Detailed study of extended gamma-ray morphology in the vicinity of the Coma cluster with Fermi-LAT

Abstract

Galaxy clusters can be sources of high-energy (HE) $\gamma$-ray radiation, due to the efficient acceleration of particles exceeding EeV energies. At present, though, the only candidate for emitting HE $\gamma$-rays is the Coma cluster, towards which an excess of $\gamma$-ray emission has been detected by the Fermi Large Area Telescope (LAT). Using $\sim 12.3$ years of \textit{Fermi}-LAT data, we explored the region of the Coma cluster between energies 100 MeV and 1 TeV by detailed spectral and morphological analysis. In the region of the Coma cluster, we detected diffuse gamma-ray emission of energies between 100 MeV and 1 TeV with a 5.4$\sigma$ extension significance and a 68\% containment radius of $0.82_{-0.05}^{+0.10}$ degrees derived with a 2D homogeneous disk model. The corresponding gamma-ray spectrum extends up to $\sim 50$ GeV, with a power-law index of $\mathrm{\Gamma }=2.23\pm 0.11$ and flux of $(3.84\pm 0.67)\times 10^{-12}\mathrm{erg}\mathrm{c}{\mathrm{m}}^{-2}{\mathrm{s}}^{-1}$. Using energy arguments we show that point-like sources such as radiogalaxies and star-forming galaxies are unlikely to explain the emission, and more likely, the emission is produced in the Coma cluster. Besides, we also identified three point-like sources in the region. However, due to the limited statistics of the detection, we could neither exclude nor conclude that the total extended emission is contributed to by these three-point like sources.

Submitted in MNRAS

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