English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

The clustering of galaxies and the matter distribution around them can bedescribed using the halo model complemented with a realistic description of theway galaxies populate dark matter haloes. This has been used successfully todescribe statistical properties of samples of galaxies at z<0.2. Withoutadjusting any model parameters, we compare the predicted weak lensing signalinduced by Luminous Red Galaxies to measurements from SDSS DR7 on much largerscales (up to ~90 h_{70}^{-1} Mpc) and at higher redshift (z~0.4). We findexcellent agreement, suggesting that the model captures the main properties ofthe galaxy-dark matter connection. To extend the comparison to lenses at evenhigher redshifts we complement the SDSS data with shape measurements from thedeeper RCS2, resulting in precise lensing measurements for lenses up to z~0.6.These measurements are also well described using the same model. Consideringsolely these weak lensing measurements, we robustly assess that, up to z~0.6,the number of central galaxies as a function of halo mass is well described bya log-normal distribution with scatter $\sigma_{\log L_{\rm c}}=0.146\pm0.011$,in agreement with previous independent studies at lower redshift. Our resultsdemonstrate the value of complementing the information about the properties ofthe (lens) galaxies provided by SDSS with deeper, high-quality imaging data.

Describing galaxy weak lensing measurements from tenths to tens of Mpc and up to z~0.6 with a single model