Cookies

We use cookies to ensure that we give you the best experience on our website. By continuing to browse this repository, you give consent for essential cookies to be used. You can read more about our Privacy and Cookie Policy.


Durham Research Online
You are in:

Environmental quenching and hierarchical cluster assembly : evidence from spectroscopic ages of red-sequence galaxies in Coma.

Smith, Russell J. and Lucey, John R. and Price, James and Hudson, Michael J. and Phillipps, Steven (2012) 'Environmental quenching and hierarchical cluster assembly : evidence from spectroscopic ages of red-sequence galaxies in Coma.', Monthly notices of the Royal Astronomical Society., 419 (4). pp. 3167-3180.

Abstract

We explore the variation in stellar population ages for Coma cluster galaxies as a function of projected cluster-centric distance, using a sample of 362 red-sequence galaxies with high signal-to-noise ratio spectroscopy. The sample spans a wide range in luminosity (0.02–4 L*) and extends from the cluster core to near the virial radius. We find a clear distinction in the observed trends of the giant and dwarf galaxies. The ages of red-sequence giants are primarily determined by galaxy mass, whether parametrized by velocity dispersion, luminosity, stellar mass or dynamical mass, with only weak modulation by environment, in the sense that galaxies at larger cluster-centric distance are slightly younger. For red-sequence dwarfs (with mass ≲ 1010 M⊙), the roles of mass and environment as predictors of age are reversed: there is little dependence on mass, but strong trends with projected cluster-centric radius are observed. The average age of dwarfs at the 2.5 Mpc limit of our sample is approximately half that of dwarfs near the cluster centre. The gradient in dwarf galaxy ages is a global cluster-centric trend, and is not driven by the ongoing merger of the NGC 4839 group to the south west of Coma. We interpret these results using environmental histories extracted from the Millennium Simulation for members of massive clusters. Hierarchical cluster assembly naturally leads to trends in the accretion times of galaxies as a function of projected cluster-centric radius. On average, simulated galaxies now located in cluster cores joined haloes above any given mass threshold earlier than those now in the outskirts of clusters. We test environmental quenching models, in which star formation is halted in galaxies when they enter haloes of a given mass, or when they become satellites. Our models broadly reproduce the gradients observed in Coma, but for dwarf galaxies the efficiency of environmental quenching must be very high to match the strong trends observed.

Item Type:Article
Full text:(VoR) Version of Record
Download PDF
(6534Kb)
Status:Peer-reviewed
Publisher Web site:http://dx.doi.org/10.1111/j.1365-2966.2011.19956.x
Publisher statement:This article has been accepted for publication in Monthly notices of the Royal Astronomical Society ©: 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Date accepted:05 October 2011
Date deposited:22 April 2016
Date of first online publication:21 February 2012
Date first made open access:No date available

Save or Share this output

Export:
Export
Look up in GoogleScholar