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Title:
Barred Galaxies in the Abell 901/2 Supercluster with Stages
Authors:
Marinova, Irina; Jogee, Shardha; Heiderman, Amanda; Barazza, Fabio D.; Gray, Meghan E.; Barden, Marco; Wolf, Christian; Peng, Chien Y.; Bacon, David; Balogh, Michael; Bell, Eric F.; Böhm, Asmus; Caldwell, John A. R.; Häußler, Boris; Heymans, Catherine; Jahnke, Knud; van Kampen, Eelco; Lane, Kyle; McIntosh, Daniel H.; Meisenheimer, Klaus; Sánchez, Sebastian F.; Somerville, Rachel; Taylor, Andy; Wisotzki, Lutz; Zheng, Xianzhong
Affiliation:
AA(Department of Astronomy, University of Texas at Austin, Austin, TX, USA ), AB(Department of Astronomy, University of Texas at Austin, Austin, TX, USA ), AC(Department of Astronomy, University of Texas at Austin, Austin, TX, USA ), AD(Laboratoire d'Astrophysique, École Polytechnique Fédéralede Lausanne, Observatoire, Sauverny, Switzerland ), AE(School of Physics and Astronomy, The University of Nottingham, Nottingham, UK ), AF(Institute for Astro- and Particle Physics, University of Innsbruck, Innsbruck, Austria ), AG(Department of Astrophysics, University of Oxford, Oxford, UK ), AH(NRC Herzberg Institute of Astrophysics, Victoria, Canada ; Space Telescope Science Institute, Baltimore, MD, USA ), AI(Institute of Cosmology and Gravitation, University of Portsmouth, Portsmouth, UK ), AJ(Department of Physics and Astronomy, University Of Waterloo, Ontario, Canada ), AK(Max-Planck-Institut für Astronomie, Heidelberg, Germany ), AL(Institute for Astro- and Particle Physics, University of Innsbruck, Innsbruck, Austria ; Astrophysikalisches Insitut Potsdam, Potsdam, Germany ), AM(University of Texas, McDonald Observatory, Fort Davis, TX, USA ), AN(School of Physics and Astronomy, The University of Nottingham, Nottingham, UK ), AO(The Scottish Universities Physics Alliance, Institute for Astronomy, University of Edinburgh, Edinburgh, UK ), AP(Max-Planck-Institut für Astronomie, Heidelberg, Germany ), AQ(Institute for Astro- and Particle Physics, University of Innsbruck, Innsbruck, Austria ), AR(School of Physics and Astronomy, The University of Nottingham, Nottingham, UK ), AS(Department of Astronomy, University of Massachusetts, Amherst, MA, USA ; Department of Physics, University of Missouri-Kansas City, Kansas City, MO 64110, USA ), AT(Max-Planck-Institut für Astronomie, Heidelberg, Germany ), AU(Centro Hispano Aleman de Calar Alto, Almeria, Spain ), AV(Max-Planck-Institut für Astronomie, Heidelberg, Germany ), AW(The Scottish Universities Physics Alliance, Institute for Astronomy, University of Edinburgh, Edinburgh, UK ), AX(Astrophysikalisches Insitut Potsdam, Potsdam, Germany ), AY(Purple Mountain Observatory, National Astronomical Observatories, Chinese Academy of Sciences, Nanjing, China)
Publication:
The Astrophysical Journal, Volume 698, Issue 2, pp. 1639-1658 (2009). (ApJ Homepage)
Publication Date:
06/2009
Origin:
IOP
ApJ Keywords:
galaxies: clusters: general, galaxies: evolution, galaxies: spiral, galaxies: structure
DOI:
10.1088/0004-637X/698/2/1639
Bibliographic Code:
2009ApJ...698.1639M

Abstract

We present a study of bar and host disk evolution in a dense cluster environment, based on a sample of ~800 bright (M V <= -18) galaxies in the Abell 901/2 supercluster at z~ 0.165. We use Hubble Space Telescope (HST) Advanced Camera for Surveys (ACS) F606W imaging from the STAGES survey, and data from Spitzer, XMM-Newton, and COMBO-17. We identify and characterize bars through ellipse-fitting, and other morphological features through visual classification. We find the following results. (1) To define the optical fraction of barred disk galaxies, we explore three commonly used methods for selecting disk galaxies. We find 625, 485, and 353 disk galaxies, respectively, via visual classification, a single component Sérsic cut (n <= 2.5), and a blue-cloud cut. In cluster environments, the latter two methods suffer from serious limitations, and miss 31% and 51%, respectively, of visually identified disks, particularly the many red, bulge-dominated disk galaxies in clusters. (2) For moderately inclined disks, the three methods of disk selection, however, yield a similar global optical bar fraction (f bar-opt) of 34%+10% -3% (115/340), 31%+10% -3% (58/189), and 30%+10% -3% (72/241), respectively. (3) We explore f bar-opt as a function of host galaxy properties and find that it rises in brighter galaxies and those which appear to have no significant bulge component. Within a given absolute magnitude bin, f bar-opt is higher in visually selected disk galaxies that have no bulge as opposed to those with bulges. Conversely, for a given visual morphological class, f bar-opt rises at higher luminosities. Both results are similar to trends found in the field. (4) For bright early-types, as well as faint late-type systems with no evident bulge, the optical bar fraction in the Abell 901/2 clusters is comparable within a factor of 1.1-1.4 to that of field galaxies at lower redshifts (z < 0.04). (5) Between the core and the virial radius of the cluster (R~ 0.25-1.2 Mpc) at intermediate environmental densities (log(Σ10) ~ 1.7-2.3), the optical bar fraction does not appear to depend strongly on the local environment density tracers (κ, Σ10, and intracluster medium (ICM) density), and varies at most by a factor of ~1.3. Inside the cluster core, we are limited by number statistics, projection effects, and different trends from different indicators, but overall f bar-opt does not show evidence for a variation larger than a factor of 1.5. We discuss the implications of our results for the evolution of bars and disks in dense environments.
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