A 20 centimeter VLA survey of Abell clusters of galaxies. III - Images and optical identifications

1993 ◽  
Vol 87 ◽  
pp. 135 ◽  
Author(s):  
Frazer N. Owen ◽  
Richard A. White ◽  
Jingping Ge
Keyword(s):  
Clusters Of Galaxies ◽  
Abell Clusters ◽  
Optical Identifications

scholarly journals Catalogue of Clusters that are Members of Superclusters

1983 ◽  
Vol 104 ◽  
pp. 185-186
Author(s):  
M. Kalinkov ◽  
K. Stavrev ◽  
I. Kuneva
Keyword(s):  
Standard Deviation ◽  
Correlation Coefficient ◽  
The Other ◽  
Clusters Of Galaxies ◽  
Number Of Clusters ◽  
Abell Clusters ◽  
The Mean ◽  
Abell Cluster ◽  
Image Position

An attempt is made to establish the membership of Abell clusters in superclusters of galaxies. The relation is used to calibrate the distances to the clusters of galaxies with two redshift estimates. One is m10, the magnitude of the ten-ranked galaxy, and the other is the “mean population,” P, defined by: where p = 40, 65, 105 … galaxies for richness groups 0, 1, 2 …, and r is the apparent radius in degrees given by: The first iteration for redshift, z1, is obtained from m10 alone: The standard deviation for Eq. (1) is 0.105, the number of clusters with known velocities is 342 and the correlation coefficient between observed and fitted values is 0.921. With zi from Eq. (1), we define Cartesian galactic coordinates Xi = Rih−1 cosBi cosLi, Yi = Rih−1 cosBi sinLi, Zi = Rih−1 sinBi for each Abell cluster, i = 1, …, 2712, where Ri is the distance to the cluster (Mpc), and Ho = 100 h km s−1 Mpc−1.

Redshifts of radio galaxies in Abell clusters of galaxies

1988 ◽  
Vol 95 ◽  
pp. 1 ◽  
Author(s):  
Frazer N. Owen ◽  
Richard A. White ◽  
Harley A., Jr. Thronson
Keyword(s):  
Radio Galaxies ◽  
Clusters Of Galaxies ◽  
Abell Clusters

Faraday rotation from Abell clusters of galaxies

1989 ◽  
Vol 347 ◽  
pp. 144 ◽  
Author(s):  
G. S. Hennessy ◽  
F. N. Owen ◽  
J. A. Eilek
Keyword(s):  
Faraday Rotation ◽  
Clusters Of Galaxies ◽  
Abell Clusters

scholarly journals Space Distribution of the Richest Abell Clusters of Galaxies

1988 ◽  
Vol 130 ◽  
pp. 533-533
Author(s):  
M Kalinkov ◽  
I Kuneva
Keyword(s):  
Space Distribution ◽  
List Type ◽  
Clusters Of Galaxies ◽  
Type Number ◽  
Abell Clusters

We discuss four samples from the Abell (1958) catalog of clusters of galaxies. Our samples are drawn out from the Abell sample and all clusters have richness 2 and 3. With Ho = 100 km/s/Mpc and qo = +1, we examine the following volumes, defined for both galactic hemispheres: (i)RG 3: b 40° for 0° < 1 360° and b 30° for 90° < 1 240°, distance 300 < R < 750 Mpc, N = 35 clusters, 30 of which with known redshift;(ii)RG 3: b −35° for 15° < 1 232°, 150 < R < 600 Mpc, N = 15 (13);(iii)RG 2: b and 1 as (i), 60 < R < 525 Mpc, N = 110 (55);(iv)RG 2: b and 1 as (ii), 120 < R < 600 Mpc, N = 102(14).

scholarly journals The correlation function of rich clusters of galaxies: a comparison of APM and Abell clusters

1992 ◽  
Vol 257 (1) ◽  
pp. 125-134 ◽  
Author(s):  
G. Efstathiou ◽  
G. B. Dalton ◽  
W. J. Sutherland ◽  
S. J. Maddox
Keyword(s):  
Correlation Function ◽  
Clusters Of Galaxies ◽  
Abell Clusters

scholarly journals Profiles of Galaxy Clusters in Cosmological Scenarios

1987 ◽  
Vol 117 ◽  
pp. 287-287
Author(s):  
Michael J. West ◽  
Avishai Dekel ◽  
Augustus Oemler
Keyword(s):  
High Resolution ◽  
Galaxy Clusters ◽  
Hierarchical Clustering ◽  
Large Scale ◽  
Power Spectra ◽  
Clusters Of Galaxies ◽  
Spatial Symmetry ◽  
Abell Clusters ◽  
Wide Range ◽  
Large Scale Simulations

We have studied the properties of rich clusters of galaxies in various cosmological scenarios by comparing high resolution N-body simulations with observations of Abell clusters. The clusters have been simulated in two steps. First, protoclusters are identified in large-scale simulations which represent a wide range of cosmological scenarios (hierarchical clustering, pancake scenarios, and hybrids of the two, spanning a range of power spectra). Then the region around each protocluster is simulated with high resolution, the particles representing L* galaxies. The protoclusters have no spatial symmetry built into them initially. The final clusters are still dynamically young, and of moderate densities, which should be representative of Abell clusters of richness classes 1 and 2.

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