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

Galaxy clusters show a variety of intra-cluster medium properties at a fixedmass, among which gas fractions, X-ray luminosity and X-ray surface brightness.In this work we investigate whether the yet-undetermined cause producingclusters of X-ray low surface brightness also affects galaxy properties, namelyrichness, richness concentration, width and location of the red sequence,colour, luminosity, and dominance of the brightest cluster galaxy. We useSDSS-DR12 photometry and our analysis factors out the mass dependency to derivetrends at fixed cluster mass. Clusters of low surface brightness for their masshave cluster richness in spite of their group-like luminosity. Gas-poor, lowX-ray surface brightness, X-ray faint clusters for their mass, display 25\%lower richness for their mass at $4.4\sigma$ level. Therefore, richness andquantities depending on gas, such as gas fraction, $M_{gas}$, and X-ray surfacebrightness, are covariant at fixed halo mass. In particular, we do not confirmthe hint of an anti-correlation of hot and cold baryons at fixed mass put forthin literature. All the remaining optical properties show no covariance at fixedmass, within the sensitivities allowed by our data and sample size. We concludethat X-ray and optical properties are disjoint, the optical properties notshowing signatures of those processes involving gas content, apart from therichness-mass scaling relation. The covariance between X-ray surface brightnessand richness is useful for an effective X-ray follow-up of low surfacebrightness clusters because it allows us to pre-select clusters using opticaldata of survey quality and prevent expensive X-ray observations.

Do gas-poor galaxy clusters have different galaxy populations? The positive covariance of hot and cold baryons