C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST03:01:59

2017A&A...606A..93Y - Astronomy and Astrophysics, volume 606A, 93-93 (2017/10-1)

Time evolution of the spectral break in the high-energy extra component of GRB 090926A.


Abstract (from CDS):

Aims. The prompt light curve of the long GRB 090926A reveals a short pulse ∼10s after the beginning of the burst emission, which has been observed by the Fermi observatory from the keV to the GeV energy domain. During this bright spike, the high-energy emission from GRB 090926A underwent a sudden hardening above 10MeV in the form of an additional power-law component exhibiting a spectral attenuation at a few hundreds of MeV. This high-energy break has been previously interpreted in terms of gamma-ray opacity to pair creation and has been used to estimate the bulk Lorentz factor of the outflow. In this article, we report on a new time-resolved analysis of the GRB 090926A broadband spectrum during its prompt phase and on its interpretation in the framework of prompt emission models.
Methods. We characterized the emission from GRB 090926A at the highest energies with Pass 8 data from the Fermi Large Area Telescope (LAT), which offer a greater sensitivity than any data set used in previous studies of this burst, particularly in the 30-100MeV energy band. Then, we combined the LAT data with the Fermi Gamma-ray Burst Monitor (GBM) in joint spectral fits to characterize the time evolution of the broadband spectrum from keV to GeV energies. We paid careful attention to the systematic effects that arise from the uncertainties on the LAT response. Finally, we performed a temporal analysis of the light curves and we computed the variability timescales from keV to GeV energies during and after the bright spike.
Results. Our analysis confirms and better constrains the spectral break, which has been previously reported during the bright spike. Furthermore, it reveals that the spectral attenuation persists at later times with an increase of the break characteristic energy up to the GeV domain until the end of the prompt phase. We discuss these results in terms of keV-MeV synchroton radiation of electrons accelerated during the dissipation of the jet energy and inverse Compton emission at higher energies. We interpret the high-energy spectral break as caused by photon opacity to pair creation. Requiring that all emissions are produced above the photosphere of GRB 090926A, we compute the bulk Lorentz factor of the outflow, Γ. The latter decreases from 230 during the spike to 100 at the end of the prompt emission. Assuming, instead, that the spectral break reflects the natural curvature of the inverse Compton spectrum, lower limits corresponding to larger values of Γ are also derived. Combined with the extreme temporal variability of GRB 090926A, these Lorentz factors lead to emission radii R∼1014cm, which are consistent with an internal origin of both the keV-MeV and GeV prompt emissions.

Abstract Copyright: © ESO, 2017

Journal keyword(s): gamma-ray burst: individual: GRB 090926A - radiation mechanisms: non-thermal - radiation mechanisms: non-thermal

Simbad objects: 6

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Number of rows : 6

N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
1 GRB 080916C gB 07 59 23.24 -56 38 16.8           ~ 315 0
2 NAME Vela Pulsar Psr 08 35 20.65525 -45 10 35.1545           ~ 2057 1
3 SN 2013cq SN* 11 32 32.84 +27 41 56.2           SNIc 378 1
4 GRB 090902B gB 17 39 45.26 +27 19 28.1           ~ 327 0
5 GRB 090510 gB 22 14 12.60 -26 35 51.1           ~ 408 1
6 GRB 090926A gB 23 33 36.18 -66 19 25.9           ~ 250 0

    Equat.    Gal    SGal    Ecl

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