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 sizes of entire systems of globular clusters (GCs) depend on theformation and destruction histories of the GCs themselves, but also on theassembly, merger and accretion history of the dark matter (DM) haloes that theyinhabit. Recent work has shown a linear relation between total mass of globularclusters in the globular cluster system and the mass of its host dark matterhalo, calibrated from weak lensing. Here we extend this to GC system sizes, bystudying the radial density profiles of GCs around galaxies in nearby galaxygroups. We find that radial density profiles of the GC systems are well fitwith a de Vaucouleurs profile. Combining our results with those from theliterature, we find tight relationship ($\sim 0.2$ dex scatter) between theeffective radius of the GC system and the virial radius (or mass) of its hostDM halo. The steep non-linear dependence of this relationship ($R_{e, GCS}\propto R_{200}^{2.5 - 3}$) is currently not well understood, but is animportant clue regarding the assembly history of DM haloes and of the GCsystems that they host.

The correlation between the sizes of globular cluster systems and their host dark matter haloes