The baryon content of groups and clusters of galaxies in the FABLE simulations

Henden, Nicholas A.; Puchwein, Ewald; Sijacki, Debora

doi:10.1093/mnras/staa2235

Cited by 48 publications

(50 citation statements)

References 190 publications

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“…From the figure, we see that our simulations tend to have overly massive BCGs with respect to observational data (a factor of two at M 500 = 3 × 10 14 M ), in line with the findings of other groups (e.g. Bahé et al 2017;Pillepich et al 2018;Henden et al 2020). Moreover, current simulations have more massive BCGs than the LR simulations from Ragone-Figueroa et al (2018, orange line in the plot), being a factor of 2.3 more massive at M 500 = 3 × 10 14 M .…”

Section: Bcg − M 500 Correlationsupporting

confidence: 92%

“…The main difference is around 10 10 M , where simulations have too many galaxies. As noted by Henden et al (2020), larger values of the softening length numerically decrease the number of galaxies at these masses. However, an investigation of the stellar feedback will be needed to better describe the GSMF at our low-mass end.…”

Section: Galaxy Stellar Mass Functionmentioning

confidence: 56%

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The DIANOGA simulations of galaxy clusters: characterising star formation in protoclusters

Bassini

Rasia

Borgani

et al. 2020

A&A

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Aims. We studied the star formation rate (SFR) in cosmological hydrodynamical simulations of galaxy (proto-)clusters in the redshift range 0 < z < 4, comparing them to recent observational studies; we also investigated the effect of varying the parameters of the star formation model on galaxy properties such as SFR, star-formation efficiency, and gas fraction. Methods. We analyse a set of zoom-in cosmological hydrodynamical simulations centred on 12 clusters. The simulations are carried out with the GADGET-3 Tree-PM smoothed-particle hydro-dynamics code which includes various subgrid models to treat unresolved baryonic physics, including AGN feedback. Results. Simulations do not reproduce the high values of SFR observed within protocluster cores, where the values of SFR are underpredicted by a factor ≳4 both at z ∼ 2 and z ∼ 4. The difference arises as simulations are unable to reproduce the observed starburst population and is greater at z ∼ 2 because simulations underpredict the normalisation of the main sequence (MS) of star forming galaxies (i.e. the correlation between stellar mass and SFR) by a factor of ∼3. As the low normalisation of the MS seems to be driven by an underestimated gas fraction, it remains unclear whether numerical simulations miss starburst galaxies due to overly underpredicted gas fractions or overly low star formation efficiencies. Our results are stable against varying several parameters of the star formation subgrid model and do not depend on the details of AGN feedback. Conclusions. The subgrid model for star formation, introduced to reproduce the self-regulated evolution of quiescent galaxies, is not suitable to describe violent events like high-redshift starbursts. We find that this conclusion holds, independently of the parameter choice for the star formation and AGN models. The increasing number of multi-wavelength high-redshift observations will help to improve the current star formation model, which is needed to fully recover the observed star formation history of galaxy clusters.

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Section: Bcg − M 500 Correlationsupporting

confidence: 92%

Section: Galaxy Stellar Mass Functionmentioning

confidence: 56%

The DIANOGA simulations of galaxy clusters: characterising star formation in protoclusters

Bassini

Rasia

Borgani

et al. 2020

A&A

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“…Gas depletion can be easily understood by analogy with the case of clusters of galaxies (e.g. Kravtsov et al 2005;Puchwein et al 2008;Planelles et al 2013;Le Brun et al 2014;Barnes et al 2017;McCarthy et al 2017;Chiu et al 2018;Henden et al 2020, and references therein). In these structures, the decrease of the gas fraction is due to the conversion of gas into stars (that lowers the gas fraction and enhances the stellar one), and the ejection of gas due to feedback events (which displace, disperse, and redistribute the gas, e.g.…”

Section: Analysis Of the Gas Depletion At R < R Intmentioning

confidence: 99%

Properties of gas phases around cosmic filaments atz= 0 in the IllustrisTNG simulation

Galárraga-Espinosa

Aghanim

Langer

et al. 2021

A&A

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We present the study of gas phases around cosmic-web filaments detected in the TNG300-1 hydro-dynamical simulation at redshift z = 0. We separate the gas into five different phases according to temperature and density. We show that filaments are essentially dominated by gas in the warm-hot intergalactic medium (WHIM), which accounts for more than 80% of the baryon budget at r ∼ 1 Mpc. Apart from WHIM gas, cores of filaments (r ≤ 1 Mpc) also host large contributions from other hotter and denser gas phases, whose fractions depend on the filament population. By building temperature and pressure profiles, we find that gas in filaments is isothermal up to r ∼ 1.5 Mpc, with average temperatures of Tcore = 4−13 × 105 K, depending on the large-scale environment. Pressure at cores of filaments is on average Pcore = 4−12 × 10−7 keV.cm−3, which is ∼1000 times lower than pressure measured in observed clusters. We also estimate that the observed Sunyaev-Zel’dovich signal from cores of filaments should range between 0.5 < y < 4.1 × 10−8, and these results are compared with recent observations. Our findings show that the state of the gas in filaments depends on the presence of haloes and on the large-scale environment.

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“…For massive clusters of galaxies, whose internal dynamics are dominated by gravity, the mass of the intracluster medium (ICM) correlates tightly with total mass (Borgani & Kravtsov 2011, and refer-2014Barnes et al 2017;Henden et al 2020;Singh et al 2020). Precise measurements of 5 gas from X-ray data thus provide a route to constraining cosmological models, and, in combination with external information on b , have provided some of the earliest and most robust constraints on the cosmic matter density, m (White et al 1993;David et al 1995;White & Fabian 1995;Evrard 1997;Ettori & Fabian 1999;Mohr et al 1999;Allen et al 2002;Ettori et al 2003).…”

Section: Introductionmentioning

confidence: 99%

Cosmological constraints from gas mass fractions of massive, relaxed galaxy clusters

Mantz

Morris

Allen

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present updated cosmological constraints from measurements of the gas mass fractions (fgas) of massive, dynamically relaxed galaxy clusters. Our new data set has greater leverage on models of dark energy, thanks to the addition of the Perseus Cluster at low redshifts, two new clusters at redshifts z ≳ 1, and significantly longer observations of four clusters at 0.6 < z < 0.9. Our low-redshift (z < 0.16) fgas data, combined with the cosmic baryon fraction measured from the cosmic microwave background (CMB), imply a Hubble constant of h = 0.722 ± 0.067. Combining the full fgas data set with priors on the cosmic baryon density and the Hubble constant, we constrain the dark energy density to be ΩΛ = 0.865 ± 0.119 in non-flat ΛCDM (cosmological constant) models, and its equation of state to be $w=-1.13_{-0.20}^{+0.17}$ in flat, constant-w models, respectively 41 and 29 per cent tighter than our previous work, and comparable to the best constraints available from other probes. Combining fgas, CMB, supernova, and baryon acoustic oscillation data, we also constrain models with global curvature and evolving dark energy. For the massive, relaxed clusters employed here, we find the scaling of fgas with mass to be consistent with a constant, with an intrinsic scatter that corresponds to just ∼3 per cent in distance.

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The baryon content of groups and clusters of galaxies in the FABLE simulations

Cited by 48 publications

References 190 publications

The DIANOGA simulations of galaxy clusters: characterising star formation in protoclusters

The DIANOGA simulations of galaxy clusters: characterising star formation in protoclusters

Properties of gas phases around cosmic filaments atz= 0 in the IllustrisTNG simulation

Cosmological constraints from gas mass fractions of massive, relaxed galaxy clusters

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