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Table 3:

Line Identifications in the GRB 021004 OA spectra.
$\lambda_{\rm vacuum}$(observed) (Å) Line ID EW (Å)a z
4008 H I Ly$\alpha $ 1215.670   2.2967
4015 Si III 1206.499   2.3275
4016 Si III 1206.499   2.3289
4028 C IV 1548.203   1.6024
4038 H I Ly$\alpha $ 1215.670   2.3216
4041 H I Ly$\alpha $ 1215.670   2.3243
4045 H I Ly$\alpha $ 1215.670   2.3275
4047 H I Ly$\alpha $ 1215.670   2.3289
4049b H I Ly$\alpha $ 1215.670   2.3304
4084.0 N V 1238.821 0.46 $\pm$ 0.16 2.2967
4097.2 N V 1242.804 0.35 $\pm$ 0.15 2.2967
4123.9 N V 1238.821 0.90 $\pm$ 0.14 2.3289
4137.2 N V 1242.804 0.66 $\pm$ 0.12 2.3289
4158.5 Si II 1260.422 0.25 $\pm$ 0.10 2.2993
4195.8 Si II 1260.422 0.71 $\pm$ 0.19 2.3289
4210.2 Si II 1264.738 0.51 $\pm$ 0.16 2.3289
4347.4 Al II 1670.787 0.49 $\pm$ 0.17 1.6020
4399.6 C II 1334.530 0.38 $\pm$ 0.15 2.2968
4403.0 C II 1334.530 0.79 $\pm$ 0.14 2.2994
4639.7 Si IV 1393.754 1.39 $\pm$ 0.83 2.3289
4669.7 Si IV 1402.770 1.29 $\pm$ 0.46 2.3289
5104.0 C IV 1548.203 1.77 $\pm$ 0.12 2.2967
5107.8 C IV 1548.203 0.16 $\pm$ 0.03 2.2992
5108.5 C IV 1548.203 0.84 $\pm$ 0.10 2.2998
5112.5 C IV 1550.777 1.15 $\pm$ 0.09 2.2967
5116.2 C IV 1550.777 0.06 $\pm$ 0.04 2.2992
5117.0 C IV 1550.777 0.67 $\pm$ 0.08 2.2998
5138.3 C IV 1548.203   2.3189
5140.0 C IV 1548.203   2.3200
5143.1 C IV 1548.203   2.3220
5146.7 C IV 1550.777   2.3188
5146.7 C IV 1548.203   2.3243
5148.5 C IV 1550.777   2.3200
5148.5 C IV 1548.203   2.3255
5151.7 C IV 1550.777   2.3220
5152.9 C IV 1548.203   2.3275+2.3289
5155.2 C IV 1550.777   2.3243
5157.6 C IV 1550.777   2.3255
5161.5 C IV 1550.777   2.3275+2.3289
5235.4 Si I 1572.718 0.80 $\pm$ 0.10 2.3289
5559.5 Al II 1670.787 0.23 $\pm$ 0.07 2.3275
5561.9 Al II 1670.787 1.73 $\pm$ 0.12 2.3289
5578.0 Fe II 2344.214 1.01 $\pm$ 0.15 1.3796
5651.2 Fe II 2374.461 0.52 $\pm$ 0.06 1.3800
5652.4 Fe II 2374.461 0.16 $\pm$ 0.05 1.3805
5652.9 Fe II 2374.461 0.13 $\pm$ 0.02 1.3807
5671.2 Fe II 2382.765 0.86 $\pm$ 0.07 1.3801
5671.9 Fe II 2382.765 0.41 $\pm$ 0.06 1.3804
5672.6 Fe II 2382.765 0.37 $\pm$ 0.06 1.3807
6099.6 Fe II 2344.214 0.59 $\pm$ 0.04 1.6020
6101.7 Fe II 2344.214 0.28 $\pm$ 0.04 1.6029
6154.5 Fe II 2586.650 0.67 $\pm$ 0.08 1.3794
6155.0 Fe II 2586.650 0.50 $\pm$ 0.09 1.3798
  Fe II 2365.552 0.50 $\pm$ 0.09 1.6020
6174.2 Al III 1854.716 1.15 $\pm$ 0.09 2.3289
6178.0 Fe II 2374.461 0.52 $\pm$ 0.08 1.6020
6187.0 Fe II 2600.173 0.67 $\pm$ 0.10 1.3794
6187.5 Fe II 2600.173 0.44 $\pm$ 0.08 1.3798
6188.0 Fe II 2599.147 0.50 $\pm$ 0.09 1.3808
6201.0 Al III 1862.790 0.73 $\pm$ 0.12 2.3289
6202.0 Fe II 2382.765 0.94 $\pm$ 0.16 1.6028
6654.0 Mg II 2796.352 1.95 $\pm$ 0.11* 1.3796
6655.5 Mg II 2796.352 1.95 $\pm$ 0.11* 1.3802
6657.0 Mg II 2796.352 0.71 $\pm$ 0.08 1.3808
6671.0 Mg II 2803.531 1.89 $\pm$ 0.41* 1.3796
6673.0 Mg II 2803.531 1.89 $\pm$ 0.41* 1.3802
6729.0 Fe II 2586.650 0.25 $\pm$ 0.07 1.6016
6730.2 Fe II 2586.650 0.60 $\pm$ 0.07 1.6020
6732.5 Fe II 2586.650 0.18 $\pm$ 0.06 1.6029
6764.0 Fe II 2600.173 0.56 $\pm$ 0.10 1.6015
6765.5 Fe II 2600.173 0.71 $\pm$ 0.09* 1.6020
  Fe II 2599.147 0.71 $\pm$ 0.09* 1.6030
6768.0 Fe II 2600.173 0.46 $\pm$ 0.09 1.6029
6788.0 Fe II 2607.866 0.14 $\pm$ 0.05 1.6030

7274.2

 Mg II 2796.352 1.11 $\pm$ 0.10 1.6015
7275.5 Mg II 2796.352 0.83 $\pm$ 0.08 1.6020
7277.0 Mg II 2796.352 0.44 $\pm$ 0.07 1.6025
7278.5 Mg II 2796.352 0.83 $\pm$ 0.08 1.6029
7293.0 Mg II 2803.531 0.89 $\pm$ 0.09 1.6015
7294.5 Mg II 2803.531 0.98 $\pm$ 0.09 1.6020
7296.0 Mg II 2803.531 0.24 $\pm$ 0.06 1.6025
7297.0 Mg II 2803.531 1.00 $\pm$ 0.10 1.6029
7803.7 Fe II 2344.214 0.71 $\pm$ 0.28 2.3289
7931.8 Fe II 2382.765 0.46 $\pm$ 0.21 2.3288
16520c [O III] 4960.295 -(16 $\pm$ 7) 2.3304
16679d [O III] 5008.240 -(21 $\pm$ 6) 2.3304
21863e H I 6564.610 -(37 $\pm$ 10) 2.3304

Notes. (a) Gaussian profile fitting (for non saturated lines only). Star symbols refer to complex systems. (b) Emission line. Partially absorbed, Ly$\alpha $ flux = (1.5 $\pm$ 0.2) $\times$ 10-16 erg cm-2 s-1. (c) Emission line [O III] flux = $(4 \pm 3) \times 10^{-17}$ erg cm-2 s-1. (d) Emission line [O III] flux = $(12 \pm 3) \times 10^{-17}$ erg cm-2 s-1. (e) Emission line H$\alpha $ flux = $(11 \pm 2) \times 10^{-17}$ erg cm-2 s-1.


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