The large-scale structure of the X-ray background and its cosmological implications

A careful analysis of the HEAO 1 A-2 2-10 keV full-sky map of the X-ray background (XRB) reveals clustering on the scale of several degrees. After removal of the contribution due to beam smearing, the intrinsic clustering of the background is found to be consistent with an autocorrelation function of the form (3.6 +/- 0.9) x 10(-4)theta(-1), where theta is measured in degrees. If current active galactic nucleus models of the hard XRB are reasonable and the cosmological constant-cold dark matter (LambdaCDM) cosmology is correct, this clustering implies an X-ray bias factor of b(X) similar to 2. Combined with the absence of a correlation between the XRB and the cosmic microwave background (CMB), this clustering can be used to limit the presence of an integrated Sachs-Wolfe (ISW) effect and thereby to constrain the value of the cosmological constant, Omega(Lambda) less than or equal to 0.60 (95% CL). This constraint is inconsistent with much of the Omega(Lambda) parameter space currently favored by other observations. Finally, we marginally detect the dipole moment of the diffuse XRB and find it to be consistent with the dipole due to our motion with respect to the mean rest frame of the XRB. The limit on the amplitude of any intrinsic dipole is deltaI/I less than or equal to 5 x 10(-3) at the 95% CL. When compared to the local bulk velocity, this limit implies a constraint on the matter density of the universe of Omega(m)(0.6)/b(x)(0)greater than or similar to0.24.