Fluctuations in the cosmic blackbody radiation due to gas in galaxy clusters

Rephaeli, Yoel

doi:10.1086/158814

Cited by 22 publications

(6 citation statements)

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“…1.3 that is used to describe primordial fluctuations. A number of different assumptions about the cosmology and evolution of large scale structure have been used to calculate the amplitude and angular pattern of the foreground fluctuations (Rephaeli 1981;Cavaliere et al 1986;Cole & Kaiser 1988;Schaeffer & Silk 1988;Thomas & Carlberg 1989;Markevitch et al 1992;Makino & Suto 1993;Bartlett & Silk 1994a, 1994bCeballos & Barcons 1994;Colafrancesco et al 1994; see also the review by Rephaeli 1995b). A uniform result of the calculations is that the distribution of sky brightness fluctuations that result is strongly non-Gaussian and asymmetrical since it is composed of negative or positive sources (depending on the frequency of observation, and the sign of j(x)) with varying numbers of sources on any line of sight or contained in a particular telescope beam (e.g., Markevitch et al 1992).…”

Section: Fluctuations In the Cmbrmentioning

confidence: 99%

The Sunyaev–Zel'dovich effect

1999

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The Sunyaev-Zel'dovich e ect causes a change in the apparent brightness of the Cosmic Microwave Background Radiation towards a cluster of galaxies or any other reservoir of hot plasma. Measurements of the e ect provide distinctly di erent information about cluster properties than X-ray imaging data, while combining X-ray and Sunyaev-Zel'dovich e ect data leads to new insights into the structures of cluster atmospheres. The e ect is redshift-independent, and so provides a unique probe of the structure of the Universe on the largest scales. The present review discusses the theory of the Sunyaev-Zel'dovich e ect and collects published results for many clusters, presents the overall conclusions that may bedrawn from the detections so far, and discusses the prospects for future research on the Sunyaev-Zel'dovich e ects.Subject headings: Sunyaev-Zel'dovich E ect; Clusters; Microwave Background Radiation Astrophysical ContextCompton scattering is one of the major physical processes that couples matter and radiation. Its importance is often stressed in highly relativistic environments where large energy transfers occur: for example, in the synchrotron self-Compton process that may beresponsible for much of the X-radiation from active galactic nuclei (e.g., Fabian et al. 1986). However, the Compton process also has observable consequences in low-energy environments, where small energy transfers occur. The Sunyaev-Zel'dovich e ect, which arises from the scattering of electrons in clusters of galaxies on the cosmic microwave 1 Also Smithsonian Institution Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138, USA { 2 { background radiation eld, is perhaps the most important astrophysical example. The e ect provides a cosmological probe, it has been used to measure the properties of gas in clusters of galaxies, and it has been discussed as a means of measuring the motions of clusters of galaxies and hence studying the evolution of structure in the Universe.The purpose of this review is to provide a comprehensive introduction to the SunyaevZel'dovich e ect. I aim to provide both a theoretical treatment that can befollowed by non-specialists, and an introduction to the observation of the e ect with a critical review of data in the literature. The latter is more di cult today than it would have been ve years ago because of the rapid increase in the number of papers on the Sunyaev-Zel'dovich e ect, and the improvement i n t h e quality o f t h e results that are being gained.

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Section: Fluctuations In the Cmbrmentioning

confidence: 99%

The Sunyaev–Zel'dovich effect

1999

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“…Observations at high multipoles (ℓ ∼ 500 → 2000), where the physics is strongly affected by photon diffusion and the thickness of the last scattering region, provide independent constraints on these fundamental parameters. At even higher multipoles (ℓ > 2000), secondary effects such as the Sunyaev-Zeldovich Effect (SZE;Sunyaev & Zel'dovich 1972) are expected to dominate (Cole & Kaiser 1988;Rephaeli 1981) and hence offer the prospect of studying the formation of large-scale structure at recent times. This paper is one in a series reporting results from the Cosmic Background Imager (CBI).…”

Section: Introductionmentioning

confidence: 99%

The Anisotropy of the Microwave Background tol= 3500: Deep Field Observations with the Cosmic Background Imager

Mason

Pearson

Readhead

et al. 2003

ApJ

265

142

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We report measurements of anisotropy in the cosmic microwave background radiation over the multipole range ℓ ∼ 200 → 3500 with the Cosmic Background Imager based on deep observations of three fields. These results confirm the drop in power with increasing ℓ first reported in earlier measurements with this instrument, and extend the observations of this decline in power out to ℓ ∼ 2000. The decline in power is consistent with the predicted damping of primary anisotropies. At larger multipoles, ℓ = 2000-3500, the power is 3.1σ greater than standard models for intrinsic microwave background anisotropy in this multipole range, and 3.5σ greater than zero. This excess power is not consistent with expected levels of residual radio source contamination but, for σ 8 1, is consistent with predicted levels due to a secondary Sunyaev-Zeldovich anisotropy. Further observations are necessary to confirm the level of this excess and, if confirmed, determine its origin.

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“…A much larger S-Z data set is now available from the interferometric BIMA and OVRO observations, and since the redshift range of the clusters in the sample is substantial, the dependence on Ω is appreciable. A fit to 33 cluster distances gives H 0 = 60 km s CMB anisotropy induced by the S-Z effect (Sunyaev 1977, Rephaeli 1981) is the main source of secondary anisotropy on angular scales of few arcminutes. Because of this, and the great interest in this range of angular scales -multipoles (in the representation of the CMB temperature in terms of spherical harmonics) ℓ ≥ 1000 -the S-Z anisotropy has been studied extensively in the last few years.…”

Section: Main: Submitted To World Scientific On June 1 2018mentioning

confidence: 99%

“…CMB anisotropy induced by the S-Z effect (Sunyaev 1977, Rephaeli 1981) is the main source of secondary anisotropy on angular scales of few arcminutes. Because of this, and the great interest in this range of angular scales -multipoles (in the representation of the CMB temperature in terms of spherical harmonics) ℓ ≥ 1000 -the S-Z anisotropy has been studied extensively in the last few years.…”

Section: The Effect As a Cosmological Probementioning

confidence: 99%

The Sunyaev-Zeldovich Effect: Current Status and Future Prospects

Rephaeli¹

2002

The Ninth Marcel Grossmann Meeting

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The detailed spectral and spatial characteristics of the signature imprinted on the cosmic microwave background (CMB) radiation by Compton scattering of the radiation by electrons in the hot gas in clusters of galaxies -the Sunyaev-Zeldovich (S-Z) effect -are of great astrophysical and cosmological significance. In recent years observations of the effect have improved tremendously; high signal-to-noise images of the effect (at low microwave frequencies) can now be obtained by interferometric arrays. In the near future, high frequency measurements of the effect will be made with ground based and balloon-borne telescopes equipped with bolometeric arrays. Towards the end of the decade the PLANCK satellite will carry out an extensive S-Z survey over a wide frequency range. Along with the improved observational capabilities, the theoretical description of the effect, and its use as a precise cosmological probe, have been considerably advanced. In this review, I briefly discuss the nature and significance of the effect, its exact theoretical description, the current observational status, and prospects for the near future.

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Fluctuations in the cosmic blackbody radiation due to gas in galaxy clusters

Cited by 22 publications

References 0 publications

The Sunyaev–Zel'dovich effect

The Sunyaev–Zel'dovich effect

The Anisotropy of the Microwave Background tol= 3500: Deep Field Observations with the Cosmic Background Imager

The Sunyaev-Zeldovich Effect: Current Status and Future Prospects

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