$\beta$ $\lambda$1025.7 3.3715
5317   5316.9   Ly$\alpha $ em. $\lambda$1215.6 3.3736
    5415.8 0.31 (3) N V $\lambda$1238.8 3.3717
    5433.5 0.20 (2) N V $\lambda$1242.8 3.3720
    5465.4 0.15 (2)    
    5467.4 0.21 (3) S II $\lambda$1250.5 3.3719
5483 0.44 (6) 5481.1 0.29 (2) S II $\lambda$1253.8 3.3716
5511 1.07 (5) 5505.0 0.33 (2) S II $\lambda$1259.5 3.3707
    5509.7 1.00 (2) Si II $\lambda$1260.4 3.3713
        or  Fe II $\lambda$1260.5 3.3709
5530 0.76 (5) 5529.2 0.75 (2) Si II* $\lambda$1264.7 3.3718
    5591.5 0.11 (2) $\oplus $, C I $\lambda$1280.1? 3.3679
    5595.7 0.10 (2)    
    5624.4 0.11 (2)    
5637 0.33 (5) 5634.7 0.16 (2)    
    5649.2 0.16 (1)    
    5652.0 0.15 (1) Fe II $\lambda$2344.2? 1.4110
5692 0.75 (6) 5692.5 0.69 (2) O I $\lambda$1302.1 3.3716
5706 1.08 (6) 5702.4 0.70 (2) Si II $\lambda$1304.3 3.3718
        and O I* $\lambda$1304.8? 3.3702
5706 1.08 (6) 5709.7 0.32 (2) O I** $\lambda$1306.0? 3.3718
5727 0.26 (5) 5723.9 0.29 (2) Si II* $\lambda$1309.2 3.3718
5838 1.71 (7) 5833.7 0.84 (3) C II $\lambda$1334.5 3.3713
    5838.9 0.79 (2) C II* $\lambda$1335.7 3.3714
6095 1.19 (6) 6092.9 1.08 (4) Si IV $\lambda$1393.7 3.3716
6135 0.98 (6) 6132.4 1.15 (4) Si IV $\lambda$1402.7 3.3716
6280 0.51 (3) 6278.0 0.42 (3) $\oplus $, Fe II$\lambda$2600.1? 1.4145
    6629.2 0.14 (2)    
6676 0.69 (4) 6673.8 0.75 (3) Si II $\lambda$1526.7 3.3714
6706 0.54 (4) 6703.7 0.34 (3) Si II* $\lambda$1533.4 3.3717
    6743.0 0.14 (2) Mg II $\lambda$2796.3? 1.4114
    6754.2 0.13 (2) Mg II $\lambda$2803.5? 1.4092
    6760.6 0.14 (3)    
6770 1.42 (4) 6766.9 0.99 (3) C IV $\lambda$1548.2 3.3708
    6769.9 0.51 (3) C IV $\lambda$1548.2 3.3728
6782 1.28 (4) 6778.2 0.84 (3) C IV $\lambda$1550.7 3.3708
    6781.0 0.53 (3) C IV $\lambda$1550.7 3.3727
6875   6870.4   $\oplus $  
    6876.5   $\oplus $  
6900   6891.9   $\oplus $  
    6902.4   $\oplus $  
7034 0.51 (4) 7031.7 0.48 (3) Fe II $\lambda$1608.4 3.3717
    7043.6 0.17 (3) Fe II $\lambda$1611.2 3.3716
    7082.0 0.15 (3)    
    7160.1 0.20 (3)    
    7202.7 0.17 (3) $\oplus $  
7307 1.08 (5) 7303.5 0.99 (7) Al II $\lambda$1670.7 3.3713
7907 0.58 (5)     Si II $\lambda$1808.0 3.3734
8112 0.45 (5)     Al III $\lambda$1854.7 3.3738
8145 0.23 (4)     Al III $\lambda$1862.7 3.3724
8237 0.34 (4)        
8802 0.55 (6)        
8859 0.82 (9)     Zn II $\lambda$2026.1 3.3725
8970 0.73 (11)     $\oplus $  
9019 0.77 (5)     $\oplus $, Zn II $\lambda$2062.6 3.3726
a Ly$\beta$ is located in the Ly$\alpha $ forest, which causes it to be blended with forest lines, and the continuum placement is highly uncertain, resulting in a large EW error.
b The lines at $\lambda\lambda$5652.0, 6278.0, 6743.0, and 6754.2 can in principle be identified with Fe II and Mg II at z=1.41; however, strong absorption is then expected from Fe II $\lambda$2382, which is not detected.
c The lines for which significant absorption was also detected in the standard star spectrum are marked with a $\oplus $.


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