Table A.1.
Bursts in the single-bin sample, synchrotron subsample.
GRB | Redshift | Liso | Ep, z | νc, z | p value | log B | Best-fit model |
---|---|---|---|---|---|---|---|
[1051 erg/s] | [keV] | [keV] | |||||
GRB081222A | 2.77 | ![]() |
![]() |
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0.19 | -0.07 | ND |
GRB090323A | 3.57 | ![]() |
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0.15 | 0.58 | S |
GRB090328A | 0.74 | ![]() |
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0.05 | -0.77 | B |
GRB090424A | 0.54 | ![]() |
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![]() |
0.09 | -2.07 | B |
GRB090618A | 0.54 | ![]() |
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0.24 | 2.27 | S |
GRB091003A | 0.9 | ![]() |
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![]() |
0.32 | -7.02 | B |
GRB091127A | 0.49 | ![]() |
![]() |
![]() |
0.22 | 1.46 | S |
GRB091208B | 1.06 | ![]() |
![]() |
![]() |
0.11 | 0.85 | S |
GRB100414A | 1.37 | ![]() |
![]() |
![]() |
0.35 | -0.72 | B |
GRB100728A | 1.57 | ![]() |
![]() |
![]() |
0.17 | -3.68 | B |
GRB100816A | 0.8 | ![]() |
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![]() |
0.44 | -8.92 | B |
GRB100906A | 1.73 | ![]() |
![]() |
![]() |
0.2 | -0.36 | ND |
GRB110213A | 1.46 | ![]() |
![]() |
![]() |
0.06 | 0.57 | S |
GRB110731A | 2.83 | ![]() |
![]() |
![]() |
0.09 | 0.02 | NS |
GRB111228A | 0.71 | ![]() |
![]() |
![]() |
0.32 | 1.78 | S |
GRB120119A | 1.73 | ![]() |
![]() |
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0.49 | 0.75 | S |
GRB120624B | 2.2 | ![]() |
![]() |
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0.23 | -0.03 | ND |
GRB120711A | 1.4 | ![]() |
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![]() |
0.25 | -1.8 | B |
GRB120716A | 2.49 | ![]() |
![]() |
![]() |
0.34 | -0.41 | ND |
GRB121128A | 2.2 | ![]() |
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![]() |
0.12 | -2.58 | B |
GRB130518A | 2.49 | ![]() |
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0.33 | 23.26 | S |
GRB131105A | 1.69 | ![]() |
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![]() |
0.25 | -0.81 | B |
GRB131108A | 2.4 | ![]() |
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0.44 | -1.34 | B |
GRB131231A | 0.64 | ![]() |
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0.05 | 0.34 | ND |
GRB140213A | 1.21 | ![]() |
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0.48 | 0.7 | S |
GRB140506A | 0.89 | ![]() |
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0.44 | -0.8 | B |
GRB140512A | 0.72 | ![]() |
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0.44 | -1.41 | B |
GRB140606B | 0.38 | ![]() |
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0.13 | -2.1 | B |
GRB140808A | 3.29 | ![]() |
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0.22 | -2.01 | B |
GRB141028A | 2.33 | ![]() |
![]() |
![]() |
0.37 | -1.14 | B |
GRB141220A | 1.32 | ![]() |
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0.43 | -5.84 | B |
GRB150403A | 2.06 | ![]() |
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0.14 | 2.44 | S |
GRB150514A | 0.81 | ![]() |
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0.03 | 0.1 | ND |
GRB150821A | 0.76 | ![]() |
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0.47 | 0.77 | S |
GRB151027A | 0.81 | ![]() |
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0.07 | -0.44 | ND |
GRB160509A | 1.17 | ![]() |
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0.49 | -1.96 | B |
GRB160625B | 1.41 | ![]() |
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0.07 | 21.36 | S |
GRB170214A | 2.53 | ![]() |
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0.2 | -0.17 | ND |
GRB170405A | 3.51 | ![]() |
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![]() |
0.22 | -2.72 | B |
GRB170607A | 0.56 | ![]() |
![]() |
![]() |
0.46 | 2.42 | S |
GRB170705A | 2.01 | ![]() |
![]() |
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0.27 | 0.08 | ND |
GRB171010A | 0.33 | ![]() |
![]() |
![]() |
0.26 | 6.41 | S |
GRB180703A | 0.67 | ![]() |
![]() |
![]() |
0.42 | 0.53 | S |
GRB180720B | 0.65 | ![]() |
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![]() |
0.08 | 13.48 | S |
GRB180728A | 0.12 | ![]() |
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![]() |
0.14 | 8.05 | S |
GRB181020A | 2.94 | ![]() |
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![]() |
0.07 | -7.82 | B |
GRB190324A | 1.17 | ![]() |
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0.5 | -4.17 | B |
GRB200524A | 1.26 | ![]() |
![]() |
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0.37 | -0.32 | ND |
GRB200613A | 1.23 | ![]() |
![]() |
![]() |
0.41 | -7.15 | B |
GRB201216C | 1.1 | ![]() |
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![]() |
0.23 | 4.97 | S |
GRB210204A | 0.88 | ![]() |
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0.36 | 0.89 | S |
GRB210610B | 1.13 | ![]() |
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![]() |
0.36 | -15.57 | B |
GRB211023A | 0.39 | ![]() |
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0.19 | 0.94 | S |
GRB211211A | 0.08 | ![]() |
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0.0 | 66.52 | S |
GRB220101A | 4.62 | ![]() |
![]() |
![]() |
0.25 | -2.51 | B |
GRB220107A | 1.25 | ![]() |
![]() |
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0.14 | -2.34 | B |
GRB230204B | 2.14 | ![]() |
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0.08 | -0.73 | B |
GRB230818A | 2.42 | ![]() |
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0.33 | -1.48 | B |
Notes. We show the results of the synchrotron fit for the burst that meet at least one of the following conditions: synchrotron is the best-fit model, synchrotron cannot be excluded by the model comparison (|log B|< 0.5), synchrotron model provides a good fit to the data. We report redshifts z (see Sec. 2.1), isotropic-equivalent luminosities Liso, rest-frame peak energies Ep,z (namely the minimum frequency νm, z) and rest-frame cooling frequencies νc, z obtained from the synchrotron fit. We report errors at 68 per cent confidence level. We further report the p value returned from the PPC analysis, the Bayes factor log B obtained comparing Band and synchrotron models, and the associated best-fit model: S = synchrotron, B = Band, and ND = not defined; in other words, when |log B|< 0.5
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