Luminous red galaxies in hierarchical cosmologies

Almeida, C., Baugh, C. M., Wake, D. A., Lacey, C. G., Benson, A. J., Bower, R. G. and Pimbblet, K. A. (2008) Luminous red galaxies in hierarchical cosmologies. Monthly Notices of the Royal Astronomical Society, 386 4: 2145-2160. doi:10.1111/j.1365-2966.2008.13179.x


Author Almeida, C.
Baugh, C. M.
Wake, D. A.
Lacey, C. G.
Benson, A. J.
Bower, R. G.
Pimbblet, K. A.
Title Luminous red galaxies in hierarchical cosmologies
Journal name Monthly Notices of the Royal Astronomical Society   Check publisher's open access policy
ISSN 0035-8711
1365-2966
Publication date 2008-06-01
Sub-type Article (original research)
DOI 10.1111/j.1365-2966.2008.13179.x
Open Access Status DOI
Volume 386
Issue 4
Start page 2145
End page 2160
Total pages 16
Editor A. C. Fabian
Place of publication Oxford, United Kingdom
Publisher Oxford University Press
Language eng
Subject 1912 Space and Planetary Science
Abstract Luminous red galaxies (LRGs) are much rarer and more massive than L* galaxies. Coupled with their extreme colours, LRGs therefore provide a demanding testing ground for the physics of massive galaxy formation. We present the first self-consistent predictions for the abundance and properties of LRGs in hierarchical structure formation models. We test two published models which use quite different mechanisms to suppress the formation of massive galaxies: the Bower et al. model which invokes 'active galactic nuclei (AGN) feedback' to prevent gas from cooling in massive haloes and the Baugh et al. model which relies upon a 'superwind' to eject gas before it is turned into stars. Without adjusting any parameters, the Bower et al. model gives an excellent match to the observed luminosity function of LRGs in the Sloan Digital Sky Survey (with a median redshift of z= 0.24 ) and to their clustering; the Baugh et al. model is less successful in these respects. Both models fail to match the observed abundance of LRGs at z= 0.5 to better than a factor of ≈2. In the models, LRGs are typically bulge-dominated systems with stellar masses of ≈2 × 1011 h−1 M⊙ and velocity dispersions of σ∼ 250 km s−1 . Around half of the stellar mass in the model LRGs is already formed by z∼ 2.2 and is assembled into one main progenitor by z∼ 1.5 ; on average, only 25 per cent of the mass of the main progenitor is added after z∼ 1 . LRGs are predicted to be found in a wide range of halo masses, a conclusion which relies on properly taking into account the scatter in the formation histories of haloes. Remarkably, we find that the correlation function of LRGs is predicted to be a power law down to small pair separations, in excellent agreement with observational estimates. Neither the Bower et al. nor the Baugh et al. model is able to reproduce the observed radii of LRGs.
Keyword galaxies: elliptical and lenticular, cD
galaxies: evolution
cosmology: theory
large-scale structure of Universe
Q-Index Code C1
Q-Index Status Confirmed Code
Institutional Status UQ

Document type: Journal Article
Sub-type: Article (original research)
Collections: 2009 Higher Education Research Data Collection
School of Mathematics and Physics
 
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Created: Thu, 26 Mar 2009, 01:33:14 EST by Jo Hughes on behalf of School of Mathematics & Physics