The angular correlation function of the soft X-ray background

Details The angular correlation function of the soft X-ray background The angular correlation function of the soft X-ray background

Aug 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...288...77s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 288, no. 1, p. 77-88

Astronomy and Astrophysics

Astronomy

29

Active Galactic Nuclei, Background Radiation, Cosmic X Rays, Flux Density, Quasars, Seyfert Galaxies, Variations, X Ray Astronomy, Autocorrelation, Cluster Analysis, Image Analysis, Luminosity, Rosat Mission, Statistical Distributions

Scientific paper

Several dozen observations with the ROSAT Position Sensitive Proportional Counter (PSPC) are used to measure fluctuations of the unresolved X-ray background using the autocorrelation function. At the lowest separation of 1 - 3 arc min a signal of (6.8 +/- 2.5) x 10-3 has been detected. At larger separations (3 - 27 arcmin) the data are dominated by statistical noise. The average amplitude of the correlation function in the range of 3 - 11 arc min amounts to (0.3 +/- 0.9) x 10-3. The tight upper limit on the angular correlation function severly constrains the clustering properties of sources producing the background. In particular, it can be shown that contribution of QSO to the residual background cannot exceed approximately 35%. Low luminosity active galactic nuclei (AGN) (probably Seyfert galaxies) are likely candidates for the unresolved background. In this case they have to be weakly clustered and show relatively strong clustering evolution.

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