Table 1 Region and electron power-law index (p) in both X-ray and optical bands using both temporal and spectral indices

From: A wind environment and Lorentz factors of tens explain gamma-ray bursts X-ray plateau

GRB name

Regions in X-ray band

pX

Regions in optical band

pU

 

Temporal

Spectral

Temporal

Spectral

Temporal

Spectral

Temporal

Spectral

Class I

        

080607

F

F

~2.5

2.0

E

E

2.0

~2.5

091029

F

F

2.3

2.0

F(E)

E

2.4(1.8)

1.9

110213A

F

F

~2.0

2.0

E

E

2.1

3.2

130831A

F

F/E

2.0

1.8/~2.4

E

—

2.1

—

Class II

        

060605

F

F

~2.1

2.3

F

F

~2.2

~2.3

060614

F

F

~2.3

1.8

F

F

2.0

0.7

060729

F

F

2.0

2.0

F

F

2.3

~1.2

080310

F

F

~2.5

2.0

F

F

2.0

1.9

100418A

F

F

2.2

~1.9

F

F

~1.8

~2.3

171205A

F

F/E

2.0

~1.8/2.4

F

F

~1.8

~1.8

Class III

        

050319

E

F/E

2.1

2.1/3.2

E

E

~1.8–2.1

2.0

060714

F/E

F/E

~2.4/2.0

2.0/2.8

F/E

E

2.0/~1.8

~2.4

061121

F/E

F/E

2.5/~2.1

2.0/~3.2

E

E

2.0

2.3

  1. In Column 1, GRB names are ordered by classes (I, II, III listed in Supplementary Tables 1–3 respectively). In columns 2–5, we use the temporal and spectral X-ray data to determine both the electron power law index (pX) and the region (E or F) characteristics of the emission, see Supplementary Fig. 17. The optical data is used in a similar way in columns 6-9. For GRBs 060614, 060729 and 110213A, the power-law indices obtained using X-ray and optical temporal indices as well as the X-ray spectral index are all consistent with each other, while the values derived using the optical spectral data deviate. Since no errors are given in the literature for GRBs 060614 and 060729 (see Supplementary Table 2), we cannot estimate the reliability of the optical spectral indices for these bursts, and we therefore accept the power law obtained using 6 out of 8 independent measurements. For GRB 110213A, there is no available spectral index in the optical band during the plateau phase, and the second peak in the optical band after the plateau phase (see, Supplementary Method 1b, Optical data and fitting process) might be affecting the spectral index during the afterglow phase (see Supplementary Table 1). In all three bursts which we categorize as being in class III, there seem to be a discrepancy between the X-ray spectral and temporal data: while the temporal data clearly indicates the X-ray to be in region E the spectral data favours region F. However, this is because, in all three bursts there is a break in the X-ray light curve during the plateau phase, or an early flare. These may indicate a change in region, and may affect the spectral measurement.
Back to article page