2025A&A...693A.156M


Query : 2025A&A...693A.156M

2025A&A...693A.156M - Astronomy and Astrophysics, volume 693A156 (2025/1-1)

Gamma-ray burst spectral-luminosity correlations in the synchrotron scenario.

MEI A., OGANESYAN G. and MACERA S.

Abstract (from CDS):

Context. For over two decades, gamma-ray burst (GRB) prompt emission spectra were modeled with smoothly broken power laws (Band function), and a positive and tight correlation between the spectral rest-frame peak energy, Ep,z, and the total isotropic-equivalent luminosity, Liso, was found, constituting the so-called Yonetoku relation. However, more recent studies show that many prompt emission spectra are well described by the synchrotron radiation model, and hence significantly deviate from the Band function.
Aims. In this work, we test the impact of a more refined spectral model such as an idealized synchrotron spectrum from nonthermal electrons on the Yonetoku relation and its connection with physical parameters.
Methods. We selected GRBs with measured redshift observed by Fermi/GBM together with high-energy observations (> 30 MeV), and performed a spectral analysis, dividing them in two samples: the single-bin sample, using the light curve peak spectrum of each GRB, and the multiple-bin sample, for which we explored the whole duration of 13 bright bursts with time-resolved spectral analysis.
Results. We observed that the Ep,z of synchrotron spectra in a fast-cooling regime (νm/νc ≫ 1) is generally larger than the one provided by the Band function. For this reason, we do not find any Ep,z-Liso correlation in our samples except for the GRBs in an intermediate-cooling regime (1< νm/νc< 3); namely, where peak and break energies are very close. We instead find in both our samples a new tight correlation between the rest-frame cooling frequency, ν_c, z_, and Liso: $ \nu_{c,z} \propto {L_{\mathrm{iso}}}^{(0.53 \pm 0.06)} $.
Conclusions. These results suggest that, assuming that prompt emission spectra are produced by synchrotron radiation, the physical relation is between ν_c, z_ and Liso. The fit of the Band function to an intrinsic synchrotron spectrum returns peak energy values of $ E_{p,z}^{\mathrm{Band}} \sim \nu_{c,z} $. This may explain why the systematic interpretation of prompt spectra through the Band function returns the E_p, z_ - Liso relation.

Abstract Copyright: © The Authors 2025

Journal keyword(s): astroparticle physics - radiation mechanisms: non-thermal - gamma-ray burst: general - gamma rays: general

Simbad objects: 77

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Number of rows : 77
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026
#notes
1 GRB 180720B gB 00 02 06.99 -02 55 07.8           ~ 215 0
2 GRB 220101A gB 00 05 24.89 +31 46 07.7           ~ 85 0
3 Fermi bn180703876 gB 00 25 52.72 -67 10 47.9           ~ 35 0
4 GRB 200826A gB 00 27 08.47 +34 01 36.5           ~ 121 0
5 GRB 170607A gB 00 29 27.84 +09 14 35.5           ~ 62 0
6 Fermi bn131231198 gB 00 42 44.0 -01 29 40           ~ 103 0
7 GRB 181020A gB 00 55 55.77 -47 22 50.6           ~ 61 0
8 Fermi bn081221681 gB 01 03 10.2 -24 32 53           ~ 186 0
9 GRB 201216C gB 01 05 28.88 +16 30 58.0           ~ 89 0
10 GRB 081222 gB 01 30 57.76 -34 05 44.0           ~ 199 0
11 GRB 100906A gB 01 54 44.19 +55 37 49.8           ~ 233 0
12 Fermi bn091208410 gB 01 57 38.50 +16 52 50.7           ~ 220 0
13 SN 2009nz SN* 02 26 19.87 -18 57 08.6           ~ 307 1
14 Fermi bn110213220 gB 02 51 51.37 +49 16 21.2           ~ 175 0
15 GRB 140801A gB 02 56 16.50 +30 56 16.8           ~ 55 0
16 GRB 190324A gB 03 18 27.77 -47 12 54.1           ~ 35 0
17 GRB 190114C gB 03 38 01.18 -26 56 47.8           ~ 343 0
18 GRB 230307A gB 04 03 26.24 -75 22 43.8           ~ 221 0
19 GRB 171010A gB 04 26 19.41 -10 27 47.9           SNIc-BL 109 0
20 Fermi bn131105087 gB 04 43 53.50 -63 00 17.7           ~ 95 0
21 GRB 211023A gB 04 49 +85.3           ~ 42 0
22 Fermi bn150514774 gB 04 59 30.45 -60 58 07.0           ~ 51 0
23 GRB 201020B gB 05 01 52.03 +77 04 05.9           ~ 34 0
24 Fermi bn100728095 gB 05 55 02.00 -15 15 20.2           ~ 157 0
25 GRB 090328 gB 06 02 39.69 -41 52 55.1           ~ 194 1
26 Fermi bn120711115 gB 06 18 42.839 -70 59 56.78           ~ 125 0
27 GRB 140213A gB 07 00 37.18 -73 08 14.1           ~ 102 0
28 GRB 210204A gB 07 48 19.37 +11 24 34.2           ~ 46 0
29 Fermi bn120119170 gB 08 00 06.940 -09 04 53.83           ~ 193 0
30 Fermi bn150314205 gB 08 26 40.82 +63 50 03.4           ~ 117 0
31 GRB 090102 gB 08 32 59.50 +33 06 25.7           ~ 253 0
32 Fermi bn140206304 gB 09 41 16.90 +66 45 42.7           ~ 149 0
33 Fermi bn111228657 gB 10 00 16.04 +18 17 52.2           ~ 201 0
34 GRB 200613A gB 10 12 10.03 +45 45 14.1           ~ 36 0
35 GRB 131108A gB 10 26 00.480 +09 39 44.05           ~ 96 0
36 GRB 220107A gB 11 19 13.68 +34 10 14.3           ~ 29 0
37 Fermi bn120624933 gB 11 23 31.98 +08 55 42.1           ~ 100 0
38 SN 2013cq SN* 11 32 32.84 +27 41 56.2           SNIc 613 1
39 GRB 090424 gB 12 38 07.40 +16 49 45.9           ~ 269 0
40 Fermi bn090323002 gB 12 42 50.28 +17 03 11.9           ~ 244 1
41 Fermi bn100414097 gB 12 48 30.0 +08 41 35           ~ 136 0
42 Fermi bn170705115 gB 12 49 +17.9           ~ 66 0
43 Fermi bn141220252 gB 13 00 15.70 +32 08 47.2           ~ 81 0
44 GRB 230204B gB 13 10 34.60 -21 43 00.8           ~ 28 0
45 SDSS J140910.47+275320.8 G 14 09 10.47535 +27 53 20.8393           ~ 279 0
46 GRB 200524A gB 14 12 10.74 +60 54 19.4           ~ 40 0
47 Fermi bn170405777 gB 14 39 18.66 -25 14 36.9           ~ 75 0
48 Fermi bn140808038 gB 14 44 53.27 +49 12 52.7           ~ 45 0
49 GRB 210610B gB 16 15 40.47 +14 23 56.3           ~ 87 0
50 GRB 230812B gB 16 36 31.49 +47 51 31.3           ~ 89 0
51 GRB 200829A gB 16 44 49.42 +72 19 45.3           ~ 55 0
52 GRB 091003A gB 16 46 04.680 +36 37 31.08           ~ 135 0
53 SN 2018fip SN* 16 54 15.64 -54 02 39.5           SNIc-BL 83 0
54 GRB 140508A gB 17 01 51.95 +46 46 49.5           ~ 76 0
55 GRB 170214A gB 17 05 21.94 -01 53 14.9           ~ 54 0
56 Fermi bn090902462 gB 17 39 45.26 +27 19 28.1           ~ 440 0
57 Fermi bn151027166 gB 18 09 56.87 +61 21 12.3           ~ 143 0
58 Fermi bn140506880 gB 18 27 06.04 -55 38 08.7           ~ 113 0
59 Fermi bn110731465 gB 18 42 00.99 -28 32 13.8           ~ 193 0
60 GRB 230818A gB 19 03 33.15 +40 53 48.2           ~ 37 0
61 GRB 221009A gB 19 13 03.85 +19 46 22.7           ~ 433 0
62 Fermi bn140512814 gB 19 17 28.81 -15 05 39.5           ~ 133 0
63 GRB 090618 gB 19 36 01.80 +78 21 07.1           ~ 358 0
64 Fermi bn121128212 gB 20 02 23.88 +54 17 59.1           ~ 128 0
65 GRB 160625B gB 20 34 23.67 +06 55 11.1           ~ 235 0
66 GRB 150403A gB 20 46 01.17 -62 42 40.1           ~ 116 0
67 Fermi bn160509374 gB 20 47 00.90 +76 06 30.1           ~ 141 0
68 Fermi bn120716712 gB 20 52 12.17 +09 35 53.9           ~ 72 0
69 GRB 210619B gB 21 18 52.39 +33 51 00.2           ~ 93 0
70 GRB 141028A gB 21 30 24.46 -00 13 55.6           ~ 109 0
71 GRB 220527A gB 21 34 06.70 +14 58 18.7           ~ 27 0
72 iPTF 14bfu SN* 21 52 30.00 +32 00 52.5           SNIc 80 0
73 Fermi bn090510016 G 22 14 12.6230 -26 34 58.550           ~ 548 0
74 Fermi bn150821406 gB 22 47 39.15 -57 53 38.2           ~ 71 0
75 Fermi bn100816026 gB 23 26 57.56 +26 34 42.6           ~ 170 0
76 Fermi bn090926181 gB 23 33 36.18 -66 19 25.9           ~ 339 0
77 GRB 130518A gB 23 42 39.79 +47 27 55.2           ~ 86 0

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