The sources of the X-ray background

Abstract

Deep X-ray surveys have shown that the cosmic X-ray background (XRB) is largely due to the accretion onto supermassive black holes, integrated over cosmic time. The ROSAT, Chandra and XMM-Newton satellites have resolved more than 80% of the 0.1-10 keV X-ray background into discrete sources. Optical spectroscopic identifications are about 90% and 60% complete for the deepest ROSAT and Chandra/ XMM-Newton surveys, respectively, and show that the sources producing the bulk of the X-ray background are a mixture of obscured (type-2) and unobscured (type-1) AGNs, as predicted by the XRB population synthesis models, following the unified AGN scenarios. The characteristic hard spectrum of the XRB can be explained if most of the AGN are heavily absorbed, and in particular a class of highly luminous type-2 AGN, so called QSO-2s exist. The deep Chandra and XMM-Newton surveys have recently detected several examples of QSO-2s. The space density of the X-ray selected AGN, as determined from ROSAT surveys does not seem to decline as rapidly as that of optically selected QSO, however, the statistics of the high-redshift samples is still rather poor. The new Chandra and XMM-Newton surveys at significantly fainter fluxes are starting to provide additional constraints here, but the preliminary observed redshift distribution peaks at much lower redshifts (z=0.5-0.7) than the predictions based on the ROSAT luminosity function.