Dark matter distribution in cluster galaxies
Abstract
Galaxy clusters are large structures of the Universe, and they are formed and grow through the accretion of smaller structures such as groups or isolated galaxies. In this scenario, during their infall into the core of a cluster, satellite galaxies are submitted to a number of interactions with their host, both on the level of dark and baryonic matter. In particular, both observations and numerical simulations suggest that part of the dark matter composing their haloes can be stripped by the host tidal forces. We present our weak lensing measurement of the Stellar-to-Halo Mass Relation for satellite galaxies in the redMaPPer clusters, using shear data fro the CS82, CFHTLenS and DES-SV surveys. To help interpret these results we then discuss our analysis of the evolution of subhaloes in the Illustris hydrodynamical simulation.
- Publication:
-
SF2A-2019: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics
- Pub Date:
- December 2019
- Bibcode:
- 2019sf2a.conf..485N
- Keywords:
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- galaxy clusters;
- galaxy evolution;
- weak lensing;
- numerical simulations