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

Knowledge of the scatter in the mass-observable relation is a key ingredientfor a cosmological analysis based on galaxy clusters in a photometric survey.In this paper we aim to quantify the capability of the correlation function ofgalaxy cluster to constrain the intrinsic scatter $\sigma_{\ln M}$. Wedemonstrate how the linear bias measured in the correlation function ofclusters can be used to determine the value of this parameter. The new methodis tested in simulations of a $5, 000 deg^2$ optical survey up to $z \sim 1$,similar to the ongoing Dark Energy Survey (DES). Our results show that ourmethod works better at lower scatter values. We can measured the intrinsicscatter $\sigma_{ln M} = 0.1$ with a standard deviation of $\sigma(\sigma_{lnM}) \sim 0.03$ using this technique. However, the expected intrinsic scatter ofthe DES RedMaPPer cluster catalog $\sigma_{ln M} \sim 0.2$ cannot be recoveredwith this method at suitable accuracy and precision because the area coverageis insufficient. For future photometric surveys with a larger area such as LSSTand Euclid, the statistical errors will be reduced. Therefore, we forecasthigher precision to measure the intrinsic scatter including the value mentionbefore. We conclude that this method can be used as an internal consistencycheck method on their simplifying assumptions and complementary tocross-calibration techniques in multi-wavelength cluster observations

Measuring the scatter of the mass-richness relation in galaxy clusters in photometric imaging surveys by means of their correlation function