Table 2
Measured redshift, host extinctions, metallicites, and star formation rates of our sample.
GRB | z | log M⋆ | A V a | 12 + ![]() |
SFR | SF-tracer | |
|
|||||||
M ⊙ | (mag) | M08 | KK04 | (M⊙ yr-1) | |||
|
|||||||
050416A | 0.6542 | 9.17![]() |
1.77![]() |
8.50![]() |
8.4 ± 0.2 | 3.45 ± 1.42 | Hα |
050525A† | 0.6063 | 8.1![]() |
– | – | – | >0.10 | [O iii] |
060614A | 0.125 | 8.09![]() |
0.65![]() |
8.46![]() |
8.4 ± 0.2 | 0.007 ± −0.003 | Hα |
060912A | 0.9362 | 9.23![]() |
0.50![]() |
8.60![]() |
8.72![]() |
5.07 ± 0.93 | Hα |
061021 | 0.3453 | 8.5![]() |
0.32![]() |
8.48![]() |
8.4 ± 0.2 | 0.04 ± 0.01 | Hα |
071112C | 0.821 | 8.89![]() |
<0.2 | 7.90![]() |
7.88![]() |
1.1 ± 0.4 | Hγb |
080430 | 0.767 | 8.15![]() |
<0.1 | 7.60![]() |
7.94![]() |
1.65 ± 0.63 | Hβb |
080916A† | 0.688 | 8.98![]() |
– | 8.44![]() |
8.00![]() ![]() |
>0.20 | [O ii] |
081007 | 0.5294 | 8.78![]() |
0.49![]() |
8.32![]() |
8.32![]() ![]() |
0.36 ± 0.07 | Hα |
090424 | 0.5445 | 9.38![]() |
1.42![]() |
8.88![]() |
8.39![]() ![]() |
2.88 ± 1.14 | Hα |
091018 | 0.9710 | 9.52![]() |
1.25![]() |
8.48![]() |
8.4 ± 0.2 | 2.98 ± 1.81 | Hα |
091127 | 0.4904 | 8.67![]() |
<0.3 | 8.50![]() |
8.47![]() |
0.25 ± 0.02 | Hα |
100621A | 0.5426 | 9.04![]() |
0.34![]() |
8.40![]() |
8.25![]() ![]() |
8.92 ± 1.44 | Hα |
Notes. Stellar masses are adopted from Vergani et al. (2015).
Extinction was measured from the Balmer decrement for all cases but GRBs 050525A and 080916A – see text for details.
Flux of the significantly detected Balmer line was first transformed to the Hα flux (see text and Osterbrock & Ferland 2006) and then to the SFR.
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