**AAS Meeting #193 - Austin, Texas, January 1999**

*Session 2. Galaxy Evolution and Surveys I - Low Redshift*

Display, Wednesday, January 6, 1999, 9:20am-6:30pm, Exhibit Hall 1
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## [2.04] Precision measurements from the Las Campanas Suryey -- two-point, three point correlation functions and the pairwise velocity dispersion of galaxies

*G. B\"orner (MPA), I.P. Jing (RESCEU), H.J. Mo (MPA)*

Three of the most fundamental quantities in the large-scale
structure studies, i.e. the real-space two--point
correlation function (2PCF), the three--point correlation
function (3PCF), and the pairwise velocity dispersion of
galaxies (PVD) can all be measured reliably from the Las
Campanas Redshift Survey (LCRS). An important aspect of our
studies is the use of a number of mock catalogs derived from
large simulations to guide the statistical analysis, such
that both the error measurement, as well as the
quantification of any systematic effect (either in the
observations or in the statistical methods) can be done
reliably.

The results for the real--space 2CPF can be well fitted by a
power law: \[ \xi(r) = (r_{0}/r)^{\}gamma\] with \[
r_{0}=(5.06±.12)h^{-1}Mpc \] and \[ \gamma = 1.862±.034
\] The PVD at a separation of 1 h{-1} Mpc is \[ 570±0 km
s{-1} \].

The 3PCF has small but significant deviations from the
well--known hierarchical form. The projected Q--value can be
fitted approximately by Q(r_{p}, u, v) = 0.7 r_{p}^{-0.3}
(r_{p} in units of h^{-1} Mpc).

A detailed comparison between these observational results
and the predictions of CDM cosmogonies is carried out. A
flat model with \Omega = 0.2 meets the 2PCF and PVD
constraints, but gives higher values for the 3PCF than
observed.

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