Modelling the propagation of very-high-energy gamma rays with the CRbeam code: Comparison with CRPropa and ELMAG codes

Understand

Very-high-energy gamma rays produce electron positron pairs in interactions with low-energy photons of extragalactic background light during propagation through the intergalactic medium.

• The electron-positron pairs generate secondary gamma rays detectable by gamma-ray telescopes.
• This secondary emission can be used to detect intergalactic magnetic fields (IGMF) in the voids of large-scale structure.
• A new gamma-ray observatory, namely, Cherenkov Telescope Array (CTA), will provide an increase in sensitivity for detections of these secondary gamma-ray emission and enable the measurement of its properties for sources at cosmological distances.