The dynamical state of brightest cluster galaxies and the formation of clusters

TL;DR

This study analyzes the dynamical properties of brightest cluster galaxies in a large sample of Abell clusters, revealing their significant peculiar velocities and implications for cluster formation and evolution.

Contribution

It provides the largest dataset to date on BCMs, showing their velocities and morphologies, supporting the merging-groups formation scenario for clusters.

Findings

Most BCMs are early-type galaxies, with 48% being cD types.

A median peculiar velocity of 32% of the cluster velocity dispersion was found for BCMs.

BCM peculiar velocities are weakly dependent on cluster richness and morphology.

Abstract

A large sample of Abell clusters of galaxies, selected for the likely presence of a dominant galaxy, is used to study the dynamical properties of brightest cluster members (BCMs). From visual inspection of Digitized Sky Survey images combined with redshift data we identify 1426 candidate BCMs in 1221 redshift components in 1169 different Abell clusters, the largest such sample published so far. By our own morphological classification we find ~92% of these BCMs to be early-type galaxies, and 48% of cD type. We confirm previous findings based on much smaller samples, namely that a large fraction of BCMs have significant peculiar velocities. For a subsample of 452 clusters with at least 10 measured radial velocities, we find a median BCM peculiar velocity of 32% of their host clusters' radial velocity dispersion. This suggests that most BCMs are not at rest in the potential well of their clusters, and that the phenomenon is thus not a special trait of clusters hosting cD galaxies. We show that the peculiar velocity of the BCM is independent of cluster richness and only slightly dependent on the Bautz-Morgan type. We also find a weak trend for the peculiar velocity to rise with the cluster velocity dispersion. The strongest dependence is with the morphological type of the BCM: cD galaxies tend to have lower relative peculiar velocities than elliptical galaxies. This result points to a connection between the formation of the BCMs and that of their clusters. Our data are qualitatively consistent with the merging-groups scenario, where BCMs in clusters formed first in smaller subsystems comparable to compact groups of galaxies. In this scenario, clusters would have formed recently from the mergers of many such groups and would still be in a dynamically unrelaxed state.