Predictions on the High-Energy Emission from the Coma Cluster

Details Predictions on the High-Energy Emission from the Coma Cluster Predictions on the High-Energy Emission from the Coma Cluster

Oct 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004esasp.552..593r&link_type=abstract

Proceedings of the 5th INTEGRAL Workshop on the INTEGRAL Universe (ESA SP-552). 16-20 February 2004, Munich, Germany. Scientific

Computer Science

Scientific paper

The Coma galaxy cluster exhibits evidence for the existence of a high-energetic non-thermal particle populations. At frequencies > 1 GHz observations of Coma's radio halo indicate a significant spec- tral steepening of the volume-integrated emission from Coma which comprise important information on the electron spectrum. We calculate the volume- averaged high-energy spectrum due to inverse Comp- ton scattering off the cosmic microwave background radiation field and non-thermal bremsstrahlung tak- ing into account an exponential cutoff in the electron spectrum. This particle distribution was deduced from the radio observations. The synchrotron ra- diation from the secondary pairs, created from the decay of charged mesons produced in hadronic pp- interactions, is found to set significant limits on the hadronic energy component in Coma when compared to the steepening radio spectrum. This leads to fur- ther constraints for the maximum flux that can be expected in the high-energy range. In particular we predict that Coma cannot be detected with INTE- GRAL's ISGRI above a few 100 keV (based on the AO-2 continuum sensitivity) nor with the current generation atmospheric Cherenkov telescopes unless significantly more than 106 sec or > 50 hrs of obser- vations are accummulated, respectively. Key words: Galaxies: clusters: Coma Gamma rays: theory Radiation mechanisms: non-thermal.

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