Sign on

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· References in the article
· Citations to the Article (89) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (36)
· NED Objects (29)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Kinematics of 13 brightest cluster galaxies
Authors:
Fisher, David; Illingworth, Garth; Franx, Marijn
Affiliation:
AA(University of California, Santa Cruz, CA, US), AB(University of California, Santa Cruz, CA, US), AC(University of Groningen, Groningen, Netherlands)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 438, no. 2, p. 539-562 (ApJ Homepage)
Publication Date:
01/1995
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
Elliptical Galaxies, Galactic Clusters, Kinematics, Luminosity, Astronomical Photometry, Astrophysics, Dispersing, Galactic Mass, Interstellar Chemistry, Stellar Cores, Stellar Rotation, Velocity
DOI:
10.1086/175100
Bibliographic Code:
1995ApJ...438..539F

Abstract

Velocity dispersion profiles and rotation curves have been determined for a sample of 13 brightest cluster galaxies (BCGs) in order to study their internal stellar kinematics and investigate their relationship to ellipticals. We find that BCGs generally display velocity dispersion profiles with gradients similar to those found in normal bright ellipticals. A rising velocity dispersion profile is found for the BCG IC 1101, the dominant member of Abell 2029, confirming Dressler's (1979) result. No other rising velocity dispersion profiles are found in our sample suggesting that they are not a feature common to brightest cluster galaxies. Significant rotation is found in only two of the galaxies, a result in agreement with previous studies showing the declining importance of rotation with increasing luminosity for elliptical galaxies. Our data suggest that environment plays a role in the kinematic characteristics of BCGs. We find a correlation between the rotation of BCGs and the velocity dispersion of their parent clusters in the sense that very slow rotating galaxies (Vm/(mean value of sigma))* less than 0.1, are predominantly found in high velocity dispersion (sigmacL greater than 650 km/s) clusters. This relation between the internal stellar kinematics of BCGs and the cluster velocity dispersion is in the sense expected if ellipticals formed by merging. Brightest cluster galaxy mass-to-light ratios derived from photometric and kinematic modeling are found to be similar to normal elliptical M/L values. For the galaxy NGC 4073, the dominant galaxy in the poor cluster MKW 4, we find that it contains a counterrotating stellar core suggestive of the occurrence of an accretion event(s).

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences



More Article Retrieval Options

HELP for Article Retrieval


Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

  New!

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints