Mass bias evolution in tSZ cluster cosmology

Galaxy clusters observed through the thermal Sunyaev–Zeldovich (tSZ) effect are a recent cosmological probe. The precision on the cosmological constraints is affected mainly by the current knowledge of cluster physics, which enters the analysis through the scaling relations. Here we aim to study one of the most important sources of systematic uncertainties, the mass bias, b. We have analysed the effects of a mass-redshift dependence, adopting a power-law parametrisation. We applied this parametrisation to the combination of tSZ number counts and power spectrum, finding a hint of redshift dependence that leads to a decreasing value of the mass bias for higher redshift. We tested the robustness of our results for different mass bias calibrations and a discrete redshift dependence. We find our results to be dependent on the clusters sample that we are considering, in particular obtaining an inverse (decreasing) redshift dependence when neglecting z < 0.2 clusters. We analysed the effects of this parametrisation on the combination of cosmic microwave background (CMB) primary anisotropies and tSZ galaxy clusters. We find a preferred constant value of mass bias, having (1 − b) = 0.62 ± 0.05. The corresponding value of b is too high with respect to weak lensing and numerical simulations estimations. Therefore we conclude that this mass-redshift parametrisation does not help in solving the remaining discrepancy between CMB and tSZ clusters observations.

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New constraints on the mass bias of galaxy clusters from the power spectra of the thermal Sunyaev–Zeldovich effect and cosmic shear

Publications of the Astronomical Society of Japan ◽

10.1093/pasj/psz147 ◽

2020 ◽

Vol 72 (2) ◽

Cited By ~ 3

Author(s):

Ryu Makiya ◽

Chiaki Hikage ◽

Eiichiro Komatsu

Keyword(s):

Power Spectrum ◽

Galaxy Clusters ◽

Cosmological Parameters ◽

Power Spectra ◽

Matter Density ◽

Density Fluctuations ◽

Microwave Background ◽

Mass Bias ◽

Cosmic Shear ◽

Hydrodynamical Simulations

Abstract The thermal Sunyaev–Zeldovich (tSZ) power spectrum is a powerful probe of the present-day amplitude of matter density fluctuations, and has been measured up to $\ell \approx 10^3$ from the Planck data. The largest systematic uncertainty in the interpretation of this data is the so-called “mass bias” parameter B, which relates the true halo mass to the mass proxy used by the Planck team as $M\,_{\rm 500c}^{\rm Planck}=M\,_{\rm 500c}^{\rm true}/B$. Since the power spectrum of the cosmic weak lensing shear is also sensitive to the amplitude of matter density fluctuations via $S_8\equiv \sigma _8 \Omega _{\rm m}^{\alpha }$ with $\alpha \sim 0.5$, we can break the degeneracy between the mass bias and the cosmological parameters by combining the tSZ and cosmic shear power spectra. In this paper, we perform a joint likelihood analysis of the tSZ power spectrum from Planck and the cosmic shear power spectrum from Subaru Hyper Suprime-Cam. Our analysis does not use the primordial cosmic microwave background (CMB) information. We obtain a new constraint on the mass bias as $B = 1.37 ^{+0.15}_{-0.23}$ or $(1-b) = B^{-1}=0.73^{+0.08}_{-0.13}$ ($68\%$ confidence limit), for $\sigma _8 < 0.9$. This value of B is lower than that needed to reconcile the tSZ data with the primordial CMB and CMB lensing data, i.e., $B = 1.64 \pm 0.19$, but is consistent with the mass bias expected from hydrodynamical simulations, $B = 1.28 \pm 0.20$. Thus our results indicate that the mass bias is consistent with the non-thermal pressure support from mass accretion of galaxy clusters via the cosmic structure formation, and that the cosmologies inferred from the tSZ and the cosmic shear are consistent with each other.

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Cluster Physics & Evolution

Proceedings of the International Astronomical Union ◽

10.1017/s1743921316004543 ◽

2015 ◽

Vol 11 (A29B) ◽

pp. 70-78

Author(s):

Daisuke Nagai ◽

Monique Arnaud ◽

Sarthak Dasadia ◽

Michael McDonald ◽

Ikuyuki Mitsuishi ◽

...

Keyword(s):

Galaxy Clusters ◽

Statistical Power ◽

Scaling Relations ◽

Intracluster Medium ◽

Physical Processes ◽

X Ray ◽

Cosmological Constraints ◽

Recent Advances

AbstractRecent advances in X-ray and microwave observations have provided unprecedented insights into the structure and evolution of the hot X-ray emitting plasma from their cores to the virialization region in outskirts of galaxy clusters. Recent Sunyaev-Zel'dovich (SZ) surveys (ACT, Planck, SPT) have provided new cluster catalogs, significantly expanding coverage of the mass-redshift plane, whileChandraandXMM-NewtonX-ray follow-up programs have improved our understanding of cluster physics and evolution as well as the surveys themselves. However, the current cluster-based cosmological constraints are still limited by uncertainties in cluster astrophysics. In order to exploit the statistical power of the current and upcoming X-ray and microwave cluster surveys, it is critical to improve our understanding of the structure and evolution of the hot X-ray emitting intracluster medium (ICM). In this session, we discussed recent advances in observations and simulations of galaxy clusters, with highlights on (i) the evolution of ICM profiles and scaling relations, (ii) physical processes operating in the outskirts of galaxy clusters, and (iii) impact of mergers on the ICM structure in groups and clusters.

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Acoustic Peaks and Dips in the Cosmic Microwave Background Power Spectrum: Observational Data and Cosmological Constraints

The Astrophysical Journal ◽

10.1086/345079 ◽

2003 ◽

Vol 583 (1) ◽

pp. 33-48 ◽

Cited By ~ 29

Author(s):

R. Durrer ◽

B. Novosyadlyj ◽

S. Apunevych

Keyword(s):

Power Spectrum ◽

Cosmic Microwave Background ◽

Observational Data ◽

Microwave Background ◽

Cosmological Constraints

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Exact joint likelihood of pseudo-Cℓ estimates from correlated Gaussian cosmological fields

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz3225 ◽

2019 ◽

Vol 491 (3) ◽

pp. 3165-3181 ◽

Cited By ~ 1

Author(s):

Robin E Upham ◽

Lee Whittaker ◽

Michael L Brown

Keyword(s):

Quadratic Form ◽

Power Spectrum ◽

Quadratic Forms ◽

Joint Distribution ◽

Large Scale ◽

Power Spectra ◽

Microwave Background ◽

Cosmological Constraints ◽

Statistical Precision ◽

Joint Likelihood

ABSTRACT We present the exact joint likelihood of pseudo-Cℓ power spectrum estimates measured from an arbitrary number of Gaussian cosmological fields. Our method is applicable to both spin-0 fields and spin-2 fields, including a mixture of the two, and is relevant to cosmic microwave background (CMB), weak lensing, and galaxy clustering analyses. We show that Gaussian cosmological fields are mixed by a mask in such a way that retains their Gaussianity and derive exact expressions for the covariance of the cut-sky spherical harmonic coefficients, the pseudo-aℓms, without making any assumptions about the mask geometry. We then show that each auto or cross-pseudo-Cℓ estimator can be written as a quadratic form, and apply the known joint distribution of quadratic forms to obtain the exact joint likelihood of a set of pseudo-Cℓ estimates in the presence of an arbitrary mask. We show that the same formalism can be applied to obtain the exact joint likelihood of quadratic maximum likelihood power spectrum estimates. Considering the polarization of the CMB as an example, we show using simulations that our likelihood recovers the full, exact multivariate distribution of EE, BB, and EB pseudo-Cℓ power spectra. Our method provides a route to robust cosmological constraints from future CMB and large-scale structure surveys in an era of ever-increasing statistical precision.

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Scaling relations and mass bias in hydrodynamical f (R) gravity simulations of galaxy clusters

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stu332 ◽

2014 ◽

Vol 440 (1) ◽

pp. 833-842 ◽

Cited By ~ 48

Author(s):

Christian Arnold ◽

Ewald Puchwein ◽

Volker Springel

Keyword(s):

Galaxy Clusters ◽

Scaling Relations ◽

Mass Bias

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Measuring the hydrostatic mass bias in galaxy clusters by combining Sunyaev–Zel’dovich and CMB lensing data

Astronomy and Astrophysics ◽

10.1051/0004-6361/201731999 ◽

2018 ◽

Vol 610 ◽

pp. L4 ◽

Cited By ~ 9

Author(s):

G. Hurier ◽

R. E. Angulo

Keyword(s):

Galaxy Clusters ◽

Cosmological Parameters ◽

Galaxy Cluster ◽

Systematic Errors ◽

Hydrostatic Equilibrium ◽

Microwave Background ◽

Mass Bias ◽

Λcdm Model ◽

Hydrodynamical Simulations ◽

Significant Mass

The cosmological parameters preferred by the cosmic microwave background (CMB) primary anisotropies predict many more galaxy clusters than those that have been detected via the thermal Sunyaev–Zeldovich (tSZ) effect. This discrepancy has attracted considerable attention since it might be evidence of physics beyond the simplest ΛCDM model. However, an accurate and robust calibration of the mass-observable relation for clusters is necessary for the comparison, which has been proven difficult to obtain so far. Here, we present new constraints on the mass–pressure relation by combining tSZ and CMB lensing measurements of optically selected clusters. Consequently, our galaxy cluster sample is independent of the data employed to derive cosmological constrains. We estimate an average hydrostatic mass bias of b = 0.26 ± 0.07, with no significant mass or redshift evolution. This value greatly reduces the discrepancy between the predictions of ΛCDM and the observed abundance of tSZ clusters but agrees with recent estimates from tSZ clustering. On the other hand, our value for b is higher than the predictions from hydrodynamical simulations. This suggests mechanisms that drive large departures from hydrostatic equilibrium and that are not included in the latest simulations, and/or unaccounted systematic errors such as biases in the cluster catalogue that are due to the optical selection.

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Planck 2013 Cosmology Results: a Review

Acta Polytechnica CTU Proceedings ◽

10.14311/app.2014.01.0049 ◽

2014 ◽

Vol 1 (1) ◽

pp. 49-55

Author(s):

José Alberto Rubino-Martín

Keyword(s):

Cosmic Microwave Background ◽

Galaxy Clusters ◽

Cosmological Parameters ◽

Power Spectra ◽

Microwave Background ◽

Statistical Characterization ◽

Number Counts ◽

Cmb Temperature

This talk presents an overview of the cosmological results derived from the first 15.5 months of observations of the ESA’s Planck mission. These cosmological results are mainly based on the Planck measurements of the cosmic microwave background (CMB) temperature and lensing-potential power spectra, although we also briefly discuss other aspects of the Planck data, as the statistical characterization of the reconstructed CMB maps, or the constraints on cosmological parameters using the number counts of galaxy clusters detected by means of the Sunyaev-Zeldovich effect in the Planck maps. All these results are described in detail in a series of papers released by ESA and the Planck collaboration in March 2013.

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The XXL Survey

Astronomy and Astrophysics ◽

10.1051/0004-6361/201833238 ◽

2018 ◽

Vol 620 ◽

pp. A1 ◽

Cited By ~ 6

Author(s):

F. Marulli ◽

A. Veropalumbo ◽

M. Sereno ◽

L. Moscardini ◽

F. Pacaud ◽

...

Keyword(s):

Correlation Function ◽

Galaxy Clusters ◽

Cluster Number ◽

X Ray ◽

Mass Scaling ◽

Cosmological Constraints ◽

Density Peaks ◽

Point Correlation ◽

Point Correlation Function ◽

Number Counts

Context.Galaxy clusters trace the highest density peaks in the large-scale structure of the Universe. Their clustering provides a powerful probe that can be exploited in combination with cluster mass measurements to strengthen the cosmological constraints provided by cluster number counts.Aims.We investigate the spatial properties of a homogeneous sample of X-ray selected galaxy clusters from the XXL survey, the largest programme carried out by theXMM-Newtonsatellite. The measurements are compared to Λ-cold dark matter predictions, and used in combination with self-calibrated mass scaling relations to constrain the effective bias of the sample,beff, and the matter density contrast, ΩM.Methods.We measured the angle-averaged two-point correlation function of the XXL cluster sample. The analysed catalogue consists of 182 X-ray selected clusters from the XXL second data release, with median redshift ⟨z⟩ = 0.317 and median mass ⟨M500⟩≃ 1.3 × 1014M⊙. A Markov chain Monte Carlo analysis is performed to extract cosmological constraints using a likelihood function constructed to be independent of the cluster selection function.Results.Modelling the redshift-space clustering in the scale range 10 <r[h−1Mpc] < 40, we obtain ΩM= 0.27−0.04+0.06andbeff= 2.73−0.20+0.18.This is the first time the two-point correlation function of an X-ray selected cluster catalogue at such relatively high redshifts and low masses has been measured. The XXL cluster clustering appears fully consistent with standard cosmological predictions. The analysis presented in this work demonstrates the feasibility of a cosmological exploitation of the XXL cluster clustering, paving the way for a combined analysis of XXL cluster number counts and clustering.

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Temperature Fluctuations of the Microwave Background in Primeval Isocurvature Baryon Models

Symposium - International Astronomical Union ◽

10.1017/s0074180900110320 ◽

1996 ◽

Vol 168 ◽

pp. 441-444

Author(s):

S. N. Dutta ◽

G. Efstathiou

Keyword(s):

Power Spectrum ◽

Power Law ◽

Large Scale ◽

Temperature Fluctuations ◽

Large Scale Structure ◽

South Pole ◽

Microwave Background ◽

Field Point ◽

Theoretical Predictions ◽

The Universe

We calculate the temperature fluctuations in the microwave background in open primeval isocurvature baryon models (Peebles, 1987) with cosmological densities in the range 0.05 ≤ ω ≤ 0.2 We assume that the power spectrum of fluctuations is a power law with the index varying between – 1 ≤n≤ 0, as indicated by observations of large scale structure in the Universe. The Universe is assumed to be always fully ionized. The South Pole 13 field point experiment (Schusteret al., 1993) is compared to our theoretical predictions, and we find that the models predict larger temperature fluctuations than are observed. The observed temperature fluctuations on intermediate scales of ≲ 1°thus seem difficult to reconcile with the isocurvature baryon model.

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