The Maximum Isotropic Energy of Gamma-Ray Bursts

被引：50

作者：

Atteia, J. -L. ^{[1
,2
,3
,4
,5
]}

Heussaff, V. ^{[1
,2
,3
,4
,5
]}

Dezalay, J. -P. ^{[1
,2
,3
,4
,5
]}

Klotz, A. ^{[1
,2
,3
,4
,5
]}

Turpin, D. ^{[1
,2
,3
,4
,5
]}

Tsvetkova, A. E. ^{[6
]}

Frederiks, D. D. ^{[6
]}

Zolnierowski, Y. ^{[7
]}

Daigne, F. ^{[8
]}

Mochkovitch, R. ^{[8
]}

机构：

[1] Univ Toulouse, Toulouse, France

[2] Univ Toulouse 3, OMP, Toulouse, France

[3] IRAP, Toulouse, France

[4] CNRS, 14 Ave Edouard Belin, F-31400 Toulouse, France

[5] IRAP, 14 Ave Edouard Belin, F-31400 Toulouse, France

[6] Ioffe Inst, Politekhnicheskaya 26, St Petersburg 194021, Russia

[7] Univ Savoie, CNRS IN2P3, LAPP, 9 chemin Bellevue,BP 110, Annecy Le Vieux, France

[8] UPMC CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France

来源：

ASTROPHYSICAL JOURNAL | 2017年 / 837卷 / 02期

关键词：

gamma-ray burst: general; STAR-FORMATION HISTORY; LUMINOSITY FUNCTION; GRB; 130427A; REDSHIFT DISTRIBUTION; JET STRUCTURE; OFF-AXIS; EVOLUTION; FERMI; AFTERGLOW; CATALOG;

D O I：

10.3847/1538-4357/aa5ffa

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The most energetic gamma-ray bursts (GRBs) are remarkable sources releasing huge amounts of energy on short timescales. Their prompt emission, which usually lasts a few seconds, is so bright that it is visible across the whole observable universe. Studying these extreme events may provide clues on the nature of GRB progenitors and on the physical processes at work in relativistic jets. In this paper, we study the bright end of the isotropic energy distribution of long GRBs. We use two samples of long GRBs with redshift detected by Fermi/GBM or Konus-Wind, two instruments that measure the spectral shape and the energetics of the prompt emission accurately. We focus on GRBs within a range of redshifts z = 1-5, a volume that contains a large number of energetic GRBs, and we propose a simple method to reconstruct the bright end of the GRB energy distribution from the observed one. We find that the GRB energy distribution cannot be described by a simple power law but requires a strong cutoff above 1-3 x 10(54) erg. We attribute this feature to an intrinsic limit on the energy per unit of solid angle radiated by GRBs.

引用

页数：12

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