A Caltech Library Service

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

Barazza, F. D. and Jablonka, P. and Desai, V. and Jogee, S. and Aragón-Salamanca, A. and De Lucia, G. and Saglia, R. P. and Halliday, C. and Poggianti, B. M. and Dalcanton, J. J. and Rudnick, G. and Milvang-Jensen, B. and Noll, S. and Simard, L. and Clowe, D. I. and Pelló, R. and White, S. D. M. and Zaritsky, D. (2009) Frequency and properties of bars in cluster and field galaxies at intermediate redshifts. Astronomy and Astrophysics, 497 (3). pp. 713-728. ISSN 0004-6361.

PDF - Published Version
See Usage Policy.


Use this Persistent URL to link to this item:


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 properties of bars and disks are determined by ellipse fits to the surface brightness distribution of the galaxies using HST/ACS images in the F814W filter. The bar identification is based on quantitative criteria after highly inclined (> 60°) systems have been excluded. 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. The question whether internal or external factors are more important for bar formation and evolution cannot be answered definitely. On the one hand, the bar fraction and properties of cluster and field samples of disk galaxies are quite similar, indicating that internal processes are crucial for bar formation. On the other hand, we find evidence that cluster centers are favorable locations for bars, which suggests that the internal processes responsible for bar growth are supported by the typical interactions taking place in such environments.

Item Type:Article
Related URLs:
URLURL TypeDescription
Desai, V.0000-0002-1340-0543
Poggianti, B. M.0000-0001-8751-8360
Rudnick, G.0000-0001-5851-1856
Milvang-Jensen, B.0000-0002-2281-2785
Zaritsky, D.0000-0002-5177-727X
Additional Information:© 2009 ESO. Received 9 June 2008; accepted 29 January 2009. Based on observations collected at the European Southern Observatory, Chile, as part of large programme 166.A-0162 (the ESO Distant Cluster Survey). Also based on observations made with the NASA/ESA Hubble S pace Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with proposal 9476. Support for this porposal was provided by NASA through a grant from Space Telescope Science Institute.
Funding AgencyGrant Number
Subject Keywords:galaxies: spiral; galaxies: structure; galaxies: clusters: general; galaxies: evolution; galaxies: formation
Issue or Number:3
Record Number:CaltechAUTHORS:20090601-135247681
Persistent URL:
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:14346
Deposited By: Jason Perez
Deposited On:25 Jun 2009 21:23
Last Modified:28 Oct 2019 17:16

Repository Staff Only: item control page