Gamma Ray Emission from Merger Shocks in the Coma Cluster of Galaxies

A numerical simulation model of the injection and cooling of nonthermal particles energized by shocks formed in merging clusters of galaxies is used to fit radio and X-ray data observed from the Coma cluster of galaxies. The results are consistent with a primary merger-shock origin for both the diff...

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Bibliographic Details
Published inarXiv.org
Main Authors Berrington, R C, Dermer, C D
Format Paper
LanguageEnglish
Published Ithaca Cornell University Library, arXiv.org 09.02.2006
Subjects
Acceleration
Activation
Computer simulation
Galactic clusters
Galaxies
Gamma rays
Ground-based observation
Observatories
Power efficiency
Radio emission
Secondary emission
Star & galaxy formation
Turbulence models
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Summary:A numerical simulation model of the injection and cooling of nonthermal particles energized by shocks formed in merging clusters of galaxies is used to fit radio and X-ray data observed from the Coma cluster of galaxies. The results are consistent with a primary merger-shock origin for both the diffuse radio halo emission and the hard X-ray excess measured with {\it Beppo-SAX} and {\it RXTE}. For equal (1%) efficiency of power injected in nonthermal protons and electrons, we predict that the Coma cluster of galaxies will be significantly detected with the space-based observatory {\it GLAST}, and marginally detectable with the ground-based \(\gamma\)-ray observatories {\it VERITAS} and {\it HESS}. Significant TeV detections are possible if the nonthermal proton intensity is greater due to a larger efficiency of nonthermal hadron acceleration, or to past merger events. The nonthermal hadronic content in Coma is also revealed by a weak, hard secondary emission component at \(\sim 10\) -- 100 GHz. The spectral softening of the radio emission at large radii from the Coma cluster core derives in this scenario from the decreasing shock speed away from cluster center for an on-axis merger event. We discuss differences between merger and delayed turbulence models.
ISSN:2331-8422