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Catalogue XRT results for GRB 060306
Data were analysed using HEASOFT version 6.32
Summary Information
| RA: | 02h 44m 22.86s | LC breaks: | 2 |
|---|---|---|---|
| Dec: | -02° 08′ 54.9′′ | LC type: | Canonical. |
| Err: | 1.4′′ | NH,intr.: | 3.97×1022 cm-2 |
| Gal long: | 175.029 | Redshift | 1.55 |
| Gal lat: | -53.190 | Γ | 2.0 |
Jump to: Light curve | Spectra | Compare to other bursts.
If you use any of these data, please cite Evans et al. (2009), which describes how these products were created (see the usage policy for more information).
Light curve
This light curve comes from the light curve repository (if you use it, please cite Evans et al [2007, 2009]. Flares, marked by cross-hatched regions, are identified automatically, but may have been manually corrected. These are excluded from the fit. Any power-law breaks added to the fit must be required at the 4-σ level (according to an f-test) to be included in the best-fit. Details of all fits attempted are given below the plot. For more information see the light curve fitting documentation.
Fit Details
| Nbreaks | χ2 | dof | Comments | Image |
|---|---|---|---|---|
| 0 | 326 | 90 |  | |
| 1 | 201 | 88 | Break required. (5.28e-08 % probability of chance improvement) |  |
| 2 | 92.1 | 86 | Break required. (2.59e-13 % probability of chance improvement). This is the best fit. |  |
| 3 | 81.6 | 84 | Break significance <4-σ (0.64 % probability of chance improvement) |  |
| 4 | 80.1 | 82 | Break significance <4-σ (2.08 % probability of chance improvement) |  |
There are no flares ignored from this fit.
The best-fitting light curve has 2 breaks.
Click on the number of breaks in the table to the right to change which fit is plotted above and detailed below.
Currently showing the best fit.
| α1 | 4.1 (+0.6, -0.8) |
|---|---|
| Tb,1 | 173 (+25, -12) s |
| α2 | 0.58 (+0.05, -0.06) |
| Tb,2 | 6501 (+2.60 × 103, -1690) s |
| α3 | 1.09 (+0.06, -0.05) |
Spectra
Spectra have been created for each power-law segment in the best fitting light curve (shown above). Times of flaring have not been removed, however this makes little difference to most spectra (see Fig 7/8c of Evans et al. 2009). For more information see the time-resolved spectroscopy documentation.
No spectra are available for this object.