An Analysis of Rich Cluster Redshift Survey Data for Large Scale Structure Studies
Session 56 -- Large-Scale Structure
Display presentation, Tuesday, 10, 1995, 9:20am - 6:30pm

## [56.04] An Analysis of Rich Cluster Redshift Survey Data for Large Scale Structure Studies

K. Slinglend, D. Batuski, S. Haase (U. Maine), J. Hill (Steward Obs.)

The results from the COBE satellite show the existence of structure on scales on the order of 10\% or more of the horizon scale of the universe. Rich clusters of galaxies from Abell's catalog show evidence of structure on scales of 100 Mpc and may hold the promise of confirming structure on the scale of the COBE result. However, many Abell clusters have zero or only one measured redshift, so present knowledge of their three dimensional distribution has quite large uncertainties. The shortage of measured redshifts for these clusters may also mask a problem of projection effects corrupting the membership counts for the clusters.

Our approach in this effort has been to use the MX multifiber spectrometer on the Steward 2.3m to measure redshifts of at least ten galaxies in each of 80 Abell cluster fields with richness class $R\ge 1$ and $mag_{10} \le 16.8$ (estimated $z\le 0.12$) and zero or one measured redshifts. This work will result in a deeper, more complete (and reliable) sample of positions of rich clusters. Our primary intent for the sample is for two-point correlation and other studies of the large scale structure traced by these clusters in an effort to constrain theoretical models for structure formation. We are also obtaining enough redshifts per cluster so that a much better sample of reliable cluster velocity dispersions will be available for other studies of cluster properties.

To date, we have collected such data for 64 clusters, and for most of them, we have seven or more cluster members with redshifts, allowing for reliable velocity dispersion calculations. Velocity histograms and stripe density plots for several interesting cluster fields are presented, along with summary tables of cluster redshift results.

Also, with 10 or more redshifts in most of our cluster fields ($30^{\prime }$ square, just about an `Abell diameter' at $z \sim 0.1$) we have investigated the extent of projection effects within the Abell catalog in an effort to quantify and understand how this may effect the Abell sample.