The Cluster HEritage project with XMM-Newton – Mass Assembly and Thermodynamics at the Endpoint of structure formation (CHEX-MATE) is a three-mega-second Multi-Year Heritage Programme to obtain X-ray observations of a minimally-biased, signal-to-noise-limited sample of 118 galaxy clusters detected by Planck through the Sunyaev–Zeldovich effect. The programme, described in detail in this paper, aims to study the ultimate products of structure formation in time and mass. It is composed of a census of the most recent objects to have formed (Tier-1: 0.05   M ⊙ 500  M ⊙ ), together with a sample of the highest mass objects in the Universe (Tier-2: z 500  > 7.25 × 1014  M ⊙ ). The programme will yield an accurate vision of the statistical properties of the underlying population, measure how the gas properties are shaped by collapse into the dark matter halo, uncover the provenance of non-gravitational heating, and resolve the major uncertainties in mass determination that limit the use of clusters for cosmological parameter estimation. We will acquire X-ray exposures of uniform depth, designed to obtain individual mass measurements accurate to 15 − 20% under the hydrostatic assumption. We present the project motivations, describe the programme definition, and detail the ongoing multi-wavelength observational (lensing, SZ, radio) and theoretical effort that is being deployed in support of the project.

/pdf/the-cluster-heritage-project-with-xmm-newton-mass-assembly-4q80q2vcle.pdf

The Cluster HEritage project with XMM-Newton: Mass Assembly and Thermodynamics at the Endpoint of structure formation - I. Programme overview

We study the connection between morphology and dynamical state of simulated clusters in $z\in[0,1.031]$ from THE THREE HUNDRED Project cluster sample. We evaluate the dynamical state using a combination of dynamical parameters -- $\chi$ from theoretical measures and compare the results with other two relaxation criteria that come from observation measures: the morphology in mock X-ray and Sunyaev-Zeldovich (SZ) effect images of galaxy clusters -- the $M$ indicator which is a combination of seven morphological parameters, and the offsets $\Delta$ between the peaks or centroids of X-ray and SZ maps and the Brightest Central Galaxy (BCG) position estimated from optical maps. We study the efficiency of morphological indicators and the correlations with the dynamical state of the combined $M$ and dynamical $\chi$ parameters, that have the advantage of proving and collecting different aspects of the cluster structures than single parameters. An evolution with the redshift of the dynamical state is present, but the populations of the dynamical state classes differ when different radii are used. The main source of contamination in relaxed fraction inferred from morphological parameters is constituted by hybrid clusters. $M$ combined parameter describes with the same efficiency the morphology in X-ray and SZ maps, with a correlation coefficient of $\rho=0.81$. A moderately strong correlation between $M$ and $\chi$ is present, with a coefficient of $\rho=-0.66$. The offset parameters based on centroids are more sensitive to dynamical state than peaks positions offsets. The correlation with $\chi$ for centroids is of the same order of $M$, with $\rho=-(0.63$-$0.67)$ if SZ or X-ray centroids are respectively used.

The Three Hundred project: dynamical state of galaxy clusters and morphology from multiwavelength synthetic maps

The knowledge of the dynamical state of galaxy clusters allows to alleviate systematics when observational data from these objects are applied in cosmological studies. Evidence of correlation between the state and the morphology of the clusters is well studied. The morphology can be inferred by images of the surface brightness in the X-ray band and of the thermal component of the Sunyaev-Zel'dovich (tSZ) effect in the millimetre range. For this purpose, we apply, for the first time, the Zernike polynomial decomposition, a common analytic approach mostly used in adaptive optics to recover aberrated radiation wavefronts at the telescopes pupil plane. With this novel way we expect to correctly infer the morphology of clusters and so possibly, their dynamical state. To verify the reliability of this new approach we use more than 300 synthetic clusters selected in THE THREE HUNDRED project at different redshifts ranging from 0 up to 1.03. Mock maps of the tSZ, quantified with the Compton parameter, $y$-maps, are modelled with Zernike polynomials inside $R_{500}$, the cluster reference radius. We verify that it is possible to discriminate the morphology of each cluster by estimating the contribution of the different polynomials to the fit of the map. The results of this new method are correlated with those of a previous analysis made on the same catalogue, using two parameters that combine either morphological or dynamical-state probes. We underline that instrumental angular resolution of the maps has an impact mainly when we extend this approach to high-redshift clusters.

The Three Hundred Project: quest of clusters of galaxies morphology and dynamical state through Zernike polynomials

The DECam Local Volume Exploration Survey: Overview and First Data Release

The dynamical state of galaxy clusters describes if clusters are relaxed dynamically or in a merging process of subclusters. By using archival images from the Chandra X-ray Observatory, we derive a set of parameters to describe the dynamical state for 964 galaxy clusters. Three widely used indicators for dynamical state, the concentration index c, the centroid shift omega and the power ratio P3/P0 are calculated in the circular central region with a radius of 500 kpc. We also derive two adaptive parameters, the profile parameter kappa and the asymmetry factor alpha, in the best fitted elliptical region. The morphology index delta is then defined by combining these two adaptive parameters, which indicates the dynamical state of galaxy clusters and has good correlations to the concentration index c, the centroid shift omega, the power ratio P3/P0, and the optical relaxation factor Gamma. For a large sample of clusters, the dynamical parameters are continuously distributed from the disturbed to relaxed states with a peak in the between, rather than the bimodal distribution for the two states. We find that the newly derived morphology index delta works for the similar fundamental plane between the radio power, cluster mass and the dynamical state for clusters with diffuse radio giant-halos and mini-halos. The offset between masses estimated from the Sunyaev-Zeldovich effect and X-ray images depends on dynamical parameters. All dynamical parameters for galaxy clusters derived from the Chandra archival images are available on this http URL.

Dynamical state for 964 galaxy clusters from Chandra X-ray images

We use imaging from the first three years of the Dark Energy Survey to characterize the dynamical state of 288 galaxy clusters at 0.1 less than or similar to z less than or similar to 0.9 detected in the South Pole Telescope (SPT) Sunyaev-Zeldovich (SZ) effect survey (SPT-SZ). We examine spatial offsets between the position of the brightest cluster galaxy (BCG) and the centre of the gas distribution as traced by the SPT-SZ centroid and by the X-ray centroid/peak position from Chandra and XMM data. We show that the radial distribution of offsets provides no evidence that SPT SZ-selected cluster samples include a higher fraction of mergers than X-ray-selected cluster samples. We use the offsets to classify the dynamical state of the clusters, selecting the 43 most disturbed clusters, with half of those at z greater than or similar to 0.5, a region seldom explored previously. We find that Schechter function fits to the galaxy population in disturbed clusters and relaxed clusters differ at z > 0.55 but not at lower redshifts. Disturbed clusters at z > 0.55 have steeper faint-end slopes and brighter characteristic magnitudes. Within the same redshift range, we find that the BCGs in relaxed clusters tend to be brighter than the BCGs in disturbed samples, while in agreement in the lower redshift bin. Possible explanations includes a higher merger rate, and a more efficient dynamical friction at high redshift. The red-sequence population is less affected by the cluster dynamical state than the general galaxy population.

/pdf/a-joint-sz-x-ray-optical-analysis-of-the-dynamical-state-of-2pkcv8hfxs.pdf

A joint SZ-X-ray-optical analysis of the dynamical state of 288 massive galaxy clusters

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A joint SZ-X-ray-optical analysis of the dynamical state of 288 massive galaxy clusters