The Galaxy Cluster Mass Scale and Its Impact on Cosmological Constraints from the Cluster Population

Pratt, G. W.; Arnaud, M.; Biviano, A.; Eckert, D.; Ettori, S.; Nagai, Daisuke; Okabe, Nobuhiko; Reiprich, T. H.

doi:10.1007/s11214-019-0591-0

Cited by 228 publications

(210 citation statements)

References 414 publications

(552 reference statements)

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“…Under the HE assumption non-thermal pressure and large-scale gas motions are neglected in the Euler equation (see e.g. the discussion in §2.3 of Pratt et al 2019). However, in massive systems in the process of assembly, there is no a priori reason to assume that simplifying assumption to hold.…”

Section: Influence Of Hydrostatic Biasmentioning

confidence: 99%

The impact of the observed baryon distribution in haloes on the total matter power spectrum

Debackere

Schaye

Hoekstra

2019

Monthly Notices of the Royal Astronomical Society

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The interpretation of upcoming weak gravitational lensing surveys depends critically on our understanding of the matter power spectrum on scales k < 10 h Mpc −1 , where baryonic processes are important. In this paper we study the impact of gas flows associated with galaxy formation on the matter power spectrum using a halo model that treats the stars and gas separately from the dark matter distribution. The baryonic components are constrained empirically: the hot gas using fits to X-ray observations of groups and clusters of galaxies, and the stellar component using a halo occupation distribution. Since X-ray observations cannot generally measure the hot gas content outside r 500c , we vary the gas density profiles beyond this radius. Compared with dark matter only models, we find a total power suppression of 1 % (5 %) on scales 0.2 − 1 h Mpc −1 (0.5 − 2 h Mpc −1 ), where lower baryon fractions result in stronger suppression. We show that groups of galaxies (10 13 < m 500c /(h −1 M ) < 10 14 ) dominate the total power at all scales k 10 h Mpc −1 . We illustrate the importance of measuring accurate halo masses by comparing models that do and do not account for a hydrostatic bias of 1−b = 0.7 in the halo masses from X-ray observations. We find that using biased halo masses results in an underestimation of the power suppression of up to 4 % at k = 1 h Mpc −1 . Contrary to work based on hydrodynamical simulations, our conclusion that baryonic effects can no longer be neglected is not subject to uncertainties associated with our poor understanding of feedback processes. Our findings highlight the need for observations to probe the outskirts of groups and clusters since these observations are the most constraining for the power suppression on scales k 1 h Mpc −1 .

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Section: Influence Of Hydrostatic Biasmentioning

confidence: 99%

The impact of the observed baryon distribution in haloes on the total matter power spectrum

Debackere

Schaye

Hoekstra

2019

Monthly Notices of the Royal Astronomical Society

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“…However, the scaling relations between a cluster's mass and its SZ signal are not very well determined, and usually they need to be calibrated for each survey. This determination of cluster masses currently provides the largest source of uncertainty when obtaining cosmological information from galaxy clusters (Planck 2015Results XXIV 2016Pratt et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Cosmological constraints from Planck galaxy clusters with CMB lensing mass bias calibration

Zubeldia

Challinor

2019

Monthly Notices of the Royal Astronomical Society

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We present a new cosmological analysis of the galaxy clusters in the Planck MMF3 cosmology sample with a cosmic microwave background (CMB) lensing calibration of the cluster masses. As demonstrated by Planck, galaxy clusters detected via the Sunyaev-Zel'dovich (SZ) effect offer a powerful way to constrain cosmological parameters such as Ω m and σ 8 . Determining the absolute cluster mass scale is, however, difficult, and some recent calibrations have yielded cosmological constraints in apparent tension with constraints in the ΛCDM model derived from the power spectra of the primary CMB anisotropies. In order to calibrate the absolute mass scale of the full Planck cluster sample, we remeasure the masses of all 433 clusters through their weak lensing signature in the CMB temperature anisotropies as measured by Planck. We perform a joint Bayesian analysis of the cluster counts and masses taking as input the estimated cluster masses, SZ signal-to-noise ratios, and redshifts. Our analysis properly accounts for selection effects in the construction of the cluster sample. We find σ 8 (Ω m /0.33) 0.25 = 0.765 ± 0.035 and 1 − b SZ = 0.71 ± 0.10, where the mass bias factor 1 − b SZ relates cluster mass to the SZ mass that appears in the X-ray-calibrated cluster scaling relations. We find no evidence for tension with the Planck primary CMB constraints on ΛCDM model parameters.

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“…Non-thermal pressure in the outer part of galaxy clusters has not yet been observed directly, and thus the cluster mass estimates based on the HSE assumption remain uncertain or inaccurate (e.g., Nagai et al 2007a;Lau et al 2009Lau et al , 2013Suto et al 2013;Nelson et al 2014a;Shi et al 2016;Biffi et al 2016;Henson et al 2017). It is important to understand the origin and the contribution of non-thermal pressure in the next decade when large cosmological surveys are conducted; inaccurate cluster masses may lead to biased inference of cosmological parameters (Pratt et al 2019, for a recent review).…”

Section: Introductionmentioning

confidence: 99%

Cross-correlation of the thermal Sunyaev–Zel’dovich effect and weak gravitational lensing: Planck and Subaru Hyper Suprime-Cam first-year data

Osato

Shirasaki

Miyatake

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Cross-correlation analysis of the thermal Sunyaev-Zel'dovich (tSZ) effect and weak gravitational lensing (WL) provides a powerful probe of cosmology and astrophysics of the intra-cluster medium. We present the measurement of the cross-correlation of tSZ and WL from Planck and Subaru Hyper-Suprime Cam. The combination enables us to study cluster astrophysics at high redshift. We use the tSZ-WL cross-correlation and the tSZ auto-power spectrum measurements to place a tight constraint on the hydrostatic mass bias, which is a measure of the degree of non-thermal pressure support in galaxy clusters. With the prior on cosmological parameters derived from the analysis of the cosmic microwave background anisotropies by Planck and taking into account foreground contributions both in the tSZ auto-power spectrum and the tSZ-WL crosscorrelation, the hydrostatic mass bias is estimated to be 26.9 +8.9 −4.4 % (68% C.L.), which is consistent with recent measurements by mass calibration techniques.

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The Galaxy Cluster Mass Scale and Its Impact on Cosmological Constraints from the Cluster Population

Cited by 228 publications

References 414 publications

The impact of the observed baryon distribution in haloes on the total matter power spectrum

The impact of the observed baryon distribution in haloes on the total matter power spectrum

Cosmological constraints from Planck galaxy clusters with CMB lensing mass bias calibration

Cross-correlation of the thermal Sunyaev–Zel’dovich effect and weak gravitational lensing: Planck and Subaru Hyper Suprime-Cam first-year data

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