Soft X-ray background fluctuations and large-scale structure in the Universe

Abstract

We have studied the fluctuations of the soft (0.9-2 keV) X-ray background intensity for ∼10 and ∼2 arcmin beam sizes, using 80 high galactic latitude medium-deep images from the ROSAT position sensitive proportional counter (PSPC). These fluctuations are dominated (and well reproduced) by confusion noise produced by sources unresolved with the beam sizes we used. We find no evidence for any excess fluctuations which could be attributed to source clustering. The 95 per cent confidence upper limits on excess fluctuations ΔIclus are: (ΔIclus/I)10arcmin≲0.12, (ΔIclus/I)2arcmin≲0.07. We have checked the possibility that low surface brightness extended objects (like groups or clusters of galaxies) may have a significant contribution to excess fluctuations, finding that they are not necessary to fit the distribution of fluctuations, and obtaining an upper limit on the surface density for this type of source. Standard cold dark matter models would produce ΔI/I larger than the above limits for any value of the density of the Universe Ω = 0.1 - 1, unless the bias parameter of the X-ray emitting matter is smaller than unity, or an important fraction of the sources of the soft X-ray background (∼ 30 per cent) is at redshifts z > 1. Limits on the 2-10 keV excess fluctuations are also considered, showing that X-ray sources in that band have to be at redshifts z > 1 unless Ω > 0.4. Finally, if the spatial correlation function of the sources that produce these excess fluctuations is instead a power law, the density contrast δρ/ρ implied by the excess s luctuations reveals that the Universe is smooth and linear on scales of tens of Mpc, while it can be highly non-linear on scales of ∼ 1 Mpc.