Cosmic-ray transport and gamma-ray emission in M31

Abstract

We study the possibility that an extended cosmic-ray leptonic and/or hadronic halo is at the origin of the large-scale gamma-ray emission detected from the Andromeda Galaxy (M31). We consider a broad ensemble of non-homogeneous diffusion scenarios and of cosmic-ray injection sources. We find that cosmic-ray electrons and protons could be, and very likely are, responsible for part, or all, of the gamma-ray emission from M31, including out to more than 100 kpc from the center of the galaxy. We also simulate possible emission from pulsars in M31, and consider the effect of regions of highly inefficient diffusion around cosmic-ray acceleration sites, as suggested by recent TeV halo observations with Cherenkov telescopes.

arXiv comment10 pages, 9 figures, to be submitted

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Cited by in corpus (3)

• Constraining Cosmic-ray Transport with Observations of the Circumgalactic Medium
• Pulsars Do Not Produce Sharp Features in the Cosmic-Ray Electron and Positron Spectra
• The Andromeda Gamma-Ray Excess: Background Systematics of the Millisecond Pulsars and Dark Matter Interpretations