Morphological estimators on Sunyaev–Zel'dovich maps of MUSIC clusters of galaxies

Cialone, Giammarco; Petris, M. De; Sembolini, Federico; Yepes, Gustavo; Baldi, A.; Rasia, Elena

doi:10.1093/mnras/sty621

Cited by 41 publications

(65 citation statements)

References 97 publications

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“…7 with the same weight to distinguish relaxed and disturbed objects. This is consistent with what has been derived by Cialone et al 2018. According to this definition, clusters which are characterised by the presence of a cool core and are morphologically regular will have M > 0 and very disturbed objects with a very diffuse core will have M < 0.…”

Section: Combined Dynamical Indicator Msupporting

confidence: 91%

The Most Massive galaxy Clusters (M2C) across cosmic time: link between radial total mass distribution and dynamical state

Bartalucci

Arnaud

Pratt

et al. 2019

A&A

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We study the dynamical state and the integrated total mass profiles of 75 massive (M 500 > 5 × 10 14 M ⊙ ) Sunyaev-Zeldovich(SZ)selected clusters at 0.08 < z < 1.1. The sample is built from the Planck catalogue, with the addition of four SPT clusters at z > 0.9. Using XMM-Newton imaging observations, we characterise the dynamical state with the centroid shift w , the concentration C SB , and their combination, M, which simultaneously probes the core and the large-scale gas morphology. Using spatially resolved spectroscopy and assuming hydrostatic equilibrium, we derive the total integrated mass profiles. The mass profile shape is quantified by the sparsity, that is the ratio of M 500 to M 2500 , the masses at density contrasts of 500 and 2500, respectively. We study the correlations between the various parameters and their dependence on redshift. We confirm that SZ-selected samples, thought to most accurately reflect the underlying cluster population, are dominated by disturbed and non-cool core objects at all redshifts. There is no significant evolution or mass dependence of either the cool core fraction or the centroid shift parameter. The M parameter evolves slightly with z, having a correlation coefficient of ρ = −0.2 ± 0.1 and a null hypothesis p-value of 0.01. In the high-mass regime considered here, the sparsity evolves minimally with redshift, increasing by 10% between z < 0.2 and z > 0.55, an effect that is significant at less than 2σ. In contrast, the dependence of the sparsity on dynamical state is much stronger, increasing by a factor of ∼ 60% from the one third most relaxed to the one third most disturbed objects, an effect that is significant at more than 3σ. This is the first observational evidence that the shape of the integrated total mass profile in massive clusters is principally governed by the dynamical state and is only mildly dependent on redshift. We discuss the consequences for the comparison between observations and theoretical predictions.

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Section: Combined Dynamical Indicator Msupporting

confidence: 91%

The Most Massive galaxy Clusters (M2C) across cosmic time: link between radial total mass distribution and dynamical state

Bartalucci

Arnaud

Pratt

et al. 2019

A&A

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“…At the same time, the techniques used to analyse the simulations and compare them to observational data, including mock images, have further enhanced their predictive power. Still, the level of the above mass bias for simulated clusters considered 'dynamically relaxed' has always been consistently found to be around 10-20 percent (Rasia et al 2006;Nagai et al 2007a;Jeltema et al 2008;Piffaretti & Valdarnini 2008;Lau et al 2009;Meneghetti et al 2010;Nelson et al 2012;Battaglia et al 2012;Rasia et al 2012;Shi et al 2015;Biffi et al 2016;Vazza et al 2016;Henson et al 2017; Barnes et al 2017a;Vazza et al 2018;Cialone et al 2018;Angelinelli et al 2019). Thanks to simulations, we understand that the main sources of the HE bias are the residual, non-thermalized gas velocity, in the form of both bulk motion and turbulence, and intra-cluster medium (ICM) inhomogeneities.…”

Section: Introductionmentioning

confidence: 96%

The Three Hundred Project: Correcting for the hydrostatic-equilibrium mass bias in X-ray and SZ surveys

Ansarifard

Rasia

Biffi

et al. 2020

A&A

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Accurate and precise measurements of masses of galaxy clusters are key to derive robust constraints on cosmological parameters. Rising evidence from observations, however, confirms that X-ray masses, obtained under the assumption of hydrostatic equilibrium, might be underestimated, as previously predicted by cosmological simulations. We analyse more than 300 simulated massive clusters, from 'The Three Hundred Project', and investigate the connection between mass bias and several diagnostics extracted from synthetic X-ray images of these simulated clusters. We find that the azimuthal scatter measured in 12 sectors of the X-ray flux maps is a statistically significant indication of the presence of an intrinsic (i.e. 3D) clumpy gas distribution. We verify that a robust correction to the hydrostatic mass bias can be inferred when estimates of the gas inhomogeneity from X-ray maps (such as the azimuthal scatter or the gas ellipticity) are combined with the asymptotic external slope of the gas density or pressure profiles, which can be respectively derived from X-ray and millimetric (Sunyaev-Zeldovich effect) observations. We also obtain that mass measurements based on either gas density and temperature or gas density and pressure result in similar distributions of the mass bias. In both cases, we provide corrections that help reduce both the dispersion and skewness of the mass bias distribution. These are effective even when irregular clusters are included leading to interesting implications for the modelling and correction of hydrostatic mass bias in cosmological analyses of current and future X-ray and SZ cluster surveys.

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“…Ribeiro et al 2013;Wen & Han 2013) and in the X-ray band (see e.g. Rasia et al 2013;Lovisari et al 2017;Nurgaliev et al 2017;Bartalucci et al 2019;Yuan & Han 2020;Cao et al 2020) or of the diffusion of the Cosmic Microwave Background (CMB) photons by tSZ effect in the millimetre band (Cialone et al 2018;De Luca et al 2020, hereafter DL20), or a combination of some of them (see e.g. Mann & Ebeling 2012;Molnar et al 2020;Ricci et al 2020;Zenteno et al 2020;The CHEX-MATE Collaboration et al 2020).…”

Section: Introductionmentioning

confidence: 99%

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

Capalbo

Petris

Luca

et al. 2020

Monthly Notices of the Royal Astronomical Society

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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 R500, 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.

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Morphological estimators on Sunyaev–Zel'dovich maps of MUSIC clusters of galaxies

Cited by 41 publications

References 97 publications

The Most Massive galaxy Clusters (M2C) across cosmic time: link between radial total mass distribution and dynamical state

The Most Massive galaxy Clusters (M2C) across cosmic time: link between radial total mass distribution and dynamical state

The Three Hundred Project: Correcting for the hydrostatic-equilibrium mass bias in X-ray and SZ surveys

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

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