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Table 2:

Characteristics of the Mg  II absorbers in the UVES sample.
GRB $z_{\rm GRB}$ $\Delta z$ $\Delta z$ $z_{\rm abs}$ $W_{\rm r}(\lambda2796)$ $v_{\rm ej}$ Remarks
    $W_{\rm r}>$ 0.3 Å $W_{\rm r}>$ 1 Å   (Å) (km s-1)  

021004

2.3295 1.754 1.756 0.5550 $0.248\pm0.025$ $\sim$192 000 blended with AlII1670 at z=1.6026
        1.3800 $1.637\pm0.020$ $\sim$97 000  
        1.6026 $1.407\pm0.024$ $\sim$72 000  

050730

3.9687 1.278 1.298 1.7732 $0.927\pm0.030$ $\sim$157 000  
        2.2531 < 0.783  (0.650) $\sim$120 000 sky contamination subtracted

050820A

2.6147 1.843 1.845 0.6896 $0.089\pm0.007$ $\sim$192 000  
        0.6915 $2.874\pm0.007$ $\sim$192 000  
        1.4288 $1.323\pm0.023$ $\sim$113 000  
        1.6204 $0.277\pm0.024$ $\sim$93 000  
        2.3598 < 0.424 (0.306) $\sim$22 000 contribution by FeII2600 at z=2.6147
              subtracted

050922C

2.1996 1.679 1.682 0.6369 $0.179\pm0.018$ $\sim$175 000  
        1.1076 $0.677\pm0.029$ $\sim$118 000  
        1.5670 < 0.102  (0.08) $\sim$62 000 sky contamination subtracted

060418

1.4900 1.242 1.265 0.6026 $1.293\pm0.010$ $\sim$124 000  
        0.6559 $1.033\pm0.006$ $\sim$116 000  
        1.1070 $1.844\pm0.014$ $\sim$50 000  

060607A

3.0748 1.710 1.713 1.5103 $0.204\pm0.011$ $\sim$135 000  
        1.8033 $1.854\pm0.006$ $\sim$107 000  
        2.2783 $0.343\pm0.058$ $\sim$64 000  

071031

2.6922 1.727 1.789 1.0743 $0.330\pm0.016$ $\sim$156 000  
        1.6419 $0.692\pm0.014$ $\sim$97 000  
        1.9520 $0.804\pm0.016$ $\sim$66 000  

080310

2.4272 1.841 1.841 1.1788 $0.047\pm0.024 $ $\sim$127 000  
        1.6711 $0.421\pm0.012$ $\sim$73 000  

080319B

0.9378 0.790 0.790 0.5308 $ 0.614\pm0.001$ $\sim$69 000  
        0.5662 $0.083\pm0.003$ $\sim$63 000  
        0.7154 $1.482\pm0.001$ $\sim$36 000  
        0.7608 $0.108\pm0.002$ $\sim$29 000  
080413A 2.4346 1.583 1.650 2.1210 $ 0.768\pm0.259$ $\sim$29 000  

Source LaTeX | All tables | In the text

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