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:

The clustering and halo occupation distribution of Lyman-break galaxies at z ˜ 4.

Park, J. and Kim, H.-S. and Wyithe, J. S. B. and Lacey, C. G. and Baugh, C. M. and Barone-Nugent, R. L. and Trenti, M. and Bouwens, R. J. (2016) 'The clustering and halo occupation distribution of Lyman-break galaxies at z ˜ 4.', Monthly notices of the Royal Astronomical Society., 461 (1). pp. 176-189.


We investigate the clustering of Lyman-break galaxies (LBGs) at z ∼ 4. Using the hierarchical galaxy formation model GALFORM, we predict, for the first time using a semi-analytical model with feedback from active galactic nuclei (AGN), the angular correlation function (ACF) of LBGs and find agreement within 3σ with new measurements of the ACF from surveys including the Hubble eXtreme Deep Field (XDF) and Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) field. Our simulations confirm the conclusion reached using independent models that although the predicted ACFs reproduce the trend of increased clustering with luminosity, the dependence is less strong than observed. We find that for the detection limits of the XDF field, central LBGs at z ∼ 4 predominantly reside in haloes of mass ∼1011–1012 h−1 M⊙ and that satellites reside in larger haloes of mass ∼1012–1013 h−1 M⊙. The model predicts fewer bright satellite LBGs at z ∼ 4 than is inferred from measurements of the ACF at small scales. By analysing the halo occupation distribution (HOD) predicted by the model, we find evidence that AGN feedback affects the HOD of central LBGs in massive haloes. This is a new high-redshift test of this important feedback mechanism. We investigate the effect of photometric errors in the observations on the ACF predictions. We find that the observational uncertainty in the galaxy luminosity reduces the clustering amplitude and that this effect increases towards faint galaxies, particularly on small scales. To compare properties of model with observed LBGs, this uncertainty must be considered.

Item Type:Article
Full text:(VoR) Version of Record
Download PDF
Publisher Web site:
Publisher statement:This article has been published in Monthly Notices of the Royal Astronomical Society ©: 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Date accepted:01 June 2016
Date deposited:06 October 2016
Date of first online publication:07 June 2016
Date first made open access:06 October 2016

Save or Share this output

Look up in GoogleScholar