The rotation of Galaxy Clusters

Abstract

The method for detection of the galaxy cluster rotation based on the study of distribution of member galaxies with velocities lower and higher of the cluster mean velocity over the cluster image is proposed. The search for rotation is made for flat clusters with $a/b>1.8$ and BMI type clusters which are expected to be rotating. For comparison there were studied also round clusters and clusters of NBMI type, the second by brightness galaxy in which does not differ significantly from the cluster cD galaxy. Seventeen out of studied 65 clusters are found to be rotating. It was found that the detection rate is sufficiently high for flat clusters, over 60\%, and clusters of BMI type with dominant cD galaxy, ~ 35%. The obtained results show that clusters were formed from the huge primordial gas clouds and preserved the rotation of the primordial clouds, unless they did not have merging with other clusters and groups of galaxies, in the result of which the rotation has been prevented.

6 pages, 17 figures

References in corpus (2)

• The Ninth Data Release of the Sloan Digital Sky Survey: First Spectroscopic Data from the SDSS-III Baryon Oscillation Spectroscopic Survey
• On the Formation of cD Galaxies and their Parent Clusters

Cited by in corpus (8)

• The mass function dependence on the dynamical state of dark matter haloes
• Galaxy cluster's rotation
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• A redshift survey of the nearby galaxy cluster Abell 2107: Global rotation of the cluster and its connection to large-scale structures in the universe
• Testing the rotation versus merger scenario in the galaxy cluster Abell 2107
• High entropy and evidence for a merger in the low surface brightness cluster Abell 2399
• The Rotational Profiles of Cluster Galaxies
• Signatures and bias assessment of rotation in galaxy cluster members