Clustering at High Redshift: Precise Constraints from a Deep, Wide Area Survey

Details Clustering at High Redshift: Precise Constraints from a Deep, Wide Area Survey Clustering at High Redshift: Precise Constraints from a Deep, Wide Area Survey

1998-04-14

arxiv.org/abs/astro-ph/9804141v2

Astronomy and Astrophysics

Astrophysics

31 pages, including 11 figures. Source file is LaTex. Figures are postscript format. Accepted for publication in the Astrophys

Scientific paper

10.1086/306245

We present constraints on the evolution of large-scale structure from a catalog of 710,000 galaxies with I_AB <= 24 derived from a KPNO 4m CCD imaging survey of a contiguous 4 deg x 4 deg region. The advantage of using large contiguous surveys for measuring clustering properties on even modest angular scales is substantial: the effects of cosmic scatter are strongly suppressed. We provide highly accurate measurements of the two-point angular correlation function, w(theta), as a function of magnitude on scales up to 1.5 degrees. The amplitude of w(theta) declines by a factor of ~10 over the range 16 <= I <= 20 but only by a factor of 2 - 3 over the range 20 < I <= 23. For a redshift dependence of the spatial correlation function, xi(r), parameterized as xi(r,z)=(r/r_o)^(-gamma)(1 + z)^(-[3+epsilon]), we find r_o=5.2 +/- 0.4 Mpc/h, and epsilon >= 0 for I <= 20. This is in good agreement with the results from local redshift surveys. At I > 20, our best fit values shift towards lower r_o and more negative epsilon. A strong covariance between r_o and epsilon prevent us from rejecting epsilon > 0 even at faint magnitudes but if epsilon > 1, we strongly reject r_o <= 4/h Mpc (co-moving). The above expression for xi(r,z) and our data give a correlation length of r_o(z=0.5) approx 3.0 +/- 0.4 Mpc/h, about a factor of 2 larger than the correlation length at z = 0.5 derived from the Canada--France Redshift Survey (CFRS). The small volume sampled by the CFRS and other deep redshift probes, however, make these spatial surveys strongly susceptible to cosmic scatter and will tend to bias their derived correlation lengths low. Our galaxy counts agree well with those from the HDF survey and, thus, argue against a significant inclusion of sub-galactic components in the latter census for I < 24.

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