Speaker
Description
Galaxy cluster formation is driven by a variety of complicated physical processes that affect their growth and evolution through cosmic time. As a result, the matter distribution within the cluster, and therefore, its shape, can be a probe of these astrophysical processes and cosmology. Clusters grow through the accretion of new material, typically along two or three main filaments, giving them an elongated, triaxial morphology. In-falling material is thermalized primarily through a series of shocks, however, the underlying physical processes governing these shocks are not well understood. To better understand the growth and evolution of clusters, we have developed a pipeline for modeling their three-dimensional triaxial morphology from which we can infer their masses and the thermalization efficiency in the cluster outskirts within a triaxial basis. This analysis will be performed on the Cluster HEritage project with XMM-Newton – Mass Assembly and Thermodynamics at the Endpoint of structure formation (CHEX-MATE) sample of galaxy clusters. Utilizing X-ray data from XMM-Newton and Sunyaev-Zeldovich effect (SZE) maps from Planck and the Atacama Cosmology Telescope, a three-dimensional triaxial description of the cluster geometry is obtained. The addition of a weak lensing (WL) analysis using shear maps constructed from Subaru Suprime-Cam observations enables a measurement of total halo mass. Additionally, the thermalization efficiency in the cluster outskirts can be measured as the level of pressure support due to non-thermal motions in the region. We obtain radial profiles of the thermal pressure ($P_{th}$) from the direct X-ray and SZE measurements and the total pressure needed to offset gravity ($P_{tot}$) from the gravitational potential corresponding to the WL derived triaxial mass. The non-thermal pressure ($P_{nt}$) is then taken to be the difference between $P_{tot}$ and $P_{th}$. In this talk, I will present the results from this pipeline on two CHEX-MATE clusters, one elongated in the line of sight (Abell 1689) and another that is elongated in the plane of sky (Abell 2390). I will also include projections for the final results that can be obtained from the full CHEX-MATE sample based on these initial demonstrations.
| Would you be interested in presenting a poster if the conference is oversubcribed? | Yes |
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