Table 2
Our final sample of 17 GRBs with afterglows best-fit by a power-law SED model and host galaxy AV detected at 90% confidence.
| GRB | z | Host dust | AV | NH,x | β | χ2 (d.o.f.) | Null hyp. |
| (mag) | (1021 cm-2) | prob. | |||||
|
|
|||||||
| 050802 | 1.71 | mw | 0.49 ± 0.10 |
|
0.72 ± 0.04 | 73.4 (73) | 0.466 |
| 060502A | 1.51 | smc |
|
|
|
23.9 (29) | 0.736 |
| 060607A | 3.082 | smc | 0.08 ± 0.04 |
|
0.52 ± 0.02 | 29.3 (31) | 0.555 |
| 060904B | 0.703 | lmc | 0.15 ± 0.04 |
|
0.85 ± 0.01 | 36.5 (29) | 0.158 |
| 060912 | 0.937 | mw |
|
|
|
16.0 (21) | 0.770 |
| 061007 | 1.262 | smc | 0.44 ± 0.01 | 6.00 ± 0.21 | 0.89 ± 0.01 | 285.5 (289) | 0.548 |
| 070318 | 0.836 | smc | 0.50 ± 0.04 |
|
1.14 ± 0.02 | 63.8 (59) | 0.312 |
| 070810A | 2.17 | mw |
|
|
|
18.3 (23) | 0.742 |
| 071112C | 0.823 | smc |
|
|
0.58 ± 0.02 | 23.7 (17) | 0.128 |
| 080319B | 0.937 | smc |
|
|
0.72 ± 0.01 | 15.1 (14) | 0.372 |
| 080319C | 1.95 | smc |
|
|
0.58 ± 0.04 | 99.7 (98) | 0.432 |
| 080710 | 0.845 | smc | 0.03 ± 0.01 |
|
0.87 ± 0.01 | 39.2 (37) | 0.370 |
| 080928 | 1.692 | smc | 0.24 ± 0.06 |
|
|
33.8 (30) | 0.288 |
| 081008 | 1.968 | lmc | 0.29 ± 0.07 |
|
|
13.2 (23) | 0.947 |
| 090927 | 1.37 | mw |
|
|
0.88 ± 0.08 | 2.2 (9) | 0.989 |
| 091020 | 1.71 | lmc |
|
|
|
40.0 (35) | 0.256 |
| 091208B | 1.063 | lmc |
|
|
|
20.9 (30) | 0.893 |
Notes. Columns (2) and (3) give the GRB redshift and the best-fit host galaxy extinction law; either smc, lmc or mw to refer to the SMC, LMC or Milky Way extinction model fit, and Cols. (4) to (6) are the best-fit host galaxy AV, host galaxy NH, and GRB energy spectral index, β. The last two columns give the χ2 and degrees of freedom (d.o.f.), and the null hypothesis probability of the best-fit solution.
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