J. Einasto, M. Einasto, P. Frisch, S. Gottlöber, V. Müller, V. Saar, A.A. Starobinsky, E. Tago, D. Tucker, and H. Andernach
and
J. Einasto, M. Einasto, P. Frisch, S. Gottlöber, V. Müller, V. Saar, A.A. Starobinsky, D. Tucker
In these papers we determine the correlation function for rich clusters of galaxies in the Northern and Southern Galactic hemispheres up to a redshift z = 0.12 and for a separation interval about 650 Mpc (Paper II). We show that superclusters of galaxies and voids between them form a moderately regular network. As a result the cluster correlation function oscillates: it has a series of regularly spaced secondary maxima and minima. The scale of the supercluster-void network, determined from the period of oscillations, is P=115 +/-15 Mpc. We compare the observed cluster correlation function with similar functions derived for popular models of structure formation, as well as for simple geometrical models of cluster distribution (Paper III). We find that the production of the observed cluster correlation function in any model with a smooth transition of the power spectrum from a Harrison-Zeldovich regime with positive spectral index on long wavelengths to a negative spectral index on short wavelengths is highly unlikely. The power spectrum must have an extra peak located at the wavelength equal to the period of oscillations of the correlation function.
The Figure shows the correlation function for clusters in rich superclusters (strongly oscillating function with error corridor given with short-dashed lines) and for clusters in poor superclusters (less oscillating function with error corridor given with long-dashed lines).
Accepted for publishing in MNRAS (April 1997).
The complete paper (postscript version) is available at ftp. aai.ee and babbage.sissa.it.