Astrophysics> Cosmology and Nongalactic Astrophysics
arXiv:1201.4910 (astro-ph)
[Submitted on 24 Jan 2012]
Title:The HST/ACS Coma Cluster Survey. VIII. Barred Disk Galaxies in the Core of the Coma Cluster
Authors:Irina Marinova (UT Austin), Shardha Jogee (UT Austin), Tim Weinzirl (UT Austin), Peter Erwin (Max-Planck, University Observatory Munich), Neil Trentham (Cambridge), Henry C. Ferguson (STScI), Derek Hammer (Johns Hopkins), Mark den Brok (Kapteyn), Alister W. Graham (Swinburne), David Carter (Liverpool), Marc Balcells (Tenerife), Paul Goudfrooij (STScI), Rafael Guzman (Florida), Carlos Hoyos (Florida), Bahram Mobasher (UC Riverside), Mustapha Mouhcine (Liverpool), Reynier F. Peletier (Kapteyn), Eric Peng (Peking University, Kavli Institute), Gijs Verdoes Kleijn (Kapteyn)
View PDF
Abstract:(ABRIDGED) We use high resolution (~0.1") F814W ACS images from the HST ACS Treasury survey of the Coma cluster at z~0.02 to study bars in massive disk galaxies (S0s), and in dwarf galaxies in the Coma core. Our study helps constrain the evolution of bars and disks in dense environments and provides a comparison point for studies in lower density environments and at higher redshifts. (1) We characterize the fraction and properties of bars in a sample of 32 bright (M_V <= -18, M_* > 10^9.5 M_sun) S0 galaxies, which dominate the population of massive disk galaxies in the Coma core. Measuring the S0 bar fraction must be handled carefully, as the results depend on the method used: the bar fraction for bright S0s in the Coma core is 50%+/-11%, 65%+/-11%, and 60%+/-11% for three methods of bar detection: strict ellipse fit criteria, relaxed ellipse fit criteria, and visual classification. (2) We compare the S0 bar fraction across different environments (Coma core, A901/902, Virgo). We find that the bar fraction among bright S0 galaxies does not show a statistically significant variation across environments spanning two orders of magnitude in galaxy number density (n~300-10,000 gal/Mpc^3). We speculate that the S0 bar fraction is not significantly enhanced in rich clusters because S0s in rich clusters are less prone to bar instabilities as they are dynamically hot and gas poor due to ram pressure stripping and accelerated star formation. In addition, high-speed encounters in rich clusters may be less effective than slow, strong encounters in inducing bars. (3) We analyze a sample of 333 faint (M_V > -18) dwarf galaxies in the Coma core. Using unsharp-masking, we find only 13 galaxies with bar and/or spiral structure. The paucity of disk structures in Coma dwarfs suggests that either disks are not common in these galaxies, or that any disks present are too hot to develop instabilities.
| Comments: | Accepted to ApJ; version with full-resolution figures can be found at this http URL |
| Subjects: | Cosmology and Nongalactic Astrophysics (astro-ph.CO) |
| Cite as: | arXiv:1201.4910 [astro-ph.CO] |
| (or arXiv:1201.4910v1 [astro-ph.CO] for this version) | |
| https://doi.org/10.48550/arXiv.1201.4910
arXiv-issued DOI via DataCite
|
|
| Related DOI: | https://doi.org/10.1088/0004-637X/746/2/136
DOI(s) linking to related resources
|
Current browse context:
astro-ph.CO
Change to browse by:
References & Citations
export BibTeX citation
Loading...
BibTeX formatted citation
×
Data provided by:
Bibliographic and Citation Tools
Bibliographic Explorer (What is the Explorer?)
Connected Papers (What is Connected Papers?)
Litmaps (What is Litmaps?)
scite Smart Citations (What are Smart Citations?)
Code, Data and Media Associated with this Article
alphaXiv (What is alphaXiv?)
CatalyzeX Code Finder for Papers (What is CatalyzeX?)
DagsHub (What is DagsHub?)
Gotit.pub (What is GotitPub?)
Hugging Face (What is Huggingface?)
Papers with Code (What is Papers with Code?)
ScienceCast (What is ScienceCast?)
Demos
Recommenders and Search Tools
Influence Flower (What are Influence Flowers?)
CORE Recommender (What is CORE?)
IArxiv Recommender
(What is IArxiv?)
arXivLabs: experimental projects with community collaborators
arXivLabs is a framework that allows collaborators to develop and share new arXiv features directly on our website.
Both individuals and organizations that work with arXivLabs have embraced and accepted our values of openness, community, excellence, and user data privacy. arXiv is committed to these values and only works with partners that adhere to them.
Have an idea for a project that will add value for arXiv's community? Learn more about arXivLabs.