The mean density and two-point correlation function for the CfA redshift survey slices

1988 ◽  
Vol 332 ◽  
pp. 44 ◽  
Author(s):  
Valerie de Lapparent ◽  
Margaret J. Geller ◽  
John P. Huchra
Keyword(s):  
Correlation Function ◽  
Point Correlation ◽  
Point Correlation Function ◽  
Redshift Survey ◽  
The Mean

scholarly journals The Anglo-Australian Redshift Survey

1983 ◽  
Vol 104 ◽  
pp. 175-175
Author(s):  
J. Bean ◽  
G. Efstathiou ◽  
R. S. Ellis ◽  
B. A. Peterson ◽  
T. Shanks ◽  
...  
Keyword(s):  
Correlation Function ◽  
Luminosity Function ◽  
Large Scale ◽  
Peculiar Velocities ◽  
Point Correlation ◽  
Point Correlation Function ◽  
Redshift Survey ◽  
Density Inhomogeneities ◽  
The Universe

The aim of the survey is to sample a relatively large, randomly chosen volume of the Universe in order to study the large-scale distribution of galaxies using the two-point correlation function, the peculiar velocities between galaxy pairs and to provide an estimate of the galaxian luminosity function that is unaffected by density inhomogeneities and Virgo infall.

scholarly journals The 2dF QSO Redshift Survey - XIV. Structure and evolution from the two-point correlation function

2005 ◽  
Vol 356 (2) ◽  
pp. 415-438 ◽  
Author(s):  
Scott M. Croom ◽  
B. J. Boyle ◽  
T. Shanks ◽  
R. J. Smith ◽  
L. Miller ◽  
...  
Keyword(s):  
Correlation Function ◽  
Point Correlation ◽  
Point Correlation Function ◽  
Redshift Survey

scholarly journals The Center for Astrophysics Redshift Survey: Luminosity Function and Two-Point Correlation Function

1988 ◽  
Vol 130 ◽  
pp. 519-519
Author(s):  
Valérie de Lapparent ◽  
Margaret J. Geller ◽  
John P. Huchra
Keyword(s):  
Correlation Function ◽  
Luminosity Function ◽  
Theoretical Models ◽  
Spatial Correlation Function ◽  
Correlation Lengths ◽  
Two Samples ◽  
Derived Properties ◽  
Point Correlation ◽  
Point Correlation Function ◽  
Redshift Survey

We compare the luminosity function and the two-point spatial correlation function for the two slices of the CfA redshift survey extension to mB(0) ≤ 15.5 [8h ≤ RA. ≤ 17h and 26.5° ≤ DEC. ≤ 38.5°], with those for the early survey limited to mB(0) ≤ 14.5 [bII ≥ 40°, and DEC. ≥ 0°]. The derived properties of the two samples agree within the errors. The parameters of the luminosity function are M* = −19.1±0.1 and α = −1.2±0.1 for the 15.5 sample, and M* = −19.3±0.1 and α = −1.1 ± 0.1 for the 14.5 sample. We use an inhomogeneity-independent method to calculate the luminosity function. The slopes of the correlation functions for the two samples are −1.5 ± 0.35, shallower than the canonical slope of −1.8. The correlation lengths are 7.5 ± 5h−1 Mpc, larger than the correlation length of 5h−1 Mpc matched to the theoretical models. Because of the 25% uncertainty in the mean density of the 15.5 sample, the correlation function is indeterminate on scales larger than ∼ 20h−1 Mpc.

scholarly journals Scale-Invariant Correlation Functions of Cosmological Density Fluctuations in the Strong Clustering Regime and the Stability

1999 ◽  
Vol 183 ◽  
pp. 274-274
Author(s):  
Taihei Yano ◽  
Naoteru Gouda
Keyword(s):  
Correlation Function ◽  
Spatial Correlation ◽  
Correlation Functions ◽  
Power Index ◽  
Nonlinear Regime ◽  
Peculiar Velocity ◽  
Strongly Nonlinear ◽  
Point Correlation ◽  
Point Correlation Function ◽  
The Mean

We have investigated the scale-invariant solutions of the BBGKY equations for spatial correlation functions of cosmological density fluctuations and the mean relative peculiar velocity in the strongly nonlinear regime. It is found that the solutions for the mean relative physical velocity depend on the three-point spatial correlation function and the skewness of the velocity fields. We find that the stable condition in which the mean relative physical velocity vanishes on the virialized regions is satisfied only under the assumptions which Davis & Peebles took in there paper. It is found, however, that their assumptions may not be general in real. The power index of the two-point correlation function in the strongly nonlinear regime depends on the mean relative peculiar velocity, the three-point correlation function and the skewness. If self-similar solutions exist, then the power index in the strongly nonlinear regime is related to the power index of the initial power spectrum and its relation depends on the three-point correlation function and the skewness through the mean relative peculiar velocity. We also investigate stability of the solutions of the BBGKY equations for two-point spatial correlation functions. In the case that the background skewness is equal to 0, we found that there is no local instability in the strongly non-linear regime.

scholarly journals The two-point correlation function of rich clusters of galaxies: results from an extended APM cluster redshift survey

1994 ◽  
Vol 271 (1) ◽  
pp. L47-L51 ◽  
Author(s):  
G. B. Dalton ◽  
R. A. C. Croft ◽  
G. Efstathiou ◽  
W. J. Sutherland ◽  
S. J. Maddox ◽  
...  
Keyword(s):  
Correlation Function ◽  
Clusters Of Galaxies ◽  
Point Correlation ◽  
Point Correlation Function ◽  
Redshift Survey
Sign in / Sign up

Export Citation Format

Share Document