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 use of galaxy clusters as cosmological probes relies on a detailedunderstanding of their properties. We aim to update the spectroscopic clusteridentification of CODEX by running the spectroscopic group finder on thefollow-up spectroscopy results and connecting the dynamical state of clustersto their scaling relations. We implemented a reproducible spectroscopicmembership determination and cleaning procedures, based on the redMaPPermembership, running the spectroscopic group finder on the follow-upspectroscopy results and cleaning the membership for spectroscopic outliers. Weapplied the Anderson-Darling test for velocity substructure and analysed itsinfluence on the scaling relations. We also tested the effect of theX-ray-to-optical centre offset on the scaling relations. We report on thescaling relations between richness, X-ray luminosity, and velocity dispersionfor a complete sample of clusters with at least 15 members. Clusters withvelocity substructure exhibit enhanced velocity dispersion for a given richnessand are characterized by 2.5 times larger scatter. Clusters that have a strongoffset in X-ray-to-optical centres have comparable scaling relations asclusters with substructure. We demonstrate that there is a consistency in theparameters of the scaling relations for the low- and high-richness galaxyclusters. Splitting the clusters by redshift, we note a decrease in scatterwith redshift in all scaling relations. We localize the redshift range where ahigh scatter is observed to $z<0.15$, which is in agreement with the literatureresults on the scatter. We note that the increase in scatter for both high- andlow-luminosity clusters is $z<0.15$, suggesting that both cooling and theresulting active galactic nucleus feedback are at the root of this scatter.Abridged.

CODEX: Role of velocity substructure in the scaling relations of galaxy clusters