The velocity of clusters of galaxies relative to the microwave background. The possibility of its measurement

Sunyaev, R.; Zel’dovich, Ya. B.

doi:10.1093/mnras/190.3.413

Cited by 582 publications

(461 citation statements)

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“…We consider the effects of and ways to mitigate astrophysical signals contaminating the CMB map required as input for reconstruction of the gravitational potential. The most difficult in this context are signals generated by the cluster itself, such as the thermal SZ (tSZ, Sunyaev & Zeldovich 1972) and the kinetic SZ (kSZ, Sunyaev & Zeldovich 1980) effects. Component separation is therefore a crucial step prior to reconstruction of the potential, and our study will demonstrate the importance of multi-frequency observations in this context.…”

Section: Introductionmentioning

confidence: 99%

Measuring cluster masses with CMB lensing: a statistical approach

Melin

Bartlett

2015

A&A

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We present a method for measuring the masses of galaxy clusters using the imprint of their gravitational lensing signal on the cosmic microwave background (CMB) temperature anisotropies. The method first reconstructs the projected gravitational potential with a quadratic estimator and then applies a matched filter to extract cluster mass. The approach is well-suited for statistical analyses that bin clusters according to other mass proxies. We find that current experiments, such as Planck, the South Pole Telescope and the Atacama Cosmology Telescope, can practically implement such a statistical methodology, and that future experiments will reach sensitivities sufficient for individual measurements of massive systems. As illustration, we use simulations of Planck observations to demonstrate that it is possible to constrain the mass scale of a set of 62 massive clusters with prior information from X-ray observations, similar to the published Planck ESZ-XMM sample. We examine the effect of the thermal (tSZ) and kinetic (kSZ) Sunyaev-Zeldovich (SZ) signals, finding that the impact of the kSZ remains small in this context. The stronger tSZ signal, however, must be actively removed from the CMB maps by component separation techniques prior to reconstruction of the gravitational potential. Our study of two such methods highlights the importance of broad frequency coverage for this purpose. A companion paper presents application to the Planck data on the ESZ-XMM sample.

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Section: Introductionmentioning

confidence: 99%

Measuring cluster masses with CMB lensing: a statistical approach

Melin

Bartlett

2015

A&A

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“…CMB temperature fluctuations are not just sourced by density fluctuations at the last scattering surface; * Electronic address: npadmana@princeton.edu anisotropies also arise due to the interaction of photons with hot electrons in galaxies and clusters (the SunyaevZeldovich [SZ,2] and kinetic-SZ [3] effects), as well as with the gravitational potentials along their propagation path (the Integrated Sachs-Wolfe [ISW,4] effect and gravitational lensing).…”

Section: Introductionmentioning

confidence: 99%

Correlating the CMB with luminous red galaxies: The integrated Sachs-Wolfe effect

et al. 2005

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We present a 2.5σ detection of the Integrated Sachs-Wolfe (ISW) effect and discuss the constraints it places on cosmological parameters. We cross-correlate microwave temperature maps from the WMAP satellite with a 4000 deg 2 luminous red galaxy (LRG) overdensity map measured by the Sloan Digital Sky Survey. These galaxies have accurate photometric redshifts (∆z ∼ 0.03) and an approximately volume limited redshift distribution from z ∼ 0.2 to z ∼ 0.6 well suited to detecting the ISW effect. Accurate photometric redshifts allow us to perform a reliable auto-correlation analysis of the LRGs, eliminating the uncertainty in the galaxy bias, and combined with cross correlation signal, constrains cosmological parameters -in particular, the matter density. We use a minimum variance power spectrum estimator that optimally weights the data according to expected theoretical templates. We find a 2.5σ signal in the Ka, Q, V, and W WMAP bands, after combining the information from multipoles 2 ≤ l < 400. This is consistent with the expected amplitude of the ISW effect, but requires a lower matter density than is usually assumed: the amplitude, parametrized by the galaxy bias assuming ΩM = 0.3, ΩΛ = 0.7 and σ8 = 0.9, is bg = 4.05 ± 1.54 for V band, with similar results for the other bands. This should be compared to bg = 1.82 ± 0.02 from the auto-correlation analysis. These data provide only a weak confirmation (2.5σ) of dark energy, but provide a significant upper limit: ΩΛ = 0.80 +0.03 −0.06 (1σ) +0.05 −0.19 (2σ), assuming a cosmology with ΩM + ΩΛ = 1, Ω b = 0.05, and σ8 = 0.9, and w = −1. The weak cross-correlation signal rules out low matter density/high dark energy density universes and, in combination with other data, strongly constrains models with w < −1.3. We provide a simple prescription to incorporate these constraints into cosmological parameter estimation methods for (ΩM , σ8, w). We find no evidence for a systematic contamination of ISW signal, either from Galactic or extragalactic sources, but we do detect some large statistical fluctuations on smaller scales that could affect analyses without the template weighting.

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“…When relative motions between free electrons and photons exist, the inverse Compton scattering will induce a shift of the brightness temperature of CMB photons via the kSZ effect [21,22]. This temperature shift will be anisotropic on our sky tracing the anisotropy of the projected free electron surface density.…”

Section: The Kinetic Sunyaev Zel'dovich Testmentioning

confidence: 99%

Confirmation of the Copernican principle through the anisotropic kinetic Sunyaev Zel'dovich effect

Zhang

Stebbins

2011

Phil. Trans. R. Soc. A.

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The Copernican principle remains largely unproven at Gpc radial scale and above. Generally, violations of this type cause a first-order anisotropic kinetic Sunyaev Zel'dovich (kSZ) effect. Here we show that, if large-scale radial inhomogeneities have amplitude large enough to explain the 'dark energy' phenomena, the induced kSZ power spectrum will be orders of magnitude larger than the Atacama cosmology telescope/South Pole telescope upper limit. This single test rules out the void model as the cause of the apparent cosmic acceleration, confirms the Copernican principle on Gpc radial scale and above, and closes a loophole in the standard cosmology.

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The velocity of clusters of galaxies relative to the microwave background. The possibility of its measurement

Cited by 582 publications

References 0 publications

Measuring cluster masses with CMB lensing: a statistical approach

Measuring cluster masses with CMB lensing: a statistical approach

Correlating the CMB with luminous red galaxies: The integrated Sachs-Wolfe effect

Confirmation of the Copernican principle through the anisotropic kinetic Sunyaev Zel'dovich effect

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