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

Intracluster Light (ICL) provides an important record of the interactionsgalaxy clusters have undergone. However, we are limited in our understanding byour measurement methods. To address this we measure the fraction of clusterlight that is held in the Brightest Cluster Galaxy and ICL (BCG+ICL fraction)and the ICL alone (ICL fraction) using observational methods (SurfaceBrightness Threshold-SB, Non-Parametric Measure-NP, Composite Models-CM,Multi-Galaxy Fitting-MGF) and new approaches under development (WaveletDecomposition-WD) applied to mock images of 61 galaxy clusters (14<log10M_200c/M_solar <14.5) from four cosmological hydrodynamical simulations. Wecompare the BCG+ICL and ICL fractions from observational measures with thoseusing simulated measures (aperture and kinematic separations). The ICLfractions measured by kinematic separation are significantly larger thanobserved fractions. We find the measurements are related and provide equationsto estimate kinematic ICL fractions from observed fractions. The differentobservational techniques give consistent BCG+ICL and ICL fractions but arebiased to underestimating the BCG+ICL and ICL fractions when compared withaperture simulation measures. Comparing the different methods and algorithms wefind that the MGF algorithm is most consistent with the simulations, and CM andSB methods show the smallest projection effects for the BCG+ICL and ICLfractions respectively. The Ahad (CM), MGF and WD algorithms are best set up toprocess larger samples, however, the WD algorithm in its current form issusceptible to projection effects. We recommend that new algorithms using thesemethods are explored to analyse the massive samples that Rubin Observatory'sLegacy Survey of Space and Time will provide.

Preparing for low surface brightness science with the Vera C. Rubin  Observatory: A Comparison of Observable and Simulated Intracluster Light  Fractions