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Catalogue XRT results for GRB 221009A

Data were analysed using HEASOFT version 6.29

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Summary Information

RA:19h 13m 03.85sLC breaks:4
Dec:+19° 46′ 22.7′′LC type:Oddball.
Err:3.5′′NH,intr.:1.44×1022 cm-2
Gal long:52.960Redshift0.151
Gal lat:4.321Γ1.8
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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

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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.

Fitted light curve of GRB 221009A

Fit Details

032151493Image of this fit
119781491Break required.

(5.34e-156 % probability of chance improvement)
Image of this fit
218991489Break required.

(5.76e-12 % probability of chance improvement)
Image of this fit
318631487Break required.

(7.76e-05 % probability of chance improvement)
Image of this fit
418381485Break required.

(5.09e-03 % probability of chance improvement).
This is the best fit.
Image of this fit
518291483Break significance <4-σ
(1.89 % probability of chance improvement)
Image of this fit

There are 2 flares excluded from the fit:

  • 5.56×104—7.31×104 s
  • 7.35×104—8.94×104 s

The best-fitting light curve has 4 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.

α11.514 (+0.003, -0.003)
Tb,11.038 (+0.011, -0.214) × 105 s
α28.00 (+0.00, -5.80)
Tb,21.079 (+0.082, -0.014) × 105 s
α31.572 (+0.027, -0.033)
Tb,38.4 (+1.6, -1.7) × 105 s
α41.99 (+0.24, -0.18)
Tb,41.49 (+0.29, -0.12) × 106 s
α51.27 (+0.08, -0.09)

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Hide the spectrum section.

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.

Jump to: phase1 0-103752.841581801|phase2 103752.841581801-107894.672222983|phase3 107894.672222983-841395.141645195|phase4 841395.141645195-1492794.409579|phase5 1492794.409579-6284848.12298334

phase1 0-103752.841581801 spectrum (T0 + 9223372036854775807 to -100 s)

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phase2 103752.841581801-107894.672222983 spectrum (T0 + 9223372036854775807 to -100 s)

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phase3 107894.672222983-841395.141645195 spectrum (T0 + 9223372036854775807 to -100 s)

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phase4 841395.141645195-1492794.409579 spectrum (T0 + 9223372036854775807 to -100 s)

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phase5 1492794.409579-6284848.12298334 spectrum (T0 + 9223372036854775807 to -100 s)

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Comparison with other bursts

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Parameter distributions

The plots below show the probability density functions of the temporal and time-averaged spectral parameters for all GRBs, with the data for GRB 221009A shown on in colour. Click the images for larger versions.

For all plots, the solid vertical lines mark the values for this GRB, and the dashed lines the 1-σ uncertainties. For α and Tb, the colour changes for each phase. For the spectral parameters, the WT fits are shown in blue and the PC in red. These figures correspond to Figs. 5,6, 7a and 8a of Evans et al. (2009). See the PDF documentation for more information.

Temporal indicesBreak TimesNHSpectral indices
Comparison of decay indices Comparison of light curve break times Comparison of intrinsic column densities Comparison of spectral energy indices

Closure Relationships

The plots below show (α, β) scatter plots for each of the different types/phases of light curves (see light-curve types), since GRB 221009A is of type, "Oddball," which has no scatter plots of its own. GRB 221009A is shown in colour, with each light curve phase, or XRT mode marked by a different colour. α and β are the temporal and spectral energy power-law indices respectively. The shaded regions mark those allowed by the standard closure relationships. These figures correspond to Fig. 10 of Evans et al. (2009). See the closure relationship documentation for more information.

No break
Comparison of nobreak closures
One-break, steep first
Steep phase
One-break, steep first
Shallow phase
Comparison of One-break, steep first, steep phase closuresComparison of One-break, steep first, shallow phase closures
One-break, shallow first
Shallow phase
One-break, shallow first
Steep phase
Comparison of One-break, shallow first, shallow phase closuresComparison of One-break, shallow first, steep phase closures
Steep phase
Post jet-break
Comparison of Canonical, steep phase closuresComparison of Canonical, plateau phase closuresComparison of Canonical, normal phase closuresComparison of Canonical, post jet-break phase closures

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