Constraining cosmological parameters using Sunyaev-Zel’dovich cluster surveys

Battye, Richard A.; Weller, J.

doi:10.1103/physrevd.68.083506

Cited by 124 publications

(168 citation statements)

References 102 publications

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“…The Jenkins et al mass function was derived from numerical simulations, and its self-similar form is demonstrated to be accurate to within ∼ 15% in three widely separated cosmologies (although see [27] who find a more significant cosmologydependence of the mass function). Jenkins et al identify simulated clusters using M 180 , the mass enclosed within a spherical overdensity of 180 with respect to the mean matter density.…”

Section: A Simulating Cluster Surveysmentioning

confidence: 99%

Constraining the evolution of dark energy with a combination of galaxy cluster observables

et al. 2004

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We show that the abundance and redshift distribution (dN/dz) of galaxy clusters in future highyield cluster surveys, combined with the spatial power spectrum (Pc(k)) of the same clusters, can place significant constraints on the evolution of the dark energy equation of state, w = w(a). We evaluate the expected errors on wa = −dw/da and other cosmological parameters using a Fisher matrix approach, and simultaneously including cluster structure evolution parameters in our analysis. We study three different types of forthcoming surveys that will identify clusters based on their X-ray emission (such as DUO, the Dark Universe Observatory), their Sunyaev-Zel'dovich (SZ) decrement (such as SPT, the South Pole Telescope), or their weak lensing (WL) shear (such as LSST, the Large Synoptic Survey Telescope). We find that combining the cluster abundance and power spectrum significantly enhances constraints from either method alone. We show that the weak-lensing survey can deliver a constraint as tight as ∆wa ∼ 0.1 on the evolution of the dark energy equation of state, and that the X-ray and SZ surveys each yield ∆wa ∼ 0.4 separately, or ∆wa ∼ 0.2 when these two surveys are combined. For the X-ray and SZ surveys, constraints on dark energy parameters are improved by a factor of two by combining the cluster data with cosmic microwave background (CMB) anisotropy measurements by Planck, but degrade by a factor of two if the survey is required to solve simultaneously for cosmological and cluster structure evolution parameters. The constraint on wa from the weak lensing survey is improved by ∼ 25% with the addition of Planck data.

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Section: A Simulating Cluster Surveysmentioning

confidence: 99%

Constraining the evolution of dark energy with a combination of galaxy cluster observables

et al. 2004

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“…The cluster distribution basically traces scales that have not yet undergone the non-linear phase of gravitationally clustering, thus simplifying their connections to the initial conditions of cosmic structure formation. In the last decade many authors have been involved in this kind of studies and have found that the main features of the large scale structures (formation epoch, shape etc) can potentially affected by the dark energy [21,22,23,24,25,26,27,28,33,34,35,36,37,38,39,40].…”

Section: Introductionmentioning

confidence: 99%

Spherical collapse model and cluster formation beyond theΛcosmology: Indications for a clustered dark energy?

2009

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We generalize the small scale dynamics of the universe by taking into account models with an equation of state which evolves with time, and provide a complete formulation of the cluster virialization attempting to address the nonlinear regime of structure formation. In the context of the current dark energy models, we find that galaxy clusters appear to form at z ∼ 1 − 2, in agreement with previous studies. Also, we investigate thoroughly the evolution of spherical matter perturbations, as the latter decouple from the background expansion and start to "turn around" and finally collapse. Within this framework, we find that the concentration parameter depends on the choice of the considered dark energy (homogeneous or clustered). In particular, if the distribution of the dark energy is clustered then we produce more concentrated structures with respect to the homogeneous dark energy. Finally, comparing the predicted concentration parameter with the observed concentration parameter, measured for four massive galaxy clusters, we find that the scenario which contains a pure homogeneous dark energy is unable to reproduce the data. The situation becomes somewhat better in the case of an inhomogeneous (clustered) dark energy.PACS numbers: 98.80.-k, 95.35.+d, 95.36.+x

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“…III 2013) and from numerical simulations (Springel et al 2001;da Silva et al 2004;Motl et al 2005;Kay et al 2012) suggests that the SZ effect is an excellent mass proxy. A number of articles have discussed the possibility of using SZ-selected cluster samples to constrain cosmological parameters (Barbosa et al 1996;Aghanim et al 1997;Haiman et al 2001;Holder et al 2001;Weller et al 2002;Diego et al 2002;Battye & Weller 2003).…”

Section: Introductionmentioning

confidence: 99%

Planck2013 results. XX. Cosmology from Sunyaev–Zeldovich cluster counts

Ade¹,

Aghanim²,

Arnaud³

et al. 2014

A&A

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We present constraints on cosmological parameters using number counts as a function of redshift for a sub-sample of 189 galaxy clusters from the Planck SZ (PSZ) catalogue. The PSZ is selected through the signature of the Sunyaev-Zeldovich (SZ) effect, and the sub-sample used here has a signal-to-noise threshold of seven, with each object confirmed as a cluster and all but one with a redshift estimate. We discuss the completeness of the sample and our construction of a likelihood analysis. Using a relation between mass M and SZ signal Y calibrated to X-ray measurements, we derive constraints on the power spectrum amplitude σ 8 and matter density parameter Ω m in a flat ΛCDM model. We test the robustness of our estimates and find that possible biases in the Y-M relation and the halo mass function are larger than the statistical uncertainties from the cluster sample. Assuming the X-ray determined mass to be biased low relative to the true mass by between zero and 30%, motivated by comparison of the observed mass scaling relations to those from a set of numerical simulations, we find that σ 8 = 0.75 ± 0.03, Ω m = 0.29 ± 0.02, and σ 8 (Ω m /0.27) 0.3 = 0.764 ± 0.025. The value of σ 8 is degenerate with the mass bias; if the latter is fixed to a value of 20% (the central value from numerical simulations) we find σ 8 (Ω m /0.27) 0.3 = 0.78 ± 0.01 and a tighter one-dimensional range σ 8 = 0.77 ± 0.02. We find that the larger values of σ 8 and Ω m preferred by Planck's measurements of the primary CMB anisotropies can be accommodated by a mass bias of about 40%. Alternatively, consistency with the primary CMB constraints can be achieved by inclusion of processes that suppress power on small scales relative to the ΛCDM model, such as a component of massive neutrinos. We place our results in the context of other determinations of cosmological parameters, and discuss issues that need to be resolved in order to make further progress in this field.

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Constraining cosmological parameters using Sunyaev-Zel’dovich cluster surveys

Cited by 124 publications

References 102 publications

Constraining the evolution of dark energy with a combination of galaxy cluster observables

Constraining the evolution of dark energy with a combination of galaxy cluster observables

Spherical collapse model and cluster formation beyond theΛcosmology: Indications for a clustered dark energy?

Planck2013 results. XX. Cosmology from Sunyaev–Zeldovich cluster counts

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