Constraints from thermal Sunyaev-Zel’dovich cluster counts and power spectrum combined with CMB

Salvati, L.; Douspis, M.; Aghanim, N.

doi:10.1051/0004-6361/201731990

Cited by 130 publications

(143 citation statements)

References 57 publications

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“…This is lower than that from the joint analysis of the tSZ and CMB including CMB lensing, B = 1.64 ± 0.19. 4 On the other hand, our result is consistent with the value expected from cosmological hydrodynamical simulations, B = 1.28 ± 0.20 (Shi et al 2016) and also with that estimated from weak lensing mass, B = 1.25 ± 0.13 (Salvati et al 2018 and references therein; see also Miyatake et al 2019;Stern et al 2019;Dietrich et al 2019 for recent attempts).…”

Section: Resultssupporting

confidence: 91%

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

Makiya

Hikage

Komatsu

2020

Publications of the Astronomical Society of Japan

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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 ≈ 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 P lanck 500c = M true 500c /B. Since the power spectrum of the cosmic weak lensing shear is also sensitive to the amplitude of matter density fluctuations via S 8 ≡ σ 8 Ω α m with α ∼ 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±0.20, or (1 − b) = B −1 = 0.73 ± 0.11 (68% C.L.), for σ 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 ± 0.19, but is consistent with the mass bias expected from hydrodynamical simulations, B = 1.28±0.20. Our results thus indicate that the mass bias can be explained mostly by 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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Section: Resultssupporting

confidence: 91%

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

Makiya

Hikage

Komatsu

2020

Publications of the Astronomical Society of Japan

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“…There is an additional connection of these high-redshift BCGs to galaxy clusters -one that could help ameliorate tension in the determination of cosmological parameters. Specifically, the value of the density fluctuation power spectrum amplitude, σ 8 , derived from galaxy cluster counts is known to disagree at ∼ 2σ with the value derived from the cosmic microwave background in the Planck mission (Planck Collaboration XX 2014;Douspis et al 2018;Salvati et al 2018). The number of massive clusters is highly sensitive to σ 8 and we expect these BCGs to preferentially exist in those clusters.…”

Section: Stellar Assembly and Growthmentioning

confidence: 99%

Rapid early coeval star formation and assembly of the most-massive galaxies in the Universe

Rennehan

Babul

Hayward

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The current consensus on the formation and evolution of the brightest cluster galaxies is that their stellar mass forms early (z 4) in separate galaxies that then eventually assemble the main structure at late times (z 1). However, advances in observational techniques have led to the discovery of protoclusters out to z ∼ 7, suggesting that the late-assembly picture may not be fully complete. Using a combination of observationally constrained hydrodynamical and dark-matter-only simulations, we show that the stellar assembly time of a sub-set of brightest cluster galaxies occurs at high redshifts (z > 3) rather than at low redshifts (z < 1), as is commonly though. We find that highly overdense protoclusters assemble their stellar mass into brightest cluster galaxies within ∼ 1 Gyr of evolution -producing massive blue elliptical galaxies at high redshifts (z 3). We argue that there is a downsizing effect on the cluster scale wherein the brightest cluster galaxies in the cores of the most-massive clusters assemble earlier than those in lower-mass clusters. The James Webb Space Telescope will be able to detect and confirm our prediction in the near future, and we discuss the implications to constraining the value of σ 8 .

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“…Although the aim of this paper is to chart a way towards the characterisation and mitigation of the impact of baryons on the matter power spectrum, it should be noted that measurements of the SZ effects hold a great deal of cosmological information themselves [e.g., [170][171][172][173][174][175][176]. Joint analyses of weak lensing, SZ effects, and their cross-correlation have the potential to yield greatly improved constraints on both cosmological and baryonic parameters.…”

Section: Cross-correlations With the Large-scale Structurementioning

confidence: 99%

Modelling baryonic feedback for survey cosmology

Chisari¹,

Mead²,

Joudaki³

et al. 2019

TheOJA

162

122

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Observational cosmology in the next decade will rely on probes of the distribution of matter in the redshift range between 0 < z < 3 to elucidate the nature of dark matter and dark energy. In this redshift range, galaxy formation is known to have a significant impact on observables such as two-point correlations of galaxy shapes and positions, altering their amplitude and scale dependence beyond the expected statistical uncertainty of upcoming experiments at separations under 10 Mpc. Successful extraction of information in such a regime thus requires, at the very least, unbiased models for the impact of galaxy formation on the matter distribution, and can benefit from complementary observational priors. This work reviews the current state of the art in the modelling of baryons for cosmology, from numerical methods to approximate analytical prescriptions, and makes recommendations for studies in the next decade, including a discussion of potential probe combinations that can help constrain the role of baryons in cosmological studies. We focus, in particular, on the modelling of the matter power spectrum, P(k, z), as a function of scale and redshift, and of the observables derived from this quantity. This work is the result of a workshop held at the University of Oxford in November of 2018.

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Constraints from thermal Sunyaev-Zel’dovich cluster counts and power spectrum combined with CMB

Cited by 130 publications

References 57 publications

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

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

Rapid early coeval star formation and assembly of the most-massive galaxies in the Universe

Modelling baryonic feedback for survey cosmology

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