The Energy Budget of GRBs Based on a Large Sample of Prompt and Afterglow Observations

Nahliel Wygoda, Dafne Guetta, M. A. Mandich, Eli Waxman

Research output: Contribution to journalArticlepeer-review


We compare the isotropic equivalent 15-2000 keV γ-ray energy, E γ, emitted by a sample of 91 swift Gamma-Ray Bursts with known redshifts, with the isotropic equivalent fireball energy, E fb, as estimated within the fireball model framework from X-ray afterglow observations of these bursts. The uncertainty in E γ, which spans the range of ∼1051 to ∼1053.5 erg, is ≈25% on average, due mainly to the extrapolation from the BAT detector band to the 15-2000 keV band. The uncertainty in E fb is approximately a factor of 2, due mainly to the X-ray measurements' scatter. We find E γ and E fb to be tightly correlated. The average(std) of are -0.34(0.60), and the upper limit on the intrinsic spread of η γ is approximately 0.5 ( is the fraction of energy carried by electrons and is inferred from the X-ray flux at x hours). and are similar, with an average(std) of of 0.04(0.28). The small variance of η γ implies that burst-to-burst variations in and in the efficiency of fireball energy conversion to γ-rays are small, and suggests that both are of order unity. The small variance of η γ and the similarity of and further imply that deviations from a simple fireball model description, if present, are small. This puts stringent constraints on models incorporating such modifications (due e.g., to radiative losses, energy injection, off-axis viewing).

Original languageEnglish
Article number127
JournalAstrophysical Journal
Issue number2
StatePublished - 21 Jun 2016


  • Cosmology: observations
  • Gamma-ray burst: general

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science


Dive into the research topics of 'The Energy Budget of GRBs Based on a Large Sample of Prompt and Afterglow Observations'. Together they form a unique fingerprint.

Cite this