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 Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

[ABRIDGED] We estimate the total mass distribution of the galaxy clusterCL0024+1654 from the measured source depletion due to lens magnification in theR band. Within a radius of 0.54Mpc/h, a total projected mass of(8.1+/-3.2)*10^14 M_sol/h (EdS) is measured, which corresponds to a mass-to-light ratio of M/L(B)=470+/-180. We compute the luminosity function ofCL0024+1654 in order to estimate contamination of the background source countsfrom cluster galaxies. Three different magnification-based reconstructionmethods are employed using both local and non-local techniques. We havemodified the standard single power-law slope number count theory to incorporatea break and applied this to our observations. Fitting analytical magnificationprofiles of different cluster models to the observed number counts, we findthat the cluster is best described either by a NFW model with scale radiusr_s=334+/-191 kpc/h and normalisation kappa_s=0.23+/-0.08 or a power-lawprofile with slope xi=0.61+/-0.11, central surface mass densitykappa_0=1.52+/-0.20 and assuming a core radius of r_core=35 kpc/h. The NFWmodel predicts that the cumulative projected mass contained within a radius Rscales as M(<R)=2.9*10^14*(R/1')^[1.3-0.5lg (R/1')] M_sol/h. Finally, we haveexploited the fact that flux magnification effectively enables us to probedeeper than the physical limiting magnitude of our observations in searchingfor a change of slope in the U band number counts. We rule out both a totalflattening of the counts with a break up to U_AB<=26.6 and a change of slope,reported by some studies, from dlog N/dm=0.4->0.15 up to U_AB<=26.4 with 95%confidence.Comment: 19 pages, 12 figures, submitted to A&A. New version includes more  robust U band break analysis and contamination estimates, plus new plot

Lens magnification by CL0024+1654 in the $\vec{U}$ and $\vec{R}$ band