1. Correlation function in z and real space and consequences A MEASURE OF  = ( Ω m 0.6 / b) Via redshift distorsions

2.  = ( Ω m 0.6 / b)

7. Redshift-space c. f. « distances » in the Z space not in real space

8. Leads to the true real space correlation function by deprojection

9.  = ( Ω m 0.6 / b)

13. Distorsion is a measure of  = ( Ω m 0.6 / b) and then to Ω m if b known

15. Dynamical effects of the cosmological constant Authors: Lahav, Ofer; Lilje, Per B.; Primack, Joel R.; Rees, Martin J. Affiliation: AA(Cambridge University Institute of Astronomy, England), AB(NORDITA, Copenhagen, Denmark), AC(California, University, Santa Cruz), AD(Cambridge University Institute of Astronomy, England) Journal: Royal Astronomical Society, Monthly Notices (ISSN 0035-8711), vol. 251, July 1, 1991, p. 128-136. (MNRAS Homepage) Abstract Dynamical tests such as density and velocity profiles around clusters and virialization are employed to theoretically determine the cosmological constant and the density parameter. Limits on the cosmological constant and dynamical tests in linear theory are reviewed, and the tests do not provide a conclusive distinction for universes with cosmological constants. The practical limitations of observing clustering at different redshifts is discussed with respect to linear theory. The nonlinear spherical infall model is then examined for cold-dark- matter power spectra, and the limitations of this method and related observations are discussed. An expression is derived to describe the final radius of a virialized cluster, in which a repulsive cosmological constant lambda gives a smaller value. Two scenarios for the universe are suggested based on the results, one with a large amount of nonbaryonic matter and a zero cosmological constant and another in which all matter is baryonic and the cosmological constant is added to save inflation.