Detection of large-scale alignment of Lick counts around Abell clusters

1986 ◽  
Vol 91 ◽  
pp. 471 ◽  
Author(s):  
P. C. Argyres ◽  
E. J. Groth ◽  
P. J. E. Peebles ◽  
M. F. Struble
Keyword(s):  
Large Scale ◽  
Abell Clusters ◽  
Large Scale Alignment

scholarly journals Abell Clusters as Tracers of Large-Scale Structure: Alignments and Substructure

1988 ◽  
Vol 130 ◽  
pp. 536-536
Author(s):  
G. Rhee ◽  
P. Katgert
Keyword(s):  
Structure Data ◽  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Abell Clusters

Binggeli (A & A, 107, 338, 1982) showed that neighbouring Abell clusters with pair distances less than 30 to 40 h50−1 Mpc show directional correlation. Binggeli's result is based on structure data of 44 Abell clusters (all with zspectr < 0.1). Binggelli's result was questioned by Struble and Peebles (A.J., 90, 582, 1985). They produce a visual estimate of the direction of cluster elongation for 237 clusters. They did not observe reduced probability for small D large Θ pairs.

Large scale alignment of a lamellar block copolymer thin film via electric fields: a time-resolved SFM study

Soft Matter ◽  
2006 ◽  
Vol 2 (12) ◽  
pp. 1089-1094 ◽  
Author(s):  
Violetta Olszowka ◽  
Markus Hund ◽  
Volker Kuntermann ◽  
Sabine Scherdel ◽  
Larisa Tsarkova ◽  
...  
Keyword(s):  
Thin Film ◽  
Block Copolymer ◽  
Electric Fields ◽  
Large Scale ◽  
Time Resolved ◽  
Large Scale Alignment

scholarly journals Simulations of Large-Scale Structure Compared to Abell Cluster Distribution

1987 ◽  
Vol 124 ◽  
pp. 323-326
Author(s):  
David J. Batuski ◽  
Adrian Melott ◽  
Jack O. Burns
Keyword(s):  
Spatial Distribution ◽  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure ◽  
High Density ◽  
Particle Model ◽  
Flat Universe ◽  
Abell Clusters ◽  
Cluster Distribution ◽  
Abell Cluster

The amount of structure present among the Abell clusters out to redshift z = 0.085 has been compared with numerical supercomputer simulations (with 643 particles) of the isothermal, neutrino, and cold particle models for large-scale structure, assuming a flat universe and H = 50 km sec−1 Mpc−1. High-density clusters of particles were identified in each simulation. Correlation and percolation tests were then used to compare the spatial distribution of these high-density points with the apparent superclustering among Abell clusters. While all of the models had some small superclusters (the neutrino model has too many), none came very close to possessing the extremely extensive structures found in the Abell clusters (generally, disagreement by 2σ or more).A second set of simulations used the cold particle model with Ω = 0.2 and 0.5. The structures found in these simulations were certainly larger than those of the Ω = 1.0 cold particle case, but still > 2σ too small in comparisons with the Abell clusters.

Pseudoscalar-photon mixing and the large scale alignment of QSO optical polarizations

Pramana ◽  
2004 ◽  
Vol 62 (3) ◽  
pp. 679-682
Author(s):  
Pankaj Jain ◽  
Sukanta Panda ◽  
S. Sarala
Keyword(s):  
Large Scale ◽  
Large Scale Alignment

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.

scholarly journals Large-Scale Structure Among Abell Clusters and Comparisons to Models

1988 ◽  
Vol 130 ◽  
pp. 543-543
Author(s):  
David J. Batuski ◽  
Jack O. Burns ◽  
Adrian Melott
Keyword(s):  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure ◽  
The North ◽  
Abell Clusters ◽  
Observation Program ◽  
North And South

In a continuing redshift observation program, we have recently determined or confirmed the redshifts of 32 R ≥ 0 Abell clusters. With these data added to the previously measured cluster redshifts, there is now a sample of Abell clusters to z = 0.085 that is 92% complete in redshift measurements. The sample consists of 225 clusters in the North and South Galactic Caps, with latitude |b| > 30° to minimize obscuration effects. The longitude range 270° < l < 360° was also excluded for this sample because of an apparent large spur of galactic absorption.

scholarly journals THE DETECTION OF THE LARGE-SCALE ALIGNMENT OF MASSIVE GALAXIES AT z ∼ 0.6

2013 ◽  
Vol 770 (1) ◽  
pp. L12 ◽  
Author(s):  
Cheng Li ◽  
Y. P. Jing ◽  
A. Faltenbacher ◽  
Jie Wang
Keyword(s):  
Large Scale ◽  
Massive Galaxies ◽  
Large Scale Alignment

Facile Method for Large Scale Alignment of One Dimensional Nanoparticles and Control over Myoblast Orientation and Differentiation

ACS Nano ◽  
2013 ◽  
Vol 7 (10) ◽  
pp. 8385-8396 ◽  
Author(s):  
Xingjie Zan ◽  
Sheng Feng ◽  
Elizabeth Balizan ◽  
Yuan Lin ◽  
Qian Wang
Keyword(s):  
Large Scale ◽  
One Dimensional ◽  
And Control ◽  
Large Scale Alignment
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