The Cluster HEritage project with <i>XMM-Newton</i>: Mass Assembly and Thermodynamics at the Endpoint of structure formation

Arnaud, M.; Ettori, S.; Pratt, G. W.; Rossetti, M.; Eckert, D.; Gastaldello, F.; Gavazzi, R.; Kay, Scott T.; Lovisari, Lorenzo; Maughan, Ben; Pointecouteau, É.; Sereno, Mauro; Bartalucci, I.; Bonafede, A.; Bourdin, H.; Cassano, R.; Duffy, Ryan; Iqbal, Asif; Maurogordato, S.; Rasia, Elena; Sayers, Jack; Andrade-Santos, Felipe; Aussel, H.; Barnes, David J.; Barrena, R.; Borgani, S.; Burkutean, S.; Clerc, N.; Corasaniti, Pier Stefano; Cuillandre, J. C.; Grandi, S. De; Petris, M. De; Dolag, K.; Donahue, M.; Ferragamo, A.; Gaspari, M.; Ghizzardi, S.; Gitti, Myriam; Haines, C. P.; Jauzac, Mathilde; Johnston‐Hollitt, M.; Jones, C.; Kéruzoré, F.; Lebrun, Aurore; Mayet, F.; Mazzotta, P.; Melin, Jean-Baptiste; Molendi, S.; Nonino, M.; Okabe, Nobuhiko; Paltani, S.; Perotto, L.; Pires, S.; Radovich, M.; Rubiño-Martín, J. A.; Salvati, Laura; Saro, A.; Sartoris, B.; Schellenberger, G.; Streblyanska, A.; Tarrío, Paula; Tozzi, P.; Umetsu, Keiichi; Burg, R. F. J. van der; Vazza, Franco; Venturi, T.; Yepes, Gustavo; Zarattini, S.

doi:10.1051/0004-6361/202039632

Cited by 48 publications

(4 citation statements)

References 161 publications

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“…For clusters at higher redshifts, combined strong and weak lensing is required to distinguish SIDM and CDM using the RAR. The ongoing CHEX-MATE project will provide such ideal multiwavelength data sets of high quality, for a minimally biased, signal-to-noise-limited sample of 118 Planck galaxy clusters at 0.05 < z < 0.6 detected through the SZ effect (CHEX-MATE Collaboration et al 2021). Extending this work to the CHEX-MATE sample will thus be a substantial step toward understanding the collisionless nature of dark matter.…”

Section: Discussionmentioning

confidence: 99%

Testing the Collisionless Nature of Dark Matter with the Radial Acceleration Relation in Galaxy Clusters

Tam¹,

Umetsu²,

Robertson³

et al. 2022

Preprint

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The radial acceleration relation (RAR) represents a tight empirical relation between the inferred total and baryonic centripetal accelerations, g tot = GM tot (< r)/r 2 and g bar = GM bar (< r)/r 2 , observed in galaxies and galaxy clusters. The tight correlation between these two quantities can provide insight into the nature of dark matter. Here we use BAHAMAS, a state-of-the-art suite of cosmological hydrodynamical simulations, to characterize the RAR in cluster-scale halos for both cold and collisionless dark matter (CDM) and selfinteracting dark matter (SIDM) models. SIDM halos generally have reduced central dark matter densities, which reduces the total acceleration in the central region when compared with CDM. We compare the RARs in galaxy clusters simulated with different dark matter models to the RAR inferred from CLASH observations. Our comparison shows that the cluster-scale RAR in the CDM model provides an excellent match to the CLASH RAR obtained by Tian et al. including the high-acceleration regime probed by the brightest cluster galaxies (BCGs). By contrast, models with a larger SIDM cross-section yield increasingly poorer matches to the CLASH RAR. Excluding the BCG regions results in a weaker but still competitive constraint on the SIDM cross-section. Using the RAR data outside the central r < 100 kpc region, an SIDM model with σ/m = 0.3 cm 2 g −1 is disfavored at the 3.8σ level with respect to the CDM model. This study demonstrates the power of the clusterscale RAR for testing the collisionless nature of dark matter.

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Section: Discussionmentioning

confidence: 99%

Testing the Collisionless Nature of Dark Matter with the Radial Acceleration Relation in Galaxy Clusters

Tam¹,

Umetsu²,

Robertson³

et al. 2022

Preprint

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“…There have been numerous studies dedicated to weak lensing, e.g. LoCuss (Okabe et al 2010), Weighing the Giants(von der Linden et al 2014), The Cluster HEritage project(CHEX-MATE Collaboration et al 2021). However, studies on caustic masses are rather scarce.…”

Section: Discussionmentioning

confidence: 99%

Scaling relations of X-ray Luminous Clusters in the Hyper Suprime-Cam Subaru Strategic Program Field

Poon¹,

Okabe²,

Fukazawa³

et al. 2023

Preprint

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We present the XMM-Newton X-ray analysis of 19 X-ray luminous galaxy clusters of low-to-mid redshift (< 0.4) selected from the MCXC cluster catalogue in the Hyper Suprime-Cam Subaru Strategic Program field. We derive the hydrostatic equilibrium mass and study scaling relations using i) the whole sample, ii) only relaxed clusters and iii) only disturbed clusters. When considering the whole sample, the 𝑌 X -𝑀 tot and 𝑀 gas -𝑀 tot relations agree with self-similarity. In terms of morphology, relaxed clusters show a flatter relation in 𝐿 X,ce -𝑀 tot , 𝐿 X,bol -𝑀 tot , 𝐿 X,ce -𝑇, 𝐿 bol,ce -𝑇, 𝑀 gas -𝑀 tot and 𝑌 X -𝑀 tot . The 𝐿 bol,ce -𝑀 tot , 𝐿 X,ce -𝑀 tot 𝐿 bol,ce -𝑇 and 𝐿 X,ce -𝑇 relations show a slope ∼3𝜎 steeper. The residuals in the 𝑀 gas -𝑀 tot and 𝑇-𝑀 tot relations and the intrinsic covariance between 𝑀 gas and 𝑇 show hints of positive correlation, casting doubt on whether the 𝑌 X parameter is a truly low scatter mass proxy. The 𝑀 gas -𝑀 tot and 𝑇-𝑀 tot plots color-coded with the offset of the 𝐿 X,ce -𝑀 tot relation show these two relations to be brightness dependent but not the 𝐿 X,ce -𝑇 relation, suggesting relations involving 𝑀 tot are biased due to sample selection based on luminosity. Following the work which studied an optical sample and combining our result with literature studies, we find the 𝑀 tot derived not using mass proxies deviate from 𝐿 X ∝ 𝑀 2 gas 𝑀 −1 tot and 𝑀 tot based on hydrostatic equilibrium are more massive than what is expected by their relation using caustic masses. This indicates mass bias plays an important role in scaling relations.

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“…Thus far, the CFP has been directly measured only for the CLASH sample, which is quite unique for its characteristics and is also composed of extremely massive objects. Therefore, it would be interesting to extend the analysis to cluster samples with a wider mass range as targeted by ongoing cluster programs, such as the CHEX-MATE program (CHEX-MATE Collaboration et al 2021), the XXL X-ray survey (Pierre et al 2016), and the eROSITA X-ray survey (Brunner et al 2021).…”

Section: Discussionmentioning

confidence: 99%

The Three Hundred Project: dissecting the fundamental plane of galaxy clusters up to $z=1$

Díaz-García,

Umetsu,

Rasia

et al. 2021

Preprint

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We carry out a systematic study of the recently discovered fundamental plane of galaxy clusters (CFP) using a sample of ∼ 250 simulated clusters from T T H project, focusing on the stability of the plane against different temperature definitions and its dependence on the dynamical relaxation state of clusters. The CFP is characterised in the form of 𝑇 ∝ 𝑀 𝛼 s 𝑟 𝛽 s , defined with the gas temperature (𝑇) and the characteristic halo scale radius and mass (𝑟 s and 𝑀 s ) assuming an NFW halo description. We explore two definitions of weighted temperatures, namely mass-weighted and spectroscopic-like temperatures, in three radial ranges: [0.1, 1.0]𝑟 200 , [0.15, 1.0]𝑟 500 , and [50, 500]ℎ −1 kpc. We find that T T H project clusters at 𝑧 = 0 lie on a thin plane whose parameters (𝛼, 𝛽) and dispersion (0.015-0.030 dex) depend on the gas temperature definition. The CFP for mass-weighted temperatures is closer to the virial equilibrium expectation (𝛼 = 1, 𝛽 = −1) with a smaller dispersion. When gas temperatures are measured inside 500ℎ −1 kpc, which is close to the median value of 𝑟 s , the resulting CFP deviates the most from the virial expectation and shifts towards the similarity solution for a secondary infall model (𝛼 = 1.5, 𝛽 = −2). Independently of the temperature definition, we find that clusters at 𝑧 = 1 form a CFP similar to the virial expectation. At all epochs, the CFP remains well defined throughout the evolution of the cluster population. The CFP of relaxed clusters is always close to the virial expectation, with a milder evolution than for the unrelaxed case. We find that only systems formed over the last 4 Gyr have a CFP that is closer to the self-similar solution. All these findings are compatible with the CFP obtained for a CLASH subsample excluding the hottest clusters with 𝑇 X > 12 keV.

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

Cited by 48 publications

References 161 publications

Testing the Collisionless Nature of Dark Matter with the Radial Acceleration Relation in Galaxy Clusters

Testing the Collisionless Nature of Dark Matter with the Radial Acceleration Relation in Galaxy Clusters

Scaling relations of X-ray Luminous Clusters in the Hyper Suprime-Cam Subaru Strategic Program Field

The Three Hundred Project: dissecting the fundamental plane of galaxy clusters up to $z=1$

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