Table 2.
GRB host sample global kinematical properties.
| GRB | Δv | σint | σ0 | log Mdyn, rot | log Mdyn, σ | log M* | vesc |
|---|---|---|---|---|---|---|---|
| (km s−1) | (km s−1) | (km s−1) | (M⊙) | (M⊙) | (M⊙) | (km s−1) | |
| 020903 | 59 | 34 | 28.4 | 8.54 | 8.96 | 8.94 | 78 |
| 030329 | 15 | 27 | 27.9 | 7.09 | 8.72 | 7.70 | 70 |
| 031203 | 53 | 39 | 11.7 | 8.51 | 8.61 | 8.86 | 47 |
| 050826 | 43 | 55 | 71.6 | 8.90 | 10.3 | 9.99 | 172 |
| 060218 | 23 | 24 | 22.2 | 7.49 | 8.43 | 7.40 | 68 |
| 100316D | 92 | 31 | 19.4 | 9.59 | 9.19 | 9.39 | 61 |
Notes. Δv are the difference between minimum and maximum velocity in the 2D velocity map, vrot = 0.5Δv is also called vshear (see Sect. 4.1). σint is derived from a single Gaussian fit to the integrated spectra of each galaxy. σ0 is the flux weighted dispersion of Hα of all spaxels with sufficient S/N in Hα (see Herenz et al. 2016). The FOV of the host of GRB 100316D does not comprise the entire galaxy. Dynamical masses are derived from Δv, σ0, r80 and r50 (see Table 1), the escape velocity of the galaxy is derived from the dynamical mass used for the respective systems. For the calculations of Mdyn, rot, Mdyn, σ and vesc (see Sect. 4.1).
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