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2016ApJ...824..127W - Astrophys. J., 824, 127-127 (2016/June-3)

The energy budget of GRBs based on a large sample of prompt and afterglow observations.


Abstract (from CDS):

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, Efb, 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 Efb is approximately a factor of 2, due mainly to the X-ray measurements' scatter. We find E_ γ_ and Efb to be tightly correlated. The average(std) of η_γ^{11 hr}≡log{10}({E}γ/(3ε{e}{E}{fb}^{11 hr})) are -0.34(0.60), and the upper limit on the intrinsic spread of η_ γ_ is approximately 0.5 ( ε_{e} is the fraction of energy carried by electrons and {E}_{fb}^{x hr} is inferred from the X-ray flux at x hours). {E}_{fb}^{3 hr} and {E}_{fb}^{11 hr} are similar, with an average(std) of log{10}({E}{fb}{3 hr}/{E}{fb}^{11 hr}) of 0.04(0.28). The small variance of η_ γ_ implies that burst-to-burst variations in ε_{e} 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 {E}_{fb}^{3 hr} and {E}_{fb}^{11 hr} 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).

Abstract Copyright: © 2016. The American Astronomical Society. All rights reserved.

Journal keyword(s): cosmology: observations - gamma-ray burst: general

Simbad objects: 11

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