Table 1
Light curve fit parameters for the afterglow of GRB 091127.
| Band | α1 | tbreak [s ] | s | α2 | χ2/d.o.f. |
|
|
|||||
| XRT | 1.019 ± 0.039 | 33472 ± 3349 | 2.367 ± 0.986 | 1.605 ± 0.038 | 373/363 |
| g′ | 0.427 ± 0.011 | 33917 ± 2047 | 1.210 ± 0.125 | 1.687 ± 0.050 | 125/144 |
| r′ | 0.376 ± 0.009 | 29287 ± 1195 | 1.274 ± 0.100 | 1.557 ± 0.033 | 143/144 |
| i′ | 0.359 ± 0.014 | 30288 ± 1671 | 1.293 ± 0.141 | 1.532 ± 0.042 | 133/144 |
| z′ | 0.321 ± 0.016 | 32368 ± 2295 | 1.054 ± 0.124 | 1.609 ± 0.056 | 131/144 |
| J | 0.300 ± 0.077 | 24462 ± 4453 | 1.483 ± 0.728 | 1.396 ± 0.147 | 26/37 |
| H | 0.164 ± 0.057 | 21677 ± 4310 | 1.005 ± 0.106 | 1.417 ± 0.068 | 34/37 |
Notes. The temporal slopes have inaccuracies caused by a very smooth break, which reduces the number of datapoints used in the power-law slopes fitting. The fitting of the NIR bands is affected by the somewhat lower signal-to-noise ratio of the NIR data as compared to the optical bands.
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