Determining the Geometry and the Cosmological Parameters of the Universe through Sunyaev‐Zeldovich Effect Cluster Counts

Chiueh, Tzihong

doi:10.1086/319780

Cited by 20 publications

(19 citation statements)

References 27 publications

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“…In order to discriminate between the cosmological models one should consider not only the cluster population at low redshift (normalization), but also the cluster population at high redshift (evolution). A recent application of this idea can be found in Fan & Chiueh (2001) where the authors study the function r = N ( z <0.5)/ N ( z >1) as a function of the limiting flux. That work suggests that a limited knowledge of the redshift of the cluster would give a constraint on the cosmological parameters.…”

Section: Sze As a Probe Of The Cosmological Modelmentioning

confidence: 99%

The Sunyaev-Zel'dovich effect as a cosmological discriminator

Diego

Martínez-González

Sanz

et al. 2002

Monthly Notices of the Royal Astronomical Society

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We show how future measurements of the Sunyaev–Zel'dovich effect (SZE) can be used to constrain the cosmological parameters. We combine the SZ information expected from the Planck full‐sky survey, N(S), where no redshift information is included, with the N(z) obtained from an optically identified SZ‐selected survey covering less than 1 per cent of the sky. We demonstrate how with a small subsample (≈300 clusters) of the whole SZ catalogue observed optically it is possible to reduce the degeneracy among the cosmological parameters drastically. We have studied the requirements for performing the optical follow‐up and we show the feasibility of such a project. Finally, we have compared the cluster expectations for Planck with those expected for Newton–XMM during their lifetimes. It is shown that, owing to its larger sky coverage, Planck will detect a factor of ∼5 times more clusters than Newton–XMM and also provide a larger redshift coverage.

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Section: Sze As a Probe Of The Cosmological Modelmentioning

confidence: 99%

The Sunyaev-Zel'dovich effect as a cosmological discriminator

Diego

Martínez-González

Sanz

et al. 2002

Monthly Notices of the Royal Astronomical Society

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“…Its statistical contribution can be modelled and subtracted given the value of σ 8 (the rms linear mass fluctuations within a sphere of 8 h −1 Mpc) which determines the abundance of galaxy clusters (e.g. White, Efstathiou & Frenk 1993; Fan & Chiueh 2001; Mei & Bartlett 2004). Also, since the thermal SZ effect is frequency‐dependent, it can be subtracted in frequency space given sufficient spectral coverage.…”

Section: Introductionmentioning

confidence: 99%

Towards accurate modelling of the integrated Sachs-Wolfe effect: the non-linear contribution

Cai

Cole

Jenkins

et al. 2009

Monthly Notices of the Royal Astronomical Society

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In a universe with a cosmological constant, the large‐scale gravitational potential varies in time and this is, in principle, observable. Using an N‐body simulation of a Λ cold dark matter universe, we show that linear theory is not sufficiently accurate to predict the power spectrum of the time derivative, , needed to compute the imprint of large‐scale structure on the cosmic microwave background (CMB). The linear part of the power spectrum [the integrated Sachs–Wolfe effect (ISW)] drops quickly as the relative importance of ΩΛ diminishes at high redshift, while the non‐linear part [the Rees–Sciama effect (RS)] evolves more slowly with redshift. Therefore, the deviation of the total power spectrum from linear theory occurs at larger scales at higher redshifts. The deviation occurs at k∼ 0.1 h Mpc−1 at z= 0. The cross‐correlation power spectrum of the density δ with behaves differently from the power spectrum of . First, the deviation from linear theory occurs at smaller scales (k∼ 1 h Mpc−1 at z= 0). Secondly, the correlation becomes negative when the non‐linear effect dominates. For the cross‐correlation power spectrum of galaxy samples with the CMB, the non‐linear effect becomes significant at l∼ 500 and rapidly makes the cross‐power spectrum negative. For high‐redshift samples, the cross‐correlation is expected to be suppressed by 5–10 per cent on arcminute scales. The RS effect makes a negligible contribution to the large‐scale ISW cross‐correlation measurement. However, on arcminute scales it will contaminate the expected cross‐correlation signal induced by the Sunyaev–Zel'dovich effect.

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“…(15) (Fan & Chiueh 2001). We have calculated the limiting mass for Planck observations at a detection level of 3σ, where σ is the total uncertainty given in Table 1.…”

Section: The Limiting Massmentioning

confidence: 99%

Probing the cosmic microwave background temperature using the Sunyaev-Zeldovich effect

Horellou¹,

Nord²,

Johansson³

et al. 2005

A&A

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Abstract.We discuss the possibility of constraining the relation between redshift and temperature of the cosmic microwave background (CMB) using multifrequency Sunyaev-Zeldovich (SZ) observations. We have simulated a catalog of clusters of galaxies detected through their SZ signature assuming the sensitivities that will be achieved by the Planck satellite at 100, 143 and 353 GHz, taking into account the instrumental noise and the contamination from the Cosmic Infrared Background and from unresolved radiosources. We have parametrized the cosmological temperature-redshift law as T ∝ (1 + z)(1−a) . Using two sets of SZ flux density ratios (100/143 GHz, which is most sensitive to the parametrization of the T − z law, and 143/353 GHz, which is most sensitive to the peculiar velocities of the clusters) we show that it is possible to recover the T − z law assuming that the temperatures and redshifts of the clusters are known. From a simulated catalog of ∼1200 clusters, the parameter a can be recovered to an accuracy of 10 −2 . Sensitive SZ observations thus appear as a potentially useful tool to test the standard law. Most cosmological models predict a linear variation of the CMB temperature with redshift. The discovery of an alternative law would have profound implications on the cosmological model, implying creation of energy in a manner that would still maintain the black-body shape of the CMB spectrum at redshift zero.

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Determining the Geometry and the Cosmological Parameters of the Universe through Sunyaev‐Zeldovich Effect Cluster Counts

Cited by 20 publications

References 27 publications

The Sunyaev-Zel'dovich effect as a cosmological discriminator

The Sunyaev-Zel'dovich effect as a cosmological discriminator

Towards accurate modelling of the integrated Sachs-Wolfe effect: the non-linear contribution

Probing the cosmic microwave background temperature using the Sunyaev-Zeldovich effect

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