nIFTy galaxy cluster simulations – II. Radiative models

Sembolini, Federico; Elahi, Pascal J.; Pearce, Frazer R.; Power, Chris; Knebe, Alexander; Kay, Scott T.; Cui, Weiguang; Yepes, Gustavo; Beck, Alexander M.; Borgani, S.; Cunnama, Daniel; Davé, Romeel; February, Sean; Huang, Shuiyao; Katz, Neal; McCarthy, Ian G.; Murante, Giuseppe; Newton, Richard; Perret, V.; Puchwein, Ewald; Saro, A.; Schaye, Joop; Teyssier, Romain

doi:10.1093/mnras/stw800

Cited by 52 publications

(42 citation statements)

References 137 publications

(171 reference statements)

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“…In Section 3, we introduced the different hot gas profiles necessary to estimate the hydrostatic mass profile of a cluster. Comparing the results from the different runs, it was found that at low mass (8 × 10 13 < M 500,true [M ] < 3 × 10 14 ) the impact of the subgrid physics was greater than the effects of changing the SPH flavour (as was also reported by Sembolini et al 2016b). However, when moving to the most massive clusters (M 500,true 10 15 M ), the effect of changing the SPH flavour can be seen in the cluster cores, whereas there is less of an effect from changing the subgrid physics as the cluster potentials are too deep.…”

Section: Hydrostatic Mass Biassupporting

confidence: 54%

“…• Within the fitting region (0.15 − 1.5 r 500,true ), the CELR-B and CELR-E density, temperature and pressure profiles ( Fig.s 5-7 respectively) become more comparable as the mass of the clusters increases. This shows how differences in the subgrid models are more important at low mass (Sembolini et al 2016b). The effect of changing the SPH flavour (specifically the inclusion of artificial conduction) is most evident in the cores of the most massive clus-ters, shown by the median profiles in Section 3.…”

Section: Summary and Future Workmentioning

confidence: 85%

“…Therefore, there is less energy available for AGN feedback events in the EAGLE model runs so less gas is removed from the centre of the clusters compared to CELR-B at this resolution. indistinguishable at high mass showing how changes in the subgrid physics are more evident at low mass (Sembolini et al 2016b).…”

Section: Summary and Future Workmentioning

confidence: 99%

“…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%

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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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Section: Hydrostatic Mass Biassupporting

confidence: 54%

Section: Summary and Future Workmentioning

confidence: 85%

Section: Summary and Future Workmentioning

confidence: 99%

Section: Bahamas Runsmentioning

confidence: 99%

See 2 more Smart Citations

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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“…However, an important caveat is that predictions of current simulations are often sensitive to the details of the 'sub-grid' modelling of important feedback processes Sembolini et al 2016;McCarthy et al 2016), as we will demonstrate here as well. Therefore, continual confrontation of the simulations with the observations (via production of realistic synthetic observations of the simulations) is also needed to test the realism of the former.…”

mentioning

confidence: 69%

The scatter and evolution of the global hot gas properties of simulated galaxy cluster populations

Brun

McCarthy

Schaye

et al. 2016

Mon. Not. R. Astron. Soc.

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We use the cosmo-OWLS suite of cosmological hydrodynamical simulations to investigate the scatter and evolution of the global hot gas properties of large simulated populations of galaxy groups and clusters. Our aim is to compare the predictions of different physical models and to explore the extent to which commonly-adopted assumptions in observational analyses (e.g. self-similar evolution) are violated. We examine the relations between (true) halo mass and the X-ray temperature, X-ray luminosity, gas mass, Sunyaev-Zel'dovich (SZ) flux, the X-ray analogue of the SZ flux (Y X ) and the hydrostatic mass. For the most realistic models, which include AGN feedback, the slopes of the various mass-observable relations deviate substantially from the self-similar ones, particularly at late times and for low-mass clusters. The amplitude of the mass-temperature relation shows negative evolution with respect to the self-similar prediction (i.e. slower than the prediction) for all models, driven by an increase in non-thermal pressure support at higher redshifts. The AGN models predict strong positive evolution of the gas mass fractions at low halo masses. The SZ flux and Y X show positive evolution with respect to self-similarity at low mass but negative evolution at high mass. The scatter about the relations is well approximated by log-normal distributions, with widths that depend mildly on halo mass. The scatter decreases significantly with increasing redshift. The exception is the hydrostatic masshalo mass relation, for which the scatter increases with redshift. Finally, we discuss the relative merits of various hot gas-based mass proxies.

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