Gonzalez-Perez, V. and Baugh, C.M. and Lacey, C.G. and Kim, J.-W. (2011) 'Massive, red galaxies in a hierarchical universe - II. Clustering of Extremely Red Objects.', Monthly notices of the Royal Astronomical Society., 417 (1). pp. 517-531.
We present predictions for the clustering of Extremely Red Objects (EROs) in a Λ cold dark matter universe, using a semi-analytical galaxy formation model in combination with a cosmological N-body simulation. EROs are red, massive galaxies observed at 0.7 ≲z≲ 3, and their numbers and properties have posed a challenge to hierarchical galaxy formation models. We analyse the halo occupation distribution and two-point correlation function of EROs, exploring how these quantities change with apparent magnitude, colour cut and redshift. Our model predicts a halo occupation distribution that is significantly different from that typically assumed. This is due to the inclusion of active galactic nuclei (AGN) feedback, which changes the slope and scatter of the luminosity–host halo mass relation above the mass where AGN feedback first becomes important. We predict that, on average, dark matter haloes with masses above 1013 h−1 M⊙ host at least one ERO at 1.5 ≤z≤ 2.5. Taking into account sample variance in observational estimates, the predicted angular clustering for EROs with either (R−K) > 5 or (i−K) > 4.5 is in reasonable agreement with current observations.
|Keywords:||Galaxies, Evolution galaxies, High-redshift galaxies, Luminosity function, Mass function large-scale structure of Universe.|
|Full text:||(VoR) Version of Record|
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|Publisher Web site:||http://dx.doi.org/10.1111/j.1365-2966.2011.19294.x|
|Publisher statement:||This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2011 The Authors. Journal compilation © 2011 RAS. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.|
|Date accepted:||No date available|
|Date deposited:||15 December 2014|
|Date of first online publication:||October 2011|
|Date first made open access:||No date available|
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