Rotation of the cluster of galaxies A2107

Abstract

We present indications of rotation in the galaxy cluster A2107 by a method that searches for the maximum gradient in the velocity field in a flat disk-like model of a cluster. Galaxies from cumulative sub-samples containing more and more distant members from the cluster centre, are projected onto an axis passing through the centre and we apply a linear regression model on the projected distances $x$ and the line-of-sight velocities $V$. The axis with the maximum linear correlation coefficient $r_{max}=\max [r(V,x)]$ defines the direction of the maximum velocity gradient, and consequently it presents the major axis of the apparently elliptical cluster. Because the effects of rotation are subtle, we put strong emphasis on the estimation of the uncertainties of the results by implementing different bootstrap techniques. We have found the rotational effects are more strongly expressed from distances $0.26÷0.54$ Mpc from the cluster centre. The total virial mass of the cluster is $(3.2\pm0.6)\times10^{14} {\cal M}_{\sun}$, while the virial mass, corrected for the rotation, is $(2.8\pm0.5) \times 10^{14}{\cal M}_{\sun}$.

7 pages, 9 figures gzipped tar file. to be published in MNRAS

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• Ellipsoidal configurations in the de Sitter spacetime
• The rotation of Galaxy Clusters
• Kinematic effect in gravitational lensing by clusters of galaxies
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• Testing the rotation versus merger scenario in the galaxy cluster Abell 2107
• The Rotational Profiles of Cluster Galaxies
• Orientation of galaxies in structures
• Revisiting Rotational Perturbations and the Microwave Background
• Effect of Composition Gradient on Magnetothermal Instability Modified by Shear and Rotation
• Signatures and bias assessment of rotation in galaxy cluster members