Table 7: Intensity of the X-ray background contributed by our sources in the various energy bands.
Energy band $S_{\rm min}$ $S_{\rm max}$ $I_{\rm CXRB}(S_{\rm min}\le S\le S_{\rm max})$ $I_{\rm CXRB}$ $f_{\rm CXRB}$
(keV) (${\rm cgs}$) (${\rm cgs}$) ( ${\rm 10^{-12}~cgs~deg^{-2}}$) ( ${\rm 10^{-12}~cgs~deg^{-2}}$)  
(1) (2) (3) (4) (5) (6)
0.5-1 $9.9\times10^{-16}$ 10-12 2.4 2.96 0.81
  10-12   0.32   0.11
1-2 $1.2\times10^{-15}$ 10-12 2.5 4.50* 0.55
  10-12   0.12   0.03
2-4.5 $3.7\times10^{-15}$ 10-12 3.3 7.80 0.42
  10-12   0.08   0.01
4.5-10 $14 \times10^{-15}$ 10-12 2.8 12.4 0.22
  10-12   0.14   0.01
0.5-2 $1.4\times10^{-15}$ 10-12 4.9 7.50* 0.65
  10-12   0.48   0.06
2-10 $9.0\times10^{-15}$ 10-12 8.0 20.2* 0.39
  10-12   0.39   0.02
(1) Energy band definition (in keV). (2) and (3) Minimum and maximum flux used in the integration. (4) Intensity of the X-ray background contributed by our sources. Note that the quoted values include the contribution from both clusters of galaxies and stars. (5) Total X-ray background intensity. Errors are 1$\sigma $ uncertainty. The values indicated with an asterisk are from Moretti et al. (2003). These values were used to estimate the CXRB intensity in the various energy bands assuming a power-law model of $\Gamma $ = 1.4 (see Sect. 3.6 for details). (6) Fraction of X-ray background resolved by our sources.

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