2022A&A...657A.124L


Query : 2022A&A...657A.124L

2022A&A...657A.124L - Astronomy and Astrophysics, volume 657A, 124-124 (2022/1-1)

Overall spectral properties of prompt emissions with diverse segments in Swift/BAT short gamma-ray bursts.

LI X.J., ZHANG Z.B. and ZHANG K.

Abstract (from CDS):

Owing to a lack of multiple components of prompt γ-ray emissions in short gamma-ray bursts (sGRBs), how these distinct components are correlated remains unclear. In this paper we investigate the spectral and temporal properties of precursors, main peaks, and extended emissions in 26 sGRBs including GRB 170817A. It has been found that peak energies (Ep) in each pulse are uncorrelated with the pulse duration (tdur). Meanwhile, we find that there is no obvious correlation between peak energy and energy fluence. Interestingly, there is no obvious spectral evolution from earlier precursors to later extended emissions in view of the correlations of tdur with either the Ep or the low-energy spectrum index, α. A power-law correlation between the average flux (Fp) and the energy fluence (Sγ), log Fp = (0.62 ±0.07) log Sγ + (0.27 ±0.07), is found to exist in the individual segments instead of mean peaks. Furthermore, we also find that the main peaks are on average brighter than the precursors or the extend emissions by about one order of magnitude. On the basis of all the above analyses, we can conclude that three emissive components could share the same radiation mechanisms, but that they might be dominated by diverse physical processes.

Abstract Copyright: © ESO 2022

Journal keyword(s): gamma-ray burst: general - stars: late-type - methods: statistical

Simbad objects: 30

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Number of rows : 30
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 Fermi bn111117510 gB 00 50 46.220 +23 00 39.22           ~ 109 0
2 Fermi bn100625773 gB 01 03 10.98 -39 05 18.3           ~ 97 0
3 GRB 120229A gB 01 20 07.90 -35 47 44.0           ~ 16 0
4 Fermi bn100206563 gB 03 08 38.94 +13 09 25.5           ~ 120 0
5 GRB 120305A gB 03 10 08.73 +28 29 30.9           ~ 40 0
6 Fermi bn130912358 gB 03 10 25.60 +13 59 55.7           ~ 42 0
7 GRB 101219A gB 04 58 20.45 -02 32 23.1           ~ 120 0
8 Fermi bn160726065 gB 06 35 -06.6           ~ 19 0
9 Fermi bn160408268 gB 08 10 29.93 +71 07 41.7           ~ 29 0
10 GRB 130603B gB 11 28 48.16 +17 04 18.2           ~ 317 0
11 GRB 070923 gB 12 18 29.5 -38 17 38           ~ 34 0
12 GRB 150710A gB 12 57 52.91 +14 19 05.0           ~ 15 0
13 GrW 170817 GWE 13 09 48.0850 -23 22 53.343           ~ 1591 0
14 GRB 120804A gB 15 35 47.55 -28 46 56.9           ~ 75 0
15 GRB 160601A gB 15 39 44.55 +64 32 28.7           ~ 26 0
16 Fermi bn150301045 gB 16 17 13.13 -48 42 47.2           ~ 22 0
17 GRB 100702A gB 16 22 47.26 -56 31 53.8           ~ 42 0
18 GRB 050724 gB 16 24 44.400 -27 32 27.90     19.70     ~ 415 1
19 Fermi bn180402406 gB 16 47 43.90 -14 58 12.1           ~ 20 0
20 GRB 071112B gB 17 20 51.0 -80 53 02           ~ 44 0
21 GRB 060502B gB 18 35 46.060 +52 37 51.45           ~ 137 1
22 Fermi bn131004904 gB 19 44 27.20 -02 57 31.0           ~ 77 0
23 Fermi bn160625945 gB 20 34 23.67 +06 55 11.1           ~ 141 0
24 Fermi bn090621922 gB 20 53 49.30 +69 02 02.9           ~ 57 0
25 GRB 140622A gB 21 08 41.56 -14 25 09.5           ~ 41 0
26 Fermi bn110420946 gB 21 20 10.90 -41 16 38.0           ~ 32 0
27 GRB 060614 gB 21 23 32.140 -53 01 36.10 18.89 20.12 19.54     ~ 560 1
28 GRB 190326A gB 22 46 36.60 +39 54 50.3           ~ 10 0
29 GRB 720427 gB 22 54 -68.0           ~ 6 0
30 GRB 180727A gB 23 06 39.86 -63 03 06.7           ~ 12 0

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2023.01.30-23:21:34

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