Frequency and properties of bars in cluster and field galaxies at intermediate redshifts

TL;DR

This study investigates the frequency, properties, and environmental dependence of large-scale bars in disk galaxies at intermediate redshifts (~0.4-0.8), revealing differences between cluster and field environments and linking bar presence to galaxy morphology.

Contribution

It provides the first comprehensive analysis of bar fractions and properties in cluster versus field galaxies at intermediate redshifts, highlighting environmental effects and morphological correlations.

Findings

Bar fraction in the redshift range 0.4-0.8 is about 25%, with 20% strong bars.

Bars are longer in clusters and more common near cluster centers.

Disk-dominated galaxies have a higher bar fraction (~45%) than bulge-dominated ones (~15%).

Abstract

We present a study of large-scale bars in field and cluster environments out to redshifts of ~0.8 using a final sample of 945 moderately inclined disk galaxies drawn from the EDisCS project. We characterize bars and their host galaxies and look for relations between the presence of a bar and the properties of the underlying disk. We investigate whether the fraction and properties of bars in clusters are different from their counterparts in the field. The total optical bar fraction in the redshift range z=0.4-0.8 (median z=0.60), averaged over the entire sample, is 25% (20% for strong bars). For the cluster and field subsamples, we measure bar fractions of 24% and 29%, respectively. We find that bars in clusters are on average longer than in the field and preferentially found close to the cluster center, where the bar fraction is somewhat higher (~31%) than at larger distances (~18%). These findings however rely on a relatively small subsample and might be affected by small number statistics. In agreement with local studies, we find that disk-dominated galaxies have a higher optical bar fraction (~45%) than bulge-dominated galaxies (~15%). This result is based on Hubble types and effective radii and does not change with redshift. The latter finding implies that bar formation or dissolution is strongly connected to the emergence of the morphological structure of a disk and is typically accompanied by a transition in the Hubble type. (abridged)