nIFTy galaxy cluster simulations – I. Dark matter and non-radiative models

Sembolini, Federico; Yepes, Gustavo; Pearce, Frazer R.; Knebe, Alexander; Kay, Scott T.; Power, Chris; Cui, Weiguang; Beck, Alexander M.; Borgani, S.; Vecchia, Claudio Dalla; Davé, Romeel; Elahi, Pascal J.; February, Sean; Huang, Shuiyao; Hobbs, Alexander; Katz, Neal; Lau, Erwin T.; McCarthy, Ian G.; Murante, G.; Nagai, Daisuke; Nelson, Keith E.; Newton, Richard; Perret, V.; Puchwein, Ewald; Read, Justin I.; Saro, A.; Schaye, Joop; Teyssier, Romain; Thacker, Robert J.

doi:10.1093/mnras/stw250

Cited by 73 publications

(70 citation statements)

References 87 publications

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“…As shown in the recent paper by Sembolini et al (2016), which presents the comparison between gas properties in a dozen different flavors of non-radiative numerical simulations, such a result cannot be explained by gravitational or hydrodynamical effects. Baryonic physics, and in particular feedback effects, must therefore be invoked to explain such a low gas fraction.…”

Section: Comparison With Numerical Simulationsmentioning

confidence: 98%

The XXL Survey

Eckert

Ettori

Coupon

et al. 2016

A&A

115

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Traditionally, galaxy clusters have been expected to retain all the material accreted since their formation epoch. For this reason, their matter content should be representative of the Universe as a whole, and thus their baryon fraction should be close to the Universal baryon fraction Ω b /Ω m . We make use of the sample of the 100 brightest galaxy clusters discovered in the XXL Survey to investigate the fraction of baryons in the form of hot gas and stars in the cluster population. Since it spans a wide range of mass (10 13 −10 15 M ) and redshift (0.05−1.1) and benefits from a large set of multiwavelength data, the XXL-100-GC sample is ideal for measuring the global baryon budget of massive halos. We measure the gas masses of the detected halos and use a mass-temperature relation directly calibrated using weak-lensing measurements for a subset of XXL clusters to estimate the halo mass. We find that the weak-lensing calibrated gas fraction of XXL-100-GC clusters is substantially lower than was found in previous studies using hydrostatic masses. Our best-fit relation between gas fraction and mass reads f gas,500 = 0.055 +0.007 −0.006 M 500 /10 14 M 0.21 +0.11 −0.10 . The baryon budget of galaxy clusters therefore falls short of the Universal baryon fraction by about a factor of two at r 500,MT . Our measurements require a hydrostatic bias 1 − b = M X /M WL = 0.72 +0.08 −0.07 to match the gas fraction obtained using lensing and hydrostatic equilibrium, which holds independently of the instrument considered. Comparing our gas fraction measurements with the expectations from numerical simulations, we find that our results favour an extreme feedback scheme in which a significant fraction of the baryons are expelled from the cores of halos. This model is, however, in contrast with the thermodynamical properties of observed halos, which might suggest that weak-lensing masses are overestimated. In light of these results, we note that a mass bias 1 − b = 0.58 as required to reconcile Planck cosmic microwave background and cluster counts should translate into an even lower baryon fraction, which poses a major challenge to our current understanding of galaxy clusters.

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Section: Comparison With Numerical Simulationsmentioning

confidence: 98%

The XXL Survey

Eckert

Ettori

Coupon

et al. 2016

A&A

115

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“…Such simple total mass scalings can be used by large-scale cosmological simulations (including both LTGs and ETGs) and semi-analytic models (SAMs) to either test their results or calibrate the subgrid parameters on the M • − M tot (instead of the more complex stellar scalings; §4.3). Another potential application is the inclusion of the AGN feedback power modeled directly from the DM mass; the latter is one of the best resolved and convergent properties in cosmological simulations (Sembolini et al 2016).…”

Section: Total Mass (Dark Matter Gas Stars)mentioning

confidence: 99%

The X-Ray Halo Scaling Relations of Supermassive Black Holes

Gaspari

Eckert

Ettori

et al. 2019

ApJ

145

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We carry out a comprehensive Bayesian correlation analysis between hot halos and direct masses of supermassive black holes (SMBHs), by retrieving the X-ray plasma properties (temperature, luminosity, density, pressure, masses) over galactic to cluster scales for 85 diverse systems. We find new key scalings, with the tightest relation being the M • − T x , followed by M • − L x . The tighter scatter (down to 0.2 dex) and stronger correlation coefficient of all the X-ray halo scalings compared with the optical counterparts (as the M • − σ e ) suggest that plasma halos play a more central role than stars in tracing and growing SMBHs (especially those that are ultramassive). Moreover, M • correlates better with the gas mass than dark matter mass. We show the important role of the environment, morphology, and relic galaxies/coronae, as well as the main departures from virialization/self-similarity via the optical/X-ray fundamental planes. We test the three major channels for SMBH growth: hot/Bondilike models have inconsistent anti-correlation with X-ray halos and too low feeding; cosmological simulations find SMBH mergers as sub-dominant over most of the cosmic time and too rare to induce a central-limit-theorem effect; the scalings are consistent with chaotic cold accretion (CCA), the rain of matter condensing out of the turbulent X-ray halos that sustains a long-term self-regulated feedback loop. The new correlations are major observational constraints for models of SMBH feeding/feedback in galaxies, groups, and clusters (e.g., to test cosmological hydrodynamical simulations), and enable the study of SMBHs not only through X-rays, but also via the Sunyaev-Zel'dovich effect (Compton parameter), lensing (total masses), and cosmology (gas fractions).

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“…It is known that the solutions to the smoothed particle hydrodynamics (SPH) equations which underpin the cosmological simulations used by Henson et al (2017) (henceforth GADGET-SPH) lead to a lack of mixing (Mitchell et al 2009;Read et al 2010;Sembolini et al 2016a) which could cause this bias. Newer SPH flavours aim to increase the mixing of gas by altering the SPH equations (e.g.…”

Section: Introductionmentioning

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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nIFTy galaxy cluster simulations – I. Dark matter and non-radiative models

Cited by 73 publications

References 87 publications

The XXL Survey

The XXL Survey

The X-Ray Halo Scaling Relations of Supermassive Black Holes

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

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