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Table A.1

Measured line fluxes (10-17 erg cm-2 s-1), corrected for Galactic extinction and stellar Balmer absorption.

GRB [O ii]a [Ne iii] Hδ Hγ Hβ [O iii] Hα [N ii]
λ3726 λ3729 λ4959 λ5007 λ6584
050416A 4.3 ± 0.5 4.1 ± 0.5 <1.3 <1.0 1.1 ± 0.3 1.9 ± 0.4 1.8 ± 0.5 6.3 ± 0.5 11.8 ± 1.4 0.8 ± 0.3
050525Ai <1.7 <1.7 <2.0 <1.6 <2.0 s 1.2 ± 0.4 2.7 ± 0.4 2.2h <2.5
060614 2.8 ± 0.5 <0.7 <1.2 <0.8 0.7 ± 0.2 s 2.8 ± 0.7 2.5 ± 0.5 <1.0
060912A 7.3 ± 0.4 10.8 ± 0.5 1.8 ± 0.5 0.7 ± 0.3 2.5 ± 0.3 5.3 ± 0.5 4.0 ± 0.5t 11.2 ± 1.2 17.4 ± 2.0 3.6 ± 2.5
061021 1.0 ± 0.2 1.0 ± 0.2 <0.6 <0.8 <2.1 0.5 ± 0.1 0.6 ± 0.1 1.7 ± 0.3 1.6 ± 0.3 <0.5
071112C† 1.9 ± 0.4 0.6 ± 0.2s 0.8 ± 0.4 1.2 ± 0.4 <2.0 2.5 ± 0.5 2.4 ± 0.5t
080430 3.5 ± 0.8 2.3 ± 0.5 3.0 ± 0.7 t 4.7 ± 1.8 5.5 ± 1.2 s
080916A 2.9 ± 0.4 s <0.4 <0.5 1.8 ± 0.7t t 3.6 ± 0.6
081007 1.3 ± 0.2 1.6 ± 0.2 <1.4 <1.4 0.8 ± 0.2 1.4 ± 0.2 1.7 ± 0.2 5.9 ± 0.3 5.0 ± 0.3 d
090424 13.8 ± 2.3 s e 1.7 ± 0.4 4.3 ± 0.6 1.3 ± 0.5t 3.5 ± 0.4 19.9 ± 3.3 s
091018b,† 1.7 ± 0.2 2.9 ± 0.4 t <0.8 <0.8 1.3 ± 0.3t 1.7 ± 0.3 4.6 ± 1.0 5.6 ± 1.6s <1.5
091127† 4.2 ± 0.7 5.4 ± 0.9 <1.4 0.7 ± 0.3 0.7 ± 0.2 2.3 ± 0.2 3.0 ± 0.2 7.8 ± 0.3 6.0 ± 0.3 0.5 ± 0.2
100621A 38.4 ± 5.4 49.0 ± 6.0 15.1 ± 3.2 11.4 ± 1.3 17.6 ± 1.3 38.0 ± 2.1 35.6 ± 1.1 130.4 ± 6.3 130.8 ± 11.5 9.7 ± 5.1s

Notes. Upper limits are estimated at 3σ level. No values are reported in cases where a line lies outside the covered spectral range or if it falls in the region of strong telluric absorption and is not detected.

(a)

If only one line is reported, the OII doublet is not resolved.

(b)

Hβ lies in a region a strong telluric absorption, but it is clearly detected. Telluric absorption was modelled with molecfit (Smette et al. 2015; Kausch et al. 2015) using the spectrum of the afterglow (has sufficiently high S/N) and applied to the spectrum. The corrected spectrum was used to measure Hβ.

(t)

Likely affected by (or, if no number, missing due to) significant telluric absorption.

(s)

Likely contaminated (or, if no number, completely dominated) by sky emission line residuals.

(d)

[N ii]lies on the extremely noisy edge of the VIS spectral arm.

(e)

Hδ is observed in absorption. Balmer correction for this host is substantial.

(h)

The line is marginally detected but lies in a very noisy region. We measured its flux by fixing the centre and width of the Gaussian in the fit. The width was assumed to be the same as the one measured from the [O iii]λ5007 line.

(i)

We note that Krühler et al. (2015) did not apply any additional correction to flux calibration for this host, given that the continuum is not detected. Our values of emission line fluxes are consistent with theirs before we applied the correction (Sect. 2.4).

(†)

Spectrum dominated by afterglow.

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