[논문]GALAXY CLUSTERS IN GAMMA-RAYS: AN ASSESSMENT FROM OBSERVATIONS

REIMER OLAF

doi:10.5303/jkas.2004.37.5.307

[국내논문] GALAXY CLUSTERS IN GAMMA-RAYS: AN ASSESSMENT FROM OBSERVATIONS 원문보기

Journal of the Korean astronomical society = 천문학회지, v.37 no.5, 2004년, pp.307 - 313

REIMER OLAF (Ruhr-Universiiit Bochum, Institut fur Theoretische Physik IV)

Abstract ▼ AI-Helper

Clusters of galaxies are believed to constitute a population of astrophysical objects potentially able to emit electromagnetic radiation up to gamma-ray energies. Evidence of the existence of non-thermal radiation processes in galaxy clusters is indicated from observations of diffuse radio halos, hard X-ray and EUV excess emission. The presence of cosmic ray acceleration processes and its confinement on cosmological timescales nearly inevitably yields in predicting energetic gamma-ray emission, either directly deduceably from a cluster's multifreqency emission characteristics or indirectly during large-scale cosmological structure formation processes. This theoretical reasoning suggests several scenarios to actually detect galaxy clusters at gamma-ray wavelengths: Either resolved as individual sources of point-like or extended gamma-ray emission, by investigating spatial-statistical correlations with unidentified gamma-ray sources or, if unresolved, through their contribution to the extragalactic diffuse gamma-ray background. In the following I review the situation concerning the proposed relation between galaxy clusters and high-energy gamma-ray observations from an observational point-of-view.

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제안 방법

The large sample size of ~4000 Abell cluster in a correlation study with unidentified gamma-ray sources invokes an additional problem: The average EGRET source location uncertainty contour includes an area of up to a few square degrees at the sky, and several Abell clusters may correlate with an individual unidentified gamma-ray source. Thus, we expect autocorrelation in the Abell cluster sample when comparing it with unidentified gamma-ray sources. Reimer et al.
background. This requires a profound understanding of the determination and theoretical modeling of the galactic diffuse emission and the extragalactic diffuse gamma-ray back-ground (EGDB), including the involved statistical and systematical uncertainties and residual contaminations. In case of an already detected source class like BL Lacs and FSRQs, such contributions can be quantitatively determined on the basis of their luminosity function or logN-logS source statistics from actual observations.
Subsequently, the gamma-ray data from individual galaxy clusters have been co-added in cluster-centered coordinates. The co-added images were again analyzed using the likelihood technique, however in conjunction with an adequately adapted diffuse gamma-ray foreground model. Fig.

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