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Catalogue XRT results for GRB 050730: XRT-team version

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Summary Information

RA:14h 08m 17.17sLC breaks:3
Dec:-03° 46′ 18.5′′LC type:Oddball   Edit.


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Err:1.4′′NH,intr.:3.72×1021 cm-2
Gal long:336.856Redshift3.97
Gal lat:53.960Γ1.6
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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 3-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 050730

Fit Details

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Nbreaksχ2dofCommentsImage
05084423Image of this fit
1797421Break required.

(4.17e-168 % probability of chance improvement)
Image of this fit
2604419Break required.

(5.77e-24 % probability of chance improvement)
Image of this fit
3521417Break required.

(4.29e-12 % probability of chance improvement)
Image of this fit
4509415Break significance <4-σ
(1.04 % probability of chance improvement)
Image of this fit
5501413Break significance <4-σ
(0.32 % probability of chance improvement)
Image of this fit

There are 3 flares excluded from the fit:

  • 213—271 s
  • 332—531 s
  • 620—763 s

Alter flare times.

To add/remove or modify times marked as "flares" and thus excluded from the fit, please enter the times in the box below, as start1-stop1,start2-stop2 etc, where the start,stop times are the boundary times (in seconds since the trigger) of the interval to be excluded. e.g. to leave times 100-150 s and 275-324 s from the fit, enter 100-150,275,324 in the box.

If you leave the box blank, nothing will happen. If there are no flares, please enter none in the box.





The best-fitting light curve has 3 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.

α12.01 (+0.28, -0.27)
Tb,1259 (+21, -17) s
α2-0.06 (+0.11, -0.11)
Tb,21832 (+397, -328) s
α30.963 (+0.093, -0.110)
Tb,31.04 (+0.04, -0.05) × 104 s
α42.49 (+0.05, -0.04)

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Spectra

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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|phase2|phase3|phase4

phase1 spectrum (T0 + 132 to 259 s)

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Plots to download

WT mode spectrum of GRB 050730

WT mode. Mean photon arrival: T0+190 s

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NH (Galactic)3.51 × 1020 cm-2
NH (intrinsic)1.5 (+0.9, -0.9) × 1022 cm-2
z of absorber3.97
Photon index1.40 (+0.06, -0.06)
Flux (0.3-10 keV)
(Observed)
1.17 (+0.06, -0.06) × 10-9 erg cm-2 s-1
Flux (0.3-10 keV)
(Unabsorbed)
1.24 (+0.05, -0.04) × 10-9 erg cm-2 s-1
Counts to flux (obs)4.55 × 10-11 erg cm-2 ct-1
Counts to flux (unabs)4.84 × 10-11 erg cm-2 ct-1
W-stat (dof)
What's this?
533.89 (595)
Spectrum exposure126 s

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phase2 spectrum (T0 + 259 to 794 s)

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WT mode spectrum of GRB 050730

WT mode. Mean photon arrival: T0+519 s

Insert manually-determined values.

NH (Galactic)3.51 × 1020 cm-2
NH (intrinsic)4 (+4, -4) × 1021 cm-2
z of absorber3.97
Photon index1.72 (+0.04, -0.04)
Flux (0.3-10 keV)
(Observed)
6.60 (+0.18, -0.18) × 10-10 erg cm-2 s-1
Flux (0.3-10 keV)
(Unabsorbed)
7.11 (+0.14, -0.17) × 10-10 erg cm-2 s-1
Counts to flux (obs)3.68 × 10-11 erg cm-2 ct-1
Counts to flux (unabs)3.96 × 10-11 erg cm-2 ct-1
W-stat (dof)
What's this?
718.89 (703)
Spectrum exposure535 s

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phase3 spectrum (T0 + 4000 to 10374 s)

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PC mode spectrum of GRB 050730

PC mode. Mean photon arrival: T0+6055 s

Insert manually-determined values.

NH (Galactic)3.51 × 1020 cm-2
NH (intrinsic)2.9 (+6.8, -2.9) × 1021 cm-2
z of absorber3.97
Photon index1.44 (+0.06, -0.05)
Flux (0.3-10 keV)
(Observed)
1.84 (+0.08, -0.08) × 10-10 erg cm-2 s-1
Flux (0.3-10 keV)
(Unabsorbed)
1.93 (+0.07, -0.06) × 10-10 erg cm-2 s-1
Counts to flux (obs)4.45 × 10-11 erg cm-2 ct-1
Counts to flux (unabs)4.65 × 10-11 erg cm-2 ct-1
W-stat (dof)
What's this?
555.88 (627)
Spectrum exposure3.2 ks

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phase4 spectrum (T0 + 10375 to 359027 s)

Download spectral files for phase4 spectrum.

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PC mode spectrum of GRB 050730

PC mode. Mean photon arrival: T0+26105 s

Insert manually-determined values.

NH (Galactic)3.51 × 1020 cm-2
NH (intrinsic)6 (+6, -5) × 1021 cm-2
z of absorber3.97
Photon index1.64 (+0.05, -0.05)
Flux (0.3-10 keV)
(Observed)
4.40 (+0.16, -0.16) × 10-12 erg cm-2 s-1
Flux (0.3-10 keV)
(Unabsorbed)
4.71 (+0.14, -0.14) × 10-12 erg cm-2 s-1
Counts to flux (obs)3.90 × 10-11 erg cm-2 ct-1
Counts to flux (unabs)4.18 × 10-11 erg cm-2 ct-1
W-stat (dof)
What's this?
589.86 (634)
Spectrum exposure65.6 ks

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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 050730 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 050730 is of type, "Oddball," which has no scatter plots of its own. GRB 050730 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
Canonical
Steep phase
Canonical
Plateau
Canonical
'Normal'
Canonical
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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