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:

Galaxy–galaxy weak gravitational lensing in f(R) gravity.

Li, Baojiu and Shirasaki, Masato (2018) 'Galaxy–galaxy weak gravitational lensing in f(R) gravity.', Monthly notices of the Royal Astronomical Society., 474 (3). pp. 3599-3614.

Abstract

We present an analysis of galaxy–galaxy weak gravitational lensing (GGL) in chameleon f(R) gravity – a leading candidate of non-standard gravity models. For the analysis, we have created mock galaxy catalogues based on dark matter haloes from two sets of numerical simulations, using a halo occupation distribution (HOD) prescription which allows a redshift dependence of galaxy number density. To make a fairer comparison between the f(R) and Λ cold dark matter (ΛCDM) models, their HOD parameters are tuned so that the galaxy two-point correlation functions in real space (and therefore the projected two-point correlation functions) match. While the f(R) model predicts an enhancement of the convergence power spectrum by up to ∼ 30 per cent compared to the standard ΛCDM model with the same parameters, the maximum enhancement of GGL is only half as large and less than 5 per cent on separations above ∼1–2 h−1 Mpc, because the latter is a cross-correlation of shear (or matter, which is more strongly affected by modified gravity) and galaxy (which is weakly affected given the good match between galaxy autocorrelations in the two models) fields. We also study the possibility of reconstructing the matter power spectrum by combination of GGL and galaxy clustering in f(R) gravity. We find that the galaxy–matter cross-correlation coefficient remains at unity down to ∼2–3 h−1 Mpc at relevant redshifts even in f(R) gravity, indicating joint analysis of GGL and galaxy clustering can be a powerful probe of matter density fluctuations in chameleon gravity. The scale dependence of the model differences in their predictions of GGL can potentially allows us to break the degeneracy between f(R) gravity and other cosmological parameters such as Ωm and σ8.

Item Type:Article
Full text:(VoR) Version of Record
Download PDF
(2710Kb)
Status:Peer-reviewed
Publisher Web site:https://doi.org/10.1093/mnras/stx3006
Publisher statement:This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2017 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Date accepted:17 November 2017
Date deposited:17 January 2018
Date of first online publication:23 November 2017
Date first made open access:17 January 2018

Save or Share this output

Export:
Export
Look up in GoogleScholar