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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 8.00/8.99 >0.20 [O ii]
081007 0.5294 8.78 0.49 8.32 8.32/8.58 0.36 ± 0.07 Hα
090424 0.5445 9.38 1.42 8.88 8.39/8.69 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 8.25/8.67 8.92 ± 1.44 Hα

Notes. Stellar masses are adopted from Vergani et al. (2015).

(a)

Extinction was measured from the Balmer decrement for all cases but GRBs 050525A and 080916A – see text for details.

(b)

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.

(†)

Because we lack the Balmer emission lines, the host extinction cannot be computed. Reported star-formation rates are therefore formally lower limits.

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