Extragalactic X-ray Sources and the X-ray Background
نویسندگان
چکیده
منابع مشابه
Angular Correlations of the X–ray Background and Clustering of Extragalactic X–ray Sources
The information content of the autocorrelation function (ACF) of intensity fluctuations of the X–ray background (XRB) is analyzed. The tight upper limits set by ROSAT deep survey data on the ACF at arcmin scales imply strong constraints on clustering properties of X–ray sources at cosmological distances and on their contribution to the soft XRB. If quasars have a clustering radius r0 = 12–20 Mp...
متن کاملThe Sources of the X–ray Background
Deep X–ray surveys have shown that the cosmic X–ray background (XRB) is largely due to the accretion onto su-permassive 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/...
متن کاملOn the intensity of the extragalactic X-ray background
Measurements of the intensity of the cosmic X-ray background (XRB) carried out over small solid angles are subject to spatial variations due to the discrete nature of the XRB. This cosmic variance can account for the dispersion of XRB intensity values found within the ASCA, BeppoSAX and ROSAT missions separately. However there are differences among the values obtained in the different missions ...
متن کاملThe X-ray Background and the Deep X-ray Surveys
The deep X-ray surveys performed by the two major X-ray observatories on flight, Chandra and XMM, are being resolving the bulk of the cosmic X-ray background (XRB) in the 2–10 keV energy band, where the sky flux is dominated by extragalactic emission. Although the actual fraction depends on the absolute sky flux, which is measured with an uncertainty of ∼ 40%, most of the XRB is already resolve...
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ژورنال
عنوان ژورنال: Monthly Notices of the Royal Astronomical Society
سال: 1975
ISSN: 0035-8711,1365-2966
DOI: 10.1093/mnras/170.1.199