Dwarf Galaxies in Clusters as Probes of Galaxy Formation and Dark Matter

TL;DR

This study uses Hubble Space Telescope observations to analyze dwarf galaxies in the Perseus Cluster, revealing environmental effects on their structure, color, and dark matter content, and proposing a new method to estimate their minimum mass.

Contribution

It introduces a novel approach to estimate dwarf galaxy masses using structural parameters without resolved spectroscopy, and provides insights into environmental influences on dwarf galaxy evolution.

Findings

Outer cluster dwarfs are more disturbed than core dwarfs.

Dwarfs in both regions follow the same colour-magnitude relation.

Core dwarfs are highly dark matter dominated to avoid disruption.

Abstract

We present the results of a Hubble Space Telescope (HST) ACS and WFPC2 study of dwarf galaxies in the nearby Perseus Cluster, down to M_V = -12, spanning the core and outer regions of this cluster. We examine how properties such as the colour magnitude relation, structure and morphology are affected by environment for the lowest mass galaxies. The low masses of dwarf galaxies allow us to determine their environmentally driven based galaxy evolution, the effects of which are harder to examine in massive galaxies. The structures of our dwarfs in both the core and outer regions of the cluster are quantified using the concentration, asymmetry and clumpiness (CAS) parameters. We find that, on average, dwarfs in the outer regions of Perseus are more disturbed than those in the cluster core, with higher asymmetries and clumpier light distributions. We measure the (V-I)_0 colours of the dEs, and find that dwarfs in both the inner and outer regions of the cluster lie on the same colour magnitude relation. Based on these results, we infer that the disturbed dwarfs in the cluster outskirts are likely "transition dwarfs", with their colours transforming before their structures. Finally, we infer from the smoothness of the cluster core population that dwarfs in the inner regions of the cluster must be highly dark matter dominated to prevent their disruption by the cluster potential. We derive a new method to determine the minimum mass the dwarfs must have to prevent this disruption without the need for resolved spectroscopy, and determine their mass-to-light ratios. At their orbit pericentre, dwarfs in the core of Perseus require mass-to-light ratios between 1 and 120 to prevent their disruption, comparable to those found for the Local Group dSphs.