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

The increasing sensitivity of current experiments, which nowadays routinelymeasure the thermal SZ effect within galaxy clusters, provide the hope thatpeculiar velocities of individual clusters of galaxies will be measured rathersoon using the kinematic SZ effect. Also next generation of X-ray telescopeswith microcalorimeters, promise first detections of the motion of the intracluster medium (ICM) within clusters. We used a large set of cosmological,hydrodynamical simulations, which cover very large cosmological volume, hostinga large number of rich clusters of galaxies, as well as moderate volumes wherethe internal structures of individual galaxy clusters can be resolved with veryhigh resolution to investigate, how the presence of baryons and theirassociated physical processes like cooling and star-formation are affecting thesystematic difference between mass averaged velocities of dark matter and theICM inside a cluster. We, for the first time, quantify the peculiar motion ofgalaxy clusters as function of the large scale environment. We also demonstratethat especially in very massive systems, the relative velocity of the ICMcompared to the cluster peculiar velocity add significant scatter onto theinferred peculiar velocity, especially when measurements are limited to thecentral regions of the cluster. Depending on the aperture used, this scattervaries between 50% and 20%, when going from the core (e.g. ten percent of thevirial radius) to the full cluster (e.g. the virial radius).

Relative velocity of dark matter and barions in clusters of galaxies and measurements of their peculiar velocities