Table C.1.
Summary of the measured supernova parameters.
| GRB | 071112C | 111228A | 120714B | 130831A |
|---|---|---|---|---|
| kg′ | ... | ... | ... | 0.87 ± 0.24 |
| kr′ | 0.53 ± 0.17 | 0.63 ± 0.14 | 0.47 ± 0.05 | 0.61 ± 0.04 |
| ki′ | 0.70 ± 0.17 | 0.73 ± 0.15 | 0.74 ± 0.06 | 0.99 ± 0.05 |
| kz′ | 0.52 ± 0.21 | 0.85 ± 0.27 | 0.78 ± 0.08 | 0.58 ± 0.12 |
| sg′ | ... | ... | ... | 0.64 ± 0.09 |
| sr′ | 0.75 ± 0.19 | 1.58 ± 0.23 | 0.66 ± 0.04 | 0.80 ± 0.02 |
| si′ | 0.78 ± 0.23 | 1.20 ± 0.25 | 0.91 ± 0.06 | 0.72 ± 0.02 |
| sz′ | 0.71 ± 0.35 | 1.45 ± 0.25 | 0.95 ± 0.09 | 0.72 ± 0.07 |
| tg′,obs, p (days) | ... | ... | ... | 13.7 ± 2.5 |
| tr′,obs, p | 23.1 ± 6.6 | 45.8 ± 9.1 | 15.6 ± 2.3 | 20.0 ± 2.8 |
| ti′,obs, p | 26.2 ± 8.7 | 37.9 ± 9.8 | 23.4 ± 4.9 | 19.6 ± 3.0 |
| tz′,obs, p | 24.7 ± 12.8 | 47.5 ± 11.3 | 25.4 ± 5.9 | 20.3 ± 3.8 |
| tg′,obs, p | ... | ... | ... | 9.3 ± 1.7 |
| tr′,obs, p | 12.7 ± 3.6 | 26.7 ± 5.3 | 11.2 ± 1.7 | 13.5 ± 1.9 |
| ti′,obs, p | 14.4 ± 4.8 | 22.1 ± 5.7 | 16.7 ± 2.8 | 13.2 ± 2.0 |
| tz′,obs, p | 13.6 ± 7.0 | 27.7 ± 6.6 | 18.1 ± 3.4 | 13.8 ± 2.6 |
| log Lbol (erg s−1) | 42.73 ± 0.08 | 42.83 ± 0.09 | 42.79 ± 0.05 | 42.84 ± 0.05 |
| tp (days) | 11.9 ± 2.4 | 22.7 ± 2.2 | 13.6 ± 0.7 | 11.9 ± 0.3 |
| vexp; obs (km s−1) | ... | ... | 43 000 ± 5300 | 20 400 ± 3500 |
| vexp; peak | ... | ... | 42 000 ± 5500 | 30 300 ± 6000 |
Notes. The first eight rows summarize the measured (s, k) values in the GROND g′r′i′z′ bands. The following rows contain the corresponding SN peak times in the observer as well as in the host galaxy frame, tp(SN) = tp(SN 1998bw) × s. Thereby we used the light-curve peak times for SN 1998bw as they follow from our SN fitting procedure (Zeh et al. 2004): tp(g′) = 14.5 ± 1.7, tp(r′) = 16.9 ± 2.3, tp(i′) = 18.4 ± 2.8, tp(z′) = 19.1 ± 3.1 days. The following two rows provide the bolometric luminosity, 
, as well as the bolometric light-curve peak time (given by 
, with 
days; Prentice et al. 2016). The two last rows list the photospheric expansion velocity as it was measured and its calculated value for the time of the peak of the bolometric light curve.
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