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Understanding the non-linear clustering of high-redshift galaxies.

Jose, C. and Baugh, C. M. and Lacey, C. G. and Subramanian, K. (2017) 'Understanding the non-linear clustering of high-redshift galaxies.', Monthly notices of the Royal Astronomical Society., 469 (4). pp. 4428-4436.

Abstract

We incorporate the non-linear clustering of dark matter haloes, as modelled by Jose et al. into the halo model to better understand the clustering of Lyman break galaxies (LBGs) in the redshift range z = 3–5. We find that, with this change, the predicted LBG clustering increases significantly on quasi-linear scales (0.1 ≤ r / h−1 Mpc ≤ 10) compared to that in the linear halo bias model. This, in turn, results in an increase in the clustering of LBGs by an order of magnitude on angular scales 5 ≤ θ ≤ 100 arcsec. Remarkably, the predictions of our new model on the whole remove the systematic discrepancy between the linear halo bias predictions and the observations. The correlation length and large-scale galaxy bias of LBGs are found to be significantly higher in the non-linear halo bias model than in the linear halo bias model. The resulting two-point correlation function retains an approximate power-law form in contrast with that computed using the linear halo bias theory. We also find that the non-linear clustering of LBGs increases with increasing luminosity and redshift. Our work emphasizes the importance of using non-linear halo bias in order to model the clustering of high-z galaxies to probe the physics of galaxy formation and extract cosmological parameters reliably.

Item Type:Article
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Status:Peer-reviewed
Publisher Web site:https://doi.org/10.1093/mnras/stx1014
Publisher statement:This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.
Date accepted:25 April 2017
Date deposited:18 July 2017
Date of first online publication:27 April 2017
Date first made open access:18 July 2017

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