Volume 408, Number 1, September II 2003
|Page(s)||39 - 42|
|Section||Cosmology (including clusters of galaxies)|
|Published online||17 November 2003|
The diffuse X-ray background
Nicolaus Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland
Corresponding author: firstname.lastname@example.org
Accepted: 16 June 2003
The deepest observations of the X-ray background approach the surface brightness of the truly diffuse component generated by Thomson scattering of cosmic X-ray photons. Available estimates of the electron density and the X-ray luminosity density of AGNs as a function of cosmological epoch are used to calculate the integral scattered X-ray background component. It is shown that the scattered component constitutes % of the total background, depending on the AGN cosmic evolution. Albeit this is a minute fragment of the total flux, it becomes a perceptible fraction of the still unresolved part of the background and should be taken into account in the future rigorous assessments of the X-ray background structure. This diffuse component at energies 1 keV sums up with the emission by WHIM to %. Consequently, one should expect that integrated counts of discrete sources account for just % for soft background and ~99% at higher energies.
Key words: X-rays: diffuse background
© ESO, 2003
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