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 Tools annual

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 monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

Cold dark matter (CDM) hierarchical structure formation models predict theexistence of large-scale accretion shocks between the virial and turnaroundradii of clusters of galaxies. Kocsis et al. (2005) suggest that theSunyaev-Zel'dovich (SZ) signal associated with such shocks might be observablewith the next generation radio interferometer, ALMA. We study thethree--dimensional distribution of accretion shocks around individual clustersof galaxies drawn from adaptive mesh refinement (AMR) and smoothed particlehydrodynamics (SPH) simulations of LCDM (dark energy dominated CDM) models. Inrelaxed clusters, we find two distinct sets of shocks. One set ("virialshocks"), with Mach numbers of 2.5-4, is located at radii 0.9-1.3 Rvir, whereRvir is the spherical infall estimate of the virial radius, covering about40-50% of the total surface area around clusters at these radii. Another set ofstronger shocks ("external shocks") is located farther out, at about 3 Rvir,with large Mach numbers (~100), covering about 40-60% of the surface area. Wesimulate SZ surface brightness maps of relaxed massive galaxy clusters drawnfrom high resolution AMR runs, and conclude that ALMA should be capable ofdetecting the virial shocks in massive clusters of galaxies. More simulationsare needed to improve estimates of astrophysical noise and to determine optimalobservational strategies.

Accretion Shocks in Clusters of Galaxies and their SZ Signature from Cosmological Simulations