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

We present a statistical study of the occurrence and effects of the coolingcores in the clusters of galaxies in a flux-limited sample, HIFLUGCS, based onROSAT and ASCA observations. About 49% of the clusters in this sample have asignificant, classically-calculated cooling-flow, mass-deposition rate. Theupper envelope of the derived mass-deposition rate is roughly proportional tothe cluster mass, and the fraction of cooling core clusters is found todecrease with it. The cooling core clusters are found to have smaller coreradii than non-cooling core clusters, while some non-cooling core clusters havehigh $\beta$ values (> 0.8). In the relation of the X-ray luminosity vs. thetemperature and the mass, the cooling core clusters show a significantly highernormalization. A systematic correlation analysis, also involving relations ofthe gas mass and the total infrared luminosity, indicates that this bias isshown to be mostly due to an enhanced X-ray luminosity for cooling coreclusters, while the other parameters, like temperature, mass, and gas mass maybe less affected by the occurrence of a cooling core. These results may beexplained by at least some of the non-cooling core clusters being indynamically young states compared with cooling core clusters, and they may turninto cooling core clusters in a later evolutionary stage.Comment: A&A accepte

Statistics of X-ray observables for the cooling-core and non-cooling core galaxy clusters