Table 4.
Fluxes and properties of the observed Lyα emission line.
| GRB host | F(Lyα) | EW0(Lyα) | FWHM0(Lyα) | Lyα red-peak shift | fesc(Lyα) | Fi(Lyα) |
|---|---|---|---|---|---|---|
| [10−17 erg s−1 cm−2] | [Å] | [km s−1] | [km s−1] | [10−17 erg s−1 cm−2] | ||
| GRB 011211 | 1.6 ± 0.2 | 14 ± 3 | 249 ± 60 | 280 ± 30 | > 0.16 | <10.4 |
| GRB 021004 | 16.9 ± 0.3 | 105 ± 10 | 228 ± 20 | 180 ± 20 | 0.59 ± 0.08 | 28.8 ± 3.5 |
| GRB 060926 | 5.3 ± 0.4 | 37 ± 7 | 417 ± 40 | 250 ± 20 | 0.13 ± 0.03 | 40.0 ± 7.9 |
| GRB 070110 | 2.8 ± 0.5 | 33 ± 8 | 412 ± 80 | 285 ± 40 | 0.36 ± 0.09 | 7.8 ± 2.7 |
Notes. The Lyα fluxes are corrected for Galactic extinction and slit loss. No correction for host-intrinsic extinction is applied. The EW0(Lyα) and FWHM0(Lyα) are the rest-frame equivalent width and FWHM of the observed Lyα line. The Lyα red-peak shift is the velocity shift of the Lyα peak redward of the theoretical Lyα line center, as calculated from the systemic redshift of the galaxy (see Table 2). The escape fraction of Lyα photons (fesc(Lyα)) and the intrinsic flux of the Lyα line (Fi(Lyα)) are determined from Balmer lines as described in Sect. 3. We stress that these escape fractions are not corrected for dust extinction, as explained in Sect. 3.
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