Galaxy cluster's rotation

TL;DR

This paper develops a new algorithm to detect and analyze rotation in galaxy clusters, applying it to SDSS data, and finds that about 23-28% of clusters show significant rotation, which relates to their dynamical state.

Contribution

The paper introduces a novel, robust algorithm for identifying rotation in galaxy clusters and applies it to real data, revealing the prevalence and dynamical implications of cluster rotation.

Findings

Approximately 23% of clusters are rotating under strict criteria.

The rotation fraction increases to about 28% with relaxed criteria.

Cluster rotation is linked to younger dynamical states and formation processes.

Abstract

We study the possible rotation of cluster galaxies, developing, testing and applying a novel algorithm which identifies rotation, if such does exist, as well as its rotational centre, its axis orientation, rotational velocity amplitude and, finally, the clockwise or counterclockwise direction of rotation on the plane of the sky. To validate our algorithms we construct realistic Monte Carlo mock rotating clusters and confirm that our method provides robust indications of rotation. We then apply our methodology on a sample of Abell clusters with z<~0.1 with member galaxies selected from the Sloan Digital Sky Survey (SDSS) DR10 spectroscopic data base. After excluding a number of substructured clusters, which could provide erroneous indications of rotation, and taking into account the expected fraction of misidentified coherent substructure velocities for rotation, provided by our Monte-Carlo simulation analysis, we find that ~23% of our clusters are rotating under a set of strict criteria. Loosening the strictness of the criteria, on the expense of introducing spurious rotation indications, we find this fraction increasing to ~28%. We correlate our rotation indicators with the cluster dynamical state, provided either by their Bautz-Morgan type or by their X-ray isophotal shape and find for those clusters showing rotation within 1.5 h -1 70 Mpc that the significance of their rotation is related to the dynamically younger phases of cluster formation but after the initial anisotropic accretion and merging has been completed. Finally, finding rotational modes in galaxy clusters could lead to the necessity of correcting the dynamical cluster mass calculations.