The MUSIC of galaxy clusters – II. X-ray global properties and scaling relations

Biffi, V.; Sembolini, Federico; Petris, M. De; Valdarnini, R.; Yepes, Gustavo; Gottlöber, Stefan

doi:10.1093/mnras/stu018

Cited by 50 publications

(72 citation statements)

References 79 publications

(180 reference statements)

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“…The latter authors use the Chandra bolometric band (0.3 − 12 keV), which explains the higher Xray luminosity compared to the MCXC data. In comparison, our clusters evolve along a scaling relation that is somewhat shallower than both Arnaud et al (2010) and Le Brun et al (2014), consistent with Biffi et al (2014) (who however used the larger spectral window) but slightly steeper than a simple self-similar scaling ∝ M 4/3 (shown as a green dashed line in the figure and whose normalisation has been obtained by fitting to the MCXC data). In fact, the best-fit slope in our case is closer to 1.2, but we do not want to make a more quantitative statement at this stage since the comparison of evolving small (autocorrelated) samples should be taken with some caution for making rigorous predictions.…”

Section: X-ray Observablessupporting

confidence: 83%

“…Due to the known biases in estimating temperatures from simulated clusters that reflect temperatures measured from X-ray spectroscopy (see e.g. Biffi et al 2014, for in-depth comparisons), we show a range of differently weighted temperature estimates in the different panels of the figure. First, we compare with the spectroscopic-like temperature as introduced by Mazzotta et al (2004) as…”

Section: X-ray Observablesmentioning

confidence: 99%

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Rhapsody-G simulations I: the cool cores, hot gas and stellar content of massive galaxy clusters

Hahn

Martizzi

et al. 2017

Mon. Not. R. Astron. Soc.

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We present the Rhapsody-G suite of cosmological hydrodynamic AMR zoom simulations of ten massive galaxy clusters at the M vir ∼ 10 15 M scale. These simulations include cooling and sub-resolution models for star formation and stellar and supermassive black hole feedback. The sample is selected to capture the whole gamut of assembly histories that produce clusters of similar final mass. We present an overview of the successes and shortcomings of such simulations in reproducing both the stellar properties of galaxies as well as properties of the hot plasma in clusters. In our simulations, a long-lived cool-core/non-cool core dichotomy arises naturally, and the emergence of non-cool cores is related to low angular momentum major mergers. Nevertheless, the cool-core clusters exhibit a low central entropy compared to observations, which cannot be alleviated by thermal AGN feedback. For cluster scaling relations we find that the simulations match well the M 500 − Y 500 scaling of Planck SZ clusters but deviate somewhat from the observed X-ray luminosity and temperature scaling relations in the sense of being slightly too bright and too cool at fixed mass, respectively. Stars are produced at an efficiency consistent with abundance matching constraints and central galaxies have star formation rates consistent with recent observations. While our simulations thus match various key properties remarkably well, we conclude that the shortcomings strongly suggest an important role for non-thermal processes (through feedback or otherwise) or thermal conduction in shaping the intra-cluster medium.

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Section: X-ray Observablessupporting

confidence: 83%

Section: X-ray Observablesmentioning

confidence: 99%

Rhapsody-G simulations I: the cool cores, hot gas and stellar content of massive galaxy clusters

Hahn

Martizzi

et al. 2017

Mon. Not. R. Astron. Soc.

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“…Biffi et al (2014) and the observational findings ofLovisari et al (2015) (1.67 ± 0.08) andMantz et al (2016b) (1.63 ± 0.04).…”

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confidence: 55%

The redshift evolution of X-ray and Sunyaev–Zel’dovich scaling relations in the fable simulations

Henden

Puchwein

Sijacki

2019

Monthly Notices of the Royal Astronomical Society

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We study the redshift evolution of the X-ray and Sunyaev-Zel'dovich (SZ) scaling relations for galaxy groups and clusters in the fable suite of cosmological hydrodynamical simulations. Using an expanded sample of 27 high-resolution zoom-in simulations, together with a uniformly-sampled cosmological volume to sample low-mass systems, we find very good agreement with the majority of observational constraints up to z ∼ 1. We predict significant deviations of all examined scaling relations from the simple self-similar expectations. While the slopes are approximately independent of redshift, the normalisations evolve positively with respect to self-similarity, even for commonly-used mass proxies such as the Y X parameter. These deviations are due to a combination of factors, including more effective AGN feedback in lower mass haloes, larger binding energy of gas at a given halo mass at higher redshifts and larger nonthermal pressure support from kinetic motions at higher redshifts. Our results have important implications for cluster cosmology from upcoming SZ surveys such as SPT-3G, ACTpol and CMB-S4, as relatively small changes in the observable-mass scaling relations (within theoretical uncertainties) have a large impact on the predicted number of high-redshift clusters and hence on our ability to constrain cosmology using cluster abundances. In addition, we find that the intrinsic scatter of the relations, which agrees well with most observational constraints, increases at lower redshifts and for lower mass systems. This calls for a more complex parametrization than adopted in current observational studies to be able to accurately account for selection biases.

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“…The initial conditions for our zoom simulations were drawn from the MUSIC-2 cluster catalog (Sembolini et al 2013;Sembolini et al 2014;Biffi et al 2014) 1 of re-simulated halos from the MultiDark cosmological simulation 2 . All the data from the parent simulation are accessible online through the MultiDark Database 3 .…”

Section: The Datamentioning

confidence: 99%

nIFTy galaxy cluster simulations – II. Radiative models

Sembolini

Elahi

Pearce

et al. 2016

Mon. Not. R. Astron. Soc.

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We have simulated the formation of a massive galaxy cluster (M crit 200 = 1.1×1015 h −1 M ) in a ΛCDM universe using 10 different codes (RAMSES, 2 incarnations of AREPO and 7 of GADGET), modeling hydrodynamics with full radiative subgrid physics. These codes include Smoothed-Particle Hydrodynamics (SPH), spanning traditional and advanced SPH schemes, adaptive mesh and moving mesh codes. Our goal is to study the consistency between simulated clusters modeled with different radiative physical implementations -such as cooling, star formation and AGN feedback. We compare images of the cluster at z = 0, global properties such as mass, and radial profiles of various dynamical and thermodynamical quantities. We find that, with respect to non-radiative simulations, dark matter is more centrally concentrated, the extent not simply depending on the presence/absence of AGN feedback. The scatter in global quantities is substantially higher than for non-radiative runs. Intriguingly, adding radiative physics seems to have washed away the marked code-based differences present in the entropy profile seen for non-radiative simulations in Sembolini et al. (2015): radiative physics + classic SPH can produce entropy cores. Furthermore, the inclusion/absence of AGN feedback is not the dividing line -as in the case of describing the stellar content-for whether a code produces an unrealistic temperature inversion and a falling central entropy profile. However, AGN feedback does strongly affect the overall stellar distribution, limiting the effect of overcooling and reducing sensibly the stellar fraction.

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The MUSIC of galaxy clusters – II. X-ray global properties and scaling relations

Cited by 50 publications

References 79 publications

Rhapsody-G simulations I: the cool cores, hot gas and stellar content of massive galaxy clusters

Rhapsody-G simulations I: the cool cores, hot gas and stellar content of massive galaxy clusters

The redshift evolution of X-ray and Sunyaev–Zel’dovich scaling relations in the fable simulations

nIFTy galaxy cluster simulations – II. Radiative models

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