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Permanent URL to this publication: http://dx.doi.org/10.5167/uzh-48292

Brough, S; Tran, K V; Sharp, R G; von der Linden, A; Couch, W J (2011). Spatial kinematics of brightest cluster galaxies and their close companions from integral field unit spectroscopy. Monthly Notices of the Royal Astronomical Society. Letters, 414(1):L80-L84.

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Abstract

We present Integral Field Unit (IFU) spectroscopy of four brightest cluster galaxies (BCGs) at z ˜ 0.1. Three of the BCGs have close companions within a projected radius of 20 kpc and one has no companion within that radius. We calculate the dynamical masses of the BCGs and their companions to be ?. We estimate the probability that the companions of the BCGs are bound using the observed masses and velocity offsets. We show that the lowest mass companion (1:4) is not bound while the two nearly equal mass (1:1.45 and 1:1.25) companions are likely to merge with their host BCGs in 0.35 Gyr in major, dry mergers. We conclude that some BCGs continue to grow from major merging even at z ˜ 0. We analyse the stellar kinematics of these systems using the λR parameter developed by the SAURON team. This offers a new and unique means to measure the stellar angular momentum of BCGs and make a direct comparison to other early-type galaxies. The BCGs and their companions have similar ellipticities to those of other early-type galaxies but are more massive. We find that not all these massive galaxies have low ? as one might expect. One of the four BCGs and the two massive companions are found to be fast-rotating galaxies with high angular momentum, thereby providing a new test for models of galaxy evolution and the formation of intracluster light.

Item Type:Journal Article, refereed, original work
Communities & Collections:07 Faculty of Science > Institute for Computational Science
DDC:530 Physics
Language:English
Date:April 2011
Deposited On:18 Feb 2012 20:08
Last Modified:26 Dec 2013 08:42
Publisher:Wiley-Blackwell
ISSN:0035-8711 (P) 1365-2966 (E)
Additional Information:The definitive version is available at www3.interscience.wiley.com
Publisher DOI:10.1111/j.1745-3933.2011.01060.x
Related URLs:http://arxiv.org/abs/1104.1239
Citations:Web of Science®. Times Cited: 14
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Scopus®. Citation Count: 17

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