Abstract
The most massive halos of matter in the Universe grow via accretion and merger events throughout cosmic times. These violent processes generate shocks at many scales and induce large-scale bulk and turbulent motions. These processes inject kinetic energy at large scales, which is transported to the viscous dissipation scales, contributing to the overall heating and virialisation of the halo, and acting as a source of non-thermal pressure in the intra-cluster medium. Characterizing the physical properties of these gas motions will help us to better understand the assembly of massive halos, hence the formation and the evolution of these large-scale structures. We base this characterization on the study of the X-ray and Sunyaev-Zel’dovich effect brightness fluctuations. Our work relies on three complementary samples covering a wide range of red-shifts, masses and dynamical states of clusters. We present the results of our X-ray analysis for the low redshift sample, X-COP, and a subsample of higher redshift clusters. We investigate the derived properties according to the dynamical state of our clusters, and the possibility of a self-similar behaviour based on the reconstructed gas motions power-spectra and the correlation with various morphological indicators.
Highlights
The baryonic content of galaxy clusters is largely dominated by the hot gas that constitutes the intracluster medium (ICM)
Direct measurements of these turbulent processes can be achieved using spatially resolved X-ray spectroscopy [2, 3], and will be fully enabled in the future with the upcoming XRISM and Athena missions [4, 5]. These turbulent processes are expected to induce fluctuations in the thermodynamic properties of the ICM, that should be detectable in the related observables [6]
To search for links between the dynamical state of the clusters and the role of turbulence in the ICM, we investigate the correlation between our 2D-spectra best parametrization and a set of morphological indicators
Summary
The baryonic content of galaxy clusters is largely dominated by the hot gas that constitutes the intracluster medium (ICM). The resulting turbulent motions transport kinetic energy, which cascades to the dissipation scale and contributes to the virialisation of the halo through non-thermal heating of the ICM [e.g. 1] Direct measurements of these turbulent processes can be achieved using spatially resolved X-ray spectroscopy [2, 3], and will be fully enabled in the future with the upcoming XRISM and Athena missions [4, 5]. We aim at characterizing the X-ray surface brightness and SZ distortion fluctuations for a large cluster sample (N > 150) spanning a large range of redshifts, masses and dynamical states This should allow us to better constrain the properties and impact of turbulence in the ICM, considering the assembly of massive halos. We present our preliminary results on the full X-COP sample, and pilot sub-samples of 8 and 4 clusters for CHEX-MATE and LPSZ@NIKA2, respectively
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