Intergalactic magnetic field studies by means of $\gamma$-ray emission from GRB 190114C

Abstract

The presence of delayed GeV emission after a strong transient, such as a GRB (Gamma-Ray Burst), in the VHE (Very-High Energy, $E>100$ GeV) band can be the signature of a non-zero magnetic field in the intergalactic medium. We used a synchrotron self-Compton multiwavelength model to infer an analytical description of the intrinsic VHE spectrum (corrected for absorption by the Extragalactic Background Light, EBL) of GRB190114C to predict the lightcurves and SEDs of the delayed emission with Monte Carlo simulations for different IGMF (Intergalactic Magnetic Field) configurations (strengths $B=8\times 10^{-21}$ G, $10^{-20}$ G, $3\times 10^{-20}$G and correlation length $\lambda >1$ Mpc), and compared them with the Fermi-LAT (Fermi Large Area Telescope) limits computed for several exposure times. We found that Fermi LAT is not sensitive enough to constrain any IGMF strengths using GRB190114C.

8 pages, 3 figures, accepted for publication to Physical Review D

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Cited by in corpus (5)

• First constraints on the strength of the extragalactic magnetic field from $\gamma$-ray observations of GRB 221009A
• Very high-energy gamma rays from GRB 180720B and GRB 190829A with external Compton emission
• Constraints on the intergalactic magnetic field from Fermi-LAT observations of GRB 221009A
• Prospects for detection of the pair-echo emission from TeV gamma-ray bursts
• Seminal Electromagnetic fields from preinflation