Table 1: Lines detected above 3$\sigma $ in the first and second epoch WHT spectraa.

$\lambda$		 $W_{\rm obs}\rm (I)$ $W_{\rm obs}\rm (II)$ ID z
4683.0b     $\rm Ly\beta~\lambda$ 1025.722 3.5656
5090.6b     $\rm Ly\beta~\lambda$ 1025.722 3.9629
5549.2b     $\rm Ly\alpha~\lambda$ 1215.668 3.5647
6031.5b     $\rm Ly\alpha~\lambda$ 1215.668 3.9615
6230.8 $1.42 \pm 0.24 $ $1.19 \pm 0.38 $ S II $\lambda$ 1253.805 3.9695
6261.9 $3.64 \pm 0.25 $ $3.50 \pm 0.41 $ Si II $\lambda$ 1260.422 3.9681
    blended with S II $\lambda$ 1259.518 3.9717
6283.9 $3.95 \pm 0.23$ $3.45 \pm 0.33$ Si II* $\lambda$ 1264.738 3.9685
6364.2 $0.51 \pm 0.17$ $0.78 \pm 0.35$ C I? $\lambda$ 1280.135 3.9715
6470.8 $1.95 \pm 0.17$ $2.43 \pm 0.39$ O I $\lambda$ 1302.169 3.9692
6482.8 $2.57 \pm 0.14$ $2.87 \pm 0.28$ O I* $\lambda$ 1304.858 3.9682
    blended with Si II $\lambda$ 1304.370 3.9700
6489.8 $0.50 \pm 0.11$ $0.82 \pm 0.20$ O I** $\lambda$ 1306.029 3.9691
6504.6 $1.86 \pm 0.16$ $2.17 \pm 0.35$ Si II* $\lambda$ 1309.276 3.9681
    blended with? Fe II $\lambda$ 2344.214 1.7747
6544.6 $0.44 \pm 0.13$ $0.47 \pm 0.17$    
6583.9 $0.42 \pm 0.10$ $0.55 \pm 0.18$    
6588.9 $0.55 \pm 0.11$ $0.57 \pm 0.17$    
6597.1 $0.82 \pm 0.12$ $1.33 \pm 0.26$    
6607.0 $1.24 \pm 0.14$ $1.58 \pm 0.23$ Fe II $\lambda$ 2382.765 1.7728
6633.4 $5.12 \pm 0.19$ $5.07 \pm 0.31$ C II $\lambda$ 1334.532 3.9706
    blended with C II* $\lambda$ 1335.663 3.9664
6721.0 $1.05 \pm 0.17$ $0.73 \pm 0.20$    
6924.1 $2.43 \pm 0.15$ $2.42 \pm 0.32$ Si IV $\lambda$ 1393.760 3.9679
6934.0 $0.88 \pm 0.09$ $1.18 \pm 0.24$    
6968.7 $2.67 \pm 0.15$ $2.32 \pm 0.28$ Si IV $\lambda$ 1402.773 3.9678
    blended with Si II $\lambda$ 1526.707 3.5645
6989.4 $1.44 \pm 0.17$ $1.28 \pm 0.22$    
7000.9 $0.52 \pm 0.09$ $0.86 \pm 0.24$ Si II* $\lambda$ 1533.432 3.5655
7066.1 $0.42 \pm 0.12$ $0.20 \pm 0.19$ C IV $\lambda$ 1548.204 3.5641
7077.7 $0.32 \pm 0.12$ $0.48 \pm 0.18$ C IV $\lambda$ 1550.781 3.5640
7107.4 $0.62 \pm 0.14$ $0.61 \pm 0.22$    
7172.6 $0.71 \pm 0.14$ $0.92 \pm 0.25$ Fe II $\lambda$ 2586.650 1.7729
7209.0 $1.46 \pm 0.17$ $0.86 \pm 0.20$ Fe II $\lambda$ 2600.173 1.7725
7586.4c $2.53 \pm 0.18$ $2.48 \pm 0.26$ Si II $\lambda$ 1526.707 3.9691
7628.5c     Al II $\lambda$ 1670.789 3.5658
7692.9 $3.79 \pm 0.14$ $3.86 \pm 0.29 $ C IV $\lambda$ 1548.204 3.9689
7705.3 $3.66 \pm 0.20$ $4.22 \pm 0.36 $ C IV $\lambda$ 1550.781 3.9687
7754.9 $4.18 \pm 0.34$ $5.15 \pm 0.63 $ Mg II $\lambda$ 2798.743 1.7709
7775.5 $2.28 \pm 0.25$ $2.67 \pm 0.36 $ Mg II $\lambda$ 2803.532 1.7735
7994.3 $3.14 \pm 0.54$ $3.27 \pm 0.74 $ Fe II $\lambda$ 1608.451 3.9716
a Blueward of Ly$\alpha$ the low resolution and Ly$\alpha$ forest hampers secure identification of metal lines, which we therefore do not list.

b Due to the uncertain continuum level, we do not attempt to measure the widths of the Ly$\alpha$ and Ly$\beta$ lines.

c This equivalent width measurement is seriously affected or made impossible by the atmospheric absorption band from 7584-7675 Å.


Source LaTeX | All tables | In the text

Article Contents
1 Introduction
2 The optical afterglow spectra
3 The absorbed X-ray afterglow
4 Discussion and conclusions
References
Online Material
List of tables
List of figures