Pressure of the hot gas in simulations of galaxy clusters

Planelles, S.; Fabjan, D.; Borgani, S.; Murante, Giuseppe; Rasia, Elena; Biffi, V.; Truong, Nhut; Ragone-Figueroa, Cinthia; Granato, G. L.; Dolag, K.; Pierpaoli, E.; Beck, Alexander M.; Steinborn, Lisa K.; Gaspari, M.

doi:10.1093/mnras/stx318

Cited by 100 publications

(144 citation statements)

References 115 publications

(259 reference statements)

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“…The slope of the Y SZ,500 −M 500 relation using the BPP is slightly steeper than the self-similar prediction (5/3), but it is consistent within the uncertainties. It is also in agreement with the recent observational work of Jimeno et al (2018) and the theoretical AGN feedback simulations from Planelles et al (2017), reporting slopes of 1.70 and 1.685 respectively (shown in Figure 4). On the other hand, the relation found using the UPP suggests a much flatter slope of 1.32 ± 0.21 that is less consistent with the self-similar scaling but is still within 2σ.…”

Section: Comparisons Of Scaling Relationssupporting

confidence: 93%

SZ Scaling Relations of Galaxy Groups and Clusters Near the North Ecliptic Pole

Pratt

Bregman

2020

ApJ

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SZ scaling relations have been used to test the self-similar prediction for massive galaxy clusters, but little attention has been given to individual galaxy groups. We investigate the scaling relations of galaxy groups and clusters near the North Ecliptic Pole using X-ray and SZ observations. This region of the sky is where both the ROSAT and Planck satellites achieved their deepest observations, permitting the investigation of lower mass systems. Our sample consists of 62 X-ray detected groups and clusters, spanning a mass range of 10 13.4 M < M 500 < 10 15 M and redshifts of 0.03 z 0.82. We extract the total SZ flux from unresolved Planck data and estimate the fraction of the SZ flux within R 500 assuming two different pressure profiles. The SZ scaling relations were derived using a Bayesian technique that accounts for censored data. We find a power law slope of 1.73 +0.19 −0.18 for the Y SZ − M 500 relation which is consistent with the self-similar prediction of 5/3. The slope of 0.89 +0.09 −0.08 for the Y SZ − L X,500 relation is in agreement with other observational studies but not the self-similar prediction of 5/4, and the Y SZ − Y X relation lies below the 1:1 relation when the slope is fixed to unity. The determined scaling relations are dependent on the selected pressure profile, so resolved data are needed to determine the effects of AGN feedback. In addition, we find a number of potential cluster candidates in the Planck Compton maps that were not identified in our X-ray sample.

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Section: Comparisons Of Scaling Relationssupporting

confidence: 93%

SZ Scaling Relations of Galaxy Groups and Clusters Near the North Ecliptic Pole

Pratt

Bregman

2020

ApJ

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“…Among the irregular (IR 3D ) sample, where we expect the largest difference between the two clumpiness profiles, we find that 95 percent of the objects have a maximum difference lower than a factor of 1.5. The artificial conduction introduced in our code, indeed, leads to better mixing of the medium and, consequently to a net reduction in the number of clumps (Biffi & Valdarnini 2015;Planelles et al 2017). In addition, the cores of the main halos and of the substructures are smoother.…”

Section: Clumpiness Factormentioning

confidence: 90%

“…Here ρ is the gas density and the brackets, , indicate the average taken over the region of interest (Mathiesen et al 1999). More precisely in our analysis, based on SPH simulated clusters, we compute the clumpiness factor by adopting the following formula discussed in Battaglia et al (2015) and Planelles et al (2017):…”

Section: Clumpiness Factormentioning

confidence: 99%

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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“…Feedback from active galactic nuclei (AGN) has been shown to be crucial in producing realistic clusters (e.g. Borgani & Kravtsov 2011;Planelles et al 2013Planelles et al , 2014Le Brun et al 2014;Pike et al 2014;Sembolini et al 2016b;Barnes et al 2017a;Mc-Carthy et al 2017;Planelles et al 2017). However, the physics of the formation of black holes (BHs) is currently not well understood.…”

Section: Bahamas Runsmentioning

confidence: 99%

Hydrostatic mass estimates of massive galaxy clusters: a study with varying hydrodynamics flavours and non-thermal pressure support

Pearce

Kay

Barnes

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We use a set of 45 simulated clusters with a wide mass range (8 × 10 13 < M 500 [M ] < 2×10 15 ) to investigate the effect of varying hydrodynamics flavours on cluster mass estimates. The cluster zooms were simulated using the same cosmological models as the BAHAMAS and C-EAGLE projects, leading to differences in both the hydrodynamic solvers and the subgrid physics but still producing clusters which broadly match observations. At the same mass resolution as BAHAMAS, for the most massive clusters (M 500 > 10 15 M ), we find changes in the SPH method produce the greatest differences in the final halo, while the subgrid models dominate at lower mass. By calculating the mass of all of the clusters using different permutations of the pressure, temperature and density profiles, created with either the true simulated data or mock spectroscopic data, we find that the spectroscopic temperature causes a bias in the hydrostatic mass estimates which increases with the mass of the cluster, regardless of the SPH flavour used. For the most massive clusters, the estimated mass of the cluster using spectroscopic density and temperature profiles is found to be as low as 50 per cent of the true mass compared to ∼ 90 per cent for low mass clusters. When including a correction for non-thermal pressure, the spectroscopic hydrostatic mass estimates are less biased on average and the mass dependence of the bias is reduced, although the scatter in the measurements does increase.Cluster masses can be estimated observationally using a variety of different techniques including X-ray observations, lensing and galaxy kinematics. In the first case, density and temperature profiles obtained from X-ray data are combined assuming hydrostatic equilibrium (e.g. Vikhlinin et al. 2006). However, many 1 We define M 500 as the mass of a cluster within a sphere of radius r 500 that encloses a density equal to 500 times the critical density of the Universe, ρ crit . 2 With the exception of halo 40 in this analysis which is halo 29 in the C-EAGLE sample.

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Pressure of the hot gas in simulations of galaxy clusters

Cited by 100 publications

References 115 publications

SZ Scaling Relations of Galaxy Groups and Clusters Near the North Ecliptic Pole

SZ Scaling Relations of Galaxy Groups and Clusters Near the North Ecliptic Pole

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

Hydrostatic mass estimates of massive galaxy clusters: a study with varying hydrodynamics flavours and non-thermal pressure support

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