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Table 1

GRB host galaxy column densities for 29 GRBs.

Galactic parameters GRB host interstellar and circumstellar parameters
GRB z log NH A V log NHI log NSiII log NSII log NFeII log NZnII log NO,X A V
log (cm-2) mag log (cm-2) log (cm-2) log (cm-2) log (cm-2) log (cm-2) log (cm-2) mag

990123 1.600 20.26 0.05 ... ... ... 13.95 ± 0.051  <0.252
000926 2.038 20.35 0.07 21.30 ± 0.203 ... 13.82 ± 0.051 0.02 0.38 ± 0.052
010222 1.475 20.22 0.07 ... 16.09 ± 0.051 ... 13.78 ± 0.071 18.75 ± 0.162
020405 0.691 20.62 0.17 ... ... ... 15.05 ± 0.754 ...  <18.695 0.42 ± 0.025
020813 1.255 20.79 0.34 ... 16.29 ± 0.046 ... 15.48 ± 0.046 13.54 ± 0.066 ... ...
030226* 1.987 20.20 0.06 20.50 ± 0.307 15.07 ± 0.047  >13.37  <12.707  <18.605 0.05 ± 0.015
1.963 20.50 ± 0.307 14.97 ± 0.037 ...  <12.607
030323 3.371 20.61 0.15 21.90 ± 0.078 15.84 ± 0.198 15.93 ± 0.088  <14.508 ... ...
050401 2.899 20.64 0.20 22.60 ± 0.309 16.50 ± 0.409 ... 16.00 ± 0.209 14.30 ± 0.309 0.45 ± 0.035
050505 4.275 20.23 0.06 22.05 ± 0.1011 15.70 ± 0.0011 16.111 15.50 ± 0.0011 ... 18.93 ± 0.0510 ...
050730 3.969 20.48 0.16 22.10 ± 0.1012 15.47 ± 0.0312 15.11 ± 0.0412 ...  <0.1713
050820A 2.615 20.64 0.14 21.05 ± 0.1012  >15.4314 15.57 ± 0.0414 14.82 ± 0.1214 12.96 ± 0.0214 0.27 ± 0.0413
050904 6.295 20.66 0.18 21.62 ± 0.2015  <16.6016 15.95 ± 0.5516 ... ...  <0.0734
050922C 2.199 20.73 0.32 21.55 ± 0.1012 14.97 ± 0.0717 14.87 ± 0.0512 ...
051111 1.549 20.72 0.50 ...  >16.1414 ... 15.32 ± 0.0114 13.47 ± 0.0414
060206 4.048 19.95 0.04 20.85 ± 0.1018 15.23 ± 0.0419 15.13 ± 0.0519  >14.6520 ...  <0.2413
060418 1.490 20.94 0.69 ... 15.92 ± 0.0321 ... 15.22 ± 0.0314 13.09 ± 0.0121
060510B 4.941 20.61 0.12 21.30 ± 0.1022 ...  >15.9023 ... ...
060526 3.221 20.70 0.21 20.01 ± 0.1524  >14.4824 14.58 ± 0.2524 14.28 ± 0.2424  <12.7324  <18.1213  <0.5913
070802 2.450 20.46 0.08 21.50 ± 0.2025 16.41 ± 0.1725 ... 16.44 ± 0.1225 13.97 ± 0.1425
071003 1.604 21.03 0.47 ... ... ...  <12.7527 ...
071031 2.692 20.09 0.04 22.15 ± 0.0512 ... ... 15.83 ± 0.0212 13.02 ± 0.0212  <0.1126
080319B 0.937 20.05 0.03 ... ... ... ...
080330 1.511 20.09 0.05 ...  >15.4129 ... 14.70 ± 0.0929 12.79 ± 0.0629  <0.1926
080413A 2.433 20.94 0.48 21.85 ± 0.1512 ... ... 15.57 ± 0.0412 12.85 ± 0.0612  <0.8813
080607 3.036 20.23 0.07 22.70 ± 0.1530  >16.2029  >16.1430  >16.3530  >13.6030 ...
080721 2.591 20.84 0.31 21.60 ± 0.1031  >16.0031 ... ... ...
090323 3.577 20.23 0.08 19.62 ± 0.335 15.46 ± 0.135 15.41 ± 0.045 14.91 ± 0.055  <12.75  <18.655 0.10 ± 0.045
3.567 20.72 ± 0.095 15.80 ± 0.055 15.80 ± 0.025 15.00 ± 0.055 13.57 ± 0.045
090328 0.736 20.70 0.18 ... ... ... ... 0.34 ± 0.045
090926A 2.106 20.44 0.07 21.73 ± 0.0733 14.97 ± 0.2633 14.96 ± 0.1533 14.36 ± 0.1433  <13.0033  <18.745  <0.15

Notes. Columns list redshift, Galactic column density and visual extinction in the line-of-sight to the GRB, the H i, Si ii, S ii, Fe ii and Zn ii column density with corresponding references, the oxygen column density measured from the X-ray spectra, NO,X, and the best-fit visual extinction, AV, with both corresponding references given. For GRB 030226 and GRB 090323, two absorbing components were detected within the GBR host galaxy, and the optical column densities for both are given where applicable.

(*)

Where two host galaxy absorption systems are reported, we used the combined column densities of the two systems in our analysis.

References. 1 Savaglio et al. (2003); 2 Starling et al. (2007); 3 Hjorth et al. (2003); 4 Masetti et al. (2003); 5 this work; 6 Savaglio & Fall (2004); 7 Shin et al. (2006); 8 Vreeswijk et al. (2004); 9 Watson et al. (2006); 10 Evans et al. (2009); 11 Berger et al. (2006); 12 Ledoux et al. (2009); 13 Schady et al. (in prep); 14 Prochaska et al. (2007a); 15 Totani (2006); 16 Kawai et al. (2006); 17 Piranomonte et al. (2008); 18 Fynbo et al. (2006); 19 Thöne et al. (2008a); 20 Aoki et al. (2009); 21 Vreeswijk et al. (2007); 22 Chary et al. (2007); 23 Price et al. (2007); 24 Thöne et al. (2008b); 25 Elíasdóttir et al. (2009); 26 Greiner et al. (2010); 27 Perley et al. (2008a); 28 D’Elia et al. (2009); 29 D’Elia et al. (2009); 30 Prochaska et al. (2009); 31 Starling et al. (2009); 32 McBreen et al. (2010); 33 Rau et al. (2010); 34 Zafar et al. (2010).

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