Imprints of mass accretion history on the shape of the intracluster medium and the TX–M relation

Chen, Huanqing; Avestruz, Camille; Kravtsov, Andrey V.; Lau, Erwin T.; Nagai, Daisuke

doi:10.1093/mnras/stz2776

Cited by 39 publications

(33 citation statements)

References 65 publications

(72 reference statements)

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“…Computing the accretion rate Γ allows us to determine the accretion phase of halos between two times, from z = 0 to z ∼ 0.5. The redshift interval of ∆z = 0.5 corresponds reasonably well to the expected relaxation timescales of halos (Power et al 2012;Diemer & Kravtsov 2014;More et al 2015;Chen et al 2019). By using the masses of halos at z = 0 and their main progenitor at z = 0.5, we thus computed the continuous accretion rate Γ 200m (z = 0.5) for each halo.…”

Section: Mass Accretion History and Formation Timementioning

confidence: 58%

“…The elliptical shape of DM halos is expected to depend on their mass and redshift, as discussed in Allgood et al (2006), Despali et al (2014), Suto et al (2016), Vega-Ferrero et al (2017), high-mass halos tend to be less spherical than low-mass objects. This mass-ellipticity correlation can be attributed to the formation time (Despali et al 2014) and the formation history (Chen et al 2019;Lau et al 2021) of halos. Following the hierarchical formation scenario, more massive structures formed more recently and are thus expected to be more widely disturbed because they did not have enough time to relax.…”

Section: Introductionmentioning

confidence: 95%

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Shape and connectivity of groups and clusters: Effect of the dynamical state and accretion history

Gouin

Bonnaire

Aghanim

2021

A&A

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Matter distribution around clusters is highly anisotropic because clusters are the nodes of the cosmic web. The shape of the clusters and the number of filaments to which they are connected, that is, their connectivity, is thought to reflect their level of anisotropic matter distribution and must in principle be related to their physical properties. We investigate the effect of the dynamical state and the formation history on both the morphology and local connectivity of about 2400 groups and clusters of galaxies from the large hydrodynamical simulation IllustrisTNG at z = 0. We find that the mass of groups and clusters mainly affects the geometry of the matter distribution: Massive halos are significantly more elliptical and are more strongly connected to the cosmic web than low-mass halos. Beyond the mass-driven effect, ellipticity and connectivity are correlated and are imprints of the growth rate of groups and clusters. Both anisotropy measures appear to trace different dynamical states, such that unrelaxed groups and clusters are more elliptical and more connected than relaxed ones. This relation between matter anisotropies and dynamical state is the sign of different accretion histories. Relaxed groups and clusters have mostly been formed a long time ago and are slowly accreting matter at the present time. They are highly spherical and weakly connected to their environment, mostly because they had enough time to relax and thus lost the connection with their preferential directions of accretion and merging. In contrast, late-formed unrelaxed objects are highly anisotropic with strong connectivities and ellipticities. These groups and clusters are in their formation phase and must be strongly affected by the infalling of materials from filaments.

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Section: Mass Accretion History and Formation Timementioning

confidence: 58%

Section: Introductionmentioning

confidence: 95%

Shape and connectivity of groups and clusters: Effect of the dynamical state and accretion history

Gouin

Bonnaire

Aghanim

2021

A&A

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“…Hydrodynamical simulations also allowed to validate these parameters with mock X-ray maps (see e.g. Poole et al 2006;Böhringer et al 2010;Morandi et al 2013;Rasia et al 2013;Weißmann et al 2013;Chon et al 2016;Chen et al 2019;Ansarifard et al 2020;Cao et al 2020).…”

Section: D Indicators Of Morphological Regularitymentioning

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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“…This causes a hydrostatic mass bias in measuring mass from SZ surveys (Planck Collaboration et al 2014;Nelson et al 2014a;Shi et al 2016). The mergers and recent accretions also tend to cause asphericity in the clusters which introduces additional scatter in projected measurements (Chen et al 2019;Lau et al 2021;Machado Poletti Valle et al 2021). Baryonic physics, such as feedback, also adds turbulent pressure support, in addition to the structure formation processes (Battaglia et al 2012;Pike et al 2014).…”

Section: Introductionmentioning

confidence: 99%

Emulating Sunyaev-Zeldovich Images of Galaxy Clusters using Auto-Encoders

Rothschild,

Nagai,

Aung

et al. 2021

Preprint

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We develop a machine learning algorithm that generates high-resolution thermal Sunyaev-Zeldovich (SZ) maps of novel galaxy clusters given only halo mass and mass accretion rate. The algorithm uses a conditional variational autoencoder (CVAE) in the form of a convolutional neural network and is trained with SZ maps generated from the IllustrisTNG simulation. Our method can reproduce the details of the aspherical turbulent galaxy clusters with a resolution similar to hydrodynamic simulations while achieving the computational feasibility of semi-analytical maps, allowing us to generate over 10 5 mock SZ maps in 30 seconds on a laptop. We show that the individual images generated by the model are novel clusters (i.e. not found in the training set) and that the model accurately reproduces the effects of mass and mass accretion rate on the SZ images, such as scatter, asymmetry, and concentration, in addition to modeling merging sub-clusters. This work demonstrates the viability of machine-learning-based methods for producing the number of realistic, high-resolution maps of galaxy clusters necessary to achieve statistical constraints from future SZ surveys.

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Imprints of mass accretion history on the shape of the intracluster medium and the TX–M relation

Cited by 39 publications

References 65 publications

Shape and connectivity of groups and clusters: Effect of the dynamical state and accretion history

Shape and connectivity of groups and clusters: Effect of the dynamical state and accretion history

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

Emulating Sunyaev-Zeldovich Images of Galaxy Clusters using Auto-Encoders

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