The mass-size relation of galaxy clusters

The outskirts of accreting dark matter haloes exhibit a sudden drop in density delimiting their multi-stream region. Due to the dynamics of accretion, the location of this physically motivated edge strongly correlates with the halo growth rate. Using hydrodynamical zoom-in simulations of high-mass c...

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Bibliographic Details
Published in:arXiv.org 2021-05
Main Authors: Contigiani, O, Bahé, Y M, Hoekstra, H
Format: Article
Language:English
Subjects:
Dark matter
Deposition
Filaments
Galactic clusters
Online Access:Get full text
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Summary:The outskirts of accreting dark matter haloes exhibit a sudden drop in density delimiting their multi-stream region. Due to the dynamics of accretion, the location of this physically motivated edge strongly correlates with the halo growth rate. Using hydrodynamical zoom-in simulations of high-mass clusters, we explore this definition in realistic simulations and find an explicit connection between this feature in the dark matter and galaxy profiles. We also show that the depth of the splashback feature correlates well with the direction of filaments and, surprisingly, the orientation of the brightest cluster galaxy. Our findings suggest that galaxy profiles and weak-lensing masses can define an observationally viable mass-size scaling relation for galaxy clusters, which can be used to extract cosmological information.
ISSN:2331-8422
DOI:10.48550/arxiv.2012.01336