1999/01/27 by L. Guzzo, J. G. Bartlett, Guzzo, L. +37
Physics and Astronomy · #Astrophysics (astro-ph) #FOS: Physical sciences #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/9901378
Latex, uses aa.cls (included); 17 pages with colour figures. Submitted to A&A
arxiv created 1999/01/27 · arxiv updated 2009/12/01
We present analyses of the two-point correlation properties of the ESP galaxy redshift survey. From the redshift-space correlation function xi(s), we see positive clustering out to separations ~50/h Mpc, with a smooth break on larger scales and zero-crossing between 60 and 80/h Mpc. xi(s) is reasonably well described by a shallow power law with γ~1.5 between 3 and 50/h Mpc, while on smaller scales (0.2-2/h Mpc) it has a shallower slope (γ~ 1). We examine the full effect of redshift-space distortions through the two-dimensional correlation function xi(rp,pi), from which we project out the real-space xi(r) below 10/h Mpc. This function is well described by a power-law model (r/ro)-γ, with ro=4.15+0.20-0.21 h-1 Mpc and γ=1.67+0.07-0.09. Comparison to other redshift surveys shows a consistent picture in which clustering remains positive out to separations of 50/h Mpc or larger, in substantial agreement with the results obtained from angular surveys like the APM and EDSGC. Also the shape of the two-point correlation function is remarkably unanimous among these data sets, in all cases requiring more power above 5/h Mpc (a `shoulder'), than a simple extrapolation of the canonical xi(r)=(r/5)-1.8. xi(s) for volume-limited subsamples shows evidence of luminosity segregation only for the most luminous sample with MbJ≤ -20.5. When redshift-space distortions are removed through projection of xi(rp,pi), however, a weak dependence on luminosity is seen at small separations also at fainter magnitudes. This effect is masked in redshift space, as the mean pairwise velocity dispersion experiences a parallel increase, basically erasing the effect of the clustering growth on xi(s).