All Figures

$\begin{figure} \par\includegraphics[height=.24\textheight,clip]{f1.eps} \end{figure}$ Figure 1: Spectral indices of blazars in the 3rd EGRET catalog (meanindex $1.37\pm 0.04$ ).
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In the text

$\begin{figure} \par\includegraphics[height=.25\textheight,clip]{f2.eps} \end{figure}$ Figure 2: Template spectra for a source of case 1 (thin lines) and case 2 (thick lines) located at different redshifts. For both cases the intrinsic spectrum (dashed lines), the absorbed spectrum (solid lines) and the cascade emission (dot-dashed lines) is shown. In the lower right panel the data are shown for Mkn 501 (see Ref. of Fig. 1 and Kneiske et al. 2004). The shaded region is the intrinsic region for different MRF models (Kneiske et al. 2004). In the lower left panel the same is shown for 1ES1959+650 at a redshift of 0.47.
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In the text

$\begin{figure} \par\includegraphics[height=.24\textheight,clip]{f3.eps}\end{figure}$ Figure 3: Same as in Fig. 2 but the flux is shown for a source of case 3. The data and intrinsic regions are for Mkn 421, PKS 2005-489 and PKS 2155-304. (see Refs. Fig. 1 and Kneiske et al. 2004).
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In the text

$\begin{figure} \par\includegraphics[height=.24\textheight,clip]{f4.eps} \end{figure}$ Figure 4: The un-absorbed spectrum (dashed line), the absorbed spectrum (thick solid line) and the cascade emission (dot-dashed line) for the extreme BL Lac 1H1428+428 at a redshift of z=0.129. The data and the shaded region indicating the allowed range for the intrinsic spectrum is taken from Kneiske et al. (2004).
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In the text

$\begin{figure} \par\includegraphics[height=.24\textheight,clip]{f5.eps} \end{figure}$ Figure 5: The intensity of the extragalactic gamma-ray background. The contribution from HBLs to the EGRB (thick solid line) for all 4 cases. (The flux without absorption: dotted line; flux with absorption: dashed line; cascade contribution alone: thin solid line.) Data are from Sreekumar et al. (1998): solid diamonds and Strong et al. (2004): open circles.
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In the text

$\begin{figure} \par\includegraphics[height=.24\textheight,clip]{f6.eps} \end{figure}$ Figure 6: Extragalactic gamma-ray background and assumed blazar contributions due to low-peaked blazars (thin solid line) and high-peaked blazars (dashed line) including the effects of intergalactic cascading.
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In the text

$\begin{figure} \par\includegraphics[height=.24\textheight,clip]{f7.eps} \end{figure}$ Figure 7: Number of BL Lacs as a function of redshift for case 1; thin solid line: total number of sources; thin dashed line: observable sources using a telescope $E_{\rm thr}=300$ GeV and a flux limit of 10^-11 cm^-2 s^-1; thick-solid line: observable sources including the effect of extragalactic absorption only; dot-dashed line: observable sources including the effect of extragalactic absorption and telescope parameters (energy threshold and sensitivity).
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In the text

$\begin{figure} \par\includegraphics[height=.24\textheight,clip]{f1.eps} \end{figure}$	Figure 1: Spectral indices of blazars in the 3rd EGRET catalog (meanindex $1.37\pm 0.04$ ).
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$\begin{figure} \par\includegraphics[height=.24\textheight,clip]{f3.eps}\end{figure}$	Figure 3: Same as in Fig. 2 but the flux is shown for a source of case 3. The data and intrinsic regions are for Mkn 421, PKS 2005-489 and PKS 2155-304. (see Refs. Fig. 1 and Kneiske et al. 2004).
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$\begin{figure} \par\includegraphics[height=.24\textheight,clip]{f4.eps} \end{figure}$	Figure 4: The un-absorbed spectrum (dashed line), the absorbed spectrum (thick solid line) and the cascade emission (dot-dashed line) for the extreme BL Lac 1H1428+428 at a redshift of z=0.129. The data and the shaded region indicating the allowed range for the intrinsic spectrum is taken from Kneiske et al. (2004).
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$\begin{figure} \par\includegraphics[height=.24\textheight,clip]{f5.eps} \end{figure}$	Figure 5: The intensity of the extragalactic gamma-ray background. The contribution from HBLs to the EGRB (thick solid line) for all 4 cases. (The flux without absorption: dotted line; flux with absorption: dashed line; cascade contribution alone: thin solid line.) Data are from Sreekumar et al. (1998): solid diamonds and Strong et al. (2004): open circles.
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$\begin{figure} \par\includegraphics[height=.24\textheight,clip]{f6.eps} \end{figure}$	Figure 6: Extragalactic gamma-ray background and assumed blazar contributions due to low-peaked blazars (thin solid line) and high-peaked blazars (dashed line) including the effects of intergalactic cascading.
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