Astronomy & Astrophysics

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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3922_f1.eps}\end{figure}$ Figure 1: Mean free path of $\gamma$ -rays calculated for the diffuse extragalactic background model described in Aharonian et al. (2002).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3922_f2.eps}\end{figure}$ Figure 2: Spectrum of non-thermal radiation from the Coma cluster (solid line). The radiation is produced via conversion of VHE $\gamma$ -rays into electron-positron pairs and subsequent synchrotron and IC radiation of secondary electrons. It is assumed that $\gamma$ -rays with spectrum given by Eq. (1) with $\Gamma =2$ , $\beta =0.5$ , E₀=700 TeV, have been injected into ICM over the last 10⁷ years. The dotted line represents the spectrum of primary $\gamma$ -rays as seen by the observer, assuming that $\gamma$ -rays are emitted isotropically. Both spectra are corrected for absorption in the intergalactic medium. The compilation of radio data are taken from Deiss et al. (1997). The open boxes in the EUV and soft X-ray domains correspond to the fluxes observed by Lieu et al. (1999). The open box and points in the hard X-ray domain correspond to fluxes reported by Fusco-Femiano et al. (1999). The magnetic field in the cluster is assumed to be $B=6~\mu$ G.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3922_f3.eps}\end{figure}$ Figure 3: The same as in Fig. 2, but for the intracluster magnetic field $B=0.3~\mu$ G.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3922_f4.eps}\end{figure}$ Figure 4: Relative surface brightness distribution of the non-thermal radiation from Coma cluster in different spectral bands for initial $\gamma$ -rays produced in central source. The cluster is divided in 10 zones. Surface brightness is normalized to the brightness of the central zone. In each zone a separate spectrum calculation has been performed. This figure corresponds to the case with large ICMF ( $B=6~\mu$ G). Relative surface brightness distribution in EUV energy band (0.064-0.240 keV) is shown by solid line, in Soft X-Rays (2-10 keV) by dashed, and in Hard X-Rays (25-80 keV) by dotted lines.
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In the text

$\begin{figure} \par\includegraphics[width=16.9cm,clip]{3922_f5.eps}\end{figure}$ Figure 5: Left panels a): non-thermal luminosities of a spherically symmetric galaxy cluster of radius 1.5 Mpc. The radiation is produced via conversion of VHE $\gamma$ -rays into electron-positron pairs and subsequent synchrotron and IC radiation of secondary electrons. It is assumed that $\gamma$ -rays with a spectrum given by Eq. (1) with $\Gamma =0$ , $\beta =1$ , and (i) E₀=10¹⁶ eV, (ii) 10¹⁸ eV and (iii) 10¹⁹ eV, have been injected into ICM by a central source during the last 10⁷ years. The spectra of the primary $\gamma$ -ray source are shown by thick dashed lines. Dotted lines show the spectra of the primary $\gamma$ -rays after propagating of 1.5 Mpc (at the edge of the cluster). The area between the dashed and dotted lines indicates the amount of energy absorbed and then reradiated in the cluster volume. The luminosity of the primary VHE $\gamma$ -ray source is assumed to be 10⁴⁴ erg/s. The magnetic field in the cluster is assumed to be $B=1~\mu$ G. The luminosities of three different zones of the cluster are shown with thin solid lines: 1 ( R=0 - 10^-3 Mpc), 2 ( R=0.01 - 0.04 Mpc) and 3 ( R=0.44 - 1.5 Mpc). The overall luminosity of the cluster is shown by the thick solid line. Right panels b): expected energy fluxes of non-thermal radiation corresponding to the luminosities shown in the right panels, calculated for a cluster at a distance of 100 Mpc, after correction for the intergalactic absorption.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{3922_f6.eps}\end{figure}$ Figure 6: Energy fluxes of non-thermal radiation from the Coma cluster initiated by products (electrons, positrons, $\gamma$ -rays) of decays of super-heavy "X''-particles. The spectra are calculated for different fragmentation functions, intracluster magnetic field, and $m_{\rm X}$ presented in Table 1. The reported fluxes at radio EUV and X-rays are same as in Fig. 2. The solid lines represent spectra corrected for intergalactic $\gamma$ -ray absorption. Unabsorbed spectra are shown by dashed lines.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3922_f1.eps}\end{figure}$	Figure 1: Mean free path of $\gamma$ -rays calculated for the diffuse extragalactic background model described in Aharonian et al. (2002).
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3922_f3.eps}\end{figure}$	Figure 3: The same as in Fig. 2, but for the intracluster magnetic field $B=0.3~\mu$ G.
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