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

To assess the effect of baryonic ‘pinching’ of galaxy cluster dark matter (DM) haloes, cosmological (Λ cold dark matter)  treesph  simulations of the formation and evolution of two galaxy clusters have been performed, with and without baryons included.  The simulations with baryons invoke star formation, chemical evolution with non‐instantaneous recycling, metallicity‐dependent radiative cooling, strong starburst‐driven galactic superwinds and the effects of a meta‐galactic ultraviolet field, including simplified radiative transfer. The two clusters have   T ≃ 3  and 6 keV, respectively, and, at   z ∼ 0 , both host a prominent, central cD galaxy.  Comparing the simulations without and with baryons, it is found for the latter that the inner DM density profiles,   r ≲ 50–100 kpc , steepen considerably:  Δα∼ 0.5–0.6 , where  −α  is the logarithmic DM density gradient. This is primarily due to the central stellar cDs becoming very massive, as a consequence of the onset of late‐time cooling flows and related star formation. Once these spurious cooling flows have been corrected for, and the cluster gravitational potentials dynamically adjusted, much smaller pinching effects are found:  Δα∼ 0.1 . Including the effects of baryonic pinching, central slopes of  α≃ 1.0  and 1.2 are found for the DM in the two clusters, interestingly close to recent observational findings for galaxy cluster Abell 1703 based on strong gravitational lensing.  For the simulations with baryons, the inner density profile of DM and cluster gas (intracluster medium) combined is found to be only very marginally steeper than that of the DM,  Δα≲ 0.05 . However, the total matter inner density profiles are found to be  Δα∼ 0.5  steeper than the inner profiles in the DM‐only simulations.

Moderate steepening of galaxy cluster dark matter profiles by baryonic pinching